[ { "id": "https://authors.library.caltech.edu/records/ym7kp-0jw27", "eprint_id": 117987, "eprint_status": "archive", "datestamp": "2023-08-22 18:04:45", "lastmod": "2023-10-24 22:44:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kauffmann-Olivier-B", "name": { "family": "Kauffmann", "given": "O. B." }, "orcid": "0000-0001-5283-4662" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Weaver-John-R", "name": { "family": "Weaver", "given": "J. R." }, "orcid": "0000-0003-1614-196X" }, { "id": "McCracken-Henry-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Milvang-Jensen-Bo", "name": { "family": "Milvang-Jensen", "given": "B." }, "orcid": "0000-0002-2281-2785" }, { "id": "Brammer-Gabriel-B", "name": { "family": "Brammer", "given": "G." }, "orcid": "0000-0003-2680-005X" }, { "id": "Davidzon-Iary", "name": { "family": "Davidzon", "given": "I." }, "orcid": "0000-0002-2951-7519" }, { "id": "Le-F\u00e8vre-Olivier", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Liu-Daizhong", "name": { "family": "Liu", "given": "D." }, "orcid": "0000-0001-9773-7479" }, { "id": "Mobasher-Bahram", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Moneti-A", "name": { "family": "Moneti", "given": "A." } }, { "id": "Shuntov-Marko", "name": { "family": "Shuntov", "given": "M." }, "orcid": "0000-0002-7087-0701" }, { "id": "Toft-Sune", "name": { "family": "Toft", "given": "S." }, "orcid": "0000-0003-3631-7176" }, { "id": "Casey-Caitlin-M", "name": { "family": "Casey", "given": "C. M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Dunlop-James-S", "name": { "family": "Dunlop", "given": "J. S." } }, { "id": "Kartaltepe-Jeyhan-S", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Koekemoer-Anton-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Sanders-David-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Tresse-Laurence", "name": { "family": "Tresse", "given": "L." }, "orcid": "0000-0001-8776-0958" } ] }, "title": "COSMOS2020: UV-selected galaxies at z \u2265 7.5", "ispublished": "pub", "full_text_status": "public", "keywords": "Space and Planetary Science; Astronomy and Astrophysics", "note": "We are grateful to the referee for a careful reading of the manuscript and useful suggestions. This paper is dedicated to Olivier Le F\u00e8vre who initiated this work and devoted so much energy and passion to building the COSMOS survey. We warmly acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. The HST-COSMOS program was supported through NASA grant HST-GO-09822. More information on the COSMOS survey is available at https://cosmos.astro.caltech.edu. This research is also partly supported by the Centre National d'Etudes Spatiales (CNES). OI acknowledges the funding of the French Agence Nationale de la Recherche for the project \"SAGACE\". HJMcC acknowledges support from the PNCG. ID has received funding from the European Union's Horizon 2020 research and innovation program under the Marie Sk\u0142odowska-Curie grant agreement No. 896225. This work used the CANDIDE computer system at the IAP supported by grants from the PNC, DIM-ACAV and the CNES and maintained by S. Rouberol. BMJ is supported in part by Independent Research Fund Denmark grant DFF \u2013 7014-00017. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. ST, GB and JW acknowledge support from the European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt, grant No. 648179). CMC thanks the National Science Foundation for support through grants AST-1814034 and AST-2009577, and the Research Corporation for Science Advancement from a 2019 Cottrell Scholar Award sponsored by IF/THEN, an initiative of Lyda Hill Philanthropies. CMC thanks the National Science Foundation for support through grants AST-1814034 and AST-2009577, and the Research Corporation for Science Advancement from a 2019 Cottrell Scholar Award sponsored by IF/THEN, an initiative of Lyda Hill Philanthropies. The authors wish to recognise and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This work is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO program ID 179.A-2005 and on data products produced by CALET and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This work is based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.", "abstract": "This paper presents a new search for z\u2004\u2265\u20047.5 galaxies using the COSMOS2020 photometric catalogues. Finding galaxies at the reionisation epoch through deep imaging surveys remains observationally challenging. The larger area covered by ground-based surveys such as COSMOS enables the discovery of the brightest galaxies at these high redshifts. Covering 1.4 deg^2, our COSMOS catalogues were constructed from the latest UltraVISTA data release (DR4) combined with the final Spitzer/IRAC COSMOS images and the Hyper-Suprime-Cam Subaru Strategic Program DR2 release. We identified 17 new 7.5\u2004<\u2004z\u2004<\u200410 candidate sources, and confirm 15 previously published candidates. Using deblended photometry extracted by fitting surface brightness models on multi-band images, we selected four candidates which would be rejected using fixed aperture photometry. We tested the robustness of all our candidates by comparing six different photometric redshift estimates. Finally, we computed the galaxy UV luminosity function in three redshift bins centred at z\u2004=\u20048,\u20069,\u200610. We find no clear evolution of the number density of the brightest galaxies M_(UV)\u2004<\u2004\u221221.5, in agreement with previous works. Rapid changes in the quenching efficiency or attenuation by dust could explain such a lack of evolution between z\u2004\u223c\u20048 and z\u2004\u223c\u20049. A spectroscopic confirmation of the redshifts, already planned with JWST and the Keck telescopes, will be essential to confirm our results.", "date": "2022-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "667", "publisher": "EDP Sciences", "pagerange": "Art. No. A65", "id_number": "CaltechAUTHORS:20221122-564647900.12", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221122-564647900.12", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Agence Nationale de la Recherche (ANR)" }, { "agency": "Marie Curie Fellowship", "grant_number": "896225" }, { "agency": "Programme National de Cosmologie et Galaxies (PNCG)" }, { "agency": "Independent Research Fund Denmark", "grant_number": "7014-00017" }, { "agency": "Danish National Research Foundation", "grant_number": "140" }, { "agency": "European Research Council (ERC)", "grant_number": "648179" }, { "agency": "NSF", "grant_number": "AST-1814034" }, { "agency": "NSF", "grant_number": "AST-2009577" }, { "agency": "Cottrell Scholar of Research Corporation" }, { "agency": "Lyda Hill Philanthropies" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/202243088", "pub_year": "2022", "author_list": "Kauffmann, O. B.; Ilbert, O.; et el." }, { "id": "https://authors.library.caltech.edu/records/n20jh-a6m95", "eprint_id": 108097, "eprint_status": "archive", "datestamp": "2023-08-22 08:57:53", "lastmod": "2023-10-23 16:27:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hovis-Afflerbach-Beryl", "name": { "family": "Hovis-Afflerbach", "given": "Beryl" }, "orcid": "0000-0002-9967-2725" }, { "id": "Steinhardt-Charles-L", "name": { "family": "Steinhardt", "given": "Charles L." }, "orcid": "0000-0003-3780-6801" }, { "id": "Masters-Daniel-C", "name": { "family": "Masters", "given": "Daniel" }, "orcid": "0000-0001-5382-6138" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" } ] }, "title": "Identifying and Repairing Catastrophic Errors in Galaxy Properties Using Dimensionality Reduction", "ispublished": "pub", "full_text_status": "public", "keywords": "Astronomy data analysis; Redshift surveys; High-redshift galaxies; Photometry; Dimensionality reduction; Galaxy properties", "note": "\u00a9 2021 The American Astronomical Society. \n\nReceived 2020 November 9; revised 2020 December 10; accepted 2020 December 11; published 2021 February 19. \n\nThe authors would like to thank Gabe Brammer, Iary Davidzon, Christian Kragh Jespersen, and John Weaver for useful discussions. B.H. thanks Kathryn McEachern for her generous contribution to the SURF program and to this research in memory of David L. Glackin. C.S. is supported by ERC grant 648179 \"ConTExt\". The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. \n\nBased on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO program ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.\n\n
Published - Hovis-Afflerbach_2021_ApJ_908_148.pdf
Submitted - 2012.07855.pdf
", "abstract": "Our understanding of galaxy evolution is derived from large surveys designed to maximize efficiency by only observing the minimum amount needed to infer properties for a typical galaxy. However, for a few percent of galaxies in every survey, these observations are insufficient and derived properties can be catastrophically wrong. Further, it is currently difficult or impossible to determine which objects have failed, so that these contaminate every study of galaxy properties. We develop a novel method to identify these objects by combining the astronomical codes that infer galaxy properties with the dimensionality reduction algorithm t-SNE, which groups similar objects to determine which inferred properties are out of place. This method provides an improvement for the COSMOS catalog, which already uses existing techniques for catastrophic error removal, and therefore should improve the quality of large catalogs and any studies that are sensitive to large redshift errors.", "date": "2021-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "908", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 148", "id_number": "CaltechAUTHORS:20210217-151708469", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210217-151708469", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech Summer Undergraduate Research Fellowship (SURF)" }, { "agency": "European Research Council (ERC)", "grant_number": "648179" }, { "agency": "Danish National Research Foundation", "grant_number": "140" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "doi": "10.3847/1538-4357/abd329", "primary_object": { "basename": "2012.07855.pdf", "url": "https://authors.library.caltech.edu/records/n20jh-a6m95/files/2012.07855.pdf" }, "related_objects": [ { "basename": "Hovis-Afflerbach_2021_ApJ_908_148.pdf", "url": "https://authors.library.caltech.edu/records/n20jh-a6m95/files/Hovis-Afflerbach_2021_ApJ_908_148.pdf" } ], "pub_year": "2021", "author_list": "Hovis-Afflerbach, Beryl; Steinhardt, Charles L.; et el." }, { "id": "https://authors.library.caltech.edu/records/gq3z9-a7e35", "eprint_id": 103747, "eprint_status": "archive", "datestamp": "2023-08-22 05:20:35", "lastmod": "2023-10-20 16:40:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hemmati-S", "name": { "family": "Hemmati", "given": "Shoubaneh" }, "orcid": "0000-0003-2226-5395" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Nayyeri-H", "name": { "family": "Nayyeri", "given": "Hooshang" }, "orcid": "0000-0001-8242-9983" }, { "id": "Shahidi-Abtin", "name": { "family": "Shahidi", "given": "Abtin" }, "orcid": "0000-0001-6975-6293" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Darvish-B", "name": { "family": "Darvish", "given": "Behnam" }, "orcid": "0000-0003-4919-9017" }, { "id": "Chartab-Nima", "name": { "family": "Chartab", "given": "Nima" }, "orcid": "0000-0003-3691-937X" }, { "id": "Jafariyazani-M", "name": { "family": "Jafariyazani", "given": "Marzyeh" } }, { "id": "Sattari-Zahra", "name": { "family": "Sattari", "given": "Zahra" }, "orcid": "0000-0002-0364-1159" } ] }, "title": "Bridging between the integrated and resolved main sequence of star formation", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxies; Star formation; Galaxy quenching; Galaxy structure; Galaxy bulges; Dynamical evolution; Astrostatistics; Galaxy evolution", "note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2019 December 3; revised 2020 January 24; accepted 2020 February 3; published 2020 June 11. \n\nWe wish to thank the referee for providing very useful suggestions and recommendations. S.H. is thankful to A. Pagul for careful reading of this manuscript and for constructive comments. B.D. acknowledges financial support from the National Science Foundation, grant No. 1716907. Parts of this research were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.\n\nPublished - Hemmati_2020_ApJL_896_L17.pdf
Submitted - 2002.01011.pdf
", "abstract": "The position of galaxies on the stellar mass, star formation rate (SFR) plane with respect to the star-forming main sequence at each redshift is a convenient way to infer where the galaxy is in its evolution compared to the rest of the population. We use Hubble Space Telescope high-resolution images in the GOODS-S field from the the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS) and fit multiwavelength lights in resolution elements of galaxies with stellar population synthesis models. We then construct resolved kpc-scale stellar mass, SFR surface density curves for galaxies at z ~ 1. Fitting these resolved main sequence curves with Schechter functions, we parameterize and explain the multiwavelength structure of galaxies with three variables: \u03c6*, \u03b1, and M*. For quenched galaxies below the main sequence, we find an average high-mass slope (\u03b1) of the resolved main sequence curves to be ~\u22120.4. The scatter of this slope is higher among the lower mass star-forming galaxies and those above the main sequence compared to quenched galaxies, due to lack of an evolved bulge. Our findings agree well with an inside-out quenching of star formation. We find that the knee of the Schechter fits (M*) for galaxies below the main sequence occurs at lower stellar mass surface densities compared to star-forming galaxies, which hints at how far quenching has proceeded outward.", "date": "2020-06-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "896", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L17", "id_number": "CaltechAUTHORS:20200608-105510415", "issn": "2041-8213", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200608-105510415", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1716907" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/2041-8213/ab7243", "primary_object": { "basename": "2002.01011.pdf", "url": "https://authors.library.caltech.edu/records/gq3z9-a7e35/files/2002.01011.pdf" }, "related_objects": [ { "basename": "Hemmati_2020_ApJL_896_L17.pdf", "url": "https://authors.library.caltech.edu/records/gq3z9-a7e35/files/Hemmati_2020_ApJL_896_L17.pdf" } ], "pub_year": "2020", "author_list": "Hemmati, Shoubaneh; Mobasher, Bahram; et el." }, { "id": "https://authors.library.caltech.edu/records/pcae0-qwy21", "eprint_id": 99308, "eprint_status": "archive", "datestamp": "2023-08-19 18:05:59", "lastmod": "2023-10-18 18:13:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Liu-Daizhong", "name": { "family": "Liu", "given": "Daizhong" }, "orcid": "0000-0001-9773-7479" }, { "id": "Lang-Philipp", "name": { "family": "Lang", "given": "P." }, "orcid": "0000-0002-5681-3575" }, { "id": "Magnelli-B", "name": { "family": "Magnelli", "given": "B." }, "orcid": "0000-0002-6777-6490" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Leslie-S", "name": { "family": "Leslie", "given": "S." } }, { "id": "Fudamoto-Y", "name": { "family": "Fudamoto", "given": "Y." } }, { "id": "Bondi-M", "name": { "family": "Bondi", "given": "M." } }, { "id": "Groves-B-A", "name": { "family": "Groves", "given": "B." }, "orcid": "0000-0002-9768-0246" }, { "id": "Jim\u00e9nez-Andrade-E-F", "name": { "family": "Jim\u00e9nez-Andrade", "given": "E." }, "orcid": "0000-0002-2640-5917" }, { "id": "Harrington-K", "name": { "family": "Harrington", "given": "K." } }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P. A." }, "orcid": "0000-0001-5851-6649" }, { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M." }, "orcid": "0000-0003-1033-9684" }, { "id": "Vardoulaki-E", "name": { "family": "Vardoulaki", "given": "E." }, "orcid": "0000-0002-4437-1773" }, { "id": "B\u01cedescu-T", "name": { "family": "B\u01cedescu", "given": "T." } }, { "id": "Moser-L", "name": { "family": "Moser", "given": "L." } }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Battisti-A-J", "name": { "family": "Battisti", "given": "A." }, "orcid": "0000-0003-4569-2285" }, { "id": "da-Cunha-E", "name": { "family": "da Cunha", "given": "E." }, "orcid": "0000-0001-9759-4797" }, { "id": "Zavala-J", "name": { "family": "Zavala", "given": "J." }, "orcid": "0000-0002-7051-1100" }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" }, { "id": "Davidzon-I", "name": { "family": "Davidzon", "given": "I." }, "orcid": "0000-0002-2951-7519" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" } ] }, "title": "Automated Mining of the ALMA Archive in the COSMOS Field (A\u00b3COSMOS). I. Robust ALMA Continuum Photometry Catalogs and Stellar Mass and Star Formation Properties for \u223c700 Galaxies at z = 0.5\u20136", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: ISM \u2013 galaxies: photometry \u2013 galaxies: star formation \u2013 submillimeter: galaxies \u2013 techniques: photometric", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 February 21; revised 2019 July 25; accepted 2019 August 5; published 2019 October 16. \n\nD.L., P.L., and E.S. acknowledge support and funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 694343). S.L. acknowledges funding from Deutsche Forschungsgemeinschaft (DFG) grant SCH 536/9-1. B.G. acknowledges the support of the Australian Research Council as the recipient of a Future Fellowship (FT140101202). Part of this research was carried out within the Collaborative Research Centre 956, subproject A1, funded by the Deutsche Forschungsgemeinschaft (DFG)\u2014project ID 184018867. We thank Annalisa Pillepich and the Max Planck Computing & Data Facility for very helpful computing cluster resources. \n\nThis paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00064.S, ADS/JAO.ALMA#2011.0.00097.S, ADS/JAO.ALMA#2011.0.00539.S, ADS/JAO.ALMA#2011.0.00742.S, ADS/JAO.ALMA#2012.1.00076.S, ADS/JAO.ALMA#2012.1.00323.S, ADS/JAO.ALMA#2012.1.00523.S, ADS/JAO.ALMA#2012.1.00536.S, ADS/JAO.ALMA#2012.1.00919.S, ADS/JAO.ALMA#2012.1.00952.S, ADS/JAO.ALMA#2012.1.00978.S, ADS/JAO.ALMA#2013.1.00034.S, ADS/JAO.ALMA#2013.1.00092.S, ADS/JAO.ALMA#2013.1.00118.S, ADS/JAO.ALMA#2013.1.00151.S, ADS/JAO.ALMA#2013.1.00171.S, ADS/JAO.ALMA#2013.1.00208.S, ADS/JAO.ALMA#2013.1.00276.S, ADS/JAO.ALMA#2013.1.00668.S, ADS/JAO.ALMA#2013.1.00815.S, ADS/JAO.ALMA#2013.1.00884.S, ADS/JAO.ALMA#2013.1.00914.S, ADS/JAO.ALMA#2013.1.01258.S, ADS/JAO.ALMA#2013.1.01292.S, ADS/JAO.ALMA#2015.1.00026.S, ADS/JAO.ALMA#2015.1.00055.S, ADS/JAO.ALMA#2015.1.00122.S, ADS/JAO.ALMA#2015.1.00137.S, ADS/JAO.ALMA#2015.1.00260.S, ADS/JAO.ALMA#2015.1.00299.S, ADS/JAO.ALMA#2015.1.00379.S, ADS/JAO.ALMA#2015.1.00388.S, ADS/JAO.ALMA#2015.1.00540.S, ADS/JAO.ALMA#2015.1.00568.S, ADS/JAO.ALMA#2015.1.00664.S, ADS/JAO.ALMA#2015.1.00704.S, ADS/JAO.ALMA#2015.1.00853.S, ADS/JAO.ALMA#2015.1.00861.S, ADS/JAO.ALMA#2015.1.00862.S, ADS/JAO.ALMA#2015.1.00928.S, ADS/JAO.ALMA#2015.1.01074.S, ADS/JAO.ALMA#2015.1.01105.S, ADS/JAO.ALMA#2015.1.01111.S, ADS/JAO.ALMA#2015.1.01171.S, ADS/JAO.ALMA#2015.1.01212.S, ADS/JAO.ALMA#2015.1.01495.S, ADS/JAO.ALMA#2015.1.01590.S, ADS/JAO.ALMA#2015.A.00026.S, ADS/JAO.ALMA#2016.1.00478.S, ADS/JAO.ALMA#2016.1.00624.S, ADS/JAO.ALMA#2016.1.00735.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. \n\nFacility: ALMA. -\n\nPublished - Liu_2019_ApJS_244_40.pdf
", "abstract": "The rich information on (sub)millimeter dust continuum emission from distant galaxies in the public Atacama Large Millimeter/submillimeter Array (ALMA) archive is contained in thousands of inhomogeneous observations from individual PI-led programs. To increase the usability of these data for studies deepening our understanding of galaxy evolution, we have developed automated mining pipelines for the ALMA archive in the COSMOS field (A\u00b3COSMOS) that efficiently exploit the available information for large numbers of galaxies across cosmic time and keep the data products in sync with the increasing public ALMA archive: (a) a dedicated ALMA continuum imaging pipeline, (b) two complementary photometry pipelines for both blind source extraction and prior source fitting, (c) a counterpart association pipeline utilizing the multiwavelength data available (including quality assessment based on machine-learning techniques), (d) an assessment of potential (sub)millimeter line contribution to the measured ALMA continuum, and (e) extensive simulations to provide statistical corrections to biases and uncertainties in the ALMA continuum measurements. Application of these tools yields photometry catalogs with ~1000 (sub)millimeter detections (spurious fraction ~8%\u201312%) from over 1500 individual ALMA continuum images. Combined with ancillary photometric and redshift catalogs and the above quality assessments, we provide robust information on redshift, stellar mass, and star formation rate for ~700 galaxies at redshifts 0.5\u20136 in the COSMOS field (with undetermined selection function). The ALMA photometric measurements and galaxy properties are released publicly within our blind extraction, prior fitting, and galaxy property catalogs, plus the images. These products will be updated on a regular basis in the future.", "date": "2019-10", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "244", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 40", "id_number": "CaltechAUTHORS:20191016-144502817", "issn": "1538-4365", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191016-144502817", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "694343" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "SCH 536/9-1" }, { "agency": "Australian Research Council", "grant_number": "FT140101202" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "184018867" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "doi": "10.3847/1538-4365/ab42da", "primary_object": { "basename": "Liu_2019_ApJS_244_40.pdf", "url": "https://authors.library.caltech.edu/records/pcae0-qwy21/files/Liu_2019_ApJS_244_40.pdf" }, "pub_year": "2019", "author_list": "Liu, Daizhong; Lang, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/ms1xj-cvx33", "eprint_id": 98132, "eprint_status": "archive", "datestamp": "2023-08-19 17:24:21", "lastmod": "2023-10-18 17:04:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cooke-K-C", "name": { "family": "Cooke", "given": "Kevin C." }, "orcid": "0000-0002-2200-9845" }, { "id": "Kartaltepe-J-S", "name": { "family": "Kartaltepe", "given": "Jeyhan S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Tyler-K-D", "name": { "family": "Tyler", "given": "K. D." } }, { "id": "Darvish-B", "name": { "family": "Darvish", "given": "Behnam" }, "orcid": "0000-0003-4919-9017" }, { "id": "Casey-C-M", "name": { "family": "Casey", "given": "Caitlin M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "Olivier" }, "orcid": "0000-0001-5891-2596" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas" }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Stellar Mass Growth of Brightest Cluster Galaxy Progenitors in COSMOS Since z \u223c 3", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: abundances \u2013 galaxies: clusters: general \u2013 galaxies: elliptical and lenticular, cD \u2013 galaxies: star formation \u2013 galaxies: structure", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 May 8; revised 2019 June 29; accepted 2019 July 8; published 2019 August 22. \n\nWe thank the referee for the constructive feedback that improved the clarity of this work. Support for this work was provided by NASA through grants HST-GO-13657.010-A and HST-AR-14298.004-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Support and observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., were also provided by NASA through grant NNX16AB36G as part of the Astrophysics Data Analysis Program. Spectral energy distribution fitting was performed using the scientific computing resources of the Rochester Institute of Technology ION cluster. B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant No. NNX12AE20G, and the National Science Foundation, grant No. 1716907. We thank Paul Torrey for his council on evolving number density methodology. We thank the generous advice of Elisabete da Cunha and Stefano Berta on the use of MAGPHYS and SED3FIT, respectively. This research made use of Astropy,7 a community-developed core Python package for Astronomy (Robitaille et al. 2013; Price-Whelan et al. 2018). This research made use of the iPython environment (Perez & Granger 2007) and the Python packages SciPy (Jones et al. 2001), NumPy (van der Walt et al. 2011), and Matplotlib (Hunter 2007). \n\nBased on observations made with the NASA Galaxy Evolution Explorer. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada\u2013France\u2013Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. Based (in part) on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. Based on observations obtained with WIRCam, a joint project of CFHT, Taiwan, Korea, Canada, and France. This work is based (in part) on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. \n\nThis work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\n\nPublished - Cooke_2019_ApJ_881_150.pdf
Accepted Version - 1907.04337.pdf
", "abstract": "We examine the role of environment on the in situ star formation (SF) hosted by the progenitors of the most massive galaxies in the present-day universe, the brightest cluster galaxies (BCGs), from z ~ 3 to present in the COSMOS field. Progenitors are selected from the COSMOS field using a stellar mass cut motivated by the evolving cumulative comoving number density of progenitors within the Illustris simulation, as well as the Millennium-II simulation and a constant comoving number density method for comparison. We characterize each progenitor using far-ultraviolet\u2013far-infrared observations taken from the COSMOS field and fitting stellar, dust, and active galactic nucleus components to their spectral energy distributions. Additionally, we compare the SF rates of our progenitor sample to the local density maps of the COSMOS field to identify the effects of environment. We find that BCG progenitors evolve in three stages, starting with an in situ SF-dominated phase (z > 2.25). This is followed by a phase until z ~ 1.25 where mass growth is driven by in situ SF and stellar mass deposited by mergers (both gas rich and poor) on the same order of magnitude independent of local environment. Finally, at low redshift dry mergers are the dominant stellar mass generation process. We also identify this final transition period as the time when progenitors quench, exhibiting quiescent NUVrJ colors.", "date": "2019-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "881", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 150", "id_number": "CaltechAUTHORS:20190822-151337974", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190822-151337974", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-13657.010-A" }, { "agency": "NASA", "grant_number": "HST-AR-14298.004-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NASA", "grant_number": "NNX16AB36G" }, { "agency": "NASA", "grant_number": "NNX12AE20G" }, { "agency": "NSF", "grant_number": "AST-1716907" }, { "agency": "NASA", "grant_number": "NAS5-98034" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ab30c9", "primary_object": { "basename": "1907.04337.pdf", "url": "https://authors.library.caltech.edu/records/ms1xj-cvx33/files/1907.04337.pdf" }, "related_objects": [ { "basename": "Cooke_2019_ApJ_881_150.pdf", "url": "https://authors.library.caltech.edu/records/ms1xj-cvx33/files/Cooke_2019_ApJ_881_150.pdf" } ], "pub_year": "2019", "author_list": "Cooke, Kevin C.; Kartaltepe, Jeyhan S.; et el." }, { "id": "https://authors.library.caltech.edu/records/5ebeq-f3n62", "eprint_id": 89369, "eprint_status": "archive", "datestamp": "2023-08-19 15:58:57", "lastmod": "2023-10-18 22:42:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kusakabe-Haruka", "name": { "family": "Kusakabe", "given": "Haruka" } }, { "id": "Shimasaku-Kazuhiro", "name": { "family": "Shimasaku", "given": "Kazuhiro" } }, { "id": "Momose-Rieko", "name": { "family": "Momose", "given": "Rieko" } }, { "id": "Ouchi-Masami", "name": { "family": "Ouchi", "given": "Masami" }, "orcid": "0000-0002-1049-6658" }, { "id": "Nakajima-Kimihiko", "name": { "family": "Nakajima", "given": "Kimihiko" } }, { "id": "Hashimoto-Takuya", "name": { "family": "Hashimoto", "given": "Takuya" } }, { "id": "Harikane-Yuichi", "name": { "family": "Harikane", "given": "Yuichi" }, "orcid": "0000-0002-6047-430X" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "John D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "The dominant origin of diffuse Ly\u03b1 halos around Ly\u03b1 emitters explored by spectral energy distribution fitting and clustering analysis", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: halos galaxies: star formation (galaxies:) intergalactic medium galaxies: high-redshift", "note": "\u00a9 The Author(s) 2019. Published by Oxford University Press on behalf of the Astronomical Society of Japan. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nReceived: 28 March 2018; Accepted: 21 February 2019; Published: 16 May 2019. \n\nWe thank the anonymous referee for constructive comments and suggestions. We are grateful to Kazuyuki Ogura and Masahiro Nagashima for kindly providing \u03bd2GC data and giving helpful comments. We are grateful to Yoshiaki Ono for giving insightful comments and suggestions on SED fitting. We would like to express our gratitude to Jorryt Matthee and Ken-ichi Tadaki for kindly providing their data, plotted in figure 4, and figures 6\u20138 and 6, respectively. We thank David Sobral for giving insightful comments and suggestions. We acknowledge Ryosuke Goto, Akira Konno, Ryota Kawamata, Taku Okamura, Kazushi Irikura, Ryota Kakuma, and Makoto Ando for constructive discussions at meetings. \n\nThis work is based on observations taken by the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. Based on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This research made use of IRAF, which is distributed by NOAO, which is operated by AURA under a cooperative agreement with the National Science Foundation, and of Python packages for astronomy: Astropy (Astropy Collaboration 2013), Colossus, CosmoloPy, and PyRAF, which is produced by the Space Telescope Science Institute, which is operated by AURA for NASA. H.K. acknowledges support from the JSPS through the JSPS Research Fellowship for Young Scientists. This work is supported in part by KAKENHI (16K05286) Grant-in-Aid for Scientific Research (C) through the JSPS.\n\nSubmitted - 1803.10265.pdf
", "abstract": "The physical origin of diffuse Ly\u03b1 halos (LAHs) around star-forming galaxies is still a matter of debate. We present the dependence of LAH luminosity [L(Ly\u03b1)_H] on the stellar mass (M\u22c6), star formation rate, color excess [E(B \u2212 V)\u22c6], and dark matter halo mass (M_h) of the parent galaxy for \u223c900 Ly\u03b1 emitters (LAEs) at z \u223c 2 divided into ten subsamples. We calculate L(Ly\u03b1)_H using the stacked observational relation between L(Ly\u03b1)H and central Ly\u03b1 luminosity of Momose et al. (2016, MNRAS, 457, 2318), which we find agrees with the average trend of VLT/MUSE-detected individual LAEs. We find that our LAEs have relatively high L(Ly\u03b1)_H despite low M\u22c6 and M_h, and that L(Ly\u03b1)_H remains almost unchanged with M\u22c6 and perhaps with M_h. These results are incompatible with the cold stream (cooling radiation) scenario and the satellite-galaxy star-formation scenario, because the former predicts fainter L(Ly\u03b1)_H and both predict steeper L(Ly\u03b1)_H vs. M\u22c6 slopes. We argue that LAHs are mainly caused by Ly\u03b1 photons escaping from the main body and then scattering in the circum-galactic medium. This argument is supported by LAH observations of H\u03b1 emitters (HAEs). When LAHs are taken into account, the Ly\u03b1 escape fractions of our LAEs are about ten times higher than those of HAEs with similar M\u22c6 or E(B \u2212 V)\u22c6, which may partly arise from lower H\u2009I gas masses implied from lower M_h at fixed M\u22c6, or from another Ly\u03b1 source in the central part.", "date": "2019-06", "date_type": "published", "publication": "Publications of the Astronomical Society of Japan", "volume": "71", "number": "3", "publisher": "Astronomical Society of Japan", "pagerange": "Art. No. 55", "id_number": "CaltechAUTHORS:20180904-155810395", "issn": "0004-6264", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180904-155810395", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "16K05286" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/pasj/psz029", "primary_object": { "basename": "1803.10265.pdf", "url": "https://authors.library.caltech.edu/records/5ebeq-f3n62/files/1803.10265.pdf" }, "pub_year": "2019", "author_list": "Kusakabe, Haruka; Shimasaku, Kazuhiro; et el." }, { "id": "https://authors.library.caltech.edu/records/dpb9v-0yr57", "eprint_id": 94025, "eprint_status": "archive", "datestamp": "2023-08-19 14:59:18", "lastmod": "2023-10-20 17:36:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Betti-S-K", "name": { "family": "Betti", "given": "S. K." }, "orcid": "0000-0002-8667-6428" }, { "id": "Pope-Alexandra", "name": { "family": "Pope", "given": "Alexandra" }, "orcid": "0000-0001-8592-2706" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "Min S." }, "orcid": "0000-0001-7095-7543" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" } ] }, "title": "Environmental Effect on the Interstellar Medium in Galaxies across the Cosmic Web at z = 0.73", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: ISM \u2013 submillimeter: galaxies", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2018 September 14; revised 2019 February 13; accepted 2019 February 15; published 2019 March 21. \n\nThe authors thank the anonymous referee for the suggestions and comments that have significantly improved this manuscript. S.K.B. and A.P. acknowledge support from NASA ADAP 13-0054. S.K.B. is thankful for the North American ALMA Science Center support staff, especially Erica Keller, for all their help with data reduction. This paper makes use of the following ALMA data: ADS/JAO.ALMA #2015.1.00055.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. \n\nFacilities: ALMA - Atacama Large Millimeter Array, HST - , Herschel - , Spitzer - . \n\nSoftware: astropy (Astropy Collaboration et al. 2013), CASA (McMullin et al. 2007).\n\nPublished - Betti_2019_ApJ_874_53.pdf
Accepted Version - 1902.08216.pdf
", "abstract": "We present new Atacama Large Millimeter Array (ALMA) dust continuum observations of 101 log(M*/M\u2299) > 9.5 galaxies in the COSMOS field to study the effect of the environment on the interstellar medium at z ~ 0.7. At this redshift, our targets span a wide range of environments allowing for a diverse sample of galaxies with densities of \u03a3 = 0.16\u201310.5 Mpc^(\u22122) (per \u0394z = 0.024). Using the ALMA observations, we calculate the total interstellar medium (ISM) mass (M_(ISM)) and look for depletion as a function of galaxy density in order to understand the quenching or triggering of star formation in galaxies in different environments. M_(ISM) is found to have a small dependence on the environment, while the depletion timescale remains constant (~200 Myr) across all environments. We find elevated M_(ISM) values at intermediate densities and lower values at high densities compared to low (field) densities. Our observed evolution in gas fraction with density in this single redshift slice is equivalent to the observed evolution with cosmic time over 2\u20133 Gyr. To explain the change in the gas mass fraction seen in galaxies in intermediate and high densities, these results suggest environmental processes such as mergers and ram pressure stripping are likely playing a role in dense filamentary cluster environments.", "date": "2019-03-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "874", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 53", "id_number": "CaltechAUTHORS:20190321-132522003", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190321-132522003", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "ADAP 13-0054" }, { "agency": "Associated Universities, Inc." } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ab07b3", "primary_object": { "basename": "1902.08216.pdf", "url": "https://authors.library.caltech.edu/records/dpb9v-0yr57/files/1902.08216.pdf" }, "related_objects": [ { "basename": "Betti_2019_ApJ_874_53.pdf", "url": "https://authors.library.caltech.edu/records/dpb9v-0yr57/files/Betti_2019_ApJ_874_53.pdf" } ], "pub_year": "2019", "author_list": "Betti, S. K.; Pope, Alexandra; et el." }, { "id": "https://authors.library.caltech.edu/records/3xmse-pej65", "eprint_id": 94289, "eprint_status": "archive", "datestamp": "2023-08-19 14:33:44", "lastmod": "2023-10-20 17:50:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gozaliasl-G", "name": { "family": "Gozaliasl", "given": "Ghassem" }, "orcid": "0000-0002-0236-919X" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Chandra centres for COSMOS X-ray galaxy groups: differences in stellar properties between central dominant and offset brightest group galaxies", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2018 November 16. Received 2018 November 15; in original form 2018 April 4. Published: 27 November 2018. \n\nThis work has been supported by grants from the Finnish Academy of Science to the University of Helsinki and the Euclid project, decision numbers 266918 and 1295113. GG wishes to thank Mr. Donald Smart for very useful comments. ST acknowledges support from the ERC Consolidator Grant funding scheme (project Context, grant no. 648179). The Cosmic Dawn Center is funded by the Danish National Research Foundation. We used data of the Millennium simulation from the web application providing online access, constructed as activities of the German Astrophysics Virtual Observatory.\n\nPublished - sty3203.pdf
Accepted Version - 1812.01604.pdf
Supplemental Material - sty3203_supplemental_file.txt
", "abstract": "We present the results of a search for galaxy clusters and groups in the \u223c2 deg^2 of the COSMOS field using all available X-ray observations from the XMM\u2013Newton and Chandra observatories. We reach an X-ray flux limit of 3\u00d710^(\u221216) erg cm^(\u22122)s^(\u22121) in the 0.5\u20132 keV range, and identify 247 X-ray groups with M_(200c) = 8\u00d710^(12) -3\u00d710^(14)M\u2299 at a redshift range of 0.08 \u2264 z < 1.53, using the multiband photometric redshift and the master spectroscopic redshift catalogues of the COSMOS. The X-ray centres of groups are determined using high-resolution Chandra imaging. We investigate the relations between the offset of the brightest group galaxies (BGGs) from halo X-ray centre and group properties and compare with predictions from semi-analytic models and hydrodynamical simulations. We find that BGG offset decreases with both increasing halo mass and decreasing redshift with no strong dependence on the X-ray flux and SNR. We show that the BGG offset decreases as a function of increasing magnitude gap with no considerable redshift-dependent trend. The stellar mass of BGGs in observations extends over a wider dynamic range compared to model predictions. At z < 0.5, the central dominant BGGs become more massive than those with large offsets by up to 0.3\u2009dex, in agreement with model prediction. The observed and predicted log-normal scatter in the stellar mass of both low- and large-offset BGGs at fixed halo mass is \u223c0.3\u2009dex.", "date": "2019-03", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "483", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "3545-3565", "id_number": "CaltechAUTHORS:20190329-084716225", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190329-084716225", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Academy of Finland", "grant_number": "266918" }, { "agency": "Academy of Finland", "grant_number": "1295113" }, { "agency": "European Research Council (ERC)", "grant_number": "648179" }, { "agency": "Danish National Research Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/sty3203", "primary_object": { "basename": "1812.01604.pdf", "url": "https://authors.library.caltech.edu/records/3xmse-pej65/files/1812.01604.pdf" }, "related_objects": [ { "basename": "sty3203.pdf", "url": "https://authors.library.caltech.edu/records/3xmse-pej65/files/sty3203.pdf" }, { "basename": "sty3203_supplemental_file.txt", "url": "https://authors.library.caltech.edu/records/3xmse-pej65/files/sty3203_supplemental_file.txt" } ], "pub_year": "2019", "author_list": "Gozaliasl, Ghassem; Capak, Peter; et el." }, { "id": "https://authors.library.caltech.edu/records/gp27p-j6r32", "eprint_id": 89367, "eprint_status": "archive", "datestamp": "2023-08-19 14:16:10", "lastmod": "2023-10-18 22:42:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "Dominik A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Pavesi-R", "name": { "family": "Pavesi", "given": "Riccardo" }, "orcid": "0000-0002-2263-646X" }, { "id": "Sharon-C-E", "name": { "family": "Sharon", "given": "Chelsea E." }, "orcid": "0000-0002-6250-5608" }, { "id": "Hodge-J-A", "name": { "family": "Hodge", "given": "Jacqueline A." }, "orcid": "0000-0001-6586-8845" }, { "id": "Decarli-R", "name": { "family": "Decarli", "given": "Roberto" }, "orcid": "0000-0002-2662-8803" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "Fabian" }, "orcid": "0000-0003-4793-7880" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "Christopher L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Aravena-M", "name": { "family": "Aravena", "given": "Manuel" }, "orcid": "0000-0002-6290-3198" }, { "id": "da-Cunha-E", "name": { "family": "da Cunha", "given": "Elisabete" }, "orcid": "0000-0001-9759-4797" }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "Emanuele" }, "orcid": "0000-0002-3331-9590" }, { "id": "Dickinson-Mark-E", "name": { "family": "Dickinson", "given": "Mark" }, "orcid": "0000-0001-5414-5131" }, { "id": "Smail-Ian-R", "name": { "family": "Smail", "given": "Ian" }, "orcid": "0000-0003-3037-257X" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "Rob J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Sargent-M", "name": { "family": "Sargent", "given": "Mark" }, "orcid": "0000-0003-1033-9684" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Wagg-Jeff", "name": { "family": "Wagg", "given": "Jeff" } } ] }, "title": "COLDz: Shape of the CO Luminosity Function at High Redshift and the Cold Gas History of the Universe", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 galaxies: active \u2013 galaxies: formation \u2013 galaxies: high-redshift \u2013 galaxies: starburst \u2013 radio lines: galaxies", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2018 August 10; revised 2018 November 27; accepted 2019 January 4; published 2019 February 6. \n\nThe authors thank Am\u00e9lie Saintonge for sharing her updated Schechter fits to the local CO luminosity function prior to publication, Rychard Bouwens for sharing the data necessary to create Figure 5, and Gerg\u00f6 Popping for helpful input on the comparison of our results to models, and for providing some new and updated model results. We also thank the anonymous referee for a helpful report. D.R. and R.P. acknowledge support from the National Science Foundation under grant number AST-1614213 to Cornell University. J.A.H. acknowledges support of the VIDI research program with project number 639.042.611, which is (partly) financed by the Netherlands Organisation for Scientific Research (NWO). I.R.S. acknowledges support from the ERC Advanced Grant DUSTYGAL (321334), STFC (ST/P000541/1), and a Royal Society/Wolfson Merit Award. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. \n\nFacility: VLA. -\n\nPublished - Riechers_2019_ApJ_872_7.pdf
Accepted Version - 1808.04371.pdf
", "abstract": "We report the first detailed measurement of the shape of the CO luminosity function at high redshift, based on >320 hr of the NSF's Karl G. Jansky Very Large Array (VLA) observations over an area of ~60 arcmin^2 taken as part of the CO Luminosity Density at High Redshift (COLDz) survey. COLDz \"blindly\" selects galaxies based on their cold gas content through CO(J = 1 \u2192 0) emission at z ~ 2\u20133 and CO(J = 2 \u2192 1) at z ~ 5\u20137 down to a CO luminosity limit of log(L'_(CO)/K km s^(\u22121) pc^2) \u2243 9.5. We find that the characteristic luminosity and bright end of the CO luminosity function are substantially higher than predicted by semi-analytical models, but consistent with empirical estimates based on the infrared luminosity function at z ~ 2. We also present the currently most reliable measurement of the cosmic density of cold gas in galaxies at early epochs, i.e., the cold gas history of the universe, as determined over a large cosmic volume of ~375,000 Mpc3. Our measurements are in agreement with an increase of the cold gas density from z ~ 0 to z ~ 2\u20133, followed by a possible decline toward z ~ 5\u20137. These findings are consistent with recent surveys based on higher-J CO line measurements, upon which COLDz improves in terms of statistical uncertainties by probing ~50\u2013100 times larger areas and in the reliability of total gas mass estimates by probing the low-J CO lines accessible to the VLA. Our results thus appear to suggest that the cosmic star formation rate density follows an increased cold molecular gas content in galaxies toward its peak about 10 billion years ago, and that its decline toward the earliest epochs is likely related to a lower overall amount of cold molecular gas (as traced by CO) bound in galaxies toward the first billion years after the Big Bang.", "date": "2019-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "872", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 7", "id_number": "CaltechAUTHORS:20180904-152724469", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180904-152724469", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1614213" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "639.042.611" }, { "agency": "European Research Council (ERC)", "grant_number": "321334" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/P000541/1" }, { "agency": "Royal Society" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aafc27", "primary_object": { "basename": "1808.04371.pdf", "url": "https://authors.library.caltech.edu/records/gp27p-j6r32/files/1808.04371.pdf" }, "related_objects": [ { "basename": "Riechers_2019_ApJ_872_7.pdf", "url": "https://authors.library.caltech.edu/records/gp27p-j6r32/files/Riechers_2019_ApJ_872_7.pdf" } ], "pub_year": "2019", "author_list": "Riechers, Dominik A.; Pavesi, Riccardo; et el." }, { "id": "https://authors.library.caltech.edu/records/nrs4v-z2v88", "eprint_id": 89325, "eprint_status": "archive", "datestamp": "2023-08-21 23:58:01", "lastmod": "2023-10-18 22:40:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jin-Shuowen", "name": { "family": "Jin", "given": "Shuowen" }, "orcid": "0000-0002-8412-7951" }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "Emanuele" }, "orcid": "0000-0002-3331-9590" }, { "id": "Liu-Daizhong", "name": { "family": "Liu", "given": "Daizhong" }, "orcid": "0000-0001-9773-7479" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "Vernesa" }, "orcid": "0000-0002-3893-8614" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Calabr\u00f2-A", "name": { "family": "Calabr\u00f2", "given": "Antonello" }, "orcid": "0000-0003-2536-1614" }, { "id": "Gu-Qiusheng", "name": { "family": "Gu", "given": "Qiusheng" }, "orcid": "0000-0002-3890-3729" }, { "id": "Delhaize-J", "name": { "family": "Delhaize", "given": "Jacinta" }, "orcid": "0000-0002-6149-0846" }, { "id": "Delvecchio-I", "name": { "family": "Delvecchio", "given": "Ivan" }, "orcid": "0000-0001-8706-2252" }, { "id": "Gao-Yu", "name": { "family": "Gao", "given": "Yu" }, "orcid": "0000-0003-0007-2197" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Puglisi-A", "name": { "family": "Puglisi", "given": "Annagrazia" }, "orcid": "0000-0001-9369-1805" }, { "id": "Dickinson-Mark-E", "name": { "family": "Dickinson", "given": "Mark" }, "orcid": "0000-0001-5414-5131" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "Frank" }, "orcid": "0000-0002-1707-1775" }, { "id": "Sargent-M", "name": { "family": "Sargent", "given": "Mark" }, "orcid": "0000-0003-1033-9684" }, { "id": "Novak-Mladen", "name": { "family": "Novak", "given": "Mladen" }, "orcid": "0000-0001-8695-825X" }, { "id": "Magdis-G-E", "name": { "family": "Magdis", "given": "Georgios" }, "orcid": "0000-0002-4872-2294" }, { "id": "Aretxaga-I", "name": { "family": "Aretxaga", "given": "Itziar" }, "orcid": "0000-0002-6590-3994" }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "Grant W." }, "orcid": "0000-0003-2705-9152" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" } ] }, "title": "\"Super-deblended\" Dust Emission in Galaxies. II. Far-IR to (Sub)millimeter Photometry and High-redshift Galaxy Candidates in the Full COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM; galaxies: photometry; galaxies: star formation; infrared: galaxies; techniques: photometric", "note": "\u00a9 2018. The American Astronomical Society. \n\nReceived 2018 February 6; revised 2018 July 3; accepted 2018 July 9; published 2018 August 30. \n\nWe are grateful to the full COSMOS team for their contributions in the buildup of such a rich multiwavelength data set. We thank the referee for useful comments and suggestions that helped improve the paper. We thank B. Magnelli, P. Lang, and the rest of the A^3COSMOS team for providing the ALMA photometry for comparison. SJ acknowledges funding from the China Scholarship Council. SJ and QG acknowledge support from the National Key Research and Development Program of China (No. 2017YFA0402703) and the National Natural Science Foundation of China (No. 11733002). D.L. and Y.G. acknowledge support from the National Key Research and Development Program (No. 2017YFA0402704) and the National Natural Science Foundation of China (No. 11420101002). V.S., J.D., and I.D. acknowledge support from the European Union's Seventh Framework program under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). ES and DL acknowledge funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 694343). The National Radio Astronomy Observatory is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc. ALMA is a partnership of the ESO (representing its member states), NSF (USA), and NINS (Japan), together with the NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by the ESO, AUI/NRAO, and NAOJ.\n\nPublished - Jin_2018_ApJ_864_56.pdf
Accepted Version - 1807.04697
", "abstract": "We present a \"super-deblended\" far-infrared (FIR) to (sub)millimeter photometric catalog in the Cosmic Evolution Survey (COSMOS), prepared with the method recently developed by Liu et al., with key adaptations. We obtain point-spread function fitting photometry at fixed prior positions including 88,008 galaxies detected in VLA 1.4, 3 GHz, and/or MIPS 24 \u03bcm images. By adding a specifically carved mass-selected sample (with an evolving stellar mass limit), a highly complete prior sample of 194,428 galaxies is achieved for deblending FIR/(sub)mm images. We performed \"active\" removal of nonrelevant priors at FIR/(sub)mm bands using spectral energy distribution fitting and redshift information. In order to cope with the shallower COSMOS data, we subtract from the maps the flux of faint nonfitted priors and explicitly account for the uncertainty of this step. The resulting photometry (including data from Spitzer, Herschel, SCUBA2, AzTEC, MAMBO, and NSF's Karl G. Jansky Very Large Array at 3 and 1.4 GHz) displays well-behaved quasi-Gaussian uncertainties calibrated from Monte Carlo simulations and tailored to observables (crowding, residual maps). Comparison to ALMA photometry for hundreds of sources provides a remarkable validation of the technique. We detect 11,220 galaxies over the 100\u20131200 \u03bcm range extending to z_(phot) ~ 7. We conservatively selected a sample of 85 z > 4 high-redshift candidates significantly detected in the FIR/(sub)mm, often with secure radio and/or Spitzer/IRAC counterparts. This provides a chance to investigate the first generation of vigorous starburst galaxies (SFRs ~ 1000 M_\u2299 yr^(\u22121)). The photometric and value-added catalogs are publicly released.", "date": "2018-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "864", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 56", "id_number": "CaltechAUTHORS:20180830-145509653", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180830-145509653", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Key Research and Development Program of China", "grant_number": "2017YFA0402703" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11733002" }, { "agency": "National Key Research and Development Program of China", "grant_number": "2017YFA0402704" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11420101002" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "European Research Council (ERC)", "grant_number": "694343" }, { "agency": "China Scholarship Council" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "doi": "10.3847/1538-4357/aad4af", "primary_object": { "basename": "1807.04697", "url": "https://authors.library.caltech.edu/records/nrs4v-z2v88/files/1807.04697" }, "related_objects": [ { "basename": "Jin_2018_ApJ_864_56.pdf", "url": "https://authors.library.caltech.edu/records/nrs4v-z2v88/files/Jin_2018_ApJ_864_56.pdf" } ], "pub_year": "2018", "author_list": "Jin, Shuowen; Daddi, Emanuele; et el." }, { "id": "https://authors.library.caltech.edu/records/jf571-nwx69", "eprint_id": 89316, "eprint_status": "archive", "datestamp": "2023-08-21 23:57:44", "lastmod": "2023-10-18 22:40:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pavesi-R", "name": { "family": "Pavesi", "given": "Riccardo" }, "orcid": "0000-0002-2263-646X" }, { "id": "Sharon-C-E", "name": { "family": "Sharon", "given": "Chelsea E." }, "orcid": "0000-0002-6250-5608" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "Dominik A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Hodge-J-A", "name": { "family": "Hodge", "given": "Jacqueline A." }, "orcid": "0000-0001-6586-8845" }, { "id": "Decarli-R", "name": { "family": "Decarli", "given": "Roberto" }, "orcid": "0000-0002-2662-8803" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "Fabian" }, "orcid": "0000-0003-4793-7880" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "Chris L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "Emanuele" }, "orcid": "0000-0002-3331-9590" }, { "id": "Smail-Ian-R", "name": { "family": "Smail", "given": "Ian" }, "orcid": "0000-0003-3037-257X" }, { "id": "Dickinson-Mark-E", "name": { "family": "Dickinson", "given": "Mark" }, "orcid": "0000-0001-5414-5131" }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "Rob J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "Mark" }, "orcid": "0000-0003-1033-9684" }, { "id": "da-Cunha-E", "name": { "family": "da Cunha", "given": "Elisabete" }, "orcid": "0000-0001-9759-4797" }, { "id": "Aravena-M", "name": { "family": "Aravena", "given": "Manuel" }, "orcid": "0000-0002-6290-3198" }, { "id": "Darling-J", "name": { "family": "Darling", "given": "Jeremy" }, "orcid": "0000-0003-2511-2060" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "Vernesa" }, "orcid": "0000-0002-3893-8614" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Wagg-Jeff", "name": { "family": "Wagg", "given": "Jeff" } } ] }, "title": "CO Luminosity Density at High-z (COLDz) Survey: A Sensitive, Large-area Blind Search for Low-J CO Emission from Cold Gas in the Early Universe with the Karl G. Jansky Very Large Array", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: ISM; radio lines: galaxies; surveys", "note": "\u00a9 2018. The American Astronomical Society. \n\nReceived 2018 February 13; revised 2018 May 29; accepted 2018 June 6; published 2018 August 29. \n\nThe National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. D.R. and R.P. acknowledge support from the National Science Foundation under grant number AST-1614213 to Cornell University. R.P. acknowledges support through award SOSPA3-008 from the NRAO. We thank Tom Loredo for helpful discussion. I.R.S. acknowledges support from the ERC Advanced Grant DUSTYGAL (321334), STFC (ST/P000541/1), and a Royal Society/Wolfson Merit Award. V.S. acknowledges support from the European Union's Seventh Frame-work program under grant agreement 337595 (ERC Starting Grant, CoSMass) RJI acknowledges ERC funding through Advanced Grant 321302 COSMICISM. This research has made use of the NASA/ IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work is based on observations taken by the CANDELS Multi-Cycle and 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. We acknowledge funding toward the 3 bit samplers used in this work from ERC Advanced Grant 321302, COSMICISM. J.A.H. acknowledges the support of the VIDI research program with project number 639.042.611, which is (partly) financed by the Netherlands Organisation for Scientific Research (NWO). M.T.S. acknowledges support from the Science and Technology Facilities Council (grant number ST/P000252/1).\n\nPublished - Pavesi_2018_ApJ_864_49.pdf
Accepted Version - 1808.04372
", "abstract": "We describe the CO Luminosity Density at High-z (COLDz) survey, the first spectral line deep field targeting CO(1\u20130) emission from galaxies at z = 1.95\u20132.85 and CO(2\u20131) at z = 4.91\u20136.70. The main goal of COLDz is to constrain the cosmic density of molecular gas at the peak epoch of cosmic star formation. By targeting both a wide (~51 arcmin2) and a deep (~9 arcmin^2) area, the survey is designed to robustly constrain the bright end and the characteristic luminosity of the CO(1\u20130) luminosity function. An extensive analysis of the reliability of our line candidates and new techniques provide detailed completeness and statistical corrections as necessary to determine the best constraints to date on the CO luminosity function. Our blind search for CO(1\u20130) uniformly selects starbursts and massive main-sequence galaxies based on their cold molecular gas masses. Our search also detects CO(2\u20131) line emission from optically dark, dusty star-forming galaxies at z > 5. We find a range of spatial sizes for the CO-traced gas reservoirs up to ~40 kpc, suggesting that spatially extended cold molecular gas reservoirs may be common in massive, gas-rich galaxies at z ~ 2. Through CO line stacking, we constrain the gas mass fraction in previously known typical star-forming galaxies at z = 2\u20133. The stacked CO detection suggests lower molecular gas mass fractions than expected for massive main-sequence galaxies by a factor of ~3\u20136. We find total CO line brightness at ~34 GHz of 0.45 \u00b1 0.2 \u03bcK, which constrains future line intensity mapping and CMB experiments.", "date": "2018-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "864", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 49", "id_number": "CaltechAUTHORS:20180830-105710950", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180830-105710950", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1614213" }, { "agency": "National Radio Astronomy Observatory", "grant_number": "SOSPA3-008" }, { "agency": "European Research Council (ERC)", "grant_number": "321334" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/P000541/1" }, { "agency": "Royal Society" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "European Research Council (ERC)", "grant_number": "321302" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "GO 12177" }, { "agency": "NASA", "grant_number": "GO 12328" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "639.042.611" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/P000252/1" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aacb79", "primary_object": { "basename": "1808.04372", "url": "https://authors.library.caltech.edu/records/jf571-nwx69/files/1808.04372" }, "related_objects": [ { "basename": "Pavesi_2018_ApJ_864_49.pdf", "url": "https://authors.library.caltech.edu/records/jf571-nwx69/files/Pavesi_2018_ApJ_864_49.pdf" } ], "pub_year": "2018", "author_list": "Pavesi, Riccardo; Sharon, Chelsea E.; et el." }, { "id": "https://authors.library.caltech.edu/records/yb13k-8yk42", "eprint_id": 89576, "eprint_status": "archive", "datestamp": "2023-08-19 10:46:25", "lastmod": "2023-10-18 22:50:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Herrera-Ruiz-N", "name": { "family": "Herrera Ruiz", "given": "N." } }, { "id": "Middelberg-E", "name": { "family": "Middelberg", "given": "E." } }, { "id": "Deller-A-T", "name": { "family": "Deller", "given": "A." }, "orcid": "0000-0001-9434-3837" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Norris-R-P", "name": { "family": "Norris", "given": "R. P." }, "orcid": "0000-0002-4597-1906" }, { "id": "Novak-Mladen", "name": { "family": "Novak", "given": "M." }, "orcid": "0000-0001-8695-825X" }, { "id": "Delvecchio-I", "name": { "family": "Delvecchio", "given": "I." }, "orcid": "0000-0001-8706-2252" }, { "id": "Best-P-N", "name": { "family": "Best", "given": "P. N." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Momjian-E", "name": { "family": "Momjian", "given": "E." }, "orcid": "0000-0003-3168-5922" }, { "id": "Dettmar-R-J", "name": { "family": "Dettmar", "given": "R.-J." } }, { "id": "Brisken-W-F", "name": { "family": "Brisken", "given": "W." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "VLBA+GBT observations of the COSMOS field and radio source counts at 1.4 GHz", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs / galaxies: active / radio continuum: galaxies", "note": "\u00a9 ESO 2018. \n\nReceived 6 March 2018 / Accepted 18 April 2018. \n\nN.H.R. acknowledges support from the Deutsche Forschungsgemeinschaft through project MI 1230/4-1. V.S., M.N. and I.D. acknowledge the European Union's Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). P.N.B. is grateful for support from STFC via grant ST/M001229/1. We thank the anonymous referee for the helpful and constructive comments, which have improved this paper. This work made use of the Swinburne University of Technology software correlator, developed as part of the Australian Major National Research Facilities Programme and operated under licence. This work made use of Topcat (Taylor 2005), available at http://www.starlink.ac.uk/topcat/. This work also made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com, and Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013). We wish to thank the staff of the VLBA and the GBT who greatly supported the experimental observations in this project. The VLBA and the GBT are operated by the Long Baseline Observatory and the Green Bank Observatory, respectively, facilities of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nPublished - aa32969-18.pdf
Accepted Version - 1804.10464
", "abstract": "We present very long baseline interferometry (VLBI) observations of 179 radio sources in the COSMOS field with extremely high sensitivity using the Green Bank Telescope (GBT) together with the Very Long Baseline Array (VLBA) (VLBA+GBT) at 1.4 GHz, to explore the faint radio population in the flux density regime of tens of \u03bcJy. Here, the identification of active galactic nuclei (AGN) is based on the VLBI detection of the source, meaning that it is independent of X-ray or infrared properties. The milli-arcsecond resolution provided by the VLBI technique implies that the detected sources must be compact and have large brightness temperatures, and therefore they are most likely AGN (when the host galaxy is located at z \u2265 0.1). On the other hand, this technique only allows us to positively identify when a radio-active AGN is present, in other words, we cannot affirm that there is no AGN when the source is not detected. For this reason, the number of identified AGN using VLBI should be always treated as a lower limit. We present a catalogue containing the 35 radio sources detected with the VLBA+GBT, ten of which were not previously detected using only the VLBA. We have constructed the radio source counts at 1.4 GHz using the samples of the VLBA and VLBA+GBT detected sources of the COSMOS field to determine a lower limit for the AGN contribution to the faint radio source population. We found an AGN contribution of >40\u221275% at flux density levels between 150 \u03bcJy and 1 mJy. This flux density range is characterised by the upturn of the Euclidean-normalised radio source counts, which implies a contribution of a new population. This result supports the idea that the sub-mJy radio population is composed of a significant fraction of radio-emitting AGN, rather than solely by star-forming galaxies, in agreement with previous studies.", "date": "2018-08", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "616", "publisher": "EDP Sciences", "pagerange": "Art. No. A128", "id_number": "CaltechAUTHORS:20180912-122527893", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180912-122527893", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "MI 1230/4-1" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/M001229/1" }, { "agency": "NSF" }, { "agency": "Associated Universities, Inc." } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1051/0004-6361/201832969", "primary_object": { "basename": "1804.10464", "url": "https://authors.library.caltech.edu/records/yb13k-8yk42/files/1804.10464" }, "related_objects": [ { "basename": "aa32969-18.pdf", "url": "https://authors.library.caltech.edu/records/yb13k-8yk42/files/aa32969-18.pdf" } ], "pub_year": "2018", "author_list": "Herrera Ruiz, N.; Middelberg, E.; et el." }, { "id": "https://authors.library.caltech.edu/records/k8ee5-ftw69", "eprint_id": 87472, "eprint_status": "archive", "datestamp": "2023-08-19 10:10:43", "lastmod": "2023-10-18 21:12:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pavesi-R", "name": { "family": "Pavesi", "given": "Riccardo" }, "orcid": "0000-0002-2263-646X" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "Dominik A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Sharon-C-E", "name": { "family": "Sharon", "given": "Chelsea E." }, "orcid": "0000-0002-6250-5608" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "Vernesa" }, "orcid": "0000-0002-3893-8614" }, { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "Andreas L." }, "orcid": "0000-0002-9382-9832" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "Christopher L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Stacey-G-J", "name": { "family": "Stacey", "given": "Gordon J." } } ] }, "title": "Hidden in Plain Sight: A Massive, Dusty Starburst in a Galaxy Protocluster at z = 5.7 in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 galaxies: formation \u2013 galaxies: high-redshift \u2013 galaxies: ISM \u2013 galaxies: starburst \u2013 radio lines: galaxies", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 March 21; revised 2018 May 15; accepted 2018 May 19; published 2018 June 29. \n\nWe thank the anonymous referee for a helpful and constructive report. R.P. and D.R. acknowledge support from the National Science Foundation under grant number AST-1614213 to Cornell University. R.P. acknowledges support through award SOSPA3-008 from the NRAO. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00928.S, 2015.1.00388.S, 2012.1.00523.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.\n\nPublished - Pavesi_2018_ApJ_861_43.pdf
Accepted Version - 1803.08048.pdf
", "abstract": "We report the serendipitous discovery of a dusty, starbursting galaxy at z = 5.667 (hereafter called CRLE) in close physical association with the \"normal\" main-sequence galaxy HZ10 at z = 5.654. CRLE was identified by detection of [C II], [N II], and CO(2\u20131) line emission, making it the highest-redshift, most luminous starburst in the COSMOS field. This massive, dusty galaxy appears to be forming stars at a rate of at least 1500 M\u2299 yr^(\u22121) in a compact region only ~3 kpc in diameter. The dynamical and dust emission properties of CRLE suggest an ongoing merger driving the starburst, which is in a potentially intermediate stage relative to other known dusty galaxies at the same epoch. The ratio of [C II] to [N II] may suggest that an important (~15%) contribution to the [C II] emission comes from a diffuse ionized gas component, which could be more extended than the dense, starbursting gas. CRLE appears to be located in a significant galaxy overdensity at the same redshift, potentially associated with a large-scale cosmic structure recently identified in a Lyman \u03b1-emitter survey. This overdensity suggests that CRLE and HZ10 reside in a protocluster environment, offering the tantalizing opportunity to study the effect of a massive starburst on protocluster star formation. Our findings support the interpretation that a significant fraction of the earliest galaxy formation may occur from the inside out, within the central regions of the most massive halos, while rapidly evolving into the massive galaxy clusters observed in the local universe.", "date": "2018-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "861", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 43", "id_number": "CaltechAUTHORS:20180629-110133993", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180629-110133993", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1614213" }, { "agency": "National Radio Astronomy Observatory", "grant_number": "SOSPA3-008" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aac6b6", "primary_object": { "basename": "1803.08048.pdf", "url": "https://authors.library.caltech.edu/records/k8ee5-ftw69/files/1803.08048.pdf" }, "related_objects": [ { "basename": "Pavesi_2018_ApJ_861_43.pdf", "url": "https://authors.library.caltech.edu/records/k8ee5-ftw69/files/Pavesi_2018_ApJ_861_43.pdf" } ], "pub_year": "2018", "author_list": "Pavesi, Riccardo; Riechers, Dominik A.; et el." }, { "id": "https://authors.library.caltech.edu/records/jhsw0-v4y15", "eprint_id": 78659, "eprint_status": "archive", "datestamp": "2023-08-19 10:08:54", "lastmod": "2023-10-26 00:16:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hatfield-P-W", "name": { "family": "Hatfield", "given": "P. W." }, "orcid": "0000-0002-3065-457X" }, { "id": "Bowler-R-A-A", "name": { "family": "Bowler", "given": "R. A. A." } }, { "id": "Jarvis-M-J", "name": { "family": "Jarvis", "given": "M. J." }, "orcid": "0000-0001-7039-9078" }, { "id": "Hale-C-L", "name": { "family": "Hale", "given": "C. L." } } ] }, "title": "The environment and host haloes of the brightest z ~ 6 Lyman-break galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "techniques: photometric \u2013 galaxies: evolution \u2013 galaxies: high-redshift \u2013 galaxies: star formation", "note": "\u00a9 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society\nThis article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/about_us/legal/notices).\n\nAccepted 2018 March 23. Received 2018 February 3; in original form 2017 February 10. Published: 04 April 2018.\n\nThe authors thank the anonymous referee for the comments that have improved the quality of this paper. PH and CH wish to acknowledge support provided through STFC studentships. PH wishes to thank the Rector and Fellows of Lincoln College for support through the Graduate Research Fund. Many thanks to Yuichi Harikane and Olmo Piana for useful discussions on high-redshift clustering, and to Steven Murray for advice for using HALOMOD. This work was supported by the Oxford Centre for Astrophysical Surveys which is funded through generous support from the Hintze Family Charitable Foundation, the award of the STFC consolidated grant (ST/N000919/1), and the John Fell Oxford University Press (OUP) Research Fund. Based on data products from observations made with ESO Telescopes at the La Silla or Paranal Observatories under ESO programme ID 179.A- 2006. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS.\n\nSubmitted - 1702.03309.pdf
", "abstract": "By studying the large-scale structure of the bright high-redshift Lyman-break galaxy (LBG) population it is possible to gain an insight into the role of environment in galaxy formation physics in the early Universe. We measure the clustering of a sample of bright (\u221222.7 < M_(UV) < \u221221.125) LBGs at z \u223c 6 and use a halo occupation distribution (HOD) model to measure their typical halo masses. We find that the clustering amplitude and corresponding HOD fits suggests that these sources are highly biased (b \u223c 8) objects in the densest regions of the high-redshift Universe. Coupled with the observed rapid evolution of the number density of these objects, our results suggest that the shape of high-luminosity end of the luminosity function is related to feedback processes or dust obscuration in the early Universe \u2013 as opposed to a scenario where these sources are predominantly rare instances of the much more numerous M_(UV) \u223c \u221219 population of galaxies caught in a particularly vigorous period of star formation. There is a slight tension between the number densities and clustering measurements, which we interpret this as a signal that a refinement of the model halo bias relation at high redshifts or the incorporation of quasi-linear effects may be needed for future attempts at modelling the clustering and number counts. Finally, the difference in number density between the fields (UltraVISTA has a surface density \u223c 1.8 times greater than UDS) is shown to be consistent with the cosmic variance implied by the clustering measurements.", "date": "2018-07-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "477", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "3760-3774", "id_number": "CaltechAUTHORS:20170628-135339879", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170628-135339879", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "SPLASH" }, { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/sty856", "primary_object": { "basename": "1702.03309.pdf", "url": "https://authors.library.caltech.edu/records/jhsw0-v4y15/files/1702.03309.pdf" }, "pub_year": "2018", "author_list": "Hatfield, P. W.; Bowler, R. A. A.; et el." }, { "id": "https://authors.library.caltech.edu/records/76vs7-18s81", "eprint_id": 87990, "eprint_status": "archive", "datestamp": "2023-08-19 10:01:16", "lastmod": "2023-10-18 21:35:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jim\u00e9nez-Andrade-E-F", "name": { "family": "Jim\u00e9nez-Andrade", "given": "E. F." }, "orcid": "0000-0002-2640-5917" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "Molecular gas in AzTEC/C159: a star-forming disk galaxy 1.3 Gyr after the Big Bang", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift \u2013 galaxies: formation \u2013 galaxies: ISM \u2013 ISM: molecules", "note": "\u00a9 2018 ESO. Article published by EDP Sciences. \n\nReceived 27 October 2017; Accepted 9 February 2018; Published online 05 July 2018. \n\nWe thank Ian Smail for his detailed comments and suggestions that helped to improve the manuscript. E.F.J.A would like to thank M. Krips for her support during the visit to IRAM/Grenoble and the hospitality of the DSOC in Socorro/New Mexico. Support for B.M. was provided by the DFG priority program 1573 \"The physics of the interstellar medium\". G.C.J. is grateful for support from NRAO through the Grote Reber Doctoral Fellowship Program. E.F.J.A, B.M., A.K., E.R.D. and F.B. acknowledge support of the Collaborative Research Center 956, subproject A1 and C4, funded by the Deutsche Forschungsgemeinschaft (DFG). C.G.G and S.T. acknowledge support from the European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt, grant number: 648179). D.R. acknowledges support from the National Science Foundation under grant number AST-1614213. M.A. acknowledges partial support from FONDECYT through grant 1140099. M.J.M. acknowledges the support of the National Science Centre, Poland through the POLONEZ grant 2015/19/P/ST9/04010; this project has received funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sk\u0142odowska-Curie grant agreement No. 665778. V.S. acknowledges support from the European Union's Seventh Frame-work program under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). The National Radio Astronomy Observatory (NRAO) is operated by Associated Universities, Inc., under cooperative agreement with the National Science Foundation. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).\n\nPublished - aa32186-17.pdf
Accepted Version - 1710.10181.pdf
", "abstract": "We studied the molecular gas properties of AzTEC/C159, a star-forming disk galaxy at z = 4.567, in order to better constrain the nature of the high-redshift end of the submillimeter-selected galaxy (SMG) population. We secured ^(12)CO molecular line detections for the J = 2 \u21921 and J = 5 \u21924 transitions using the Karl G. Jansky Very Large Array (VLA) and the NOrthern Extended Millimeter Array (NOEMA) interferometer. The broad (FWHM ~ 750 km s^(\u22121)) and tentative double-peaked profiles of the two ^(12)CO lines are consistent with an extended molecular gas reservoir, which is distributed in a rotating disk, as previously revealed from [CII] 158 \u03bcm line observations. Based on the 12CO(2 \u21921) emission line, we derived L\u2032_(CO)=(3.4\u00b10.6)\u00d710^(10)\u2009K\u2009km\u2009s^(\u22121)\u2009pc^2, which yields a molecular gas mass of M_(H2)(\u03b1_(CO)/4.3)=(1.5\u00b10.3)\u00d710^(11)\u2009M\u2299 and unveils a gas-rich system with \u03bc_(gas)(\u03b1_(CO)/4.3)\u2261M_(H2)/M\u22c6=3.3\u00b10.7. The extreme star formation efficiency of AzTEC/C159, parametrized by the ratio L_(IR)/L\u2032_(CO)=(216\u00b180)\u2009L\u2299\u2009(K\u2009km\u2009s^(\u22121)\u2009pc^2)^(\u22121), is comparable to merger-driven starbursts such as local ultra-luminous infrared galaxies and SMGs. Likewise, the ^(12)CO(5 \u21924)/CO(2 \u21921) line brightness temperature ratio of r_(52)= 0.55 \u00b1 0.15 is consistent with high-excitation conditions as observed in SMGs. Based on mass budget considerations, we constrained the value for the L\u2032_(CO) \u2013 H_2 mass conversion factor in AzTEC/C159, that is, \u03b1_(CO)=3.9_(\u22121.3)^(+2.7)\u2009M\u2299\u2009K^(\u22121)\u2009km^(\u22121)\u2009s\u2009pc^(\u22122), which is consistent with a self-gravitating molecular gas distribution as observed in local star-forming disk galaxies. Cold gas streams from cosmological filaments might be fueling a gravitationally unstable gas-rich disk in AzTEC/C159, which breaks into giant clumps and forms stars as efficiently as in merger-driven systems and generates high gas excitation. These results support the evolutionary connection between AzTEC/C159-like systems and massive quiescent disk galaxies at z ~ 2.", "date": "2018-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "615", "publisher": "EDP Sciences", "pagerange": "Art. No. A25", "id_number": "CaltechAUTHORS:20180719-083430626", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180719-083430626", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "1573" }, { "agency": "National Radio Astronomy Observatory" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "956" }, { "agency": "European Research Council (ERC)", "grant_number": "648179" }, { "agency": "NSF", "grant_number": "AST-1614213" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1140099" }, { "agency": "National Science Centre (Poland)", "grant_number": "2015/19/P/ST9/04010" }, { "agency": "Marie Curie Fellowship", "grant_number": "665778" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "Institute for Studies in Theoretical Physics and Mathematics (Iran)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201732186", "primary_object": { "basename": "1710.10181.pdf", "url": "https://authors.library.caltech.edu/records/76vs7-18s81/files/1710.10181.pdf" }, "related_objects": [ { "basename": "aa32186-17.pdf", "url": "https://authors.library.caltech.edu/records/76vs7-18s81/files/aa32186-17.pdf" } ], "pub_year": "2018", "author_list": "Jim\u00e9nez-Andrade, E. F. and Capak, P. L." }, { "id": "https://authors.library.caltech.edu/records/pqhte-j8f58", "eprint_id": 87216, "eprint_status": "archive", "datestamp": "2023-08-19 09:51:02", "lastmod": "2023-10-18 20:57:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Darvish-B", "name": { "family": "Darvish", "given": "Behnam" }, "orcid": "0000-0003-4919-9017" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "D\u00edaz-Santos-T", "name": { "family": "D\u00edaz-Santos", "given": "Tanio" }, "orcid": "0000-0003-0699-6083" }, { "id": "Shen-Lu", "name": { "family": "Shen", "given": "Lu" } } ] }, "title": "Similar Scaling Relations for the Gas Content of Galaxies Across Environments to z ~ 3.5", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: groups: general \u2013 galaxies: high-redshift \u2013 galaxies: ISM \u2013 galaxies: star formation \u2013 galaxies: starburst", "note": "\u00a9 2018 The American Astronomical Society.\nOriginal content from this work may be used under the terms\nof the Creative Commons Attribution 3.0 licence. Any further\ndistribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.\n\nReceived 2017 November 18; revised 2018 May 22; accepted 2018 May 25; published 2018 June 19.\n\nWe are immensely grateful to the anonymous referee for their useful comments and suggestions that significantly improved the quality of this paper. B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G, and the National Science Foundation, grant number 1716907. B.D. is grateful to Alexandra Pope for her constructive comments and suggestions on the manuscript. B.D. is grateful to Shoubaneh Hemmati, Kirsten Larson, and Iary Davidzon for their thoughtful comments. B.D. wishes to thank Nicola Malavasi for providing their data. T.D.-S. acknowledges support from ALMA-CONICYT project 31130005 and FONDECYT regular project 1151239. This paper makes use of the following ALMA data: ADS/JAO.ALMA 2011.0.00097.S, 2012.1.00076.S, 2012.1.00523.S, 2013.1.00034.S, 2013.1.00111.S, 2015.1.00137.S, 2013.1.00118.S, and 2013.1.00151.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The ALFALFA team at Cornell is supported by NSF grants AST-0607007 and AST-1107390 and by grants from the Brinson Foundation. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), and in alliance with Ana G. Mendez-Universidad Metropolitana, and the Universities Space Research Association. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, The Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.\n\nPublished - Darvish_2018_ApJ_860_111.pdf
Accepted Version - 1805.10291.pdf
", "abstract": "We study the effects of the local environment on the molecular gas content of a large sample of log(M*/M\u2299) \u2273 10 star-forming and starburst galaxies with specific star formation rates (sSFRs) on and above the main sequence (MS) to z ~ 3.5. ALMA observations of the dust continuum in the COSMOS field are used to estimate molecular gas masses at z \u2248 0.5\u20133.5. We also use a local universe sample from the ALFALFA H I survey after converting it into molecular masses. The molecular mass (M_(ISM)) scaling relation shows a dependence on z, M *, and sSFR relative to the MS, but no dependence on environmental overdensity \u0394(M_(ISM) \u221d \u0394^(0.03)). Similarly, gas mass fraction (f_(gas)) and depletion timescale (\u03c4) show no environmental dependence to z ~ 3.5. At\u3008z\u3009~ 1.8, the average\u3008M_(ISM) \u3009,\u3008f_(gas) \u3009, and\u3008\u03c4\u3009in densest regions is (1.6 \u00b1 0.2) \u00d7 10^(11) M\u2299, 55 \u00b1 2%, and 0.8 \u00b1 0.1 Gyr, respectively, similar to those in the lowest density bin. Independent of the environment, f_(gas) decreases and \u03c4increases with increasing cosmic time. Cosmic molecular mass density (\u03c1) in the lowest density bins peaks at z ~ 1\u20132, and this peak happens at z < 1 in densest bins. This differential evolution of \u03c1 across environments is likely due to the growth of the large-scale structure with cosmic time. Our results suggest that the molecular gas content and the subsequent star formation activity of log(M*/M\u2299) \u2273 10 star-forming and starburst galaxies is primarily driven by internal processes, and not by their local environment since z ~ 3.5.", "date": "2018-06-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "860", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 111", "id_number": "CaltechAUTHORS:20180619-094911274", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180619-094911274", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX12AE20G" }, { "agency": "NSF", "grant_number": "AST-1716907" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "31130005" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1151239" }, { "agency": "NSF", "grant_number": "AST-0607007" }, { "agency": "NSF", "grant_number": "AST-1107390" }, { "agency": "Brinson Foundation" }, { "agency": "NSF", "grant_number": "AST-1100968" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aac836", "primary_object": { "basename": "1805.10291.pdf", "url": "https://authors.library.caltech.edu/records/pqhte-j8f58/files/1805.10291.pdf" }, "related_objects": [ { "basename": "Darvish_2018_ApJ_860_111.pdf", "url": "https://authors.library.caltech.edu/records/pqhte-j8f58/files/Darvish_2018_ApJ_860_111.pdf" } ], "pub_year": "2018", "author_list": "Darvish, Behnam; Scoville, Nick Z.; et el." }, { "id": "https://authors.library.caltech.edu/records/zk5y0-svy49", "eprint_id": 86620, "eprint_status": "archive", "datestamp": "2023-08-19 09:40:14", "lastmod": "2023-10-18 19:47:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Harikane-Yuichi", "name": { "family": "Harikane", "given": "Yuichi" }, "orcid": "0000-0002-6047-430X" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "Andreas L." }, "orcid": "0000-0002-9382-9832" }, { "id": "Davidzon-I", "name": { "family": "Davidzon", "given": "Iary" }, "orcid": "0000-0002-2951-7519" } ] }, "title": "SILVERRUSH. V. Census of Ly\u03b1, [O III] \u03bb5007, H\u03b1, and [C II] 158 \u03bcm Line Emission with ~1000 LAEs at z = 4.9\u20137.0 Revealed with Subaru/HSC", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: formation \u2013 galaxies: high-redshift", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2017 November 10; revised 2018 April 6; accepted 2018 April 9; published 2018 May 25. \n\nWe thank the anonymous referee for a careful reading and valuable comments that improved the clarity of the paper. We are grateful to Richard Ellis, Anna Feltre, Max Gronke, Toshihiro Kawaguchi, Kimihiko Nakajima, Kazuhiro Shimasaku, and David Sobral for their useful comments and discussions. We thank Stefano Carniani for providing their data points. \n\nThe Hyper-Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. \n\nThe Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, the Max Planck Institute for Extraterrestrial Physics, Garching, Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant no. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). \n\nThis paper makes use of software developed for the Large Synoptic Survey Telescope. We thank the LSST Project for making their code available as free software at http://dm.lsst.org. \n\nThis work is supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and KAKENHI (15H02064) Grant-in-Aid for Scientific Research (A) through Japan Society for the Promotion of Science (JSPS). Y.H. acknowledges support from the Advanced Leading Graduate Course for Photon Science (ALPS) grant and the JSPS through the JSPS Research Fellowship for Young Scientists. J.C. and S.C. acknowledge support from the European Research Council (ERC) via an Advanced Grant under grant agreement no. 321323-NEOGAL. S.T. acknowledge support from the ERC Consolidator Grant funding scheme (project ConTExt, grant No. 648179). The Cosmic Dawn Center is funded by the Danish National Research Foundation.\n\nPublished - Harikane_2018_ApJ_859_84.pdf
Accepted Version - 1711.03735.pdf
", "abstract": "We investigate Ly\u03b1, [O III] \u03bb5007, H\u03b1, and [C II] 158 \u03bcm emission from 1124 galaxies at z = 4.9\u20137.0. Our sample is composed of 1092 Ly\u03b1 emitters (LAEs) at z = 4.9, 5.7, 6.6, and 7.0 identified by Subaru/Hyper-Suprime-Cam (HSC) narrowband surveys covered by Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH) and 34 galaxies at z = 5.148\u20137.508 with deep ALMA [C II] 158 \u03bcm data in the literature. Fluxes of strong rest-frame optical lines of [O III] and H\u03b1 (H\u03b2) are constrained by significant excesses found in the SPLASH 3.6 and 4.5 \u03bcm photometry. At z = 4.9, we find that the rest-frame H\u03b1 equivalent width and the Ly\u03b1 escape fraction f_(Ly\u03b1) positively correlate with the rest-frame Ly\u03b1 equivalent width EW^0_( Ly\u03b1). The f_(Ly\u03b1)-EW^0_( Ly\u03b1) correlation is similarly found at z ~ 0\u20132, suggesting no evolution of the correlation over z \u2243 0\u20135. The typical ionizing photon production efficiency of LAEs is log(\u03be_(ion)/[Hz erg^(\u22121)]) \u2243 25.5, significantly (60%\u2013100%) higher than those of LBGs at a given UV magnitude. At z = 5.7\u20137.0, there exists an interesting turnover trend that the [O III]/H\u03b1 flux ratio increases in EW^0_( Ly\u03b1) \u2243 0-30 \u00c5 and then decreases out to EW^0_( Ly\u03b1) \u2243 130 \u00c5. We also identify an anticorrelation between a ratio of [C II] luminosity to star formation rate (L [C II]/SFR) and EW^0_( Ly\u03b1) at the >99% confidence level.. We carefully investigate physical origins of the correlations with stellar-synthesis and photoionization models and find that a simple anticorrelation between EW^0_( Ly\u03b1) and metallicity explains self-consistently all of the correlations of Ly\u03b1, H\u03b1, [O III]/H\u03b1, and [C II] identified in our study, indicating detections of metal-poor (~0.03 Z\u2299) galaxies with EW^0_( Ly\u03b1) \u2243 200 \u00c5.", "date": "2018-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "859", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 84", "id_number": "CaltechAUTHORS:20180525-095446696", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180525-095446696", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX08AR22G" }, { "agency": "NSF", "grant_number": "AST-1238877" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15H02064" }, { "agency": "Advanced Leading Graduate Course for Photon Science" }, { "agency": "European Research Council (ERC)", "grant_number": "321323-NEOGAL" }, { "agency": "European Research Council (ERC)", "grant_number": "648179" }, { "agency": "Danish National Research Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/aabd80", "primary_object": { "basename": "1711.03735.pdf", "url": "https://authors.library.caltech.edu/records/zk5y0-svy49/files/1711.03735.pdf" }, "related_objects": [ { "basename": "Harikane_2018_ApJ_859_84.pdf", "url": "https://authors.library.caltech.edu/records/zk5y0-svy49/files/Harikane_2018_ApJ_859_84.pdf" } ], "pub_year": "2018", "author_list": "Harikane, Yuichi; Capak, Peter L.; et el." }, { "id": "https://authors.library.caltech.edu/records/96mk8-w6s62", "eprint_id": 86316, "eprint_status": "archive", "datestamp": "2023-08-19 09:11:24", "lastmod": "2023-10-18 19:27:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Barger-A-J", "name": { "family": "Barger", "given": "A. J." }, "orcid": "0000-0002-3306-1606" }, { "id": "Cowie-L-L", "name": { "family": "Cowie", "given": "L. L." }, "orcid": "0000-0002-6319-1575" }, { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "A." }, "orcid": "0000-0002-9382-9832" }, { "id": "Hemmati-S", "name": { "family": "Hemmati", "given": "S." }, "orcid": "0000-0003-2226-5395" }, { "id": "Kakazu-Yuko", "name": { "family": "Kakazu", "given": "Y." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "D." }, "orcid": "0000-0001-5382-6138" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Nayyeri-H", "name": { "family": "Nayyeri", "given": "H." }, "orcid": "0000-0001-8242-9983" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Suh-Hyewon", "name": { "family": "Suh", "given": "H." }, "orcid": "0000-0002-2536-1633" }, { "id": "Steinhardt-C-L", "name": { "family": "Steinhardt", "given": "C." }, "orcid": "0000-0003-3780-6801" }, { "id": "Yang-Fengwei", "name": { "family": "Yang", "given": "Fengwei" } } ] }, "title": "The DEIMOS 10K Spectroscopic Survey Catalog of the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs \u2013 galaxies: distances and redshifts \u2013 surveys", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2017 December 27; revised 2018 March 12; accepted 2018 March 13; published 2018 May 9. \n\nThe data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. \n\nWe would like to thank the anonymous referee for very useful feedback, which helped to improve the presentation significantly. Support for this work was provided in part by NASA through ADAP grant NNX16AF29G. A.J.B. acknowledges support from NASA ADAP grant NNX14AJ66G and NSF grant AST-1715145. We would also like to recognize the contributions from all of the members of the COSMOS Team who helped in obtaining and reducing the large amount of multi-wavelength data that are now publicly available through the NASA Infrared Science Archive (IRSA) at http://irsa.ipac.caltech.edu/Missions/cosmos.html. In particular, we would like to acknowledge the contribution of several colleagues who have provided interesting targets for the multislit masks throughout the years: H. Aussel, M. Brusa, M. Civano, E. Daddi, J. Donley, E. Le Floch, K. Jahnke, T. Nagao, C. Scarlata, J. Silverman, and V. Smolcic. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We thank the IfA graduate students Jason Chu and Travis Berger for observing some of our multi-slit masks with DEIMOS. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are extremely grateful to have the opportunity to conduct observations from this mountain. \n\nFacilities: Keck:2 - . \n\nSoftware: Dsimulator (http://www2.keck.hawaii.edu/inst/deimos/dsim.html), spec2d (Cooper et al. 2012a; Newman et al. 2013), SpecPro (Masters & Capak 2011).\n\nPublished - Hasinger_2018_ApJ_858_77.pdf
Submitted - 1803.09251.pdf
", "abstract": "We present a catalog of 10,718 objects in the COSMOS field, observed through multi-slit spectroscopy with the Deep Imaging Multi-Object Spectrograph (DEIMOS) on the Keck II telescope in the wavelength range ~5500\u20139800 \u00c5. The catalog contains 6617 objects with high-quality spectra (two or more spectral features), and 1798 objects with a single spectroscopic feature confirmed by the photometric redshift. For 2024 typically faint objects, we could not obtain reliable redshifts. The objects have been selected from a variety of input catalogs based on multi-wavelength observations in the field, and thus have a diverse selection function, which enables the study of the diversity in the galaxy population. The magnitude distribution of our objects is peaked at I_(AB) ~ 23 and K_(AB) ~ 21, with a secondary peak at K_(AB) ~ 24. We sample a broad redshift distribution in the range 0 < z < 6, with one peak at z ~ 1, and another one around z ~ 4. We have identified 13 redshift spikes at z > 0.65 with chance probabilities < 4 \u00d7 10^(\u22124), some of which are clearly related to protocluster structures of sizes >10 Mpc. An object-to-object comparison with a multitude of other spectroscopic samples in the same field shows that our DEIMOS sample is among the best in terms of fraction of spectroscopic failures and relative redshift accuracy. We have determined the fraction of spectroscopic blends to about 0.8% in our sample. This is likely a lower limit and at any rate well below the most pessimistic expectations. Interestingly, we find evidence for strong lensing of Ly\u03b1 background emitters within the slits of 12 of our target galaxies, increasing their apparent density by about a factor of 4.", "date": "2018-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "858", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 77", "id_number": "CaltechAUTHORS:20180509-124803673", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180509-124803673", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX16AF29G" }, { "agency": "NASA", "grant_number": "NNX14AJ66G" }, { "agency": "NSF", "grant_number": "AST-1715145" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aabacf", "primary_object": { "basename": "1803.09251.pdf", "url": "https://authors.library.caltech.edu/records/96mk8-w6s62/files/1803.09251.pdf" }, "related_objects": [ { "basename": "Hasinger_2018_ApJ_858_77.pdf", "url": "https://authors.library.caltech.edu/records/96mk8-w6s62/files/Hasinger_2018_ApJ_858_77.pdf" } ], "pub_year": "2018", "author_list": "Hasinger, G.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/yf3rp-gzc11", "eprint_id": 85529, "eprint_status": "archive", "datestamp": "2023-08-19 08:39:44", "lastmod": "2023-10-18 18:18:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "G\u00f3mez-Guijarro-C", "name": { "family": "G\u00f3mez-Guijarro", "given": "C." }, "orcid": "0000-0002-4085-9165" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "Starburst to Quiescent from HST/ALMA: Stars and Dust Unveil Minor Mergers in Submillimeter Galaxies at z ~ 4.5", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: formation \u2013 galaxies: high-redshift \u2013 galaxies: interactions \u2013 galaxies: ISM \u2013 galaxies: starburst", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2017 November 1; revised 2018 January 16; accepted 2018 February 20; published 2018 March 30. \n\nWe thank I. Smail for his detailed comments and suggestions that help improve this manuscript; J. M. Simpson for providing the SCUBA2 data; C. Y. Peng and G. Barro for their advice on GALFIT; S. Zibetti for his support with ADAPTSMOOTH; C. M. Casey for providing the DSFG comparison data plotted in Figure 4; and D. Watson, J. Hjorth, I. Davidzon, H. Rhodin, K. K. Knudsen, P. Laursen, D. B. Sanders, M. P. Haynes, R. Pavesi, T. K. D. Leung, and S. Mart\u00edn-\u00c1lvarez for helpful comments and suggestions. We are grateful to the anonymous referee, whose comments have been very useful to improving our work. \n\nC.G.G. and S.T. acknowledge support from the European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt, grant number 648179). A.K., E.J.A., and F.B. acknowledge support by the Collaborative Research Centre 956, subproject A1, funded by the Deutsche Forschungsgemeinschaft (DFG). Support for B.M. was provided by the DFG priority program 1573, \"The physics of the interstellar medium.\" D.R. acknowledges support from the National Science Foundation under grant number AST-1614213. V.S. acknowledges support from the European Union's Seventh Framework program under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). M.A. acknowledges partial support from FONDECYT through grant 1140099. ERD also acknowledge support by the Collaborative Research Centre 956, subproject C4, funded by the DFG. M.J.M. acknowledges the support of the National Science Centre, Poland, through POLONEZ grant 2015/19/P/ST9/04010; this project has received funding from the European Union's Horizon 2020 research and innovation program under Marie Sk\u0142odowska-Curie grant agreement No. 665778. \n\nBased on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program #13294. Support for program #13294 was provided by NASA through a grant from the Space Telescope Science Institute. \n\nThis research made use of the following ALMA data: ADS/JAO.ALMA#2012.1.00978.S. ALMA is a partnership of the ESO (representing its member states), NSF (USA), and NINS (Japan), together with the NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by the ESO, AUI/NRAO, and NAOJ. \n\nThis paper employed Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013); APLpy, an open-source plotting package for Python (Robitaille & Bressert 2012); CASA (McMullin et al. 2007); Matplotlib (Hunter 2007); Numpy; Photutils (Bradley et al. 2016); PyBDSF; and R, a language and environment for statistical computing.\n\nPublished - G\u00f3mez-Guijarro_2018_ApJ_856_121.pdf
Accepted Version - 1802.07751.pdf
", "abstract": "Dust-enshrouded, starbursting, submillimeter galaxies (SMGs) at z \u2265 3 have been proposed as progenitors of z \u2265 2 compact quiescent galaxies (cQGs). To test this connection, we present a detailed spatially resolved study of the stars, dust, and stellar mass in a sample of six submillimeter-bright starburst galaxies at z ~ 4.5. The stellar UV emission probed by HST is extended and irregular and shows evidence of multiple components. Informed by HST, we deblend Spitzer/IRAC data at rest-frame optical, finding that the systems are undergoing minor mergers with a typical stellar mass ratio of 1:6.5. The FIR dust continuum emission traced by ALMA locates the bulk of star formation in extremely compact regions (median r e = 0.70 \u00b1 0.29 kpc), and it is in all cases associated with the most massive component of the mergers (median log(M*/M\u2299) = 10.49 \u00b1 0.32). We compare spatially resolved UV slope (\u03b2) maps with the FIR dust continuum to study the infrared excess (IRX = L_(IR)/L_(UV))\u2013\u03b2 relation. The SMGs display systematically higher IRX values than expected from the nominal trend, demonstrating that the FIR and UV emissions are spatially disconnected. Finally, we show that the SMGs fall on the mass\u2013size plane at smaller stellar masses and sizes than the cQGs at z = 2. Taking into account the expected evolution in stellar mass and size between z = 4.5 and z = 2 due to the ongoing starburst and mergers with minor companions, this is in agreement with a direct evolutionary connection between the two populations.", "date": "2018-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "856", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 121", "id_number": "CaltechAUTHORS:20180330-103323375", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180330-103323375", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "648179" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "956" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "1573" }, { "agency": "NSF", "grant_number": "AST-1614213" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1140099" }, { "agency": "National Science Centre (Poland)", "grant_number": "2015/19/P/ST9/04010" }, { "agency": "Marie Curie Fellowship", "grant_number": "665778" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/aab206", "primary_object": { "basename": "G\u00f3mez-Guijarro_2018_ApJ_856_121.pdf", "url": "https://authors.library.caltech.edu/records/yf3rp-gzc11/files/G\u00f3mez-Guijarro_2018_ApJ_856_121.pdf" }, "related_objects": [ { "basename": "1802.07751.pdf", "url": "https://authors.library.caltech.edu/records/yf3rp-gzc11/files/1802.07751.pdf" } ], "pub_year": "2018", "author_list": "G\u00f3mez-Guijarro, C. and Capak, P. L." }, { "id": "https://authors.library.caltech.edu/records/x4c8n-zc397", "eprint_id": 86196, "eprint_status": "archive", "datestamp": "2023-08-19 08:34:11", "lastmod": "2023-10-18 19:21:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Molecular outflow and feedback in the obscured quasar XID2028 revealed by ALMA", "ispublished": "pub", "full_text_status": "public", "keywords": "quasars: individual: XID2028 \u2013 galaxies: star formation \u2013 galaxies: active \u2013 galaxies: ISM", "note": "\u00a9 2018 ESO. Article published by EDP Sciences. \n\nReceived 25 July 2017; Accepted 12 December 2017; Published online 16 April 2018. \n\nThis paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00299.S (PI: Brusa), #2015.1.00137.S (PI: Scoville), and #20015.1.00171.S (PI: Daddi). ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC, and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. XID2028 is an interesting target from several perspectives (e.g. massive MS galaxy; bright FIR/Herschel source with substantial SFR), and as such, in addition to our deep dedicated follow-up, it has also been targeted independently by two different ALMA snapshot programmes as part of large samples (100+) of high-z galaxies. A careful scrutiny of the ALMA archive and an open collaboration with the PIs of the programmesallowed us to make the best use of ALMA data. We thank the ARGOS team for obtaining the K-band imaging of XID2028 during a commissioning run. We gratefully thank the staff of the Italian ARC node for their support in data reduction. This research was finalised at the Munich Institute for Astro- and Particle Physics (MIAPP) ofthe DFG cluster of excellence \"Origin and Structure of the Universe\", during the programme \"In & Out: What rules the galaxy baryon cycle?\" (July 2017). MB, MP, and GL acknowledge support from the FP7 Career Integration Grant \"eEASy\" (\"SMBH evolution through cosmic time: from current surveys to eROSITA-Euclid AGN Synergies\", CIG 321913). EL is supported by a European Union COFUND/Durham Junior Research Fellowship (under EU grant agreement no. 609412). MTS was supported by a Royal Society Leverhulme Trust Senior Research Fellowship (LT150041). CF acknowledges support from the European Union Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No 664931. SC acknowledges financial support from the Science and Technology Facilities Council (STFC). We acknowledge financial support from INAF under the contract PRIN-INAF-2014 (\"Windy Black Holes combing Galaxy evolution\"). We gratefully thank Maurilio Pannella, Renzo Sancisi, Margherita Talia, Anna Cibinel, Roberto Decarli, Andrea Lapi, Gerg\u00f6 Popping, David Rosario, Kartik Sheth, and John Silverman for useful discussions, and Darshan Kakkad for providing data prior to publication. We thank the anonymous referee for her/his constructive criticisms, which considerably improved the presentation of the results.\n\nPublished - aa31641-17.pdf
Submitted - 1712.04505.pdf
", "abstract": "We imaged, with ALMA and ARGOS/LUCI, the molecular gas and dust and stellar continuum in XID2028, which is an obscured quasi-stellar object (QSO) at z = 1.593, where the presence of a massive outflow in the ionised gas component traced by the [OIII]5007 emission has been resolved up to 10 kpc. This target represents a unique test case to study QSO feedback in action at the peak epoch of AGN-galaxy co-evolution. The QSO was detected in the CO(5 \u2212 4) transition and in the 1.3 mm continuum at ~30 and ~20\u03c3 significance, respectively; both emissions are confined in the central (<2 kpc) radius area. Our analysis suggests the presence of a fast rotating molecular disc (v ~ 400 km s^(\u22121)) on very compact scales well inside the galaxy extent seen in the rest-frame optical light (~10 kpc, as inferred from the LUCI data). Adding available measurements in additional two CO transitions, CO(2 \u2212 1) and CO(3 \u2212 2), we could derive a total gas mass of ~10^(10) M\u2299, thanks to a critical assessment of CO excitation and the comparison with the Rayleigh\u2013Jeans continuum estimate. This translates into a very low gas fraction (<5%) and depletion timescales of 40\u201375 Myr, reinforcing the result of atypical gas consumption conditions in XID2028, possibly because of feedback effects on the host galaxy. Finally, we also detect the presence of high velocity CO gas at ~5\u03c3, which we interpret as a signature of galaxy-scale molecular outflow that is spatially coincident with the ionised gas outflow. XID2028 therefore represents a unique case in which the measurement of total outflowing mass, of ~500\u2013800 M\u2299 yr^(\u22121) including the molecular and atomic components in both the ionised and neutral phases, was attempted for a high-z QSO.", "date": "2018-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "612", "publisher": "EDP Sciences", "pagerange": "Art. No. A29", "id_number": "CaltechAUTHORS:20180502-132142575", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180502-132142575", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "321913 eEasy" }, { "agency": "European Research Council (ERC)", "grant_number": "609412" }, { "agency": "Royal Society", "grant_number": "LT150041" }, { "agency": "Marie Curie Fellowship", "grant_number": "664931" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-INAF-2014" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1051/0004-6361/201731641", "primary_object": { "basename": "1712.04505.pdf", "url": "https://authors.library.caltech.edu/records/x4c8n-zc397/files/1712.04505.pdf" }, "related_objects": [ { "basename": "aa31641-17.pdf", "url": "https://authors.library.caltech.edu/records/x4c8n-zc397/files/aa31641-17.pdf" } ], "pub_year": "2018", "author_list": "Brusa, M. and Scoville, N. Z." }, { "id": "https://authors.library.caltech.edu/records/nvwc7-ha845", "eprint_id": 85698, "eprint_status": "archive", "datestamp": "2023-08-21 23:04:18", "lastmod": "2023-10-18 18:41:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mehta-V", "name": { "family": "Mehta", "given": "Vihang" }, "orcid": "0000-0001-7166-6035" }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "Claudia" }, "orcid": "0000-0002-9136-8876" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Davidzon-I", "name": { "family": "Davidzon", "given": "Iary" }, "orcid": "0000-0002-2951-7519" }, { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "Andreas" }, "orcid": "0000-0002-9382-9832" }, { "id": "Hsieh-Bau-Ching", "name": { "family": "Hsieh", "given": "Bau Ching" }, "orcid": "0000-0001-5615-4904" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Jarvis-M-J", "name": { "family": "Jarvis", "given": "Matt" }, "orcid": "0000-0001-7039-9078" }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "Clotilde" } }, { "id": "Phillips-J", "name": { "family": "Phillips", "given": "John" } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "John" }, "orcid": "0000-0002-0000-6977" }, { "id": "Strauss-M-A", "name": { "family": "Strauss", "given": "Michael A." }, "orcid": "0000-0002-0106-7755" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "Masayuki" }, "orcid": "0000-0002-5011-5178" }, { "id": "Bowler-R-A-A", "name": { "family": "Bowler", "given": "Rebecca" } }, { "id": "Coupon-J", "name": { "family": "Coupon", "given": "Jean" } }, { "id": "Foucaud-S", "name": { "family": "Foucaud", "given": "S\u00e9bastien" }, "orcid": "0000-0001-5603-6262" }, { "id": "Hemmati-S", "name": { "family": "Hemmati", "given": "Shoubaneh" }, "orcid": "0000-0003-2226-5395" }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "Daniel" }, "orcid": "0000-0001-5382-6138" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "Henry Joy" }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Ouchi-Masami", "name": { "family": "Ouchi", "given": "Masami" }, "orcid": "0000-0002-1049-6658" }, { "id": "Shibuya-Takatoshi", "name": { "family": "Shibuya", "given": "Takatoshi" } }, { "id": "Wang-Wei-Hao", "name": { "family": "Wang", "given": "Wei-Hao" }, "orcid": "0000-0003-2588-1265" } ] }, "title": "SPLASH-SXDF Multi-wavelength Photometric Catalog", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: high-redshift; galaxies: photometry; methods: observational; techniques: photometric", "note": "\u00a9 2018. The American Astronomical Society. \n\nReceived 2017 November 13; revised 2018 March 5; accepted 2018 March 10; published 2018 April 9. \n\nV.M. would like to thank Micaela Bagley for a helpful discussion regarding the photometric errors. V.M. and C.S. acknowledge the support from Jet Propulsion Laboratory under the grant award #RSA-1516084. V.M. also acknowledges support from the University of Minnesota Doctoral Dissertation Fellowship 2016\u201317. W.H.W. acknowledges the support from the Ministry of Science and Technology of Taiwan grant 105-2112-M- 001-029-MY3. O.I. acknowledges the funding of the French Agence Nationale de la Recherche for the SAGACE project. \n\nThe Cosmic Dawn Center is funded by the Danish National Research Foundation. \n\nThis work is based in part on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by Subaru Telescope and Astronomy Data Center at National Astronomical Observatory of Japan. \n\nThis work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. \n\nThe Hyper-Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. \n\nThis paper makes use of software developed for the Large Synoptic Survey Telescope. We thank the LSST Project for making their code available as free software at http://dm.lsst.org/. \n\nThis work is based in part on observations obtained with MegaPrime and MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada\u2013France\u2013Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada\u2013France\u2013Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. \n\nThis research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. \n\nFacilities: Spitzer - Spitzer Space Telescope satellite, Subaru - , CFHT - , UKIRT - , VISTA - . \n\nSoftware: NumPy, SciPy, AstroPy, Matplotlib, PhotUtils, LePhare, SExtractor, SCAMP, SWARP, PSFEx.\n\nPublished - Mehta_2018_ApJS_235_36.pdf
Accepted Version - 1711.05280
", "abstract": "We present a multi-wavelength catalog in the Subaru/XMM-Newton Deep Field (SXDF) as part of the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH). We include the newly acquired optical data from the Hyper-Suprime-Cam Subaru Strategic Program, accompanied by IRAC coverage from the SPLASH survey. All available optical and near-infrared data is homogenized and resampled on a common astrometric reference frame. Source detection is done using a multi-wavelength detection image including the u-band to recover the bluest objects. We measure multi-wavelength photometry and compute photometric redshifts as well as physical properties for ~1.17 million objects over ~4.2 deg^2, with ~800,000 objects in the 2.4 deg^2 HSC-Ultra-Deep coverage. Using the available spectroscopic redshifts from various surveys over the range of 0 < z < 6, we verify the performance of the photometric redshifts and we find a normalized median absolute deviation of 0.023 and outlier fraction of 3.2%. The SPLASH-SXDF catalog is a valuable, publicly available resource, perfectly suited for studying galaxies in the early universe and tracing their evolution through cosmic time.", "date": "2018-04", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "235", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 36", "id_number": "CaltechAUTHORS:20180409-153352660", "issn": "1538-4365", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180409-153352660", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "JPL", "grant_number": "RSA-1516084" }, { "agency": "University of Minnesota" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "105-2112-M- 001-029-MY3" }, { "agency": "Agence Nationale pour la Recherche (ANR)" }, { "agency": "Danish National Research Foundation" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "SPLASH" }, { "id": "COSMOS" } ] }, "doi": "10.3847/1538-4365/aab60c", "primary_object": { "basename": "1711.05280", "url": "https://authors.library.caltech.edu/records/nvwc7-ha845/files/1711.05280" }, "related_objects": [ { "basename": "Mehta_2018_ApJS_235_36.pdf", "url": "https://authors.library.caltech.edu/records/nvwc7-ha845/files/Mehta_2018_ApJS_235_36.pdf" } ], "pub_year": "2018", "author_list": "Mehta, Vihang; Scarlata, Claudia; et el." }, { "id": "https://authors.library.caltech.edu/records/935hx-x0764", "eprint_id": 85480, "eprint_status": "archive", "datestamp": "2023-08-21 22:57:15", "lastmod": "2023-10-18 18:15:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "Andreas L." }, "orcid": "0000-0002-9382-9832" }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "Daniel" }, "orcid": "0000-0001-5382-6138" }, { "id": "Wang-Yun", "name": { "family": "Wang", "given": "Yun" } }, { "id": "Merson-A-I", "name": { "family": "Merson", "given": "Alexander" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Malhotra-S", "name": { "family": "Malhotra", "given": "Sangeeta" }, "orcid": "0000-0002-9226-5350" }, { "id": "Rhoads-J-E", "name": { "family": "Rhoads", "given": "James E." }, "orcid": "0000-0002-1501-454X" } ] }, "title": "Empirical Modeling of the Redshift Evolution of the [N II]/H\u03b1 Ratio for Galaxy Redshift Surveys", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: fundamental parameters; galaxies: ISM", "note": "\u00a9 2018. The American Astronomical Society. \n\nReceived 2017 September 8; revised 2018 February 12; accepted 2018 February 15; published 2018 March 16. \n\nThe authors thank J. Colbert for helpful comments and discussions. We also thank the referee for the very useful comments, which helped to improve this paper. A.M. acknowledges sponsorship of a NASA Postdoctoral Program Fellowship. A.M. was supported by JPL, which is run under contract by the California Institute of Technology for NASA.\n\nPublished - Faisst_2018_ApJ_855_132.pdf
Accepted Version - 1710.00834
", "abstract": "We present an empirical parameterization of the [N ii]/H\u03b1 flux ratio as a function of stellar mass and redshift valid at 0 < z < 2.7 and 8.5 < log(M/M_\u2299) < 11.0. This description can (i) easily be applied to simulations for modeling [N ii]\u03bb6584 line emission, (ii) deblend [N ii] and H\u03b1 in current low-resolution grism and narrow-band observations to derive intrinsic H\u03b1 fluxes, and (iii) reliably forecast the number counts of H\u03b1 emission-line galaxies for future surveys, such as those planned for Euclid and the Wide Field Infrared Survey Telescope (WFIRST). Our model combines the evolution of the locus on the Baldwin, Phillips & Terlevich (BPT) diagram measured in spectroscopic data out to z ~ 2.5 with the strong dependence of [N ii]/H\u03b1 on stellar mass and [O iii]/H\u03b2 observed in local galaxy samples. We find large variations in the [N ii]/H\u03b1 flux ratio at a fixed redshift due to its dependency on stellar mass; hence, the assumption of a constant [N ii] flux contamination fraction can lead to a significant under- or overestimate of H\u03b1 luminosities. Specifically, measurements of the intrinsic H\u03b1 luminosity function derived from current low-resolution grism spectroscopy assuming a constant 29% contamination of [N ii] can be overestimated by factors of ~8 at log(L) > 43.0 for galaxies at redshifts z ~ 1.5. This has implications for the prediction of H\u03b1 emitters for Euclid and WFIRST. We also study the impact of blended H\u03b1 and [N ii] on the accuracy of measured spectroscopic redshifts.", "date": "2018-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "855", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 132", "id_number": "CaltechAUTHORS:20180328-133307813", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180328-133307813", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Postdoctoral Program" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "doi": "10.3847/1538-4357/aab1fc", "primary_object": { "basename": "Faisst_2018_ApJ_855_132.pdf", "url": "https://authors.library.caltech.edu/records/935hx-x0764/files/Faisst_2018_ApJ_855_132.pdf" }, "related_objects": [ { "basename": "1710.00834", "url": "https://authors.library.caltech.edu/records/935hx-x0764/files/1710.00834" } ], "pub_year": "2018", "author_list": "Faisst, Andreas L.; Masters, Daniel; et el." }, { "id": "https://authors.library.caltech.edu/records/715v3-mn306", "eprint_id": 84360, "eprint_status": "archive", "datestamp": "2023-08-19 07:21:18", "lastmod": "2023-10-18 16:09:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gilbert-Karoline-M", "name": { "family": "Gilbert", "given": "Karoline M." }, "orcid": "0000-0003-0394-8377" }, { "id": "Tollerud-Erik-J", "name": { "family": "Tollerud", "given": "Erik J." }, "orcid": "0000-0002-9599-310X" }, { "id": "Beaton-Rachael-L", "name": { "family": "Beaton", "given": "Rachael L." }, "orcid": "0000-0002-1691-8217" }, { "id": "Guhathakurta-Puragra", "name": { "family": "Guhathakurta", "given": "Puragra" }, "orcid": "0000-0001-8867-4234" }, { "id": "Bullock-James-S", "name": { "family": "Bullock", "given": "James S." }, "orcid": "0000-0003-4298-5082" }, { "id": "Chiba-Masashi", "name": { "family": "Chiba", "given": "Masashi" }, "orcid": "0000-0002-9053-860X" }, { "id": "Kalirai-Jason-S", "name": { "family": "Kalirai", "given": "Jason S." }, "orcid": "0000-0001-9690-4159" }, { "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "orcid": "0000-0001-6196-5162" }, { "id": "Majewski-Steven-R", "name": { "family": "Majewski", "given": "Steven R." }, "orcid": "0000-0003-2025-3147" }, { "id": "Tanaka-Mikito", "name": { "family": "Tanaka", "given": "Mikito" } } ] }, "title": "Global Properties of M31's Stellar Halo from the SPLASH Survey. III. Measuring the Stellar Velocity Dispersion Profile", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2017 April 30. Accepted 2017 November 20. Published 2018 January 15. \n\nSupport for this work was provided by NASA through a Giacconi Fellowship (E.J.T.) and Hubble Fellowship grants 51316.01 and 51386.01 awarded to E.J.T. and R.L.B. by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. K.M.G. and E.N.K. acknowledge support from NSF grants AST-1614569 and AST-1614081. R.L.B. and S.R.M. acknowledge support from NSF grants AST-1413269 and AST-1009882. P.G. and J.S.B. acknowledge support from collaborative NSF grants AST-1412648, AST-1010039, AST-1009973. M.T. and M.C. acknowledge support from Grant-in-Aid for Scientific Research (2580098 for M.T., 16H01086 and 17H01101 for M.C.) of the Ministry of Education, Culture, Sports, Science, and Technology of Japan. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048.\n\nPublished - Gilbert_2018_ApJ_852_128.pdf
Submitted - 1711.02700.pdf
", "abstract": "We present the velocity dispersion of red giant branch stars in M31's halo, derived by modeling the line-of-sight velocity distribution of over 5000 stars in 50 fields spread throughout M31's stellar halo. The data set was obtained as part of the Spectroscopic and Photometric Landscape of Andromeda's Stellar Halo (SPLASH) Survey, and covers projected radii of 9 to 175 kpc from M31's center. All major structural components along the line of sight in both the Milky Way (MW) and M31 are incorporated in a Gaussian Mixture Model, including all previously identified M31 tidal debris features in the observed fields. The probability that an individual star is a constituent of M31 or the MW, based on a set of empirical photometric and spectroscopic diagnostics, is included as a prior probability in the mixture model. The velocity dispersion of stars in M31's halo is found to decrease only mildly with projected radius, from 108 km s_(\u22121) in the innermost radial bin (8.2 to 14.1 kpc) to ~80 to 90 km s^(\u22121) at projected radii of ~40\u2013130 kpc, and can be parameterized with a power law of slope \u22120.12 \u00b1 0.05. The quoted uncertainty on the power-law slope reflects only the precision of the method, although other sources of uncertainty we consider contribute negligibly to the overall error budget.", "date": "2018-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "852", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 128", "id_number": "CaltechAUTHORS:20180117-095337937", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180117-095337937", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Giacconi Fellowship" }, { "agency": "NASA Hubble Fellowship", "grant_number": "51316.01" }, { "agency": "NASA Hubble Fellowship", "grant_number": "51386.01" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NSF", "grant_number": "AST-1614569" }, { "agency": "NSF", "grant_number": "AST-1614081" }, { "agency": "NSF", "grant_number": "AST-1413269" }, { "agency": "NSF", "grant_number": "AST-1009882" }, { "agency": "NSF", "grant_number": "AST-1412648" }, { "agency": "NSF", "grant_number": "AST-1010039" }, { "agency": "NSF", "grant_number": "AST-1009973" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "2580098" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "16H01086" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "17H01101" }, { "agency": "NSF", "grant_number": "AST-0071048" } ] }, "local_group": { "items": [ { "id": "SPLASH" }, { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aa9f26", "primary_object": { "basename": "1711.02700.pdf", "url": "https://authors.library.caltech.edu/records/715v3-mn306/files/1711.02700.pdf" }, "related_objects": [ { "basename": "Gilbert_2018_ApJ_852_128.pdf", "url": "https://authors.library.caltech.edu/records/715v3-mn306/files/Gilbert_2018_ApJ_852_128.pdf" } ], "pub_year": "2018", "author_list": "Gilbert, Karoline M.; Tollerud, Erik J.; et el." }, { "id": "https://authors.library.caltech.edu/records/t6rwz-k5h07", "eprint_id": 84291, "eprint_status": "archive", "datestamp": "2023-08-21 22:35:18", "lastmod": "2023-10-18 16:04:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Davidzon-I", "name": { "family": "Davidzon", "given": "Iary" }, "orcid": "0000-0002-2951-7519" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "Andreas L." }, "orcid": "0000-0002-9382-9832" }, { "id": "Sparre-M", "name": { "family": "Sparre", "given": "Martin" }, "orcid": "0000-0002-9735-3851" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "An Alternate Approach to Measure Specific Star Formation Rates at 2 < z < 7", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: star formation", "note": "\u00a9 2018. The American Astronomical Society. \n\nReceived 2017 September 6; revised 2017 November 13; accepted 2017 December 11; published 2018 January 12. \n\nWe thank Paola Santini for providing their data in a convenient digital format and Bahram Mobasher for his useful comments. This work is based on observations and archival data made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research is also based on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by the Subaru Telescope and Astronomy Data Center at the National Astronomical Observatory of Japan. O.I. acknowledges funding of the French Agence Nationale de la Recherche for the SAGACE project. We acknowledge the financial support the COSMOS team receives from the Centre National d'\u00c9tudes Spatiales.\n\nPublished - Davidzon_2018_ApJ_852_107.pdf
Submitted - 1712.03959
", "abstract": "We trace the specific star formation rate (sSFR) of massive star-forming galaxies (\u2273 (10)^(10) M_\u2299) from z ~ 2 to 7. Our method is substantially different from previous analyses, as it does not rely on direct estimates of star formation rate, but on the differential evolution of the galaxy stellar mass function (SMF). We show the reliability of this approach by means of semianalytical and hydrodynamical cosmological simulations. We then apply it to real data, using the SMFs derived in the COSMOS and CANDELS fields. We find that the sSFR is proportional to (1+z)^(1.1 \u00b1 0.2) at z > 2, in agreement with other observations but in tension with the steeper evolution predicted by simulations from z ~ 4 to 2. We investigate the impact of several sources of observational bias, which, however, cannot account for this discrepancy. Although the SMF of high-redshift galaxies is still affected by significant errors, we show that future large-area surveys will substantially reduce them, making our method an effective tool to probe the massive end of the main sequence of star-forming galaxies.", "date": "2018-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "852", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 107", "id_number": "CaltechAUTHORS:20180112-092947647", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180112-092947647", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Agence Nationale pour la Recherche (ANR)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "doi": "10.3847/1538-4357/aaa19e", "primary_object": { "basename": "1712.03959", "url": "https://authors.library.caltech.edu/records/t6rwz-k5h07/files/1712.03959" }, "related_objects": [ { "basename": "Davidzon_2018_ApJ_852_107.pdf", "url": "https://authors.library.caltech.edu/records/t6rwz-k5h07/files/Davidzon_2018_ApJ_852_107.pdf" } ], "pub_year": "2018", "author_list": "Davidzon, Iary; Ilbert, Olivier; et el." }, { "id": "https://authors.library.caltech.edu/records/h65p3-0tp15", "eprint_id": 85199, "eprint_status": "archive", "datestamp": "2023-08-19 07:16:22", "lastmod": "2023-10-18 17:57:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kusakabe-Haruka", "name": { "family": "Kusakabe", "given": "Haruka" } }, { "id": "Shimasaku-Kazuhiro", "name": { "family": "Shimasaku", "given": "Kazuhiro" } }, { "id": "Ouchi-Masami", "name": { "family": "Ouchi", "given": "Masami" }, "orcid": "0000-0002-1049-6658" }, { "id": "Nakajima-Kimihiko", "name": { "family": "Nakajima", "given": "Kimihiko" } }, { "id": "Goto-Ryosuke", "name": { "family": "Goto", "given": "Ryosuke" } }, { "id": "Hashimoto-Takuya", "name": { "family": "Hashimoto", "given": "Takuya" } }, { "id": "Konno-Akira", "name": { "family": "Konno", "given": "Akira" } }, { "id": "Harikane-Yuichi", "name": { "family": "Harikane", "given": "Yuichi" }, "orcid": "0000-0002-6047-430X" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "John D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "The stellar mass, star formation rate and dark matter halo properties of LAEs at z \u223c 2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: halos galaxies: star formation galaxies: evolution galaxies: high-redshift", "note": "\u00a9 The Author(s) 2018. Published by Oxford University Press on behalf of the Astronomical Society of Japan. \n\nReceived: 28 July 2017; Accepted: 22 November 2017; Published: 13 January 2018. \n\nWe thank the anonymous referee for his/her helpful comments and suggestions. We are grateful to Lihwai Lin and Li-Ting Hsu for kindly providing us with J, H, and Ks images of the HDFN field and data in Lin et al. (2012) plotted in figures 8, 9, and 10. We are also grateful to Yoshiaki Ono for giving insightful comments and suggestions on SED fitting. We would like to show our appreciation to Takashi Hamana for helpful comments on cosmic variance and computer programs of the covariance of dark matter angular correlation function and the EPS model. We would like to express our gratitude to David Sobral, Naveen A. Reddy, Giulia Rodighiero, and Shogo Ishikawa for kindly providing their data plotted in figures 5a, 7, 8, and 9, respectively. We would like to thank Alex Hagen, James E. Rhoads, Jorryt Matthee, and Peter S. Behroozi for useful comments on their results. We also would like to thank Akio K. Inoue, Cai-Na Hao, Hidenobu Yajima, Ikkoh Shimizu, Ken Mawatari, Kotaro Kohno, Kyoung-Soo Lee, Tsutomu T. Takeuchi, Mana Niida and Yuki Yoshimura for insightful discussion. We acknowledge Ryota Kawamata, Taku Okamura, and Kazushi Irikura for constructive discussions at weekly meetings. This work is based on observations taken by the Subaru Telescope which is operated by the National Astronomical Observatory of Japan. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This research made use of IRAF, which is distributed by NOAO, which is operated by AURA under a cooperative agreement with the National Science Foundation and of Python packages for Astronomy: Astropy (Astropy Collaboration et al. 2013), Colossus, CosmoloPy and PyRAF, which is produced by the Space Telescope Science Institute, which is operated by AURA for NASA. H.K acknowledges support from the JSPS through the JSPS Research Fellowship for Young Scientists. This work is supported in part by KAKENHI (16K05286) Grant-in-Aid for Scientific Research (C) through the JSPS.\n\nAccepted Version - 1707.09373.pdf
", "abstract": "We present average stellar population properties and dark matter halo masses of z \u223c 2 Ly\u03b1 emitters (LAEs) from spectral energy distribution fitting and clustering analysis, respectively, using \u2243 1250 objects (NB387 \u2264 25.5) in four separate fields of \u2243 1\u2009deg^2 in total. With an average stellar mass of 10.2\u2009\u00b1\u20091.8 \u00d7 10^8\u2009M\u2299 and star formation rate of 3.4\u2009\u00b1\u20090.4\u2009M\u2299\u2009yr^(\u22121), the LAEs lie on an extrapolation of the star-formation main sequence (MS) to low stellar mass. Their effective dark matter halo mass is estimated to be 4.0^(+5.1)_(\u22122.9)\u00d710^(10) M\u2299 with an effective bias of 1.22^(+0.16)_(\u22120.18, which is lower than that of z \u223c 2 LAEs (1.8\u2009\u00b1\u20090.3) obtained by a previous study based on a three times smaller survey area, with a probability of 96%. However, the difference in the bias values can be explained if cosmic variance is taken into account. If such a low halo mass implies a low H\u2009I gas mass, this result appears to be consistent with the observations of a high Ly\u03b1 escape fraction. With the low halo masses and ongoing star formation, our LAEs have a relatively high stellar-to-halo mass ratio (SHMR) and a high efficiency of converting baryons into stars. The extended Press\u2013Schechter formalism predicts that at z = 0 our LAEs are typically embedded in halos with masses similar to that of the Large Magellanic Cloud (LMC); they will also have similar SHMRs to the LMC, if their star formation rates are largely suppressed after z \u223c 2 as some previous studies have reported for the LMC itself.", "date": "2018-01-01", "date_type": "published", "publication": "Publications of the Astronomical Society of Japan", "volume": "70", "number": "1", "publisher": "Astronomical Society of Japan", "pagerange": "Art. No. 4", "id_number": "CaltechAUTHORS:20180308-102934270", "issn": "0004-6264", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180308-102934270", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "16K05286" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/pasj/psx148", "primary_object": { "basename": "1707.09373.pdf", "url": "https://authors.library.caltech.edu/records/h65p3-0tp15/files/1707.09373.pdf" }, "pub_year": "2018", "author_list": "Kusakabe, Haruka; Shimasaku, Kazuhiro; et el." }, { "id": "https://authors.library.caltech.edu/records/k97b3-1t577", "eprint_id": 85030, "eprint_status": "archive", "datestamp": "2023-08-19 07:11:16", "lastmod": "2023-10-18 17:04:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aihara-Hiroaki", "name": { "family": "Aihara", "given": "Hiroaki" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "The Hyper Suprime-Cam SSP Survey: Overview and survey design", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations galaxies: general surveys (cosmology:) large-scale structure of universe", "note": "\u00a9 2017 The Author. Published by Oxford University Press on behalf of the Astronomical Society of Japan. \n\nReceived: 20 April 2017; Accepted: 26 June 2017; Published: 04 September 2017. \n\nThe Hyper Suprime-Cam (HSC) collaboration includes the\nastronomical communities of Japan and Taiwan, and Princeton\nUniversity. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan\n(NAOJ), the Kavli Institute for the Physics and Mathematics\nof the Universe (Kavli IPMU), the University of Tokyo, the\nHigh Energy Accelerator Research Organization (KEK), the\nAcademia Sinica Institute for Astronomy and Astrophysics\nin Taiwan (ASIAA), and Princeton University. Funding was\ncontributed by the FIRST program from Japanese Cabinet\nOffice, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK,\nASIAA, and Princeton University. HM is supported by the Jet Propulsion Laboratory, California Institute of Technology,\nunder a contract with the National Aeronautics and Space\nAdministration. This paper makes use of software developed\nfor the Large Synoptic Survey Telescope. We thank the LSST\nProject for making their code available as free software at\nhttp://dm.lsst.org. \n\nThe Pan-STARRS1 Surveys (PS1) have been made possible\nthrough contributions of the Institute for Astronomy,\nthe University of Hawaii, the Pan-STARRS Project Office,\nthe Max-Planck Society and its participating institutes, the\nMax Planck Institute for Astronomy, Heidelberg and the Max\nPlanck Institute for Extraterrestrial Physics, Garching, The\nJohns Hopkins University, Durham University, the University\nof Edinburgh, Queen's University Belfast, the Harvard-\nSmithsonian Center for Astrophysics, the Las Cumbres\nObservatory Global Telescope Network Incorporated, the\nNational Central University of Taiwan, the Space Telescope\nScience Institute, the National Aeronautics and Space\nAdministration under Grant No. NNX08AR22G issued through\nthe Planetary Science Division of the NASA Science Mission\nDirectorate, the National Science Foundation under Grant No.\nAST-1238877, the University of Maryland, and Eotvos Lorand\nUniversity (ELTE) and the Los Alamos National Laboratory.\nBased on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by Subaru Telescope and Astronomy Data Center at National Astronomical Observatory of Japan. \n\nThis work is supported in part by JSPS KAKENHI\n(Grant Number JP 15H03654) as well as MEXT Grant-in-\nAid for Scientific Research on Innovative Areas (15H05887,\n15H05892, 15H05893, 15K21733).\n\nAccepted Version - 1704.05858.pdf
", "abstract": "Hyper Suprime-Cam (HSC) is a wide-field imaging camera on the prime focus of the 8.2-m Subaru telescope on the summit of Mauna Kea in Hawaii. A team of scientists from Japan, Taiwan, and Princeton University is using HSC to carry out a 300-night multi-band imaging survey of the high-latitude sky. The survey includes three layers: the Wide layer will cover 1400\u2009deg^2 in five broad bands (grizy), with a 5\u2009\u03c3 point-source depth of r \u2248 26. The Deep layer covers a total of 26\u2009deg^2 in four fields, going roughly a magnitude fainter, while the UltraDeep layer goes almost a magnitude fainter still in two pointings of HSC (a total of 3.5\u2009deg^2). Here we describe the instrument, the science goals of the survey, and the survey strategy and data processing. This paper serves as an introduction to a special issue of the Publications of the Astronomical Society of Japan, which includes a large number of technical and scientific papers describing results from the early phases of this survey.", "date": "2018-01", "date_type": "published", "publication": "Publications of the Astronomical Society of Japan", "volume": "70", "number": "SP1", "publisher": "Astronomical Society of Japan", "pagerange": "Art. No. S4", "id_number": "CaltechAUTHORS:20180301-094420951", "issn": "0004-6264", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180301-094420951", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "NX08AR22G" }, { "agency": "NSF", "grant_number": "AST-1238877" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "JP 15H03654" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "15H05887" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "15H05892" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "15H05893" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "15K21733" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/pasj/psx066", "primary_object": { "basename": "1704.05858.pdf", "url": "https://authors.library.caltech.edu/records/k97b3-1t577/files/1704.05858.pdf" }, "pub_year": "2018", "author_list": "Aihara, Hiroaki and Capak, P." }, { "id": "https://authors.library.caltech.edu/records/z441s-gp578", "eprint_id": 78644, "eprint_status": "archive", "datestamp": "2023-08-19 06:48:24", "lastmod": "2023-10-26 00:15:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Stefanon-M", "name": { "family": "Stefanon", "given": "Mauro" }, "orcid": "0000-0001-7768-5309" }, { "id": "Labb\u00e9-I", "name": { "family": "Labb\u00e9", "given": "Ivo" }, "orcid": "0000-0002-2057-5376" }, { "id": "Bouwens-R-J", "name": { "family": "Bouwens", "given": "Rychard J." }, "orcid": "0000-0002-4989-2471" }, { "id": "Brammer-G-B", "name": { "family": "Brammer", "given": "Gabriel B." }, "orcid": "0000-0003-2680-005X" }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "Pascal" }, "orcid": "0000-0001-5851-6649" }, { "id": "Franx-M", "name": { "family": "Franx", "given": "Marijn" }, "orcid": "0000-0002-8871-3026" }, { "id": "Fynbo-J-P-U", "name": { "family": "Fynbo", "given": "Johan P. U." }, "orcid": "0000-0002-8149-8298" }, { "id": "Milvang-Jensen-B", "name": { "family": "Milvang-Jensen", "given": "Bo" }, "orcid": "0000-0002-2281-2785" }, { "id": "Muzzin-A", "name": { "family": "Muzzin", "given": "Adam" }, "orcid": "0000-0002-9330-9108" }, { "id": "Illingworth-G-D", "name": { "family": "Illingworth", "given": "Garth D." }, "orcid": "0000-0002-6668-2011" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "Olivier" }, "orcid": "0000-0001-5891-2596" }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "Karina I." }, "orcid": "0000-0001-8183-1460" }, { "id": "Holwerda-B-W", "name": { "family": "Holwerda", "given": "Benne W." }, "orcid": "0000-0002-4884-6756" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "Henry J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Smit-Renske", "name": { "family": "Smit", "given": "Renske" }, "orcid": "0000-0001-8034-7802" }, { "id": "Magee-D", "name": { "family": "Magee", "given": "Dan" } } ] }, "title": "HST Imaging of the Brightest z ~ 8\u20139 Galaxies from UltraVISTA: The Extreme Bright End of the UV Luminosity Function", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: formation \u2013 galaxies: high-redshift \u2013 galaxies: luminosity function, mass function", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 June 14; revised 2017 November 8; accepted 2017 November 9; published 2017 December 11. \n\nThe authors would like to thank the referee for their careful reading of the manuscript and for providing constructive comments that helped improving the quality of the paper. M.S. would like to thank Pieter van Dokkum, Jorryt Matthee, and Corentin Schreiber for useful discussion. K.I.C. acknowledges funding from the European Research Council through the award of the Consolidator Grant ID 681627-BUILDUP. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO program ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based in part on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by Subaru Telescope and Astronomy Data Center at National Astronomical Observatory of Japan. The Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. This paper makes use of software developed for the Large Synoptic Survey Telescope. We thank the LSST Project for making their code available as free software at http://dm.lsst.org. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queens University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics, and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE) and the Los Alamos National Laboratory. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada\u2013France\u2013Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada\u2013France\u2013Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. This research has made use of the NASA/ IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has benefited from the SpeX Prism Spectral Libraries, maintained by Adam Burgasser at http://pono.ucsd.edu/~adam/browndwarfs/spexprism.\n\nSubmitted - 1706.04613.pdf
", "abstract": "We report on the discovery of three especially bright candidate z_(phot) \u2273 8 galaxies. Five sources were targeted for follow-up with the Hubble Space Telescope (HST)/Wide Field Camera 3 (WFC3), selected from a larger sample of 16 bright (24.8 \u227e H \u227e 25.5 mag) candidate z \u2273 8 Lyman break galaxies (LBGs) identified over 1.6 degrees^2 of the COSMOS/UltraVISTA field. These were selected as Y and J dropouts by leveraging the deep (Y-to-K_s ~ 25.3-24.8 mag, 5\u03c3) NIR data from the UltraVISTA DR3 release, deep ground-based optical imaging from the CFHTLS and Suprime-Cam programs, and Spitzer/IRAC mosaics combining observations from the SMUVS and SPLASH programs. Through the refined spectral energy distributions, which now also include new HyperSuprimeCam g-, r-, i-, z-, and Y-band data, we confirm that 3/5 galaxies have robust z_(phot) ~ 8.0-8.7, consistent with the initial selection. The remaining 2/5 galaxies have a nominal z_(phot) ~ 2. However, with HST data alone, these objects have increased probability of being at z ~ 9. We measure mean UV continuum slopes \u03b2 = -1.74 \u00b1 0.35 for the three z ~ 8-9 galaxies, marginally bluer than similarly luminous z ~ 4-6 in CANDELS but consistent with previous measurements of similarly luminous galaxies at z ~ 7. The circularized effective radius for our brightest source is 0.9 \u00b1 0.3 kpc, similar to previous measurements for a bright z ~ 11 galaxy and bright z ~ 7 galaxies. Finally, enlarging our sample to include the six brightest z ~ 8 LBGs identified over UltraVISTA (i.e., including three other sources from Labb\u00e9 et al.) we estimate for the first time the volume density of galaxies at the extreme bright end (M_(UV) ~ -22 mag) of the z ~ 8 UV luminosity function. Despite this exceptional result, the still large statistical uncertainties do not allow us to discriminate between a Schechter and a double-power-law form.", "date": "2017-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "851", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 43", "id_number": "CaltechAUTHORS:20170628-104503624", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170628-104503624", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "SPLASH" }, { "id": "COSMOS" } ] }, "doi": "10.3847/1538-4357/aa9a40", "primary_object": { "basename": "1706.04613.pdf", "url": "https://authors.library.caltech.edu/records/z441s-gp578/files/1706.04613.pdf" }, "pub_year": "2017", "author_list": "Stefanon, Mauro; Labb\u00e9, Ivo; et el." }, { "id": "https://authors.library.caltech.edu/records/0mfqd-evs60", "eprint_id": 83601, "eprint_status": "archive", "datestamp": "2023-08-19 06:27:56", "lastmod": "2023-10-17 23:15:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jones-G-C", "name": { "family": "Jones", "given": "G. C." }, "orcid": "0000-0002-0267-9024" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Shao-Y", "name": { "family": "Shao", "given": "Y." } }, { "id": "Wang-R", "name": { "family": "Wang", "given": "R." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Pavesi-R", "name": { "family": "Pavesi", "given": "R." }, "orcid": "0000-0002-2263-646X" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D. A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Neeleman-M", "name": { "family": "Neeleman", "given": "M." }, "orcid": "0000-0002-9838-8191" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "F." }, "orcid": "0000-0003-4793-7880" } ] }, "title": "Dynamical Characterization of Galaxies at z \u223c 4\u20136 via Tilted Ring Fitting to ALMA [C II] Observations", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift \u2013 galaxies: kinematics and dynamics", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 May 23; revised 2017 September 7; accepted 2017 September 14; published 2017 November 30. \n\nThis work makes use of the following ALMA data: 2011.0.00206.S, 2012.1.00240.S, 2012.1.00523.S, 2012.1.00978.S, and 2015.1.01564.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. G.J. is grateful for support from NRAO through the Grote Reber Doctoral Fellowship Program. Y.S. acknowledges support from the China Scholarship Council. R.W. acknowledges support from the National Key Research and Development Program of China (2016YFA0400703), the Thousand Youth Talents Program of China, and the National Science Foundation of China (NSFC) grant No. 11473004. D.R. and R.P. acknowledge support from the National Science Foundation under grant number AST-1614213 to Cornell University. R.P. acknowledges support through award SOSPA3-008 from the NRAO. A.K. acknowledges support by the Collaborative Research Center 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG).\n\nPublished - Jones_2017_ApJ_850_180.pdf
Submitted - 1709.04954.pdf
", "abstract": "Until recently, determining the rotational properties of galaxies in the early universe (z > 4, universe age <1.5 Gyr) was impractical, with the exception of a few strongly lensed systems. Combining the high resolution and sensitivity of ALMA at (sub-)millimeter wavelengths with the typically high strength of the [C II] 158 \u03bcm emission line from galaxies and long-developed dynamical modeling tools raises the possibility of characterizing the gas dynamics in both extreme starburst galaxies and normal star-forming disk galaxies at z ~ 4-7. Using a procedure centered around GIPSY's ROTCUR task, we have fit tilted ring models to some of the best available ALMA [C II] data of a small set of galaxies: the MS galaxies HZ9 and HZ10, the damped Ly\u03b1 absorber host galaxy ALMA J0817+1351, the submm galaxies AzTEC/C159 and COSMOS J1000+0234, and the quasar host galaxy ULAS J1319+0950. This procedure directly derives rotation curves and dynamical masses as functions of radius for each object. In one case, we present evidence for a dark matter halo of O(10^(11))M\u2299. We present an analysis of the possible velocity dispersions of two sources based on matching simulated observations to the integrated [C II] line profiles. Finally, we test the effects of observation resolution and sensitivity on our results. While the conclusions remain limited at the resolution and signal-to-noise ratios of these observations, the results demonstrate the viability of the modeling tools at high redshift, and the exciting potential for detailed dynamical analysis of the earliest galaxies, as ALMA achieves full observational capabilities.", "date": "2017-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "850", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 180", "id_number": "CaltechAUTHORS:20171130-124108209", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171130-124108209", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Radio Astronomy Observatory" }, { "agency": "China Scholarship Council" }, { "agency": "National Key Research and Development Program of China", "grant_number": "2016YFA0400703" }, { "agency": "Thousand Youth Talents Program of China" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11473004" }, { "agency": "NSF", "grant_number": "AST-1614213" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "956" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/aa8df2", "primary_object": { "basename": "1709.04954.pdf", "url": "https://authors.library.caltech.edu/records/0mfqd-evs60/files/1709.04954.pdf" }, "related_objects": [ { "basename": "Jones_2017_ApJ_850_180.pdf", "url": "https://authors.library.caltech.edu/records/0mfqd-evs60/files/Jones_2017_ApJ_850_180.pdf" } ], "pub_year": "2017", "author_list": "Jones, G. C.; Carilli, C. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/sd3sx-ggq65", "eprint_id": 83792, "eprint_status": "archive", "datestamp": "2023-08-19 06:20:12", "lastmod": "2023-10-17 23:30:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Hemmati-S", "name": { "family": "Hemmati", "given": "Shoubaneh" }, "orcid": "0000-0003-2226-5395" } ] }, "title": "Scientific Synergy between LSST and Euclid", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmological parameters \u2013 cosmology: dark energy \u2013 galaxies: clusters: general \u2013 gravitational lensing:\nweak \u2013 surveys \u2013 telescopes", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 July 31; revised 2017 October 17; accepted 2017 October 18; published 2017 December 7. \n\nJ.R. and A.K. were supported by JPL, which is run under a contract for NASA by Caltech. J.R., A.K., P.C., R.B., R.L., and R. Mandelbaum were supported in part by NASA ROSES grant 12-EUCLID12-0004. A.N.T. is supported by a UK Space Agency Euclid grant and a Royal Society Wolfson Research Merit Award. Y.M. was supported by the French CNES Space Agency and Institut National des Sciences de l'Univers of CNRS. T.S. acknowledges travel support from the German Federal Ministry for Economic Affairs and Energy (BMWi) provided via DLR under project No. 50QE1103. T.K. is supported by a Royal Society University Research Fellowship. V.F.C. is funded by the Italian Space Agency (ASI) through contract Euclid\u2014IC (I/031/10/0) and acknowledges financial contribution from the agreement ASI/INAF/I/023/12/0. R. Massey acknowledges support from UK STFC grant ST/N001494/1. B.N. is supported by a UK Space Agency Euclid grant. This paper benefited from ideas developed in the UK Dark Energy Strategy 2020 Document.(37) We thank Michael Brown, Elisa Chisari, Henk Hoekstra, \u017deljko Ivezi\u0107 Bhuvnesh Jain, Roberto Scaramella, and Peter Schneider for useful feedback on this paper. We thank Katrin Heitmann for useful discussions on high-performance computing. We thank the anonymous referee for useful suggestions on adding quantitative rigor to sections of this paper and useful feedback on the structure of the paper.\n\nPublished - Rhodes_2017_ApJS_233_21.pdf
Submitted - 1710.08489.pdf
", "abstract": "Euclid and the Large Synoptic Survey Telescope (LSST) are poised to dramatically change the astronomy landscape early in the next decade. The combination of high-cadence, deep, wide-field optical photometry from LSST with high-resolution, wide-field optical photometry, and near-infrared photometry and spectroscopy from Euclid will be powerful for addressing a wide range of astrophysical questions. We explore Euclid/LSST synergy, ignoring the political issues associated with data access to focus on the scientific, technical, and financial benefits of coordination. We focus primarily on dark energy cosmology, but also discuss galaxy evolution, transient objects, solar system science, and galaxy cluster studies. We concentrate on synergies that require coordination in cadence or survey overlap, or would benefit from pixel-level co-processing that is beyond the scope of what is currently planned, rather than scientific programs that could be accomplished only at the catalog level without coordination in data processing or survey strategies. We provide two quantitative examples of scientific synergies: the decrease in photo-z errors (benefiting many science cases) when high-resolution Euclid data are used for LSST photo-z determination, and the resulting increase in weak-lensing signal-to-noise ratio from smaller photo-z errors. We briefly discuss other areas of coordination, including high-performance computing resources and calibration data. Finally, we address concerns about the loss of independence and potential cross-checks between the two missions and the potential consequences of not collaborating.", "date": "2017-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "233", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 21", "id_number": "CaltechAUTHORS:20171211-101259862", "issn": "1538-4365", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171211-101259862", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "12-EUCLID12-0004" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Royal Society" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Bundesministerium f\u00fcr Wirtschaft und Energie (BMWi)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50QE1103" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/031/10/0" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/023/12/0" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/N001494/1" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4365/aa96b0", "primary_object": { "basename": "1710.08489.pdf", "url": "https://authors.library.caltech.edu/records/sd3sx-ggq65/files/1710.08489.pdf" }, "related_objects": [ { "basename": "Rhodes_2017_ApJS_233_21.pdf", "url": "https://authors.library.caltech.edu/records/sd3sx-ggq65/files/Rhodes_2017_ApJS_233_21.pdf" } ], "pub_year": "2017", "author_list": "Rhodes, Jason; Capak, Peter; et el." }, { "id": "https://authors.library.caltech.edu/records/w44s8-vjp90", "eprint_id": 84000, "eprint_status": "archive", "datestamp": "2023-08-19 06:20:58", "lastmod": "2023-10-18 14:35:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brisbin-D", "name": { "family": "Brisbin", "given": "Drew" }, "orcid": "0000-0002-4795-419X" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" } ] }, "title": "An ALMA survey of submillimeter galaxies in the COSMOS field: Multiwavelength counterparts and redshift distribution", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: distances and redshifts \u2013 galaxies: evolution \u2013 galaxies: statistics \u2013 galaxies: high-redshift \u2013 catalogs", "note": "\u00a9 2017 ESO. Article published by EDP Sciences. \n\nReceived 3 February 2017; Accepted 21 August 2017; Published online 29 November 2017. \n\nWe thank the anonymous referee for insightful comments and advice. D.B. acknowledges partial support from ALMA-CONICYT FUND No. 31140010. and FONDECYT postdoctorado project 3170974. M.A. acknowledges partial support from FONDECYT through grant 1140099. V.S., O.M. and I.D. acknowledge funding from the European Union's Seventh Framework program under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). The work of O.M. was performed in part at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1066293. The work of O.M. was partially supported by a grant from the Simons Foundation. A.K. acknowledges support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). C.M.C. thanks UT Austin's college of natural science for support. D.R. acknowledges support from the National Science Foundation under grant number AST-1614213 to Cornell University. C.J. acknowledges support from Shanghai Municipal Natural Science Foundation (grant 15ZR1446600) The Flatiron Institute is supported by the Simons Foundation. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00118.S and 2011.0.00539.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This research has made use of data from HerMES project (http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists and a mission scientist. HerMES is described in Oliver et al. (2012).\n\nPublished - aa30558-17.pdf
Submitted - 1708.05748.pdf
", "abstract": "We carried out targeted ALMA observations of 129 fields in the COSMOS region at 1.25 mm, detecting 152 galaxies at S/N \u2265 5with an average continuum RMS of 150 \u03bcJy. These fields represent a S/N-limited sample of AzTEC/ASTE sources with 1.1 mm S/N\u2265 4 over an area of 0.72 square degrees. Given ALMA's fine resolution and the exceptional spectroscopic and multiwavelength photometric data available in COSMOS, this survey allows us unprecedented power in identifying submillimeter galaxy counterparts and determining their redshifts through spectroscopic or photometric means. In addition to 30 sources with prior spectroscopic redshifts, we identified redshifts for 113 galaxies through photometric methods and an additional nine sources with lower limits, which allowed a statistically robust determination of the redshift distribution. We have resolved 33 AzTEC sources into multi-component systems and our redshifts suggest that nine are likely to be physically associated. Our overall redshift distribution peaks at z ~ 2.0 with a high-redshift tail skewing the median redshift to z = 2.48\u2009\u00b1\u20090.05. We find that brighter millimeter sources are preferentially found at higher redshifts. Our faintestsources, with S_(1.25 mm) < 1.25 mJy, have a median redshift of z = 2.18\u2009\u00b1\u20090.09, while the brightest sources, S_(1.25 mm) > 1.8 mJy, have a median redshift of z = 3.08\u2009\u00b1\u20090.17. After accounting for spectral energy distribution shape and selection effects, these results are consistent with several previous submillimeter galaxy surveys, and moreover, support the conclusion that the submillimeter galaxy redshift distribution is sensitive to survey depth.", "date": "2017-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "608", "publisher": "EDP Sciences", "pagerange": "Art. No. A15", "id_number": "CaltechAUTHORS:20171221-075735416", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171221-075735416", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "31140010" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "3170974" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1140099" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "Simons Foundation" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "956" }, { "agency": "University of Texas at Austin" }, { "agency": "NSF", "grant_number": "AST-1614213" }, { "agency": "Shanghai Municipal Natural Science Foundation", "grant_number": "15ZR1446600" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201730558", "primary_object": { "basename": "1708.05748.pdf", "url": "https://authors.library.caltech.edu/records/w44s8-vjp90/files/1708.05748.pdf" }, "related_objects": [ { "basename": "aa30558-17.pdf", "url": "https://authors.library.caltech.edu/records/w44s8-vjp90/files/aa30558-17.pdf" } ], "pub_year": "2017", "author_list": "Brisbin, Drew and Capak, Peter" }, { "id": "https://authors.library.caltech.edu/records/zj8bz-c3474", "eprint_id": 83995, "eprint_status": "archive", "datestamp": "2023-08-19 05:51:08", "lastmod": "2023-10-18 14:35:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Herrera-Ruiz-N", "name": { "family": "Herrera Ruiz", "given": "N." } }, { "id": "Middelberg-E", "name": { "family": "Middelberg", "given": "E." } }, { "id": "Deller-A-T", "name": { "family": "Deller", "given": "A." }, "orcid": "0000-0001-9434-3837" }, { "id": "Norris-R-P", "name": { "family": "Norris", "given": "R. P." }, "orcid": "0000-0002-4597-1906" }, { "id": "Best-P-N", "name": { "family": "Best", "given": "P. N." } }, { "id": "Brisken-W-F", "name": { "family": "Brisken", "given": "W." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Delvecchio-I", "name": { "family": "Delvecchio", "given": "I." }, "orcid": "0000-0001-8706-2252" }, { "id": "Momjian-E", "name": { "family": "Momjian", "given": "E." }, "orcid": "0000-0003-3168-5922" }, { "id": "Bomans-D", "name": { "family": "Bomans", "given": "D." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C." }, "orcid": "0000-0001-6647-3861" } ] }, "title": "The faint radio sky: VLBA observations of the COSMOS field", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs \u2013 galaxies: active \u2013 radio continuum: galaxies", "note": "\u00a9 ESO, 2017. \n\nReceived 12 May 2017; Accepted 13 July 2017; Published online 28 November 2017.\n\nThe full Tables 2 and 3 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/607/A132.\n \n\nN.H.R. acknowledges support from the Deutsche Forschungsgemeinschaft through project MI 1230/4-1. V.S. and I.D. acknowledge the European Union's Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). P.N.B. is grateful for support from STFC via grant ST/M001229/1. We wish to thank the anonymous referee for the helpful comments, which have improved this paper. This research made use of Topcat (Taylor 2005), available at http://www.starlink.ac.uk/topcat/. This research also made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com, and Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013). We wish to thank the staff of the VLBA who greatly supported the experimental observations in this project. The VLBA is operated by the Long Baseline Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nPublished - aa31163-17.pdf
Submitted - 1707.07512.pdf
", "abstract": "Context. Quantifying the fraction of active galactic nuclei (AGN) in the faint radio population and understanding their relation with star-forming activity are fundamental to studies of galaxy evolution. Very long baseline interferometry (VLBI) observations are able to identify AGN above relatively low redshifts (z> 0.1) since they provide milli-arcsecond resolution. \n\nAims. We have created an AGN catalogue from 2865 known radio sources observed in the Cosmic Evolution Survey (COSMOS) field, which has exceptional multi-wavelength coverage. With this catalogue we intend to study the faint radio sky with statistically relevant numbers and to analyse the AGN \u2013 host galaxy co-evolution, making use of the large amount of ancillary data available in the field. \n\nMethods. Wide-field VLBI observations were made of all known radio sources in the COSMOS field at 1.4 GHz to measure the AGN fraction, in particular in the faint radio population. We describe in detail the observations, data calibration, source detection and flux density measurements, parts of which we have developed for this survey. The combination of number of sources, sensitivity, and area covered with this project are unprecedented. \n\nResults. We have detected 468 radio sources, expected to be AGN, with the Very Long Baseline Array (VLBA). This is, to date, the largest sample assembled of VLBI detected sources in the sub-mJy regime. The input sample was taken from previous observations with the Very Large Array (VLA). We present the catalogue with additional optical, infrared and X-ray information. \n\nConclusions. We find a detection fraction of 20 \u00b1 1%, considering only those sources from the input catalogue which were in principle detectable with the VLBA (2361). As a function of the VLA flux density, the detection fraction is higher for higher flux densities, since at high flux densities a source could be detected even if the VLBI core accounts for a small percentage of the total flux density. As a function of redshift, we see no evolution of the detection fraction over the redshift range 0.5 1.5 we find that spiral galaxies become the most prevalent (48%). The number of detections is high enough to study the faint radio population with statistically significant numbers. We demonstrate that wide-field VLBI observations, together with new calibration methods such as multi-source self-calibration and mosaicing, result in information which is difficult or impossible to obtain otherwise.", "date": "2017-11", "date_type": "published", "publication": "Astronomy & Astrophysics", "volume": "607", "publisher": "EDP Sciences", "pagerange": "Art. No. A132", "id_number": "CaltechAUTHORS:20171220-145748048", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171220-145748048", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "MI 1230/4-1" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/M001229/1" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1051/0004-6361/201731163", "primary_object": { "basename": "1707.07512.pdf", "url": "https://authors.library.caltech.edu/records/zj8bz-c3474/files/1707.07512.pdf" }, "related_objects": [ { "basename": "aa31163-17.pdf", "url": "https://authors.library.caltech.edu/records/zj8bz-c3474/files/aa31163-17.pdf" } ], "pub_year": "2017", "author_list": "Herrera Ruiz, N.; Middelberg, E.; et el." }, { "id": "https://authors.library.caltech.edu/records/d9bwg-chz79", "eprint_id": 82724, "eprint_status": "archive", "datestamp": "2023-08-19 05:22:01", "lastmod": "2023-10-17 22:37:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Miettinen-O", "name": { "family": "Miettinen", "given": "O." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "An ALMA survey of submillimetre galaxies in the COSMOS field: Physical properties derived from energy balance spectral energy distribution modelling", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: formation \u2013 galaxies: starburst \u2013 galaxies: star formation \u2013 submillimeter: galaxies", "note": "\u00a9 2017 ESO. Article published by EDP Sciences.\n\nReceived 10 March 2017; Accepted 27 June 2017; Published online 28 September 2017. \n\nWe would like to thank the anonymous referee for providing comments and suggestions. This research was funded by the European Union's Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). M.A. acknowledges partial support from FONDE-CYT through grant 1140099. A.K. acknowledges support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). E.S. acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No. 694343). D.R. acknowledges support from the National Science Foundation under grant number AST-1614213 to Cornell University.\n\nThis work was performed in part at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1066293. This work was partially supported by a grant from the Simons Foundation. The Flatiron Institute is supported by the Simons Foundation. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2012.1.00978.S and ADS/JAO.ALMA#2013.1.00118.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This paper is also partly based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This research has made use of NASA's Astrophysics Data System, and the NASA/IPAC Infrared Science Archive, which is operated by the JPL, California Institute of Technology, under contract with the NASA. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013). We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information on the COSMOS survey is available at http://cosmos.astro.caltech.edu.\n\nPACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). \n\nSPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (PR China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (PR China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).\n\nPublished - aa30762-17.pdf
Submitted - 1707.00637.pdf
", "abstract": "Context. Submillimetre galaxies (SMGs) represent an important source population in the origin and cosmic evolution of the most massive galaxies. Hence, it is imperative to place firm constraints on the fundamental physical properties of large samples of SMGs.\nAims. We determine the physical properties of a sample of SMGs in the COSMOS field that were pre-selected at the observed-frame wavelength of \u03bb_(obs) = 1.1 mm, and followed up at \u03bb_(obs) = 1.3 mm with the Atacama Large Millimetre/submillimetre Array (ALMA).\nMethods. We used the MAGPHYS model package to fit the panchromatic (ultraviolet to radio) spectral energy distributions (SEDs) of 124 of the target SMGs, which lie at a median redshift of z = 2.30 (19.4% are spectroscopically confirmed). The SED analysis was complemented by estimating the gas masses of the SMGs by using the \u03bb_(obs) = 1.3 mm dust emission as a tracer of the molecular gas component.\nResults. The sample median and 16th\u201384th percentile ranges of the stellar masses, obscured star formation rates, dust temperatures, and dust and gas masses were derived to be log(M\u22c6/M\u2299)\u202f=\u202f11.09^(+0.41)_(-0.53), SFR\u202f=\u202f402^(+661)_(-233) M\u2299 yr^(-1), T_(dust)\u202f=\u202f39.7^(+9.7)_(-7.4) K, log(M_(dust)/M\u2299)\u202f=\u202f9.01^(+0.20)_(-0.31), and log(M_(gas)/M\u2299\u202f=\u202f11.34^(+0.20)_(-0.23), respectively. The M_(dust)/M\u22c6 ratio was found to decrease as a function of redshift, while the M_(gas)/M_(dust) ratio shows the opposite, positive correlation with redshift. The derived median gas-to-dust ratio of 120^(+73)_(-30) agrees well with the canonical expectation. The gas fraction (M_(gas)/(M_(gas) + M\u22c6)) was found to range from 0.10 to 0.98 with a median of 0.62^(+0.27)_(-0.23). We found that 57.3% of our SMGs populate the main sequence (MS) of star-forming galaxies, while 41.9% of the sources lie above the MS by a factor of greater than three (one source lies below the MS). These super-MS objects, or starbursts, are preferentially found at z \u2273 3, which likely reflects the sensitivity limit of our source selection. We estimated that the median gas consumption timescale for our SMGs is ~535 Myr, and the super-MS sources appear to consume their gas reservoir faster than their MS counterparts. We found no obvious stellar mass\u2013size correlations for our SMGs, where the sizes were measured in the observed-frame 3 GHz radio emission and rest-frame UV. However, the largest 3 GHz radio sizes are found among the MS sources. Those SMGs that appear irregular in the rest-frame UV are predominantly starbursts, while the MS SMGs are mostly disk-like.\nConclusions. The physical parameter distributions of our SMGs and those of the equally bright, 870 \u03bcm selected SMGs in the ECDFS field (the so-called ALESS SMGs) are unlikely to be drawn from common parent distributions. This might reflect the difference in the pre-selection wavelength. Albeit being partly a selection bias, the abrupt jump in specific SFR and the offset from the MS of our SMGs at z \u2273 3 might also reflect a more efficient accretion from the cosmic gas streams, higher incidence of gas-rich major mergers, or higher star formation efficiency at z \u2273 3. We found a rather flat average trend between the SFR and dust mass, but a positive SFR\u2212M_(gas) correlation. However, to address the questions of which star formation law(s) our SMGs follow, and how they compare with the Kennicutt-Schmidt law, the dust-emitting sizes of our sources need to be measured. Nonetheless, the larger radio-emitting sizes of the MS SMGs compared to starbursts is a likely indication of their more widespread, less intense star formation activity. The irregular rest-frame UV morphologies of the starburst SMGs are likely to echo their merger nature. The current stellar mass content of the studied SMGs is very high, so they must quench to form the so-called red-and-dead massive ellipticals. Our results suggest that the transition from high-z SMGs to local ellipticals via compact, quiescent galaxies (cQGs) at z ~ 2 might not be universal, and the latter population might also descend from the so-called blue nuggets. However, z \u2273 4 SMGs could be the progenitors of higher redshift, z \u2273 3 cQGs, while our results are also consistent with the possibility that ultra-massive early-type galaxies found at 1.2 \u2272 z \u2272 2 experienced an SMG phase at z \u2264 3.", "date": "2017-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "606", "publisher": "EDP Sciences", "pagerange": "Art. No. A17", "id_number": "CaltechAUTHORS:20171027-081208066", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171027-081208066", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1140099" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "956" }, { "agency": "European Research Council (ERC)", "grant_number": "694343" }, { "agency": "NSF", "grant_number": "AST-1614213" }, { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "Simons Foundation" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201730762", "primary_object": { "basename": "1707.00637.pdf", "url": "https://authors.library.caltech.edu/records/d9bwg-chz79/files/1707.00637.pdf" }, "related_objects": [ { "basename": "aa30762-17.pdf", "url": "https://authors.library.caltech.edu/records/d9bwg-chz79/files/aa30762-17.pdf" } ], "pub_year": "2017", "author_list": "Miettinen, O. and Capak, P. L." }, { "id": "https://authors.library.caltech.edu/records/mgfk8-s2835", "eprint_id": 78660, "eprint_status": "archive", "datestamp": "2023-08-19 05:11:53", "lastmod": "2023-10-26 00:16:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Andrews-S-K", "name": { "family": "Andrews", "given": "S. K." } }, { "id": "Driver-S-P", "name": { "family": "Driver", "given": "S. P." } }, { "id": "Davies-L-J-M", "name": { "family": "Davies", "given": "L. J. M." } }, { "id": "Kafle-P-R", "name": { "family": "Kafle", "given": "Prajwal R." } }, { "id": "Robotham-A-S-G", "name": { "family": "Robotham", "given": "Aaron S. G." } }, { "id": "Wright-A-H", "name": { "family": "Wright", "given": "Angus H." } } ] }, "title": "G10/COSMOS: 38 band (far-UV to far-IR) panchromatic photometry using LAMBDAR", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 September 21. Received 2016 September 16; in original form 2016 April 21.", "abstract": "We present a consistent total flux catalogue for a \u223c1 deg2 subset of the Cosmic Evolution Survey (COSMOS) region (RA \u2208 [149\n\u2218.\n.\u2218\n \n55,\u2009150\n\u2218.\n.\u2218\n \n65], Dec. \u2208 [1\n\u2218.\n.\u2218\n \n80,\u20092\n\u2218.\n.\u2218\n \n73]) with near-complete coverage in 38 bands from the far-ultraviolet to the far-infrared. We produce aperture matched photometry for 128 304 objects with i < 24.5 in a manner that is equivalent to the Wright et al. catalogue from the low-redshift (z < 0.4) Galaxy and Mass Assembly (GAMA) survey. This catalogue is based on publicly available imaging from GALEX, Canada\u2013France\u2013Hawaii Telescope, Subaru, Visible and Infrared Survey Telescope for Astronomy, Spitzer and Herschel, contains a robust total flux measurement or upper limit for every object in every waveband and complements our re-reduction of publicly available spectra in the same region. We perform a number of consistency checks, demonstrating that our catalogue is comparable to existing data sets, including the recent COSMOS2015 catalogue. We also release an updated Davies et al. spectroscopic catalogue that folds in new spectroscopic and photometric redshift data sets. The catalogues are available for download at http://cutout.icrar.org/G10/dataRelease.php. Our analysis is optimised for both panchromatic analysis over the full wavelength range and for direct comparison to GAMA, thus permitting measurements of galaxy evolution for 0 < z < 1 while minimizing the systematic error resulting from disparate data reduction methods.", "date": "2017-09-22", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "464", "number": "2", "publisher": "Oxford University Press", "pagerange": "1569-1590", "id_number": "CaltechAUTHORS:20170628-135713279", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170628-135713279", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "SPLASH" }, { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stw2395", "pub_year": "2017", "author_list": "Andrews, S. K.; Driver, S. P.; et el." }, { "id": "https://authors.library.caltech.edu/records/1j6hk-d5s33", "eprint_id": 78661, "eprint_status": "archive", "datestamp": "2023-08-19 04:51:07", "lastmod": "2023-10-26 00:16:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Davidzon-I", "name": { "family": "Davidzon", "given": "I." }, "orcid": "0000-0002-2951-7519" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "C." } }, { "id": "Coupon-J", "name": { "family": "Coupon", "given": "J." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Delvecchio-I", "name": { "family": "Delvecchio", "given": "I." }, "orcid": "0000-0001-8706-2252" }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "D." }, "orcid": "0000-0001-5382-6138" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Hsieh-Bau-Ching", "name": { "family": "Hsieh", "given": "B. C." }, "orcid": "0000-0001-5615-4904" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "B\u00e9thermin-Matthieu", "name": { "family": "B\u00e9thermin", "given": "M." }, "orcid": "0000-0002-3915-2015" }, { "id": "Chang-Yen-Yung", "name": { "family": "Chang", "given": "Y.-Y." }, "orcid": "0000-0002-6441-980X" }, { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "A. L." }, "orcid": "0000-0002-9382-9832" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Steinhardt-C-L", "name": { "family": "Steinhardt", "given": "C." }, "orcid": "0000-0003-3780-6801" }, { "id": "Toft-S", "name": { "family": "Toft", "given": "S." }, "orcid": "0000-0003-3631-7176" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Dubois-C", "name": { "family": "Dubois", "given": "C." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" } ] }, "title": "The COSMOS2015 galaxy stellar mass function: Thirteen billion years of stellar mass assembly in ten snapshots", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: luminosity function, mass function \u2013 galaxies: statistics \u2013 galaxies: high-redshift", "note": "\u00a9 2017 ESO.\nArticle published by EDP Sciences.\n\nReceived 10 January 2017; Accepted 17 May 2017; Published online 12 September 2017.\n\nBased on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium (http://ultravista.org/). Based on data produced by the SPLASH team from observations made with the Spitzer Space Telescope (http://splash.caltech.edu).\n\nThe authors warmly thank the anonymous referee for her/his constructive comments. The authors thank Shoubaneh Hemmati and Hooshang Nayyeri for providing us with the CANDELS Multiwavelength Catalog in the COSMOS field, and Andrea Grazian and Thibault Garel for sending their results in a convenient digitalised format. I.D. thanks Marta Volonteri, Jeremy Blaizot, Yohan Dubois, Andrea Grazian, Roberto Maiolino for very useful discussions. I.D. and O.I. acknowledge funding of the French Agence Nationale de la Recherche for the SAGACE project. C.L. acknowledges support from a Beecroft fellowship. I.D. acknowledges the European Union's Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). A.F. acknowledges support from the Swiss National Science Foundation. The COSMOS team in France acknowledges support from the Centre National d'\u00c9tudes Spatiales.\n\nPublished - aa30419-17.pdf
Submitted - 1701.02734.pdf
", "abstract": "We measure the stellar mass function (SMF) and stellar mass density of galaxies in the COSMOS field up to z ~ 6. We select them in the near-IR bands of the COSMOS2015 catalogue, which includes ultra-deep photometry from UltraVISTA-DR2, SPLASH, and Subaru/Hyper Suprime-Cam. At z > 2.5 we use new precise photometric redshifts with error \u03c3_z = 0.03(1 + z) and an outlier fraction of 12%, estimated by means of the unique spectroscopic sample of COSMOS (~100 000 spectroscopic measurements in total, more than one thousand having robust z_(spec)> 2.5). The increased exposure time in the DR2, along with our panchromatic detection strategy, allow us to improve the completeness at high z with respect to previous UltraVISTA catalogues (e.g. our sample is >75% complete at 10^(10)M\u2299 and z = 5). We also identify passive galaxies through a robust colour\u2013colour selection, extending their SMF estimate up to z = 4. Our work provides a comprehensive view of galaxy-stellar-mass assembly between z = 0.1 and 6, for the first time using consistent estimates across the entire redshift range. We fit these measurements with a Schechter function, correcting for Eddington bias. We compare the SMF fit with the halo mass function predicted from \u039bCDM simulations, finding that at z > 3 both functions decline with a similar slope in thehigh-mass end. This feature could be explained assuming that mechanisms quenching star formation in massive haloes become less effective at high redshifts; however further work needs to be done to confirm this scenario. Concerning the SMF low-mass end, it shows a progressive steepening as it moves towards higher redshifts, with \u03b1 decreasing from -1.47^(+0.02)_(-0.02) at z \u2243 0.1 to -2.11^(+0.30)_(-0.13) at z \u2243 5. This slope depends on the characterisation of the observational uncertainties, which is crucial to properly remove the Eddington bias. We show that there is currently no consensus on the method to quantify such errors: different error models result in different best-fit Schechter parameters.", "date": "2017-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "605", "publisher": "EDP Sciences", "pagerange": "Art. No. A70", "id_number": "CaltechAUTHORS:20170628-140248161", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170628-140248161", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agence Nationale pour la Recherche (ANR)" }, { "agency": "Beecroft fellowship" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "SPLASH" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1051/0004-6361/201730419", "primary_object": { "basename": "1701.02734.pdf", "url": "https://authors.library.caltech.edu/records/1j6hk-d5s33/files/1701.02734.pdf" }, "related_objects": [ { "basename": "aa30419-17.pdf", "url": "https://authors.library.caltech.edu/records/1j6hk-d5s33/files/aa30419-17.pdf" } ], "pub_year": "2017", "author_list": "Davidzon, I.; Ilbert, O.; et el." }, { "id": "https://authors.library.caltech.edu/records/kp2vt-y5d15", "eprint_id": 80025, "eprint_status": "archive", "datestamp": "2023-08-21 21:34:32", "lastmod": "2023-10-26 17:31:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bari\u0161i\u0107-I", "name": { "family": "Barisic", "given": "Ivana" }, "orcid": "0000-0001-6371-6274" }, { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "A. L." }, "orcid": "0000-0002-9382-9832" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Pavesi-R", "name": { "family": "Pavesi", "given": "R." }, "orcid": "0000-0002-2263-646X" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D. A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Cooke-K-C", "name": { "family": "Cooke", "given": "K." }, "orcid": "0000-0002-2200-9845" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Casey-C-M", "name": { "family": "Casey", "given": "C. M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" } ] }, "title": "Dust Properties of C II Detected z \u223c 5.5 Galaxies: New HST/WFC3 Near-IR Observations", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: ISM", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 March 17; revised 2017 May 19; accepted 2017 July 6; published 2017 August 9. \n\nD.R. and R.P. acknowledge support from the National Science Foundation under grant number AST-1614213 to Cornell University. R.P. acknowledges support through award SOSPA3-008 from the NRAO. V.S. acknowledges support from the European Union's Seventh Frame-work program under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). Based on observations made with the NASA/ESA Hubble Space Telescope, obtained (from the Data Archive) at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program #13641 and #13384. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2012.1. 00523.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nPublished - Barisic_2017_ApJ_845_41.pdf
Submitted - 1707.02980.pdf
", "abstract": "We examine the rest-frame ultraviolet (UV) properties of 10 [C II]\u03bb158 \u03bcm-detected galaxies at z ~ 5.5 in COSMOS using new Hubble Space Telescope/Wide Field Camera 3 near-infrared imaging. Together with pre-existing 158 \u03bcm continuum and [C II] line measurements by the Atacama Large Millimeter/submillimeter Array, we study their dust attenuation properties on the IRX\u2013\u03b2 diagram, which connects the total dust emission (\u221d IRX = log(L_(FIR)/L_(1600)) to the line-of-sight dust column (\u221d \u03b2). We find systematically bluer UV continuum spectral slopes (\u03b2) compared to previous low-resolution ground-based measurements, which relieves some of the tension between models of dust attenuation and observations at high redshifts. While most of the galaxies are consistent with local starburst or Small Magellanic Cloud\u2013like dust properties, we find galaxies with low IRX values and a large range in \u03b2 that cannot be explained by models of a uniform dust distribution well mixed with stars. A stacking analysis of Keck/DEIMOS optical spectra indicates that these galaxies are metal-poor with young stellar populations that could significantly alter their spatial dust distribution.", "date": "2017-08-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "845", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 41", "id_number": "CaltechAUTHORS:20170809-140222043", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170809-140222043", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1614213" }, { "agency": "National Radio Astronomy Observatory (NRAO)", "grant_number": "SOSPA3-008" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aa7eda", "primary_object": { "basename": "1707.02980.pdf", "url": "https://authors.library.caltech.edu/records/kp2vt-y5d15/files/1707.02980.pdf" }, "related_objects": [ { "basename": "Barisic_2017_ApJ_845_41.pdf", "url": "https://authors.library.caltech.edu/records/kp2vt-y5d15/files/Barisic_2017_ApJ_845_41.pdf" } ], "pub_year": "2017", "author_list": "Barisic, Ivana; Faisst, A. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/k183n-p9236", "eprint_id": 78668, "eprint_status": "archive", "datestamp": "2023-08-19 04:02:13", "lastmod": "2023-10-26 00:17:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Stefanon-M", "name": { "family": "Stefanon", "given": "Mauro" }, "orcid": "0000-0001-7768-5309" }, { "id": "Bouwens-R-J", "name": { "family": "Bouwens", "given": "Rychard J." }, "orcid": "0000-0002-4989-2471" }, { "id": "Labb\u00e9-I", "name": { "family": "Labb\u00e9", "given": "Ivo" }, "orcid": "0000-0002-2057-5376" }, { "id": "Muzzin-A", "name": { "family": "Muzzin", "given": "Adam" }, "orcid": "0000-0002-9330-9108" }, { "id": "Marchesini-D", "name": { "family": "Marchesini", "given": "Danilo" }, "orcid": "0000-0001-9002-3502" }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "Pascal" }, "orcid": "0000-0001-5851-6649" }, { "id": "Gonzalez-V", "name": { "family": "Gonzalez", "given": "Valentino" }, "orcid": "0000-0002-3120-0510" } ] }, "title": "The rest-frame optical (900nm) galaxy luminosity function at z ~ 4-7: abundance matching points to limited evolution in the M_(STAR)/M_(HALO) ratio at z \u2a7e 4", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: formation \u2013 galaxies: high-redshift \u2013 galaxies: luminosity function, mass function", "note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2016 November 24; revised 2017 March 26; accepted 2017 May 10; published 2017 June 28.\n\nWe are appreciative to Adriano Fontana for a very helpful referee report that greatly improved this paper. M.S. would like to thank Adriano Fontana for constructive discussions. M.S. and R.B. are grateful to Karina Caputi, Yuichi Harikane, Michele Trenti, and Stuart Wyithe for helpful feedback on an advanced draft of this manuscript. This work is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory, under ESO programme ID 179.A-2005, and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is based on observations taken by the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.\n\nSubmitted - 1611.09354.pdf
", "abstract": "We present the first determination of the galaxy luminosity function (LF) at z ~ 4, 5, 6, and 7, in the rest-frame optical at \u03bb_(res) ~ 900 nm (z' band). The rest-frame optical light traces the content in low-mass evolved stars (~stellar mass\u2014M*), minimizing potential measurement biases for M*. Moreover, it is less affected by nebular line emission contamination and dust attenuation, is independent of stellar population models, and can be probed up to z ~ 8 through Spitzer/IRAC. Our analysis leverages the unique full-depth Spitzer/IRAC 3.6\u20138.0 \u03bcm data over the CANDELS/GOODS-N, CANDELS/GOODS-S, and COSMOS/UltraVISTA fields. We find that, at absolute magnitudes where M_z' is fainter than \u2273-23 mag, M_z' linearly correlates with M_(UV, 1600). At brighter M_z', M_(UV, 1600) presents a turnover, suggesting that the stellar mass-to-light ratio M*/L_(UV, 1600) could be characterized by a very broad range of values at high stellar masses. Median-stacking analyses recover an M*/L_z' roughly independent on M_z' for M_z' \u2273 -23 mag, but exponentially increasing at brighter magnitudes. We find that the evolution of the LF marginally prefers a pure luminosity evolution over a pure density evolution, with the characteristic luminosity decreasing by a factor of _5x between z ~ 4 and z ~ 7. Direct application of the recovered M*/L_z' generates stellar mass functions consistent with average measurements from the literature. Measurements of the stellar-to-halo mass ratio at fixed cumulative number density show that it is roughly constant with redshift for M_h \u2273 10^(12) M\u2299. This is also supported by the fact that the evolution of the LF at 4 \u227e z \u227e 7 can be accounted for by a rigid displacement in luminosity, corresponding to the evolution of the halo mass from abundance matching.", "date": "2017-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "843", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 36", "id_number": "CaltechAUTHORS:20170628-142531971", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170628-142531971", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "SPLASH" }, { "id": "COSMOS" } ] }, "doi": "10.3847/1538-4357/aa72d8", "primary_object": { "basename": "1611.09354.pdf", "url": "https://authors.library.caltech.edu/records/k183n-p9236/files/1611.09354.pdf" }, "pub_year": "2017", "author_list": "Stefanon, Mauro; Bouwens, Rychard J.; et el." }, { "id": "https://authors.library.caltech.edu/records/s9cqr-cdr50", "eprint_id": 78568, "eprint_status": "archive", "datestamp": "2023-08-19 03:53:22", "lastmod": "2023-10-26 00:11:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "name": { "family": "Micha\u0142owski", "given": "Micha\u0142 J." } }, { "name": { "family": "Dunlop", "given": "J. S." } }, { "name": { "family": "Koprowski", "given": "M. P." } }, { "name": { "family": "Cirasuolo", "given": "M." } }, { "name": { "family": "Geach", "given": "J. E." } }, { "name": { "family": "Bowler", "given": "R. A. A." } }, { "name": { "family": "Mortlock", "given": "A." } }, { "name": { "family": "Caputi", "given": "K. I." } }, { "name": { "family": "Aretxaga", "given": "I." } }, { "name": { "family": "Arumugam", "given": "V." } }, { "name": { "family": "Chen", "given": "Chian-Chou" } }, { "name": { "family": "McLure", "given": "R. J." } }, { "name": { "family": "Birkinshaw", "given": "M." } }, { "name": { "family": "Bourne", "given": "N." } }, { "name": { "family": "Farrah", "given": "D." } }, { "name": { "family": "Ibar", "given": "E." } }, { "name": { "family": "van der Werf", "given": "P." } }, { "name": { "family": "Zemcov", "given": "M." } } ] }, "title": "The SCUBA-2 Cosmology Legacy Survey: the nature of bright submm galaxies from 2 deg\u00b2 of 850-\u03bcm imaging", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nWe thank Joanna Baradziej, Ian Smail, James Simpson, and our anonymous referee for comments and suggestions.\n\nMJM acknowledges the support of the UK Science and Technology Facilities Council (STFC), British Council Researcher Links Travel Grant and the hospitality at the Instituto Nacional de Astrof\u00edsica, \u00d3ptica y Electr\u00f3nica. JSD acknowledges the support of the European Research Council via the award of an Advanced Grant, and the contribution of the EC FP7 SPACE project ASTRODEEP (ref. no: 312725). MPK acknowledges the STFC Studentship Enhancement Programme grant and the Carnegie Trust Research Incentive Grant (PI: Micha\u0142owski).\n\nThe James Clerk Maxwell Telescope has historically been operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the National Research Council of Canada and the Netherlands Organization for Scientific Research. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation.\n\nThis work is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory as part of programme ID 179.A-2005, using data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.\n\nThis study was based in part on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada\u2013France\u2013Hawaii Telescope (CFHT) that is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the CFHT Legacy Survey, a collaborative project of NRC and CNRS.\n\nThe National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nThis work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA.\n\nThis research has made use of data from HerMES project (http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists and a mission scientist. The HerMES data were accessed through the Herschel Database in Marseille (HeDaM \u2013 http://hedam.lam.fr) operated by CeSAM and hosted by the Laboratoire d'Astrophysique de Marseille. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK) and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA (USA).\n\nThis work is based on observations taken by the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Program 185.A-0791, and made available by the VUDS team at the CESAM data centre, Laboratoire d'Astrophysique de Marseille, France. The HST data matched to the VUDS-DR1 are described in Grogin et al. (2011) and Koekemoer et al. (2011) for CANDELS and include data from the ERS (Windhorst et al. 2011). This paper uses data from the VIMOS Public Extragalactic Redshift Survey (VIPERS). VIPERS has been performed using the ESO Very Large Telescope, under the 'Large Programme' 182.A-0886. The participating institutions and funding agencies are listed at http://vipers.inaf.it, based on zCOSMOS observations carried out using the Very Large Telescope at the ESO Paranal Observatory under Programme ID: LP175.A-0839. \n\nThis research has made use of the Tool for OPerations on Catalogues And Tables (TOPCAT; Taylor 2005): www.starlink.ac.uk/topcat/; SAOImage DS9, developed by Smithsonian Astrophysical Observatory (Joye & Mandel 2003); SEXTRACTOR: Software for source extraction (Bertin & Arnouts 1996) and NASA's Astrophysics Data System Bibliographic Services.", "abstract": "We present physical properties [redshifts (z), star-formation rates (SFRs) and stellar masses\n(Mstar)] of bright (S850 \u2265 4 mJy) submm galaxies in the 2 deg2 COSMOS and UDS fields\nselected with SCUBA-2/JCMT. We complete the galaxy identification process for all (2000)\nS/N \u2265 3.5 850-\u00b5m sources, but focus our scientific analysis on a high-quality subsample of\n651 S/N \u2265 4 sources with complete multiwavelength coverage including 1.1-mm imaging.\nWe check the reliability of our identifications, and the robustness of the SCUBA-2 fluxes\nby revisiting the recent ALMA follow-up of 29 sources in our sample. Considering >4 mJy\nALMA sources, our identification method has a completeness of 86 per cent with a reliability\nof 92 per cent, and only 15\u201320 per cent of sources are significantly affected by multiplicity\n(when a secondary component contributes >1/3 of the primary source flux). The impact of\nsource blending on the 850-\u00b5m source counts as determined with SCUBA-2 is modest; scaling\nthe single-dish fluxes by 0.9 reproduces the ALMA source counts. For our final SCUBA-\n2 sample, we find median z = 2.40+0.10 \u22120.04, SFR = 287 \u00b1 6 M\ufffd yr\u22121 and log(Mstar/M\ufffd) =\n11.12 \u00b1 0.02 (the latter for 349/651 sources with optical identifications). These properties\nclearly locate bright submm galaxies on the high-mass end of the 'main sequence' of starforming\ngalaxies out to z 6, suggesting that major mergers are not a dominant driver of the\nhigh-redshift submm-selected population. Their number densities are also consistent with the\nevolving galaxy stellar mass function. Hence, the submm galaxy population is as expected,\nalbeit reproducing the evolution of the main sequence of star-forming galaxies remains a\nchallenge for theoretical models/simulations.\nKey", "date": "2017-07", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "469", "number": "1", "publisher": "Monthly Notices of the Royal Astronomical Society", "pagerange": "492-515", "id_number": "CaltechAUTHORS:20170625-172150566", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170625-172150566", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "SPLASH" }, { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stx861", "pub_year": "2017", "author_list": "Micha\u0142owski, Micha\u0142 J.; Dunlop, J. S.; et el." }, { "id": "https://authors.library.caltech.edu/records/qh6z4-zsz83", "eprint_id": 77770, "eprint_status": "archive", "datestamp": "2023-08-19 03:32:42", "lastmod": "2023-10-25 23:26:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Masters-D-C", "name": { "family": "Masters", "given": "Daniel C." }, "orcid": "0000-0001-5382-6138" }, { "id": "Stern-D", "name": { "family": "Stern", "given": "Daniel K." }, "orcid": "0000-0003-2686-9241" }, { "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason D." }, "orcid": "0000-0002-4485-8549" }, { "id": "Castander-F-J", "name": { "family": "Castander", "given": "Francisco J." }, "orcid": "0000-0001-7316-4573" }, { "id": "Paltani-St\u00e9phane", "name": { "family": "Paltani", "given": "St\u00e9phane" } } ] }, "title": "The Complete Calibration of the Color-Redshift Relation (C3R2) Survey: Survey Overview and Data Release 1", "ispublished": "pub", "full_text_status": "public", "keywords": "astronomical databases: catalogs \u2013 astronomical databases: surveys \u2013 cosmology: observations \u2013 galaxies: distances and redshifts", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 February 27; revised 2017 April 19; accepted 2017 April 19; published 2017 May 31. \n\nThe authors thank the referee, Marcin Sawicki, for a helpful report that improved this paper. D.M. would like to thank Giuseppe Longo, Audrey Galametz, Sotiria Fotopoulou, and George Helou for helpful conversations. D.M., P.C., D.S., and J.R. acknowledge support by NASA ROSES grant 12-EUCLID12-0004. J.R. and D.S. are supported by JPL, run by Caltech for NASA. F.C. acknowledges support by MINECO grant ESP2015-88861. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\n\nPublished - Masters_2017_ApJ_841_111.pdf
Submitted - 1704.06665.pdf
", "abstract": "A key goal of the Stage IV dark energy experiments Euclid, LSST, and WFIRST is to measure the growth of structure with cosmic time from weak lensing analysis over large regions of the sky. Weak lensing cosmology will be challenging: in addition to highly accurate galaxy shape measurements, statistically robust and accurate photometric redshift (photo-z) estimates for billions of faint galaxies will be needed in order to reconstruct the three-dimensional matter distribution. Here we present an overview of and initial results from the Complete Calibration of the Color\u2013Redshift Relation (C3R2) survey, which is designed specifically to calibrate the empirical galaxy color\u2013redshift relation to the Euclid depth. These redshifts will also be important for the calibrations of LSST and WFIRST. The C3R2 survey is obtaining multiplexed observations with Keck (DEIMOS, LRIS, and MOSFIRE), the Gran Telescopio Canarias (GTC; OSIRIS), and the Very Large Telescope (VLT; FORS2 and KMOS) of a targeted sample of galaxies that are most important for the redshift calibration. We focus spectroscopic efforts on undersampled regions of galaxy color space identified in previous work in order to minimize the number of spectroscopic redshifts needed to map the color\u2013redshift relation to the required accuracy. We present the C3R2 survey strategy and initial results, including the 1283 high-confidence redshifts obtained in the 2016A semester and released as Data Release 1.", "date": "2017-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "841", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 111", "id_number": "CaltechAUTHORS:20170525-151351304", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170525-151351304", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "12-EUCLID12-0004" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)", "grant_number": "ESP2015-88861" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aa6f08", "primary_object": { "basename": "1704.06665.pdf", "url": "https://authors.library.caltech.edu/records/qh6z4-zsz83/files/1704.06665.pdf" }, "related_objects": [ { "basename": "Masters_2017_ApJ_841_111.pdf", "url": "https://authors.library.caltech.edu/records/qh6z4-zsz83/files/Masters_2017_ApJ_841_111.pdf" } ], "pub_year": "2017", "author_list": "Masters, Daniel C.; Stern, Daniel K.; et el." }, { "id": "https://authors.library.caltech.edu/records/xje1c-64862", "eprint_id": 77916, "eprint_status": "archive", "datestamp": "2023-08-19 03:33:25", "lastmod": "2023-10-25 23:33:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Suh-Hyewon", "name": { "family": "Suh", "given": "Hyewon" }, "orcid": "0000-0002-2536-1633" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "Francesca" }, "orcid": "0000-0002-2115-1137" }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G\u00fcnther" }, "orcid": "0000-0002-0797-0646" }, { "id": "Lusso-E", "name": { "family": "Lusso", "given": "Elisabeta" }, "orcid": "0000-0003-0083-1157" }, { "id": "Lanzuisi-G", "name": { "family": "Lanzuisi", "given": "Giorgio" }, "orcid": "0000-0001-9094-0984" }, { "id": "Marchesi-S", "name": { "family": "Marchesi", "given": "Stefano" }, "orcid": "0000-0001-5544-0749" }, { "id": "Trakhtenbrot-B", "name": { "family": "Trakhtenbrot", "given": "Benny" }, "orcid": "0000-0002-3683-7297" }, { "id": "Allevato-V", "name": { "family": "Allevato", "given": "Viola" } }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "Nico" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "id": "Griffiths-R-E", "name": { "family": "Griffiths", "given": "Richard E." } }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "Clotilde" } }, { "id": "Lira-P", "name": { "family": "Lira", "given": "Paulina" } }, { "id": "Riguccini-L", "name": { "family": "Riguccini", "given": "Laurie" } }, { "id": "Rosario-D-J-V", "name": { "family": "Rosario", "given": "David J." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Schawinski-K", "name": { "family": "Schawinski", "given": "Kevin" }, "orcid": "0000-0001-5464-0888" }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "Cristian" }, "orcid": "0000-0002-8853-9611" } ] }, "title": "Type 2 AGN Host Galaxies in the Chandra-COSMOS Legacy Survey: No Evidence of AGN-driven Quenching", "ispublished": "pub", "full_text_status": "public", "keywords": "black hole physics \u2013 galaxies: active \u2013 galaxies: nuclei \u2013 quasars: general", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 December 28; revised 2017 May 1; accepted 2017 May 8; published 2017 May 31. \n\nThis work was supported in part by NASA Chandra grant number GO3-14150C, GO3-14150B, and also GO5-16150A. K.S. acknowledges support from Swiss National Science Foundation Grants PP00P2_138979 and PP00P2_166159. E.L. is supported by a European Union COFUND/Durham Junior Research Fellowship (under EU grant agreement No. 609412).\n\nPublished - Suh_2017_ApJ_841_102.pdf
Submitted - 1705.03890.pdf
", "abstract": "We investigate the star formation properties of a large sample of ~2300 X-ray-selected Type 2 Active Galactic Nuclei (AGNs) host galaxies out to z ~ 3 in the Chandra COSMOS Legacy Survey in order to understand the connection between the star formation and nuclear activity. Making use of the existing multi-wavelength photometric data available in the COSMOS field, we perform a multi-component modeling from far-infrared to near-ultraviolet using a nuclear dust torus model, a stellar population model and a starburst model of the spectral energy distributions (SEDs). Through detailed analyses of SEDs, we derive the stellar masses and the star formation rates (SFRs) of Type 2 AGN host galaxies. The stellar mass of our sample is in the range of 9 < log M_(stellar)/M\u2299 < 12 with uncertainties of ~0.19 dex. We find that Type 2 AGN host galaxies have, on average, similar SFRs compared to the normal star-forming galaxies with similar M_(stellar) and redshift ranges, suggesting no significant evidence for enhancement or quenching of star formation. This could be interpreted in a scenario, where the relative massive galaxies have already experienced substantial growth at higher redshift (z > 3), and grow slowly through secular fueling processes hosting moderate-luminosity AGNs.", "date": "2017-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "841", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 102", "id_number": "CaltechAUTHORS:20170602-105033523", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170602-105033523", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO3-14150C" }, { "agency": "NASA", "grant_number": "GO3-14150B" }, { "agency": "NASA", "grant_number": "GO5-16150A" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "PP00P2_138979/1" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "PP00P2_166159" }, { "agency": "European Research Council (ERC)", "grant_number": "609412" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/aa725c", "primary_object": { "basename": "1705.03890.pdf", "url": "https://authors.library.caltech.edu/records/xje1c-64862/files/1705.03890.pdf" }, "related_objects": [ { "basename": "Suh_2017_ApJ_841_102.pdf", "url": "https://authors.library.caltech.edu/records/xje1c-64862/files/Suh_2017_ApJ_841_102.pdf" } ], "pub_year": "2017", "author_list": "Suh, Hyewon; Civano, Francesca; et el." }, { "id": "https://authors.library.caltech.edu/records/mrmwe-tz587", "eprint_id": 81896, "eprint_status": "archive", "datestamp": "2023-08-19 03:26:38", "lastmod": "2023-10-17 21:54:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Delhaize-J", "name": { "family": "Delhaize", "given": "J." }, "orcid": "0000-0002-6149-0846" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "The VLA-COSMOS 3\u2009GHz Large Project: The infrared-radio correlation of star-forming galaxies and AGN to z \u2272 6", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: star formation \u2013 radio continuum: galaxies \u2013 infrared: galaxies", "note": "\u00a9 2017 ESO. Article published by EDP Sciences. \n\nReceived 29 July 2016; Accepted 17 February 2017; Published online 13 June 2017. \n\nWe thank the anonymous referee for useful comments which have helped to improve this paper. We also thank Tijana Prodanovi\u0107 for valuable discussions. This research was funded by the European Unions Seventh Frame-work programme under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). This research was supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence \"Origin and Structure of the Universe\". N.B. acknowledges the European Unions Seventh Framework programme under grant agreement 333654 (CIG, AGN feedback). M.B. and P.\u2009Ciliegi acknowledge support from the PRIN-INAF 2014. A.K. acknowledges support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). M.T.S. acknowledges support from a Royal Society Leverhulme Trust Senior Research Fellowship. Support for B.M. was provided by the DFG priority programme 1573 \"The physics of the interstellar medium\". M.A. acknowledges partial support from FONDECYT through grant 1140099.\n\nSubmitted - aa29430-16.pdf
", "abstract": "We examine the behaviour of the infrared-radio correlation (IRRC) over the range 0", "date": "2017-06", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "602", "publisher": "EDP Sciences", "pagerange": "Art. No. A4", "id_number": "CaltechAUTHORS:20170928-104505397", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170928-104505397", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "Munich Institute for Astro- and Particle Physics (MIAPP)" }, { "agency": "European Research Council (ERC)", "grant_number": "333654" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "956" }, { "agency": "Royal Society" }, { "agency": "Leverhulme Trust" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "1573" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1140099" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201629430", "primary_object": { "basename": "aa29430-16.pdf", "url": "https://authors.library.caltech.edu/records/mrmwe-tz587/files/aa29430-16.pdf" }, "pub_year": "2017", "author_list": "Delhaize, J. and Capak, P." }, { "id": "https://authors.library.caltech.edu/records/d4p2k-xpb36", "eprint_id": 81903, "eprint_status": "archive", "datestamp": "2023-08-19 03:27:38", "lastmod": "2023-10-17 21:54:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Delvecchio-I", "name": { "family": "Delvecchio", "given": "I." }, "orcid": "0000-0001-8706-2252" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Baran-N", "name": { "family": "Baran", "given": "N." } }, { "id": "Novak-Mladen", "name": { "family": "Novak", "given": "M." }, "orcid": "0000-0001-8695-825X" }, { "id": "Delhaize-J", "name": { "family": "Delhaize", "given": "J." }, "orcid": "0000-0002-6149-0846" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Berta-S", "name": { "family": "Berta", "given": "S." }, "orcid": "0000-0002-0320-1532" }, { "id": "Bondi-M", "name": { "family": "Bondi", "given": "M." } }, { "id": "Ciliegi-P", "name": { "family": "Ciliegi", "given": "P." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "C." } }, { "id": "Marchesi-S", "name": { "family": "Marchesi", "given": "S." }, "orcid": "0000-0001-5544-0749" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Tasca-L", "name": { "family": "Tasca", "given": "L." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Vardoulaki-E", "name": { "family": "Vardoulaki", "given": "E." }, "orcid": "0000-0002-4437-1773" } ] }, "title": "The VLA-COSMOS 3 GHz Large Project: Multiwavelength counterparts and the composition of the faint radio population", "ispublished": "pub", "full_text_status": "public", "keywords": "radio continuum: galaxies \u2013 catalogs", "note": "\u00a9 2017 ESO. Article published by EDP Sciences. \n\nReceived 9 December 2016; Accepted 12 April 2017; Published online 13 June 2017. \n\nZgal group: European Union's Seventh Framework program under grant agreement 333654 (CIG, \"AGN feedback\"; N.B., V.S.) and grant agreement 337595 (ERC Starting Grant, \"CoSMass\"; V.S., I.D., J.D., M.N.). C.L. acknowledges the funding by a Discovery Early Career Researcher Award (DE150100618). Partially based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Programs 175.A-0839 (the zCOSMOS Spectroscopic Redshift Survey) and 185.A-0791 (the VIMOS Ultra Deep Survey). A.K. and E.V. acknowledge support from the collaborative research center 956 (sub-project A1) funded by the Deutsche Forschungsgemeinschaft (DFG).\n\nPublished - aa30223-16.pdf
Submitted - 1703.09719.pdf
", "abstract": "We study the composition of the faint radio population selected from the Karl G. Jansky Very Large Array Cosmic Evolution Survey (VLA-COSMOS) 3 GHz Large Project, which is a radio continuum survey performed at 10 cm wavelength. The survey covers a 2.6 square degree area with a mean rms of ~ 2.3 \u03bcJy/beam, cataloging 10\u2009830 sources above 5\u03c3, and enclosing the full 2 square degree COSMOS field. By combining these radio data with optical, near-infrared (UltraVISTA), and mid-infrared (Spitzer/IRAC) data, as well as X-ray data (Chandra), we find counterparts to radio sources for ~93% of the total radio sample reaching out to z \u2272 6; these sources are found in the unmasked areas of the COSMOS field, i.e., those not affected by saturated or bright sources in the optical to near-infrared (NIR) bands. We further classify the sources as star-forming galaxies or AGN based on various criteria, such as X-ray luminosity; observed mid-infrared color; UV\u2013far-infrared spectral energy distribution; rest-frame, near-UV optical color that is corrected for dust extinction; and radio excess relative to that expected from the star formation rate of the hosts. We separate the AGN into subsamples dominated by low-to-moderate and moderate-to-high radiative luminosity AGN, i.e., candidates for high-redshift analogs to local low- and high-excitation emission line AGN, respectively. We study the fractional contributions of these subpopulations down to radio flux levels of ~11 \u03bcJy at 3 GHz (or ~20 \u03bcJy at 1.4 GHz assuming a spectral index of \u20130.7). We find that the dominant fraction at 1.4 GHz flux densities above ~200 \u03bcJy is constituted of low-to-moderate radiative luminosity AGN. Below densities of ~100 \u03bcJy the fraction of star-forming galaxies increases to ~ 60%, followed by the moderate-to-high radiative luminosity AGN (~ 20%) and low-to-moderate radiative luminosity AGN (~ 20%). Based on this observational evidence, we extrapolate the fractions down to sensitivities of the Square Kilometer Array (SKA). Our estimates suggest that at the faint flux limits to be reached by the (Wide, Deep, and UltraDeep) SKA1 surveys, a selection based only on radio flux limits can provide a simple tool to efficiently identify samples highly (>75%) dominated by star-forming galaxies.", "date": "2017-06", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "602", "publisher": "EDP Sciences", "pagerange": "Art. No. A2", "id_number": "CaltechAUTHORS:20170928-133150522", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170928-133150522", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "333654" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "Australian Research Council", "grant_number": "DE150100618" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "956" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201630223", "primary_object": { "basename": "1703.09719.pdf", "url": "https://authors.library.caltech.edu/records/d4p2k-xpb36/files/1703.09719.pdf" }, "related_objects": [ { "basename": "aa30223-16.pdf", "url": "https://authors.library.caltech.edu/records/d4p2k-xpb36/files/aa30223-16.pdf" } ], "pub_year": "2017", "author_list": "Smol\u010di\u0107, V.; Delvecchio, I.; et el." }, { "id": "https://authors.library.caltech.edu/records/vx8cn-z2q09", "eprint_id": 81894, "eprint_status": "archive", "datestamp": "2023-08-19 03:26:06", "lastmod": "2023-10-17 21:54:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Mooley-Kunal-Prakash", "name": { "family": "Mooley", "given": "K. P." }, "orcid": "0000-0002-2557-5180" }, { "id": "Bourke-S-A", "name": { "family": "Bourke", "given": "S" } }, { "id": "Balokovi\u0107-M", "name": { "family": "Balokovi\u0107", "given": "M." }, "orcid": "0000-0003-0476-6647" }, { "id": "Hallinan-G", "name": { "family": "Hallinan", "given": "G." }, "orcid": "0000-0002-7083-4049" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "The VLA-COSMOS 3 GHz Large Project: Continuum data and source catalog release", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs \u2013 cosmology: observations \u2013 radio continuum: galaxies", "note": "\u00a9 2017 ESO.\nArticle published by EDP Sciences.\n\nReceived 13 April 2016; Accepted 20 June 2017; Published online 13 June 2017.\n\nWe thank the referee, Jim Condon, for insightful comments that helped improve the manuscript. Based on observations with the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research was funded by the European Union's Seventh Frame-work programs under grant agreements 333654 (CIG, \"AGN feedback\") and 337595 (ERC Starting Grant, \"CoSMass\"). M.B. and P.C. acknowlege support from the PRIN-INAF 2014. A.K. and F.B. acknowledge support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). B.M. and F.B. acknowledge support through DFG priority program 1573 founded by the DFG.\n\nPublished - aa28704-16.pdf
Submitted - 1703.09713.pdf
", "abstract": "We present the VLA-COSMOS 3 GHz Large Project based on 384 h of observations with the Karl G. Jansky Very Large Array (VLA) at 3 GHz (10 cm) toward the two square degree Cosmic Evolution Survey (COSMOS) field. The final mosaic reaches a median rms of 2.3 \u03bcJy beam^(-1) over the two square degrees at an angular resolution of 0.75\u2033. To fully account for the spectral shape and resolution variations across the broad (2 GHz) band, we image all data with a multiscale, multifrequency synthesis algorithm. We present a catalog of 10\u2009830 radio sources down to 5\u03c3, out of which 67 are combined from multiple components.Comparing the positions of our 3 GHz sources with those from the Very Long Baseline Array (VLBA)-COSMOS survey, we estimate that the astrometry is accurate to 0.01\u2033 at the bright end (signal-to-noise ratio, S/N_(3 GHz) > 20). Survival analysis on our data combined with the VLA-COSMOS 1.4 GHz Joint Project catalog yields an expected median radio spectral index of \u03b1 = \u22120.7. We compute completeness corrections via Monte Carlo simulations to derive the corrected 3 GHz source counts. Our counts are in agreement with previously derived 3 GHz counts based on single-pointing (0.087 square degrees) VLA data. In summary, the VLA-COSMOS 3 GHz Large Project simultaneously provides the largest and deepest radio continuum survey at high (0.75\u2033) angular resolution to date, bridging the gap between last-generation and next-generation surveys.", "date": "2017-06", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "602", "publisher": "EDP Sciences", "pagerange": "Art. No. A1", "id_number": "CaltechAUTHORS:20170928-101836348", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170928-101836348", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "333654" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "956" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "1573" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "COSMOS", "value": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)", "value": "Infrared Processing and Analysis Center (IPAC)" }, { "id": "Astronomy-Department", "value": "Astronomy Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences", "value": "Division of Geological and Planetary Sciences" } ] }, "doi": "10.1051/0004-6361/201628704", "primary_object": { "basename": "aa28704-16.pdf", "url": "https://authors.library.caltech.edu/records/vx8cn-z2q09/files/aa28704-16.pdf" }, "related_objects": [ { "basename": "1703.09713.pdf", "url": "https://authors.library.caltech.edu/records/vx8cn-z2q09/files/1703.09713.pdf" } ], "pub_year": "2017", "author_list": "Smol\u010di\u0107, V.; Mooley, K. P.; et el." }, { "id": "https://authors.library.caltech.edu/records/taqmt-gdf76", "eprint_id": 81895, "eprint_status": "archive", "datestamp": "2023-08-19 03:26:33", "lastmod": "2023-10-17 21:54:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Delvecchio-I", "name": { "family": "Delvecchio", "given": "I." }, "orcid": "0000-0001-8706-2252" }, { "id": "Mooley-Kunal-Prakash", "name": { "family": "Mooley", "given": "K. P." }, "orcid": "0000-0002-2557-5180" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "The VLA-COSMOS 3 GHz Large Project: AGN and host-galaxy properties out to z\u2009 \u2272 \u20096", "ispublished": "pub", "full_text_status": "public", "keywords": "radio continuum: galaxies \u2013 galaxies: nuclei \u2013 galaxies: active \u2013 galaxies: evolution", "note": "\u00a9 2017 ESO. Article published by EDP Sciences. \n\nReceived 21 July 2016; Accepted 21 October 2016; Published online 13 June 2017. \n\nThe authors are grateful to the anonymous referee for his/her careful reading and useful comments, which improved the content of this manuscript. I.D., V.S., J.D., M.N., and O.M. acknowledge the European Union's Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). N.B. acknowledges the European Union's Seventh Framework programme under grant agreement 333654 (CIG, \"AGN feedback\"). C.L. is funded by a Discovery Early Career Researcher Award (DE150100618). Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. M.B. and P.C. acknowledge supports from the PRIN-INAF 2014. M.A. acknowledges partial support from FONDECYT through grant 1140099. A.K. acknowledges support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). This work was partially supported by NASA Chandra grant number GO3-14150C and GO3-14150B (FC, S.M.). I.D. is grateful to B. Magnelli for useful suggestions and to Takamitsu Miyaji for his help with CSTACK.\n\nPublished - aa29367-16.pdf
Submitted - 1703.09720.pdf
", "abstract": "We explore the multiwavelength properties of AGN host galaxies for different classes of radio-selected AGN out to z \u2272 6 via a multiwavelength analysis of about 7700 radio sources in the COSMOS field. The sources were selected with the Very Large Array (VLA) at 3 GHz (10 cm) within the VLA\u2013COSMOS 3 GHz Large Project, and cross-matched with multiwavelength ancillary data. This is the largest sample of high-redshift (z \u2272 6) radio sources with exquisite photometric coverage and redshift measurements available. We constructed a sample of moderate-to-high radiative luminosity AGN (HLAGN) via spectral energy distribution decomposition combined with standard X-ray and mid-infrared diagnostics. Within the remainder of the sample we further identified low-to-moderate radiative luminosity AGN (MLAGN) via excess in radio emission relative to the star formation rates in their host galaxies. We show that at each redshift our HLAGN havesystematically higher radiative luminosities than MLAGN and that their AGN power occurs predominantly in radiative form, while MLAGN display a substantial mechanical AGN luminosity component. We found significant differences in the host properties of the two AGN classes, as a function of redshift. At z< 1.5, MLAGN appear to reside in significantly more massive and less star-forming galaxies compared to HLAGN. At z> 1.5, we observed a reversal in the behaviour of the stellar mass distributions with the HLAGN populating the higher stellar mass tail. We interpret this finding as a possible hint of the downsizing of galaxies hosting HLAGN, with the most massive galaxies triggering AGN activity earlier than less massive galaxies, and then fading to MLAGN at lower redshifts. Our conclusion is that HLAGN and MLAGN samples trace two distinct galaxy and AGN populations in a wide range of redshifts, possibly resembling the radio AGN types often referred to as radiative- and jet-mode (or high- and low-excitation), respectively, whose properties might depend on the different availability of cold gas supplies.", "date": "2017-06", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "602", "publisher": "EDP Sciences", "pagerange": "Art. No. A3", "id_number": "CaltechAUTHORS:20170928-103303952", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170928-103303952", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "European Research Council (ERC)", "grant_number": "333654" }, { "agency": "Australian Research Council", "grant_number": "DE150100618" }, { "agency": "Australian Research Council", "grant_number": "CE110001020" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1140099" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "956" }, { "agency": "NASA", "grant_number": "GO3-14150C" }, { "agency": "NASA", "grant_number": "GO3-14150B" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201629367", "primary_object": { "basename": "1703.09720.pdf", "url": "https://authors.library.caltech.edu/records/taqmt-gdf76/files/1703.09720.pdf" }, "related_objects": [ { "basename": "aa29367-16.pdf", "url": "https://authors.library.caltech.edu/records/taqmt-gdf76/files/aa29367-16.pdf" } ], "pub_year": "2017", "author_list": "Delvecchio, I.; Mooley, K. P.; et el." }, { "id": "https://authors.library.caltech.edu/records/h37kz-dmb05", "eprint_id": 81897, "eprint_status": "archive", "datestamp": "2023-08-19 03:26:45", "lastmod": "2023-10-17 21:54:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Novak-Mladen", "name": { "family": "Novak", "given": "M." }, "orcid": "0000-0001-8695-825X" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Delhaize-J", "name": { "family": "Delhaize", "given": "J." }, "orcid": "0000-0002-6149-0846" }, { "id": "Delvecchio-I", "name": { "family": "Delvecchio", "given": "I." }, "orcid": "0000-0001-8706-2252" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Baran-N", "name": { "family": "Baran", "given": "N." } }, { "id": "Bondi-M", "name": { "family": "Bondi", "given": "M." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Ciliegi-P", "name": { "family": "Ciliegi", "given": "P." } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "C." } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Marchesi-S", "name": { "family": "Marchesi", "given": "S." }, "orcid": "0000-0001-5544-0749" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Miettinen-O", "name": { "family": "Miettinen", "given": "O." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M." }, "orcid": "0000-0003-1033-9684" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Tasca-L", "name": { "family": "Tasca", "given": "L." } } ] }, "title": "The VLA-COSMOS 3 GHz Large Project: Cosmic star formation history since z ~ 5", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: star formation \u2013 cosmology: observations \u2013 radio continuum: galaxies", "note": "\u00a9 2017 ESO. Article published by EDP Sciences. \n\nReceived 29 July 2016; Accepted 15 January 2017; Published online 13 June 2017. \n\nThis research was funded by the European Unions Seventh Frame-work program under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). E.S. warmly acknowledges support from the National Radio Astronomy Observatory for visits to the Array Operations Center in Socorro, NM, in conjunction with this project. A.K. acknowledges support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). M.B. and P.C. acknowledge support from the PRIN-INAF 2014.\n\nPublished - aa29436-16.pdf
Submitted - 1703.09724.pdf
", "abstract": "We make use of the deep Karl G. Jansky Very Large Array (VLA) COSMOS radio observations at 3 GHz to infer radio luminosity functions of star-forming galaxies up to redshifts of z ~ 5 based on approximately 6000 detections with reliable optical counterparts. This is currently the largest radio-selected sample available out to z ~ 5 across an area of 2 square degrees with a sensitivity of rms \u2248 2.3 \u03bcJy beam^(-1). By fixing the faint and bright end shape of the radio luminosity function to the local values, we find a strong redshift trend that can be fitted with a pure luminosity evolution L_(1.4 GHz) \u221d (1 + z)^((3.16 \u00b1 0.2)\u2212(0.32 \u00b1 0.07)z). We estimate star formation rates (SFRs) from our radio luminosities using an infrared (IR)-radio correlation that is redshift dependent. By integrating the parametric fits of the evolved luminosity function we calculate the cosmic SFR density (SFRD) history since z ~ 5. Our data suggest that the SFRD history peaks between 2 < z < 3 and that the ultraluminous infrared galaxies (100 M\u2299 yr^(-1) < SFR < 1000 M\u2299 yr^(-1)) contribute up to ~25% to the total SFRD in the same redshift range. Hyperluminous infrared galaxies (SFR > 1000 M\u2299 yr^(-1)) contribute an additional \u22722% in the entire observed redshift range. We find evidence of a potential underestimation of SFRD based on ultraviolet (UV) rest-frame observations of Lyman break galaxies at high redshifts (z \u2273 4) on the order of 15\u201320%, owing to appreciable star formation in highly dust-obscured galaxies, which might remain undetected in such UV observations.", "date": "2017-06", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "602", "publisher": "EDP Sciences", "pagerange": "Art. No. A5", "id_number": "CaltechAUTHORS:20170928-105757119", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170928-105757119", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "956" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201629436", "primary_object": { "basename": "1703.09724.pdf", "url": "https://authors.library.caltech.edu/records/h37kz-dmb05/files/1703.09724.pdf" }, "related_objects": [ { "basename": "aa29436-16.pdf", "url": "https://authors.library.caltech.edu/records/h37kz-dmb05/files/aa29436-16.pdf" } ], "pub_year": "2017", "author_list": "Novak, M.; Smol\u010di\u0107, V.; et el." }, { "id": "https://authors.library.caltech.edu/records/vqbg9-m3t26", "eprint_id": 81904, "eprint_status": "archive", "datestamp": "2023-08-19 03:27:45", "lastmod": "2023-10-17 21:54:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Miettinen-O", "name": { "family": "Miettinen", "given": "O." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "An ALMA survey of submillimetre galaxies in the COSMOS field: The extent of the radio-emitting region revealed by 3 GHz imaging with the Very Large Array", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: formation \u2013 galaxies: starburst \u2013 galaxies: star formation \u2013 radio continuum: galaxies \u2013 submillimeter: galaxies", "note": "\u00a9 2017 ESO. Article published by EDP Sciences. \n\nReceived 16 January 2017; Accepted 16 February 2017; Published online 09 June 2017. \n\nBased on observations with the Karl G. Jansky Very Large Array (VLA) of the National Radio Astronomy Observatory (NRAO). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. \n\nWe appreciate the exceptionally constructive and positive feedback from the referee. This research was funded by the European Union's Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). M.A. acknowledges partial support from FONDE-CYT through grant 1140099. A.K. acknowledges support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). E.S. acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No. 694343). D.R. acknowledges support from the National Science Foundation under grant number AST-1614213 to Cornell University. \n\nThis work was performed in part at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1066293. This work was partially supported by a grant from the Simons Foundation. The Flatiron Institute is supported by the Simons Foundation. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2012.1.00978.S and ADS/JAO.ALMA#2013.1.00118.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This research has made use of NASA's Astrophysics Data System, and the NASA/IPAC Infrared Science Archive, which is operated by the JPL, California Institute of Technology, under contract with the NASA. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013). We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information on the COSMOS survey is available at http://cosmos.astro.caltech.edu\n\nPublished - aa30443-17.pdf
Submitted - 1702.07527.pdf
", "abstract": "Context. The observed spatial scale of the radio continuum emission from star-forming galaxies can be used to investigate the spatial extent of active star formation, constrain the importance of cosmic-ray transport, and examine the effects of galaxy interactions.\nAims. We determine the radio size distribution of a large sample of 152 submillimetre galaxies (SMGs) in the COSMOS field that were pre-selected at 1.1 mm, and later detected with the Atacama Large Millimetre/submillimetre Array (ALMA) in the observed-frame 1.3 mm dust continuum emission at a signal-to-noise ratio (S/N) of \u22655.\nMethods. We used the deep, subarcsecond-resolution (1\u03c3 = 2.3\u03bcJy beam^(-1); .\u030b 75) centimetre radio continuum observations taken by the Karl G. Jansky Very Large Array (VLA)-COSMOS 3 GHz Large Project.\nResults. One hundred and fifteen of the 152 target SMGs (76% \u00b1 7%) were found to have a 3 GHz counterpart (\u2265 4.2\u03c3), which renders the radio detection rate notably high. The median value of the deconvolved major axis full width at half maximum (FWHM) size at 3 GHz is derived to be 0.\u030b59 \u00b1 0.\u030b05 , or 4.6 \u00b1 0.4 kpc in physical units, where the median redshift of the sources is z = 2.23 \u00b1 0.13 (23% are spectroscopic and 77% are photometric values). The radio sizes are roughly log-normally distributed, and they show no evolutionary trend with redshift, or difference between different galaxy morphologies. We also derived the spectral indices between 1.4 and 3 GHz, and 3 GHz brightness temperatures for the sources, and the median values were found to be \u03b1_(1.4 GHz)^(3 GHz) = -0.67 (S_\u03bd \u221d \u03bd^\u03b1) and T_B = 12.6 \u00b1 2 K. Three of the target SMGs, which are also detected with the Very Long Baseline Array (VLBA) at 1.4 GHz (AzTEC/C24b, 61, and 77a), show clearly higher brightness temperatures than the typical values, reaching T_B(3 GHz) > 10^(4.03) K for AzTEC/C61.\nConclusions. The derived median radio spectral index agrees with a value expected for optically thin non-thermal synchrotron radiation, and the low median 3 GHz brightness temperature shows that the observed radio emission is predominantly powered by star formation and supernova activity. However, our results provide a strong indication of the presence of an active galactic nucleus in the VLBA and X-ray-detected SMG AzTEC/C61 (high TB and an inverted radio spectrum). The median radio-emitting size we have derived is ~ 1.5\u20133 times larger than the typical far-infrared dust-emitting sizes of SMGs, but similar to that of the SMGs' molecular gas component traced through mid-J line emission of carbon monoxide. The physical conditions of SMGs probably render the diffusion of cosmic-ray electrons inefficient, and hence an unlikely process to lead to the observed extended radio sizes. Instead, our results point towards a scenario where SMGs are driven by galaxy interactions and mergers. Besides triggering vigorous starbursts, galaxy collisions can also pull out the magnetised fluids from the interacting disks, and give rise to a taffy-like synchrotron-emitting bridge. This provides an explanation for the spatially extended radio emission of SMGs, and can also cause a deviation from the well-known infrared-radio correlation owing to an excess radio emission. Nevertheless, further high-resolution observations are required to examine the other potential reasons for the very compact dust-emitting sizes of SMGs, such as the radial dust temperature and metallicity gradients.", "date": "2017-06", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "602", "publisher": "EDP Sciences", "pagerange": "Art. No. A54", "id_number": "CaltechAUTHORS:20170928-135012692", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170928-135012692", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1140099" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "956" }, { "agency": "European Research Council (ERC)", "grant_number": "694343" }, { "agency": "NSF", "grant_number": "AST-1614213" }, { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "Simons Foundation" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201730443", "primary_object": { "basename": "1702.07527.pdf", "url": "https://authors.library.caltech.edu/records/vqbg9-m3t26/files/1702.07527.pdf" }, "related_objects": [ { "basename": "aa30443-17.pdf", "url": "https://authors.library.caltech.edu/records/vqbg9-m3t26/files/aa30443-17.pdf" } ], "pub_year": "2017", "author_list": "Miettinen, O. and Capak, P. L." }, { "id": "https://authors.library.caltech.edu/records/cgvf9-eez45", "eprint_id": 76651, "eprint_status": "archive", "datestamp": "2023-08-21 20:51:32", "lastmod": "2023-10-25 16:11:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "A. L." }, "orcid": "0000-0002-9382-9832" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Tacchella-S", "name": { "family": "Tacchella", "given": "S." }, "orcid": "0000-0002-8224-4505" }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Constraints on Quenching of Z \u2272 2 Massive Galaxies from the Evolution of the Average Sizes of Star-forming and Quenched Populations in COSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: fundamental parameters; galaxies: structure", "note": "\u00a9 2017 American Astronomical Society. \n\nReceived 2016 July 15. Accepted 2017 March 23. Published 2017 April 17. \n\nWe would like to thank Dan Masters, Charles Steinhardt, Behnam Darvish, and Bahram Mobasher for valuable discussions. Furthermore, we would like to thank the referee for valuable feedback that greatly improved this manuscript. A.F. acknowledges support from the Swiss National Science Foundation. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.\n\nPublished - Constraints_on_Quenching_of_Z\u00a0\u2272\u00a02_Massi...ing_and_Quenched_Populations_in_COSMOS.pdf
Submitted - 1703.09234.pdf
", "abstract": "We use >9400 log(m/M\u2609) > 10 quiescent and star-forming galaxies at z \u227e 2 in COSMOS/UltraVISTA to study the average size evolution of these systems, with focus on the rare ultra-massive population at log(m/M_\u2609) > 11.4. The large 2 square degree survey area delivers a sample of ~400 such ultra-massive systems. Accurate sizes are derived using a calibration based on high-resolution images from the Hubble Space Telescope. We find that at these very high masses, the size evolution of star-forming and quiescent galaxies is almost indistinguishable in terms of normalization and power-law slope. We use this result to investigate possible pathways of quenching massive m > M^* galaxies at z < 2. We consistently model the size evolution of quiescent galaxies from the star-forming population by assuming different simple models for the suppression of star formation. These models include an instantaneous and delayed quenching without altering the structure of galaxies and a central starburst followed by compaction. We find that instantaneous quenching reproduces the observed mass-size relation of massive galaxies at z > 1 well. Our starburst+compaction model followed by individual growth of the galaxies by minor mergers is preferred over other models without structural change for log(m/M_\u2609) > 11.0 galaxies at z > 0.5. None of our models is able to meet the observations at m > M^* and z < 1 without significant contribution of post-quenching growth of individual galaxies via mergers. We conclude that quenching is a fast process in galaxies with m \u2265 10^(11) M_ \u2299, and that major mergers likely play a major role in the final steps of their evolution.", "date": "2017-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "839", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 71", "id_number": "CaltechAUTHORS:20170419-064155706", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170419-064155706", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aa697a", "primary_object": { "basename": "Constraints_on_Quenching_of_Z\u00a0\u2272\u00a02_Massi...ing_and_Quenched_Populations_in_COSMOS.pdf", "url": "https://authors.library.caltech.edu/records/cgvf9-eez45/files/Constraints_on_Quenching_of_Z\u00a0\u2272\u00a02_Massi...ing_and_Quenched_Populations_in_COSMOS.pdf" }, "related_objects": [ { "basename": "1703.09234.pdf", "url": "https://authors.library.caltech.edu/records/cgvf9-eez45/files/1703.09234.pdf" } ], "pub_year": "2017", "author_list": "Faisst, A. L.; Carollo, C. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/29x1b-wfq89", "eprint_id": 78645, "eprint_status": "archive", "datestamp": "2023-08-19 02:33:06", "lastmod": "2023-10-26 00:15:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bowler-R-A-A", "name": { "family": "Bowler", "given": "R. A. A." } }, { "id": "McLure-R-J", "name": { "family": "McLure", "given": "R. J." } }, { "id": "Dunlop-J-S", "name": { "family": "Dunlop", "given": "J. S." } }, { "id": "McLeod-D-J", "name": { "family": "McLeod", "given": "D. J." } }, { "id": "Stanway-E-R", "name": { "family": "Stanway", "given": "E. R." } }, { "id": "Eldridge-J-J", "name": { "family": "Eldridge", "given": "J. J." } }, { "id": "Jarvis-M-J", "name": { "family": "Jarvis", "given": "M. J." }, "orcid": "0000-0001-7039-9078" } ] }, "title": "No evidence for Population III stars or a direct collapse black hole in the z = 6.6 Lyman \u03b1 emitter 'CR7'", "ispublished": "pub", "full_text_status": "restricted", "note": "C 2017 The Authors\nPublished by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2017 April 3. Received 2017 March 14; in original form 2016 September 5.\n\nThis work was supported by the Oxford Centre for Astrophysical\nSurveys, which is funded through generous support from the Hintze\nFamily Charitable Foundation. JSD acknowledges the support of the\nEuropean Research Council via the award of an Advanced Grant\n(PI: J. Dunlop), and the contribution of the EC FP7 SPACE project\nASTRODEEP (Ref.No: 312725). RJM and DJM acknowledge the\nsupport from the European Research Council via the award of a\nConsolidator Grant (PI: R. McLure). ERS acknowledges support\nfrom UK Science and Technology Facilities Council (STFC) consolidated\ngrant ST/L000733/1. MJJ acknowledges support from the\nUK STFC [ST/N000919/1]. This publication arises from research\npartly funded by the John Fell Oxford University Press (OUP) Research\nFund. ERS and JJE wish to acknowledge the contribution\nof the high-performance computing facilities and the staff at the\nCentre for eResearch at the University of Auckland. New Zealand's\nnational facilities are provided by the New Zealand eScience Infrastructure\n(NeSI) and funded jointly by NeSI's collaborator institutions\nand through the Ministry of Business, Innovation and Employment\nInfrastructure programme (http://www.nesi.org.nz). This work\nis based in part on observations made with the NASA/ESA HST,\nwhich is operated by the Association of Universities for Research\nin Astronomy, Inc., under NASA contract NAS5-26555. This work\nis based on data products from observations made with ESO telescopes\nat the La Silla Paranal Observatories under ESO programme\nID 179.A-2005 and on data products produced by TERAPIX and the\nCambridge Astronomy survey Unit on behalf of the UltraVISTA\nconsortium. This work is based in part on observations made with\nthe Spitzer Space Telescope, which is operated by the Jet Propulsion\nLaboratory, California Institute of Technology under a NASA\ncontract.", "abstract": "The z = 6.6 Lyman\u2009\u03b1 emitter 'CR7' has been claimed to have a Population III (Pop III) like stellar population, or alternatively, be a candidate direct collapse black hole (DCBH). In this paper, we investigate the evidence for these exotic scenarios using recently available, deeper, optical, near-infrared and mid-infrared imaging. We find strong Spitzer/Infrared Array Camera detections for the main component of CR7 at 3.6 and 4.5\u2009\u03bcm, and show that it has a blue colour ([3.6] \u2212 [4.5] = \u22121.2 \u00b1 0.3). This colour cannot be reproduced by current Pop III or pristine DCBH models. Instead, the results suggest that the [3.6] band is contaminated by the [O\u2009III]\u03bb\u03bb\u20094959, 5007 emission line with an implied rest-frame equivalent width of EW0(H\u2009\u03b2 + [O\u2009III]) \u2273 2000 \u00c5. Furthermore, we find that new near-infrared data from the UltraVISTA survey supports a weaker He\u2009II\u2009\u03bb1640 emission line than previously measured, with EW0 = 40 \u00b1 30 \u00c5. For the fainter components of CR7 visible in Hubble Space Telescope imaging, we find no evidence that they are particularly red as previously claimed, and show that the derived masses and ages are considerably uncertain. In light of the likely detection of strong [O\u2009III] emission in CR7, we discuss other more standard interpretations of the system that are consistent with the data. We find that a low-mass, narrow-line active galactic nucleus can reproduce the observed features of CR7, including the lack of radio and X-ray detections. Alternatively, a young, low-metallicity (\u223c1/200\u2009Z\u2299) starburst, modelled including binary stellar pathways, can reproduce the inferred strength of the He\u2009II line and simultaneously the strength of the observed [O\u2009III] emission, but only if the gas shows supersolar \u03b1-element abundances (O/Fe \u2243 5\u2009(O/Fe)\u2299).", "date": "2017-04-05", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "469", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "448-458", "id_number": "CaltechAUTHORS:20170628-105400473", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170628-105400473", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "SPLASH" }, { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stx839", "pub_year": "2017", "author_list": "Bowler, R. A. A.; McLure, R. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/0mtha-z3s10", "eprint_id": 78654, "eprint_status": "archive", "datestamp": "2023-08-19 02:27:50", "lastmod": "2023-10-26 00:16:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bowler-R-A-A", "name": { "family": "Bowler", "given": "R. A. A." } }, { "id": "Dunlop-J-S", "name": { "family": "Dunlop", "given": "J. S." } }, { "id": "McLure-R-J", "name": { "family": "McLure", "given": "R. J." } }, { "id": "McLeod-D-J", "name": { "family": "McLeod", "given": "D. J." } } ] }, "title": "Unveiling the nature of bright z \u2243 7 galaxies with the Hubble Space Telescope", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 December 13. Received 2016 December 12; in original form 2016 May 18.", "abstract": "We present new Hubble Space Telescope/Wide Field Camera 3 (HST/WFC3) imaging of 25 extremely luminous (\u221223.2 \u2264 MUV \u2272 \u221221.2) Lyman-break galaxies (LBGs) at z \u2243 7. The sample was initially selected from 1.65 deg2 of ground-based imaging in the UltraVISTA/COSMOS and UDS/SXDS fields, and includes the extreme Lyman \u03b1 emitters, 'Himiko' and 'CR7'. A deconfusion analysis of the deep Spitzer photometry available suggests that these galaxies exhibit strong rest-frame optical nebular emission lines (EW0(H\u03b2 + [O\u2009III]) > 600\u2009\u00c5). We find that irregular, multiple-component morphologies suggestive of clumpy or merging systems are common (fmulti > 0.4) in bright z \u2243 7 galaxies, and ubiquitous at the very bright end (MUV < \u221222.5). The galaxies have half-light radii in the range r1/2 \u223c 0.5\u20133\u2009kpc. The size measurements provide the first determination of the size\u2013luminosity relation at z \u2243 7 that extends to MUV \u223c \u221223. We find the relation to be steep with r1/2\u2009\u221d\u2009L1/2. Excluding clumpy, multicomponent galaxies however, we find a shallower relation that implies an increased star formation rate surface density in bright LBGs. Using the new, independent, HST/WFC3 data we confirm that the rest-frame UV luminosity function at z \u2243 7 favours a power-law decline at the bright end, compared to an exponential Schechter function drop-off. Finally, these results have important implications for the Euclid mission, which we predict will detect >1000 similarly bright galaxies at z \u2243 7. Our new HST imaging suggests that the vast majority of these galaxies will be spatially resolved by Euclid, mitigating concerns over dwarf star contamination.", "date": "2017-04", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "466", "number": "3", "publisher": "Oxford University Press", "pagerange": "3612-3635", "id_number": "CaltechAUTHORS:20170628-131233779", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170628-131233779", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "SPLASH" }, { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stw3296", "pub_year": "2017", "author_list": "Bowler, R. A. A.; Dunlop, J. S.; et el." }, { "id": "https://authors.library.caltech.edu/records/agxg5-0x581", "eprint_id": 81906, "eprint_status": "archive", "datestamp": "2023-08-19 02:08:00", "lastmod": "2023-10-17 21:54:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chang-Yu-Yen", "name": { "family": "Chang", "given": "Yu-Yen" } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "Emeric" } }, { "id": "Juneau-S", "name": { "family": "Juneau", "given": "St\u00e9phanie" } }, { "id": "da-Cunha-E", "name": { "family": "da Cunha", "given": "Elisabete" }, "orcid": "0000-0001-9759-4797" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "Francesca" }, "orcid": "0000-0002-2115-1137" }, { "id": "Marchesi-S", "name": { "family": "Marchesi", "given": "Stefano" }, "orcid": "0000-0001-5544-0749" }, { "id": "Gabor-J-M", "name": { "family": "Gabor", "given": "J. M." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "Clotilde" } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Hsieh-Bau-Ching", "name": { "family": "Hsieh", "given": "Bau-Ching" }, "orcid": "0000-0001-5615-4904" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" } ] }, "title": "Obscured active galactic nuclei triggered in compact star-forming galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active \u2013 galaxies: star formation \u2013 infrared: galaxies", "note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 December 6. Received 2016 December 6; in original form 2016 July 12. Published: 10 December 2016. \n\nWe thank the referee as well as A. Dekel and D. Elbaz for helpful comments and discussions. We acknowledge the contribution of the entire COSMOS collaboration as well as a financial support from ANR (#ANR-12-JS05-0008-01).\n\nPublished - Chang_2017pL103.pdf
Submitted - 1612.02429.pdf
", "abstract": "We present a structural study of 182 obscured active galactic nuclei (AGNs) at z \u2264\u20091.5, selected in the Cosmic Evolution Survey field from their extreme infrared to X-ray luminosity ratio and their negligible emission at optical wavelengths. We fit optical to far-infrared spectral energy distributions and analyse deep Hubble Space Telescope imaging to derive the physical and morphological properties of their host galaxies. We find that such galaxies are more compact than normal star-forming sources at similar redshift and stellar mass, and we show that it is not an observational bias related to the emission of the AGN. Based on the distribution of their UVJ colours, we also argue that this increased compactness is not due to the additional contribution of a passive bulge. We thus postulate that a vast majority of obscured AGNs reside in galaxies undergoing dynamical compaction, similar to processes recently invoked to explain the formation of compact star-forming sources at high redshift.", "date": "2017-03-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society: Letters", "volume": "466", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "L103-L107", "id_number": "CaltechAUTHORS:20170928-142402442", "issn": "1745-3925", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170928-142402442", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-12-JS05-0008-01" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "COSMOS", "value": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)", "value": "Infrared Processing and Analysis Center (IPAC)" } ] }, "doi": "10.1093/mnrasl/slw247", "primary_object": { "basename": "1612.02429.pdf", "url": "https://authors.library.caltech.edu/records/agxg5-0x581/files/1612.02429.pdf" }, "related_objects": [ { "basename": "Chang_2017pL103.pdf", "url": "https://authors.library.caltech.edu/records/agxg5-0x581/files/Chang_2017pL103.pdf" } ], "pub_year": "2017", "author_list": "Chang, Yu-Yen; Le Floc'h, Emeric; et el." }, { "id": "https://authors.library.caltech.edu/records/wqjb8-j7y65", "eprint_id": 75088, "eprint_status": "archive", "datestamp": "2023-08-19 01:59:15", "lastmod": "2023-10-25 14:43:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "N." } }, { "id": "Vanden-Bout-P-A", "name": { "family": "Vanden Bout", "given": "P." } }, { "id": "D\u00edaz-Santos-T", "name": { "family": "D\u00edaz-Santos", "given": "T." }, "orcid": "0000-0003-0699-6083" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Darvish-B", "name": { "family": "Darvish", "given": "B." }, "orcid": "0000-0003-4919-9017" }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Casey-C-M", "name": { "family": "Casey", "given": "C. M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Murchikova-L", "name": { "family": "Murchikova", "given": "L." } }, { "id": "Koda-Jin", "name": { "family": "Koda", "given": "J." }, "orcid": "0000-0002-8762-7863" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Vlahakis-Catherine", "name": { "family": "Vlahakis", "given": "Catherine" }, "orcid": "0000-0003-3745-4228" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Morokuma-Matsui-K", "name": { "family": "Morokuma-Matsui", "given": "K." } }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Pope-Alexandra", "name": { "family": "Pope", "given": "A." }, "orcid": "0000-0001-8592-2706" }, { "id": "Toft-S", "name": { "family": "Toft", "given": "S." }, "orcid": "0000-0003-3631-7176" }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "D." }, "orcid": "0000-0001-5382-6138" } ] }, "title": "Evolution of Interstellar Medium, Star Formation, and Accretion at High Redshift", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks \u2013 evolution \u2013 galaxies: ISM \u2013 galaxies: starburst", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 December 2; revised 2017 February 15; accepted 2017 February 16; published 2017 March 15. \n\nWe thank Zara Scoville for proofreading the manuscript, and we thank the referee for a number of constructive suggestions. In addition, several useful references on the Galactic GMCs were provided by John Carpenter and John Bally, and good suggestions were provided by Fabian Walter. This paper makes use of the following ALMA data: ADS/JAO.ALMA 2011.0.00097.S, 2012.1.00076.S, 2012.1.00523.S, 2013.1.00034.S, 2013.1.00111.S, 2015.1.00137.S, 2013.1.00118.S, and 2013.1.00151.S. We plan to release the images used here via the IPAC/IRSA COSMOS archive at http://irsa.ipac.caltech.edu/data/COSMOS/ in 2017. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. R.J.I. acknowledges support from the European Research Council (ERC) in the form of Advanced Grant 321302, COSMICISM. S.T. acknowledges support from the European Research Council in the form of Consolidator Grant 648179, ConTExt. B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G.\n\nPublished - Scoville_2017_ApJ_837_150.pdf
Submitted - 1702.04729.pdf
", "abstract": "ALMA observations of the long wavelength dust continuum are used to estimate the interstellar medium (ISM) masses in a sample of 708 galaxies at z = 0.3 to 4.5 in the COSMOS field. The galaxy sample has known far-infrared luminosities and, hence, star formation rates (SFRs) and stellar masses (M\u2217) from the optical\u2013infrared spectrum fitting. The galaxies sample SFRs from the main sequence (MS) to 50 times above the MS. The derived ISM masses are used to determine the dependence of gas mass on redshift, M\u2217, and specific SFR (sSFR) relative to the MS. The ISM masses increase approximately with the 0.63 power of the rate of increase in SFRs with redshift and the 0.32 power of the sSFR/sSFRMS. The SF efficiencies also increase as the 0.36 power of the SFR redshift evolution and the 0.7 power of the elevation above the MS; thus the increased activities at early epochs are driven by both increased ISM masses and SF efficiency. Using the derived ISM mass function, we estimate the accretion rates of gas required to maintain continuity of the MS evolution (> 100 M\u2299 yr^(\u22121) at z > 2.5). Simple power-law dependencies are similarly derived for the gas accretion rates. We argue that the overall evolution of galaxies is driven by the rates of gas accretion. The cosmic evolution of total ISM mass is estimated and linked to the evolution of SF and active galactic nucleus activity at early epochs.", "date": "2017-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "837", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 150", "id_number": "CaltechAUTHORS:20170314-095505234", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170314-095505234", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "321302" }, { "agency": "European Research Council (ERC)", "grant_number": "648179" }, { "agency": "NASA", "grant_number": "NNX12AE20G" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "COSMOS", "value": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)", "value": "Infrared Processing and Analysis Center (IPAC)" }, { "id": "Astronomy-Department", "value": "Astronomy Department" } ] }, "doi": "10.3847/1538-4357/aa61a0", "primary_object": { "basename": "Scoville_2017_ApJ_837_150.pdf", "url": "https://authors.library.caltech.edu/records/wqjb8-j7y65/files/Scoville_2017_ApJ_837_150.pdf" }, "related_objects": [ { "basename": "1702.04729.pdf", "url": "https://authors.library.caltech.edu/records/wqjb8-j7y65/files/1702.04729.pdf" } ], "pub_year": "2017", "author_list": "Scoville, N.; Lee, N.; et el." }, { "id": "https://authors.library.caltech.edu/records/jc2ea-9dn42", "eprint_id": 74592, "eprint_status": "archive", "datestamp": "2023-08-19 01:54:58", "lastmod": "2023-10-24 22:47:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Darvish-B", "name": { "family": "Darvish", "given": "Behnam" }, "orcid": "0000-0003-4919-9017" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Sobral-D", "name": { "family": "Sobral", "given": "David" }, "orcid": "0000-0001-8823-4845" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Stroe-A", "name": { "family": "Stroe", "given": "Andra" } }, { "id": "Hemmati-S", "name": { "family": "Hemmati", "given": "Shoubaneh" }, "orcid": "0000-0003-2226-5395" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "Jeyhan" }, "orcid": "0000-0001-9187-3605" } ] }, "title": "Cosmic Web of Galaxies in the COSMOS Field: Public Catalog and Different Quenching for Centrals and Satellites", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: high-redshift \u2013 large-scale structure of universe", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 November 3; revised 2016 December 23; accepted 2017 January 5; published 2017 February 28. \n\nWe are immensely grateful to the anonymous referee for their useful comments that greatly improved the quality of this work. B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. B.D. wishes to thank Adam Muzzin for his useful comments. D.S. acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. This work is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.\n\nPublished - Darvish_2017_ApJ_837_16.pdf
Submitted - 1611.05451.pdf
", "abstract": "We use a mass complete (log(M/M\u2299) \u2a7e 9.6) sample of galaxies with accurate photometric redshifts in the COSMOS field to construct the density field and the cosmic web to z = 1.2. The comic web extraction relies on the density field Hessian matrix and breaks the density field into clusters, filaments, and the field. We provide the density field and cosmic web measures to the community. We show that at z \u227e 0.8, the median star formation rate (SFR) in the cosmic web gradually declines from the field to clusters and this decline is especially sharp for satellites (~1 dex versus ~0.5 dex for centrals). However, at z \u2273 0.8, the trend flattens out for the overall galaxy population and satellites. For star-forming (SF) galaxies only, the median SFR is constant at z \u2273 0.5 but declines by ~0.3\u20130.4 dex from the field to clusters for satellites and centrals at z \u227e 0.5. We argue that for satellites, the main role of the cosmic web environment is to control their SF fraction, whereas for centrals, it is mainly to control their overall SFR at z \u227e 0.5 and to set their fraction at z \u2273 0.5. We suggest that most satellites experience a rapid quenching mechanism as they fall from the field into clusters through filaments, whereas centrals mostly undergo a slow environmental quenching at z \u227e 0.5 and a fast mechanism at higher redshifts. Our preliminary results highlight the importance of the large-scale cosmic web on galaxy evolution.", "date": "2017-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "837", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 16", "id_number": "CaltechAUTHORS:20170228-105001611", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170228-105001611", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX12AE20G" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "Lancaster University", "grant_number": "A100679" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "COSMOS", "value": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)", "value": "Infrared Processing and Analysis Center (IPAC)" }, { "id": "Astronomy-Department", "value": "Astronomy Department" } ] }, "doi": "10.3847/1538-4357/837/1/16", "primary_object": { "basename": "Darvish_2017_ApJ_837_16.pdf", "url": "https://authors.library.caltech.edu/records/jc2ea-9dn42/files/Darvish_2017_ApJ_837_16.pdf" }, "related_objects": [ { "basename": "1611.05451.pdf", "url": "https://authors.library.caltech.edu/records/jc2ea-9dn42/files/1611.05451.pdf" } ], "pub_year": "2017", "author_list": "Darvish, Behnam; Mobasher, Bahram; et el." }, { "id": "https://authors.library.caltech.edu/records/9xmmb-b7662", "eprint_id": 76598, "eprint_status": "archive", "datestamp": "2023-08-22 19:47:32", "lastmod": "2023-10-25 16:08:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pelliccia-D", "name": { "family": "Pelliccia", "given": "D." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Epinat-B", "name": { "family": "Epinat", "given": "B." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Amram-P", "name": { "family": "Amram", "given": "P." } }, { "id": "Lemaux-B-C", "name": { "family": "Lemaux", "given": "B. C." }, "orcid": "0000-0002-1428-7036" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } } ] }, "title": "HR-COSMOS: Kinematics of star-forming galaxies at z ~ 0.9", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution galaxies: kinematics and dynamics; galaxies: high-redshift; galaxies: statistics, surveys", "note": "\u00a9 2017 ESO. \n\nReceived: 6 June 2016. Accepted: 19 September 2016. \n\nWe wish to thank the ESO staff at Paranal Observatory and especially the VIMOS team at ESO for their support during observations. We thank Bodo Ziegler for useful discussion, comments, and suggestions during the preparation of the observations and Katarina Kova\u010d for kindly providing us with their environment measurements. D.P. and L.T. wish to thank Alisson Michel and Bruno Ribeiro for their help with programming codes. We thank Marco Scodeggio for his assistance during the preparation of the observations and the data reduction. D.P. gratefully acknowledges Lori Lubin and UC Davis hospitality during the last phases of the project. We thank Alfred Tiley for providing us with their non-public measurements. This paper is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.\n\nPublished - aa29064-16.pdf
Submitted - 1606.01934.pdf
", "abstract": "We present the kinematic analysis of a sub-sample of 82 galaxies at 0.75 < z < 1.2 from our new survey HR-COSMOS aimed to obtain the first statistical sample to study the kinematics of star-forming galaxies in the treasury COSMOS field at 0 < z < 1.2. We observed 766 emission line galaxies using the multi-slit spectrograph ESO-VLT/VIMOS in high-resolution mode (R = 2500). To better extract galaxy kinematics, VIMOS spectral slits have been carefully tilted along the major axis orientation of the galaxies, making use of the position angle measurements from the high spatial resolution HST/ACS COSMOS images. We constrained the kinematics of the sub-sample at 0.75 < z < 1.2 by creating high-resolution semi-analytical models. We established the stellar-mass Tully-Fisher relation at z \u2243 0.9 with high-quality stellar mass measurements derived using the latest COSMOS photometric catalog, which includes the latest data releases of UltraVISTA and Spitzer. In doubling the sample at these redshifts compared with the literature, we estimated the relation without setting its slope, and found it consistent with previous studies in other deep extragalactic fields assuming no significant evolution of the relation with redshift at z \u2272 1. We computed dynamical masses within the radius R_(2.2) and found a median stellar-to-dynamical mass fraction equal to 0.2 (assuming Chabrier IMF), which implies a contribution of gas and dark matter masses of 80% of the total mass within R_(2.2), in agreement with recent integral field spectroscopy surveys. We find no dependence of the stellar-mass Tully-Fisher relation with environment probing up to group scale masses. This study shows that multi-slit galaxy surveys remain a powerful tool to derive kinematics for large numbers of galaxies at both high and low redshift.", "date": "2017-03", "date_type": "published", "publication": "Astronomy & Astrophysics", "volume": "599", "publisher": "EDP Sciences", "pagerange": "Art. No. A25", "id_number": "CaltechAUTHORS:20170417-111541471", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170417-111541471", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1051/0004-6361/201629064", "primary_object": { "basename": "1606.01934.pdf", "url": "https://authors.library.caltech.edu/records/9xmmb-b7662/files/1606.01934.pdf" }, "related_objects": [ { "basename": "aa29064-16.pdf", "url": "https://authors.library.caltech.edu/records/9xmmb-b7662/files/aa29064-16.pdf" } ], "pub_year": "2017", "author_list": "Pelliccia, D.; Tresse, L.; et el." }, { "id": "https://authors.library.caltech.edu/records/qp0dq-ss803", "eprint_id": 78576, "eprint_status": "archive", "datestamp": "2023-08-19 01:36:44", "lastmod": "2023-10-26 00:11:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pacucci-F", "name": { "family": "Pacucci", "given": "Fabio" }, "orcid": "0000-0001-9879-7780" }, { "id": "Pallottini-A", "name": { "family": "Pallottini", "given": "Andrea" } }, { "id": "Ferrara-A", "name": { "family": "Ferrara", "given": "Andrea" }, "orcid": "0000-0002-9400-7312" }, { "id": "Gallerani-S", "name": { "family": "Gallerani", "given": "Simona" } } ] }, "title": "The nature of the Lyman \u03b1 emitter CR7: a persisting puzzle", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nWe thank Rebecca Bowler and Eli Visbal for their valuable comments. FP acknowledges the ADAP grant No. MA160009.", "abstract": "The peculiar emission properties of the z \u223c 6.6 Ly\u03b1 emitter COSMOS redshift 7 (CR7) have been initially interpreted with the presence of either a direct collapse black hole (DCBH) or a substantial mass of Pop III stars. Instead, updated photometric observations by Bowler et al. seem to suggest that CR7 is a more standard system. Here, we confirm that the original DCBH hypothesis is consistent also with the new data. Using radiation-hydrodynamic simulations, we reproduce the new infrared photometry with two models involving a Compton-thick DCBH of mass \u22487 \u00d7 106\u2009M\u2299 accreting (a) metal-free (Z = 0) gas with column density NH = 8 \u00d7 1025\u2009cm\u22122 or (b) low-metallicity gas (Z = 5 \u00d7 10\u22123\u2009Z\u2299) with NH = 3 \u00d7 1024\u2009cm\u22122. The best-fitting model reproduces the photometric data to within 1\u03c3. Such metals can be produced by weak star-forming activity occurring after the formation of the DCBH. The main contribution to the Spitzer/IRAC 3.6\u2009\u03bcm photometric band in both models is due to He\u2009I/He\u2009II \u03bb\u03bb4714, 4687 emission lines, while the contribution of [O\u2009III] \u03bb\u03bb4959, 5007 emission lines, if present, is sub-dominant. Spectroscopic observations with JWST will be required to ultimately clarify the nature of CR7.", "date": "2017-02-20", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society: Letters", "volume": "468", "number": "1", "publisher": "Oxford University Press", "pagerange": "L77-L81", "id_number": "CaltechAUTHORS:20170626-150842064", "issn": "1745-3925", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170626-150842064", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "SPLASH", "value": "SPLASH" }, { "id": "COSMOS", "value": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)", "value": "Infrared Processing and Analysis Center (IPAC)" } ] }, "doi": "10.1093/mnrasl/slx029", "pub_year": "2017", "author_list": "Pacucci, Fabio; Pallottini, Andrea; et el." }, { "id": "https://authors.library.caltech.edu/records/kba2b-39f23", "eprint_id": 74001, "eprint_status": "archive", "datestamp": "2023-08-19 01:22:17", "lastmod": "2023-10-24 21:59:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Walter-F", "name": { "family": "Walter", "given": "Fabian" }, "orcid": "0000-0003-4793-7880" }, { "id": "Bolatto-A-D", "name": { "family": "Bolatto", "given": "Alberto D." }, "orcid": "0000-0002-5480-5686" }, { "id": "Leroy-A-K", "name": { "family": "Leroy", "given": "Adam K." }, "orcid": "0000-0002-2545-1700" }, { "id": "Veilleux-S", "name": { "family": "Veilleux", "given": "Sylvain" }, "orcid": "0000-0002-3158-6820" }, { "id": "Warren-S-R", "name": { "family": "Warren", "given": "Steven R." } }, { "id": "Hodge-J-A", "name": { "family": "Hodge", "given": "Jacqueline" }, "orcid": "0000-0001-6586-8845" }, { "id": "Levy-R-C", "name": { "family": "Levy", "given": "Rebecca C." } }, { "id": "Meier-D-S", "name": { "family": "Meier", "given": "David S." }, "orcid": "0000-0001-9436-9471" }, { "id": "Ostriker-E-C", "name": { "family": "Ostriker", "given": "Eve C." } }, { "id": "Ott-J", "name": { "family": "Ott", "given": "J\u00fcrgen" }, "orcid": "0000-0001-8224-1956" }, { "id": "Rosolowsky-E", "name": { "family": "Rosolowsky", "given": "Erik" }, "orcid": "0000-0002-5204-2259" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Weiss-Axel", "name": { "family": "Weiss", "given": "Axel" }, "orcid": "0000-0003-4678-3939" }, { "id": "Zschaechner-L-K", "name": { "family": "Zschaechner", "given": "Laura" }, "orcid": "0000-0002-9919-8672" }, { "id": "Zwaan-M", "name": { "family": "Zwaan", "given": "Martin" } } ] }, "title": "Dense Molecular Gas Tracers in the Outflow of the Starburst Galaxy NGC 253", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 August 8; revised 2016 December 16; accepted 2016 December 28; published 2017 February 1. \n\nWe thank the referee for excellent comments that improved the paper. D.S.M. acknowledges partial support by the National Science Foundation through grant AST-1009620. S.V. acknowledges NSF grant AST-1009583. A.D.B. acknowledges visiting support by the Alexander von Humboldt Foundation, and support by the National Science Foundation through a CAREER grant AST-0955836 and AST-1412419. E.C.O. is supported by the National Science Foundation through grant AST-1312006. This paper makes use of the following ALMA data: ADS/JAO.ALMA #2011.0.00172.S, #2012.1.00108.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute (STScI). Some of the HST data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST), others were acquired under program HST-GO-13730 with support provided by NASA through a grant from the STScI. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. The Mopra radio telescope is part of the Australia Telescope National Facility, which is funded by the Australian Government for operation as a National Facility managed by CSIRO. Based on observations carried out under project number 209-14 with the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).\n\nPublished - Walter_2017_ApJ_835_265.pdf
Submitted - 1701.05040v1.pdf
", "abstract": "We present a detailed study of a molecular outflow feature in the nearby starburst galaxy NGC 253 using ALMA. We find that this feature is clearly associated with the edge of NGC 253's prominent ionized outflow, has a projected length of ~300 pc, with a width of ~50 pc, and a velocity dispersion of ~40 km s^(\u22121), which is consistent with an ejection from the disk about 1 Myr ago. The kinematics of the molecular gas in this feature can be interpreted (albeit not uniquely) as accelerating at a rate of 1 km s^(\u22121) pc^(\u22121). In this scenario, the gas is approaching an escape velocity at the last measured point. Strikingly, bright tracers of dense molecular gas (HCN, CN, HCO^+, CS) are also detected in the molecular outflow: we measure an HCN(1\u20130)/CO(1\u20130) line ratio of ~1/10 in the outflow, similar to that in the central starburst region of NGC 253 and other starburst galaxies. By contrast, the HCN/CO line ratio in the NGC 253 disk is significantly lower (~1/30), similar to other nearby galaxy disks. This strongly suggests that the streamer gas originates from the starburst, and that its physical state does not change significantly over timescales of ~1 Myr during its entrainment in the outflow. Simple calculations indicate that radiation pressure is not the main mechanism for driving the outflow. The presence of such dense material in molecular outflows needs to be accounted for in simulations of galactic outflows.", "date": "2017-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "835", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 265", "id_number": "CaltechAUTHORS:20170203-075924919", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170203-075924919", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1009620" }, { "agency": "NSF", "grant_number": "AST-1009583" }, { "agency": "Alexander von Humboldt Foundation" }, { "agency": "NSF", "grant_number": "AST-0955836" }, { "agency": "NSF", "grant_number": "AST-1412419" }, { "agency": "NSF", "grant_number": "AST-1312006" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "Australian Government" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "COSMOS", "value": "COSMOS" }, { "id": "Astronomy-Department", "value": "Astronomy Department" } ] }, "doi": "10.3847/1538-4357/835/2/265", "primary_object": { "basename": "Walter_2017_ApJ_835_265.pdf", "url": "https://authors.library.caltech.edu/records/kba2b-39f23/files/Walter_2017_ApJ_835_265.pdf" }, "related_objects": [ { "basename": "1701.05040v1.pdf", "url": "https://authors.library.caltech.edu/records/kba2b-39f23/files/1701.05040v1.pdf" } ], "pub_year": "2017", "author_list": "Walter, Fabian; Bolatto, Alberto D.; et el." }, { "id": "https://authors.library.caltech.edu/records/enmt0-yc948", "eprint_id": 73790, "eprint_status": "archive", "datestamp": "2023-08-22 19:40:19", "lastmod": "2023-10-24 16:27:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Manohar-S", "name": { "family": "Manohar", "given": "Swarnima" } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" } ] }, "title": "What Lurks in ULIRGs?\u2014Probing the Chemistry and Excitation of Molecular Gas in the Nuclei of Arp 220 and NGC 6240", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (Arp 220 and NGC 6240); galaxies: starburst", "note": "\u00a9 2017. The American Astronomical Society. \n\nReceived 2016 February 23; revised 2016 November 25; accepted 2016 December 7; published 2017 January 23. \n\nWe thank our referee for the thorough report which has helped improve the paper. We gratefully acknowledge the assistance of Anneila Sargent for suggestions and improvements on the manuscript. We thank the staff of CARMA for their help with carrying out the observations and calibrations. We thank Marc W. Pound and Peter Teuben for their invaluable help with data reduction. CARMA development and operations were supported by the National Science Foundation grants AST-0838260 and AST-1140063 under a cooperative agreement, and by the CARMA partner universities. We acknowledge student support from NRAO under grants AST-0956545 and AST-0836064. We thank Jin Koda for lending us the LVG modeling code.\n\nPublished - Manohar_2017_ApJ_835_127.pdf
", "abstract": "We have imaged the dense star-forming regions of Arp 220 and NGC 6240 in the 3 mm band transitions of CO, HCN, HCO^+, HNC, and CS at 0farcs5\u20130farcs8 resolution using CARMA. Our data set images all these lines at similar resolutions and high sensitivity, and can be used to derive line ratios of faint high excitation lines. In both the nuclei of Arp 220, the HCN/HNC ratios suggest chemistry of X-ray Dominated Regions (XDRs)\u2014a likely signature of an active galactic nucleus. In NGC 6240, there is no evidence of XDR type chemistry, but there the bulk of the molecular gas is concentrated between the nuclei rather than on them. We calculated molecular H_2 densities from excitation analysis of each of the molecular species. It appears that the abundances of HNC and HCO^+ in Ultra Luminous Infrared Galaxies may be significantly different from those in galactic molecular clouds. The derived H_2 volume densities are ~5 \u00d7 10^4 cm^(\u22123) in the Arp 220 nuclei and ~10^4 cm^(\u22123) in NGC 6240.", "date": "2017-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "835", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 127", "id_number": "CaltechAUTHORS:20170127-144614468", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170127-144614468", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0838260" }, { "agency": "NSF", "grant_number": "AST-1140063" }, { "agency": "CARMA partner universities" }, { "agency": "NSF", "grant_number": "AST-0956545" }, { "agency": "NSF", "grant_number": "AST-0836064" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/835/2/127", "primary_object": { "basename": "Manohar_2017_ApJ_835_127.pdf", "url": "https://authors.library.caltech.edu/records/enmt0-yc948/files/Manohar_2017_ApJ_835_127.pdf" }, "pub_year": "2017", "author_list": "Manohar, Swarnima and Scoville, Nick" }, { "id": "https://authors.library.caltech.edu/records/jnsjm-gp344", "eprint_id": 73577, "eprint_status": "archive", "datestamp": "2023-08-22 19:25:31", "lastmod": "2023-10-24 15:29:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nayyeri-H", "name": { "family": "Nayyeri", "given": "H." }, "orcid": "0000-0001-8242-9983" }, { "id": "Hemmati-S", "name": { "family": "Hemmati", "given": "S." }, "orcid": "0000-0003-2226-5395" }, { "id": "Darvish-B", "name": { "family": "Darvish", "given": "B." }, "orcid": "0000-0003-4919-9017" } ] }, "title": "CANDELS Multi-wavelength Catalogs: Source Identification and Photometry in the CANDELS COSMOS Survey Field", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: high-redshift; galaxies: photometry; methods: data analysis; techniques: image processing", "note": "\u00a9 2017. The American Astronomical Society. \n\nReceived 2016 May 17. Accepted 2016 November 24. Published 2017 January 13. \n\nWe wish to thank the anonymous referee for carefully reading the original manuscript and providing very useful suggestions. We also thank S. Fleming for his help with the MAST archive. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Financial support for this work was provided by NSF through AST-1313319 for H.N. and A.C. H.N. further acknowledges support from NASA (grant No. NNX16AF39G). This work is based in part on data products from observations made with ESO Telescopes at the La Silla Paranal Observatories under ESO programme ID 179.A-2005 and on data products produced by TER- APIX and the Cambridge Astronomy survey Unit on be- half of the UltraVISTA consortium. This study was based in part on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada\u2013France\u2013Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scienti que (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada\u2013France\u2013Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS.\n\nPublished - Nayyeri_2017_ApJS_228_7.pdf
Submitted - 1612.07364v1.pdf
", "abstract": "We present a multi-wavelength photometric catalog in the COSMOS field as part of the observations by the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. The catalog is based on Hubble Space Telescope Wide Field Camera 3 (HST/WFC3) and Advanced Camera for Surveys observations of the COSMOS field (centered at R.A.: 10^h00^m28^s, Decl.:+02^\u00ba12^'21^\"). The final catalog has 38671 sources with photometric data in 42 bands from UV to the infrared (~ 0.3-8 \u00b5m). This includes broadband photometry from HST, CFHT, Subaru, the Visible and Infrared Survey Telescope for Astronomy, and Spitzer Space Telescope in the visible, near-infrared, and infrared bands along with intermediate- and narrowband photometry from Subaru and medium-band data from Mayall NEWFIRM. Source detection was conducted in the WFC3 F160W band (at 1.6 \u03bcm) and photometry is generated using the Template FITting algorithm. We further present a catalog of the physical properties of sources as identified in the HST F160W band and measured from the multi-band photometry by fitting the observed spectral energy distributions of sources against templates.", "date": "2017-01", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "228", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 7", "id_number": "CaltechAUTHORS:20170120-113640786", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170120-113640786", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "AST-1313319" }, { "agency": "NASA", "grant_number": "NNX16AF39G" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "doi": "10.3847/1538-4365/228/1/7", "primary_object": { "basename": "1612.07364v1.pdf", "url": "https://authors.library.caltech.edu/records/jnsjm-gp344/files/1612.07364v1.pdf" }, "related_objects": [ { "basename": "Nayyeri_2017_ApJS_228_7.pdf", "url": "https://authors.library.caltech.edu/records/jnsjm-gp344/files/Nayyeri_2017_ApJS_228_7.pdf" } ], "pub_year": "2017", "author_list": "Nayyeri, H.; Hemmati, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/56s6g-t6443", "eprint_id": 75025, "eprint_status": "archive", "datestamp": "2023-08-19 00:51:41", "lastmod": "2023-10-25 14:40:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Miettinen-O", "name": { "family": "Miettinen", "given": "O." } }, { "id": "Delvecchio-I", "name": { "family": "Delvecchio", "given": "I." }, "orcid": "0000-0001-8706-2252" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Novak-Mladen", "name": { "family": "Novak", "given": "M." }, "orcid": "0000-0001-8695-825X" }, { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Intema-H-T", "name": { "family": "Intema", "given": "H. T." }, "orcid": "0000-0002-5880-2730" }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" } ] }, "title": "(Sub)millimetre interferometric imaging of a sample of COSMOS/AzTEC submillimetre galaxies. IV. Physical properties derived from spectral energy distributions", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: formation \u2013 galaxies: starburst \u2013 galaxies: star formation \u2013 radio continuum: galaxies \u2013 submillimeter: galaxies", "note": "\u00a9 2016 ESO. \n\nReceived: 14 January 2016; Accepted: 2 September 2016; Published online 19 December 2016. \n\nWe would like to thank the anonymous referee for \u2009providing us with comments and suggestions.\u2009This research was funded by the European Union's Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). This work was completed at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1066293. This work was partially supported by a grant from the Simons Foundation. M.A. acknowledges partial support from FONDECYT through grant 1140099. A.K. acknowledges support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2012.1.00978.S and ADS/JAO.ALMA#2013.1.00118.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This paper is also partly based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This research has made use of NASA's Astrophysics Data System, and the NASA/IPAC Infrared Science Archive, which is operated by the JPL, California Institute of Technology, under contract with the NASA. We greatfully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information on the COSMOS survey is available at http://cosmos.astro.caltech.edu. \n\nPACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). \n\nSPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).\n\nPublished - aa28128-16.pdf
Submitted - 1609.01157.pdf
", "abstract": "Context. Submillimetre galaxies (SMGs) in the early Universe are potential antecedents of the most massive galaxies we see in the present-day Universe. An important step towards quantifying this galactic evolutionary connection is to investigate the fundamental physical properties of SMGs, such as their stellar mass content (M\u22c6) and star formation rate (SFR).\nAims. We attempt to characterise the physical nature of a 1.1 mm selected, flux-limited, and interferometrically followed up sample of SMGs in the COSMOS field.\nMethods. We used the latest release of the MAGPHYS code to fit the multiwavelength (UV to radio) spectral energy distributions (SEDs) of 16 of the target SMGs, which lie at redshifts z \u2243 1.6\u22125.3. We also constructed the pure radio SEDs of our SMGs using three different radio bands (325 MHz, 1.4 GHz, and 3 GHz). Moreover, since two SMGs in our sample, AzTEC 1 and AzTEC 3, benefit from previous ^(12)C^(16)O line observations, we studied their properties in more detail.\nResults. The median and 16th\u201384th percentile ranges of M\u22c6, infrared (8\u22121000 \u03bcm) luminosity (L_(IR)), SFR, dust temperature (T_(dust)), and dust mass (M_(dust)) were derived to be log\u2009(M\u22c6/M\u2299) = 10.96^(+0.34)_(-0.19), log\u2009(L_(IR)/L\u2299) = 12.93^(+0.09)_(-0.19), SFR = 856^(+191)_(-310)M\u2299 yr^(-1), T_(dust) = 40.6^(+7.5)_(-8.1) K, and log\u2009(M_(dust)/M\u2299) = 9.17^(+0.03)_(-0.33), respectively. We found that 63% of our target SMGs lie above the galaxy main sequence by more than a factor of 3 and, hence, are starbursts. The 3 GHz radio sizes we have previously measured for the target SMGs were compared with the present M\u22c6 estimates, and we found that the z > 3 SMGs are fairly consistent with the mass\u2013size relationship of z ~ 2 compact, quiescent galaxies (cQGs). The median radio spectral index is found to be \u03b1 = \u22120.77^(+0.28)_(-0.42). The median IR-radio correlation parameter is found to be q = 2.27^(+0.27)_(-0.13), which is lower than was measured locally (median q = 2.64). The gas-to-dust mass ratio for AzTEC 1 is derived to be \u03b4_(gdr) = 90^(+23)_(-19), while that for AzTEC 3 is 33^(+28)_(-18). AzTEC 1 is found to have a sub-Eddington SFR surface density (by a factor of 2.6^(+0.2)_(-0.1)), while AzTEC 3 appears to be an Eddington-limited starburster. The gas reservoir in these two high-z SMGs would be exhausted in only ~ 86 and 19 Myr at the current SFR, respectively.\nConclusions. A comparison of the MAGPHYS-based properties of our SMGs with those of equally bright SMGs in the ECDFS field (the ALESS SMGs) that are 870 \u03bcm selected and followed up by ALMA, suggests that the two populations share fairly similar physical characteristics, including the q parameter. The somewhat higher L_(dust) for our sources (factor of 1.9^(+9.3)_(-1.6) on average) can originate in the longer selection wavelength of 1.1 mm. Although the derived median \u03b1 is consistent with a canonical synchrotron spectral index, some of our SMGs exhibit spectral flattening or steepening, which can be attributed to different cosmic-ray energy gain and loss mechanisms. A hint of negative correlation is found between the 3 GHz size and the level of starburstiness and, hence, cosmic-ray electrons in more compact starbursts might be more susceptible to free-free absorption. Some of the derived low and high q values (compared to the local median) could be the result of a specific merger or post-starburst phase of galaxy evolution. Overall, our results, such as the M\u22c6\u20133 GHz radio size analysis and comparison with the stellar masses of z ~ 2 cQGs in concert with the star formation properties of AzTEC 1 and 3, support the scenario where z > 3 SMGs evolve into the present day giant, gas-poor ellipticals.", "date": "2017-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "597", "publisher": "EDP Sciences", "pagerange": "Art. No. A5", "id_number": "CaltechAUTHORS:20170310-104204574", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170310-104204574", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "Simons Foundation" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1140099" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "NASA/JPL/Caltech" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "COSMOS", "value": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)", "value": "Infrared Processing and Analysis Center (IPAC)" }, { "id": "SPLASH", "value": "SPLASH" } ] }, "doi": "10.1051/0004-6361/201628128", "primary_object": { "basename": "1609.01157.pdf", "url": "https://authors.library.caltech.edu/records/56s6g-t6443/files/1609.01157.pdf" }, "related_objects": [ { "basename": "aa28128-16.pdf", "url": "https://authors.library.caltech.edu/records/56s6g-t6443/files/aa28128-16.pdf" } ], "pub_year": "2017", "author_list": "Miettinen, O.; Delvecchio, I.; et el." }, { "id": "https://authors.library.caltech.edu/records/j8mra-79x80", "eprint_id": 75022, "eprint_status": "archive", "datestamp": "2023-08-19 00:51:28", "lastmod": "2023-10-25 14:40:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Miettinen-O", "name": { "family": "Miettinen", "given": "O." } }, { "id": "Tomi\u010di\u0107-N", "name": { "family": "Tomi\u010di\u0107", "given": "N." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Lemaux-B-C", "name": { "family": "Lemaux", "given": "B. C." }, "orcid": "0000-0002-1428-7036" }, { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Chiang-Yi-Kuan", "name": { "family": "Chiang", "given": "Y.-K." } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Delvecchio-I", "name": { "family": "Delvecchio", "given": "I." }, "orcid": "0000-0001-8706-2252" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Jurlin-N", "name": { "family": "Jurlin", "given": "N." } }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "C." } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Marchesi-S", "name": { "family": "Marchesi", "given": "S." }, "orcid": "0000-0001-5544-0749" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D. A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Toft-S", "name": { "family": "Toft", "given": "S." }, "orcid": "0000-0003-3631-7176" } ] }, "title": "(Sub)millimetre interferometric imaging of a sample of COSMOS/AzTEC submillimetre galaxies. III. Environments", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general \u2013 galaxies: evolution \u2013 galaxies: formation \u2013 large-scale structure of Universe \u2013 submillimeter: galaxies", "note": "\u00a9 2016 ESO. \n\nReceived: 17 July 2015; Accepted: 4 April 2016; Published online 19 December 2016. \n\nThis research was funded by the European Union's Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). A.F. wishes to acknowledge Finnish Academy award, decision 266918. This work was supported in part by the National Science Foundation under Grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics. This work is partly based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and and 185.A-0791 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This research has made use of NASA's Astrophysics Data System, and the NASA/IPAC Infrared Science Archive, which is operated by the JPL, California Institute of Technology, under contract with the NASA. We greatfully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/~cosmos. We thank the VUDS team for making the data in the COSMOS field available prior to public release.\n\nPublished - aa26989-15.pdf
Submitted - 1604.01775.pdf
", "abstract": "We investigate the environment of 23 submillimetre galaxies (SMGs) drawn from a signal-to-noise (S/N)-limited sample of SMGs originally discovered in the James Clerk Maxwell Telescope (JCMT)/AzTEC 1.1 mm continuum survey of a Cosmic Evolution Survey (COSMOS) subfield and then followed up with the Submillimetre Array and Plateau de Bure Interferometer at 890 \u03bcm and 1.3 mm, respectively. These SMGs already have well-defined multiwavelength counterparts and redshifts. We also analyse the environments of four COSMOS SMGs spectroscopically confirmed to lie at redshifts z_(spec) > 4.5, and one at z_(spec) = 2.49 resulting in a total SMG sample size of 28. We search for overdensities using the COSMOS photometric redshifts based on over 30 UV-NIR photometric measurements including the new UltraVISTA data release 2 and Spitzer/SPLASH data, and reaching an accuracy of \u03c3_(\u0394z/ (1 + z)) = 0.0067 (0.0155) at z < 3.5 (>3.5). To identify overdensities we apply the Voronoi tessellation analysis, and estimate the redshift-space overdensity estimator \u03b4_g as a function of distance from the SMG and/or overdensity centre. We test and validate our approach via simulations, X-ray detected groups or clusters, and spectroscopic verifications using VUDS and zCOSMOS catalogues which show that even with photometric redshifts in the COSMOS field we can efficiently retrieve overdensities out to z \u2248 5. Our results yield that 11 out of 23 (48%) JCMT/AzTEC 1.1 mm SMGs occupy overdense environments. Considering the entire JCMT/AzTEC 1.1 mm S/N \u2265 4 sample and taking the expected fraction of spurious detections into account, this means that 35\u201361% of the SMGs in the S/N-limited sample occupy overdense environments. We perform an X-ray stacking analysis in the 0.5\u20132 keV band using a 32\u2033 aperture and our SMG positions, and find statistically significant detections. For our z < 2 subsample we find an average flux of (4.0 \u00b1 0.8) \u00d7 10^(-16) erg s^(-1) cm^(-2) and a corresponding total mass of M_(200) = 2.8 \u00d7 10^(13)M\u2299. The z > 2 subsample yields an average flux of (1.3 \u00b1 0.5) \u00d7 10^(-16) erg s^(-1) cm^(-2) and a corresponding total massof M_(200) = 2 \u00d7 10^(13)M\u2299. Our results suggest a higher occurrence of SMGs occupying overdense environments at z \u2265 3 than at z < 3. This may be understood if highly star-forming galaxies can only be formed in the highest peaks of the density field tracing the most massive dark matter haloes at early cosmic epochs, while at later times cosmic structure may have matured sufficiently that more modest overdensities correspond to sufficiently massive haloes to form SMGs.", "date": "2017-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "597", "publisher": "EDP Sciences", "pagerange": "Art. No. A4", "id_number": "CaltechAUTHORS:20170310-101901398", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170310-101901398", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "Academy of Finland", "grant_number": "266918" }, { "agency": "NSF", "grant_number": "PHYS-1066293" }, { "agency": "NASA/JPL/Caltech" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "COSMOS", "value": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)", "value": "Infrared Processing and Analysis Center (IPAC)" }, { "id": "SPLASH", "value": "SPLASH" } ] }, "doi": "10.1051/0004-6361/201526989", "primary_object": { "basename": "1604.01775.pdf", "url": "https://authors.library.caltech.edu/records/j8mra-79x80/files/1604.01775.pdf" }, "related_objects": [ { "basename": "aa26989-15.pdf", "url": "https://authors.library.caltech.edu/records/j8mra-79x80/files/aa26989-15.pdf" } ], "pub_year": "2017", "author_list": "Smol\u010di\u0107, V.; Miettinen, O.; et el." }, { "id": "https://authors.library.caltech.edu/records/pepap-vs691", "eprint_id": 75021, "eprint_status": "archive", "datestamp": "2023-08-19 00:51:20", "lastmod": "2023-10-25 14:40:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Thomas-R", "name": { "family": "Thomas", "given": "R." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "VIMOS Ultra-Deep Survey (VUDS): IGM transmission towards galaxies with 2.5 < z < 5.5 and the colour selection of high-redshift galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxy: evolution \u2013 Galaxy: formation \u2013 galaxies: high-redshift \u2013 cosmology: observations \u2013 large-scale structure of Universe", "note": "\u00a9 2017 ESO. \n\nReceived 14 November 2014; Accepted 28 June; Published online 09 January 2017. \n\nBased on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Program 185.A-0791. \n\nWe thank G. Becker, J. M. Deharveng, A. Inoue, C. P\u00e9roux, and M. Pieri for useful discussions. This work is supported by funding from the European Research Council Advanced Grant ERC-2010-AdG-268107-EARLY and by INAF Grants PRIN 2010, PRIN 2012 and PICS 2013. A.C., O.C., M.T. and V.S. acknowledge the grant MIUR PRIN 2010\u20132011. This work is based on data products made available at the CESAM data center, Laboratoire d'Astrophysique de Marseille, France.\n\nPublished - aa25342-14.pdf
Submitted - 1411.5692.pdf
", "abstract": "The observed UV rest-frame spectra of distant galaxies are the result of their intrinsic emission combined with absorption along the line of sight produced by the inter-galactic medium (IGM). Here we analyse the evolution of the mean IGM transmission Tr(Ly\u03b1) and its dispersion along the line of sight for 2127 galaxies with 2.5 < z < 5.5 in the VIMOS Ultra Deep Survey (VUDS). We fitted model spectra combined with a range of IGM transmission to the galaxy spectra using the spectral fitting algorithm GOSSIP+. We used these fits to derive the mean IGM transmission towards each galaxy for several redshift slices from z = 2.5 to z = 5.5. We found that the mean IGM transmission defined as Tr(Ly\u03b1) = e^(\u2212\u03c4) (with \u03c4 as the HI optical depth) is 79%, 69%, 59%, 55%, and 46% at redshifts 2.75, 3.22, 3.70, 4.23, and 4.77, respectively. We compared these results to measurements obtained from quasar lines of sight and found that the IGM transmission towards galaxies is in excellent agreement with quasar values up to redshift z ~ 4. We found tentative evidence for a higher IGM transmission at z \u2265 4 compared to results from QSOs, but a degeneracy between dust extinction and IGM prevents us from firmly concluding whether the internal dust extinction for star-forming galaxies at z > 4 takes a mean value significantly in excess of E(B\u2212V) > 0.15. Most importantly, we found a large dispersion of IGM transmission along the lines of sight towards distant galaxies with 68% of the distribution within 10 to 17% of the median value in \u03b4z = 0.5 bins, similar to what is found on the lines of sight towards QSOs. We demonstrate that taking this broad range of IGM transmission into account is important when selecting high-redshift galaxies based on their colour properties (e.g. LBG or photometric redshiftselection) because failing to do so causes a significant incompleteness in selecting high-redshift galaxy populations. We finally discuss the observed IGM properties and speculate that the broad range of observed transmissions might be the result of cosmic variance and clustering along lines of sight. This clearly shows that the sources that cause this extinction need to be more completely modelled.", "date": "2017-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "597", "publisher": "EDP Sciences", "pagerange": "Art. No. A88", "id_number": "CaltechAUTHORS:20170310-100841812", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170310-100841812", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "ERC-2010-AdG-268107-EARLY" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2010" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2012" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PICS 2013" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)", "grant_number": "PRIN 2010-2011" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "COSMOS", "value": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)", "value": "Infrared Processing and Analysis Center (IPAC)" }, { "id": "Astronomy-Department", "value": "Astronomy Department" } ] }, "doi": "10.1051/0004-6361/201425342", "primary_object": { "basename": "aa25342-14.pdf", "url": "https://authors.library.caltech.edu/records/pepap-vs691/files/aa25342-14.pdf" }, "related_objects": [ { "basename": "1411.5692.pdf", "url": "https://authors.library.caltech.edu/records/pepap-vs691/files/1411.5692.pdf" } ], "pub_year": "2017", "author_list": "Thomas, R.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/0z0h0-5b386", "eprint_id": 78657, "eprint_status": "archive", "datestamp": "2023-08-19 00:41:39", "lastmod": "2023-10-26 00:16:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mortlock-A", "name": { "family": "Mortlock", "given": "Alice" } }, { "id": "McLure-R-J", "name": { "family": "McLure", "given": "Ross J." } }, { "id": "Bowler-R-A-A", "name": { "family": "Bowler", "given": "Rebecca A. A." } }, { "id": "McLeod-D-J", "name": { "family": "McLeod", "given": "Derek J." } }, { "id": "M\u00e1rmol-Queralt\u00f3-E", "name": { "family": "M\u00e1rmol-Queralt\u00f3", "given": "Esther" } }, { "id": "Parsa-S", "name": { "family": "Parsa", "given": "Shaghayegh" } }, { "id": "Dunlop-J-S", "name": { "family": "Dunlop", "given": "James S." } }, { "id": "Bruce-V-A", "name": { "family": "Bruce", "given": "Victoria A." } } ] }, "title": "Characterizing the evolving K-band luminosity function using the UltraVISTA, CANDELS and HUDF surveys", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 October 18. Received 2016 October 15; in original form 2016 September 7.", "abstract": "We present the results of a new study of the K-band galaxy luminosity function (KLF) at redshifts z \u2264 3.75, based on a nested combination of the UltraVISTA, Cosmic Assembly Near-infrared Deep Legacy Extragalactic Survey and HUDF surveys. The large dynamic range in luminosity spanned by this new data set (3\u20134 dex over the full redshift range) is sufficient to clearly demonstrate for the first time that the faint-end slope of the KLF at z \u2265 0.25 is relatively steep (\u22121.3 \u2264 \u03b1 \u2264 \u22121.5 for a single Schechter function), in good agreement with recent theoretical and phenomenological models. Moreover, based on our new data set, we find that a double Schechter function provides a significantly improved description of the KLF at z \u2264 2. At redshifts z \u2265 0.25, the evolution of the KLF is remarkably smooth, with little or no evolution evident at faint (MK \u2265 \u221220.5) or bright magnitudes (MK \u2264 \u221224.5). Instead, the KLF is seen to evolve rapidly at intermediate magnitudes, with the number density of galaxies at MK \u2243\u221223 dropping by a factor of \u22435 over the redshift interval 0.25 \u2264 z \u2264 3.75. Motivated by this, we explore a simple description of the evolving KLF based on a double Schechter function with fixed faint-end slopes (\u03b11 = \u22120.5, \u03b12 = \u22121.5) and a shared characteristic magnitude (M\u22c6K MK\u22c6). According to this parametrization, the normalization of the component which dominates the faint end of the KLF remains approximately constant, with \n\u03d5\u22c62 \u03d52\u22c6 decreasing by only a factor of \u22432 between z \u22430 and 3.25. In contrast, the component which dominates the bright end of the KLF at low redshifts evolves dramatically, becoming essentially negligible by z \u22433. Finally, we note that within this parametrization, the observed evolution of \nM\u22c6K MK\u22c6between z \u22430 and 3.25 is entirely consistent with M\u22c6K MK\u22c6 corresponding to a constant stellar mass of M\u22c6 \u22435 \u00d7 1010\u2009\u2009M\u2299 at all redshifts.", "date": "2017", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "465", "number": "1", "publisher": "Oxford University Press", "pagerange": "672-687", "id_number": "CaltechAUTHORS:20170628-134813790", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170628-134813790", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "SPLASH", "value": "SPLASH" }, { "id": "COSMOS", "value": "COSMOS" } ] }, "doi": "10.1093/mnras/stw2728", "pub_year": "2017", "author_list": "Mortlock, Alice; McLure, Ross J.; et el." }, { "id": "https://authors.library.caltech.edu/records/3vj6v-f8h98", "eprint_id": 78666, "eprint_status": "archive", "datestamp": "2023-08-19 00:31:40", "lastmod": "2023-10-26 00:16:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Groves-B-A", "name": { "family": "Groves", "given": "B." }, "orcid": "0000-0002-9768-0246" }, { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M. T." }, "orcid": "0000-0003-1033-9684" }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P. A." }, "orcid": "0000-0001-5851-6649" }, { "id": "Magnelli-B", "name": { "family": "Magnelli", "given": "B." }, "orcid": "0000-0002-6777-6490" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "LeFevre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" } ] }, "title": "Gas Fraction and depletion time of massive star-forming galaxies at z \u223c 3.2: No change in global star formation process out to z > 3", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2016. The American Astronomical Society.", "abstract": "The observed evolution of the gas fraction and its associated depletion time in main-sequence (MS) galaxies provides insights on how star formation proceeds over cosmic time. We report ALMA detections of the rest-frame ~300 \u03bcm continuum observed at 240 GHz for 45 massive ($\\langle \\mathrm{log}({M}_{\\star }({M}_{\\odot }))\\rangle =10.7$), normal star-forming ($\\langle \\mathrm{log}(\\mathrm{sSFR}({\\mathrm{yr}}^{-1}))\\rangle =-8.6$), i.e., MS, galaxies at $z\\approx 3.2$ in the COSMOS field. From an empirical calibration between cold neutral, i.e., molecular and atomic, gas mass ${M}_{\\mathrm{gas}}$ and monochromatic (rest-frame) infrared luminosity, the gas mass for this sample is derived. Combined with stellar mass ${M}_{\\star }$ and star formation rate (SFR) estimates (from MagPhys fits) we obtain a median gas fraction of ${\\mu }_{\\mathrm{gas}}={M}_{\\mathrm{gas}}/{M}_{\\star }={1.65}_{-0.19}^{+0.18}$ and a median gas depletion time ${t}_{\\mathrm{depl}.}(\\mathrm{Gyr})={M}_{\\mathrm{gas}/\\mathrm{SFR}}={0.68}_{-0.08}^{+0.07};$ correction for the location on the MS will only slightly change the values. The reported uncertainties are the $1\\sigma $ error on the median. Our results are fully consistent with the expected flattening of the redshift evolution from the 2-SFM (2 star formation mode) framework which empirically prescribes the evolution assuming a universal, log-linear relation between SFR and gas mass coupled to the redshift evolution of the specific star formation rate (sSFR) of MS galaxies. While ${t}_{\\mathrm{depl}.}$ shows only a mild dependence on location within the MS, a clear trend of increasing ${\\mu }_{\\mathrm{gas}}$ across the MS is observed (as known from previous studies). Further, we comment on trends within the MS and (in)consistencies with other studies.", "date": "2016-12-12", "date_type": "published", "publication": "Astrophysical Journal", "volume": "833", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art No 112", "id_number": "CaltechAUTHORS:20170628-141332941", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170628-141332941", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "COSMOS", "value": "COSMOS" }, { "id": "SPLASH", "value": "SPLASH" } ] }, "doi": "10.3847/1538-4357/833/1/112", "pub_year": "2016", "author_list": "Schinnerer, E.; Groves, B.; et el." }, { "id": "https://authors.library.caltech.edu/records/28556-hbw10", "eprint_id": 72734, "eprint_status": "archive", "datestamp": "2023-08-22 19:16:55", "lastmod": "2023-10-23 22:53:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zschaechner-L-K", "name": { "family": "Zschaechner", "given": "Laura K." }, "orcid": "0000-0002-9919-8672" }, { "id": "Ott-J", "name": { "family": "Ott", "given": "J\u00fcrgen" }, "orcid": "0000-0001-8224-1956" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "Fabian" }, "orcid": "0000-0003-4793-7880" }, { "id": "Meier-D-S", "name": { "family": "Meier", "given": "David S." }, "orcid": "0000-0001-9436-9471" }, { "id": "Momjian-E", "name": { "family": "Momjian", "given": "Emmanuel" }, "orcid": "0000-0003-3168-5922" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" } ] }, "title": "High-resolution Observations of Molecular Lines in Arp 220: Kinematics, Morphology, and Limits on the Applicability of the Ammonia Thermometer", "ispublished": "pub", "full_text_status": "public", "keywords": "astrochemistry; galaxies: evolution; galaxies: individual (Arp 220); galaxies: ISM; galaxies: nuclei; galaxies: starburst", "note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2015 October 29; revised 2016 September 9; accepted 2016 September 13; published 2016 December 6. \n\nThe National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00175.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. The authors thank Brent Groves and Yancy Shirley for insightful discussions concerning ammonia properties and LVG analysis. We also thank Elizabeth Mills for insight concerning ammonia masers and column densities. Finally, we thank the anonymous referee for exceptionally insightful and relevant comments leading to substantial improvement of this manuscript.\n\nPublished - Zschaechner_2016_ApJ_833_41.pdf
", "abstract": "We observe Arp 220, the nearest ultra-luminous infrared galaxy, over 4 GHz in the K and Ka bands, providing constraints for the kinematics and morphology, and identifying molecular species on scales resolving both nuclei (0\".6 or 230 pc). We detect multiple molecular species, including hydroxyl (OH ^2\u03a0_(3/2)J = 9/2 F= 4-4; 5-5) in both cores, and tentatively detect H_2O(6_(15)-5_(23)) at ~21.84 GHz in both nuclei, indicating the likely presence of maser emission. The observed frequency range also contains metastable ammonia transitions from (J, K) = (1, 1)\u2013(5, 5), as well as the (9, 9) inversion line; together, they are a well-known thermometer of dense molecular gas. Furthermore, the non-metastable (4, 2) and (10, 9), and possibly the (3, 1), lines are also detected. We apply a standard temperature analysis to Arp 220; however, the analysis is complicated in that standard local thermal equilibrium (LTE) assumptions do not hold. There are indications that a substantial fraction of ammonia could be in the non-metastable transitions, as opposed to only the metastable ones. Thus, the non-metastable transitions could be essential to constraining the temperature. We compare all of these data to ALMA observations of this source, confirming the outflow previously observed by other tracers in both nuclei.", "date": "2016-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "833", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 41", "id_number": "CaltechAUTHORS:20161212-153120377", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161212-153120377", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.3847/1538-4357/833/1/41", "primary_object": { "basename": "Zschaechner_2016_ApJ_833_41.pdf", "url": "https://authors.library.caltech.edu/records/28556-hbw10/files/Zschaechner_2016_ApJ_833_41.pdf" }, "pub_year": "2016", "author_list": "Zschaechner, Laura K.; Ott, J\u00fcrgen; et el." }, { "id": "https://authors.library.caltech.edu/records/0jn25-pr956", "eprint_id": 73491, "eprint_status": "archive", "datestamp": "2023-08-19 00:27:03", "lastmod": "2023-10-24 15:23:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pavesi-R", "name": { "family": "Pavesi", "given": "Riccardo" }, "orcid": "0000-0002-2263-646X" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "Dominik A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "Christopher L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Sharon-C-E", "name": { "family": "Sharon", "given": "Chelsea E." }, "orcid": "0000-0002-6250-5608" }, { "id": "Stacey-G-J", "name": { "family": "Stacey", "given": "Gordon J." } }, { "id": "Karim-A", "name": { "family": "Karim", "given": "Alexander" }, "orcid": "0000-0002-8414-9579" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "Vernesa" }, "orcid": "0000-0002-3893-8614" } ] }, "title": "ALMA Reveals Weak [N II] Emission in \"Typical\" Galaxies and Intense Starbursts at z = 5\u20136", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 galaxies: formation \u2013 galaxies: high-redshift \u2013 galaxies: ISM \u2013 galaxies:\nstarburst \u2013 radio lines: galaxies", "note": "\u00a9 2016 The American Astronomical Society.\n\nReceived 2016 July 8; revised 2016 August 24; accepted 2016 September 15; published 2016 November 29.\n\nWe thank the anonymous referee for a helpful and constructive report and T.K. Daisy Leung for helpful discussion. D.R. and R.P. acknowledge support from the National Science Foundation under grant number AST-1614213 to Cornell University. R.P. acknowledges support through award SOSPA3-008 from the NRAO. A.K. acknowledges support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). D.R. acknowledges the hospitality at the Aspen Center for Physics and the Kavli Institute for Theoretical Physics during part of the writing of this manuscript. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00928.S, 2011.0.00064.S, 2012.1.00523.S, 2011.0.00006.SV, and 2013.1.00745.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.\n\nPublished - Pavesi_2016_ApJ_832_151.pdf
Submitted - 1607.02520v3.pdf
", "abstract": "We report interferometric measurements of [N II] 205 \u03bcm fine-structure line emission from a representative sample of three galaxies at z = 5\u20136 using the Atacama Large (sub)Millimeter Array (ALMA). These galaxies were previously detected in [C II] and far-infrared continuum emission and span almost two orders of magnitude in star formation rate (SFR). Our results show at least two different regimes of ionized interstellar medium properties for galaxies in the first billion years of cosmic time, separated by their L_([C II])/L_([N II]) ratio. We find extremely low [N II] emission compared to [C II] (L_([C II])/L_([N II]) = 68^(+200)_(-28)) from a \"typical\" ~L_*(UV) star-forming galaxy, likely directly or indirectly (by its effect on the radiation field) related to low dust abundance and low metallicity. The infrared-luminous modestly star-forming Lyman-break galaxy (LBG) in our sample is characterized by an ionized-gas fraction (L_([C II])/L_([N II]) \u227e 20) typical of local star-forming galaxies and shows evidence for spatial variations in its ionized-gas fraction across an extended gas reservoir. The extreme SFR, warm and compact dusty starburst AzTEC-3 shows an ionized fraction higher than expected given its SFR surface density (L_([C II])/L_([N II]) = 22 \u00b1 8) suggesting that [N II] dominantly traces a diffuse ionized medium rather than star-forming H II regions in this type of galaxy. This highest redshift sample of [N II] detections provides some of the first constraints on ionized and neutral gas modeling attempts and on the structure of the interstellar medium at z = 5\u20136 in \"normal\" galaxies and starbursts.", "date": "2016-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "832", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 151", "id_number": "CaltechAUTHORS:20170113-131905422", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170113-131905422", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1614213" }, { "agency": "National Radio Astronomy Observatory (NRAO)", "grant_number": "SOSPA3-008" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "956" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.3847/0004-637X/832/2/151", "primary_object": { "basename": "1607.02520v3.pdf", "url": "https://authors.library.caltech.edu/records/0jn25-pr956/files/1607.02520v3.pdf" }, "related_objects": [ { "basename": "Pavesi_2016_ApJ_832_151.pdf", "url": "https://authors.library.caltech.edu/records/0jn25-pr956/files/Pavesi_2016_ApJ_832_151.pdf" } ], "pub_year": "2016", "author_list": "Pavesi, Riccardo; Riechers, Dominik A.; et el." }, { "id": "https://authors.library.caltech.edu/records/2mwb8-crd22", "eprint_id": 60318, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:55", "lastmod": "2023-10-24 16:25:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XXV. Diffuse low-frequency Galactic foregrounds", "ispublished": "pub", "full_text_status": "public", "keywords": "diffuse radiation / ISM: general / radiation mechanisms: general / radio continuum: ISM / polarization / local insterstellar matter", "note": "\u00a9 2016 ESO. \n\nReceived: 22 June 2015; Accepted: 20 April 2016; Published online 20 September 2016. \n\nThis paper is dedicated to the memory of the late Professor Rodney Deane Davies CBE FRS and Professor Richard John Davis OBE, both of whom contributed greatly to the Planck project. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This research was supported by an ERC Starting (Consolidator) Grant (no. 307209) and STFC Consolidated Grant (no. ST/L000768/1). We have made extensive use of the HEALPix package and the IDL astronomy library. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.\n\nPublished - aa26803-15.pdf
Submitted - 1506.06660v1.pdf
", "abstract": "We discuss the Galactic foreground emission between 20 and 100\u2009GHz based on observations by Planck and WMAP. The total intensity in this part of the spectrum is dominated by free-free and spinning dust emission, whereas the polarized intensity is dominated by synchrotron emission. The Commander component-separation tool has been used to separate the various astrophysical processes in total intensity. Comparison with radio recombination line templates verifies the recovery of the free-free emission along the Galactic plane. Comparison of the high-latitude H\u03b1 emission with our free-free map shows residuals that correlate with dust optical depth, consistent with a fraction (\u224830%) of H\u03b1 having been scattered by high-latitude dust. We highlight a number of diffuse spinning dust morphological features at high latitude. There is substantial spatial variation in the spinning dust spectrum, with the emission peak (in I_\u03bd) ranging from below 20\u2009GHz to more than 50\u2009GHz. There is a strong tendency for the spinning dust component near many prominent H\u2009II regions to have a higher peak frequency, suggesting that this increase in peak frequency is associated with dust in the photo-dissociation regions around the nebulae. The emissivity of spinning dust in these diffuse regions is of the same order as previous detections in the literature. Over the entire sky, the Commander solution finds more anomalous microwave emission (AME) than the WMAP component maps, at the expense of synchrotron and free-free emission. This can be explained by the difficulty in separating multiple broadband components with a limited number of frequency maps. Future surveys, particularly at 5\u201320\u2009GHz, will greatly improve the separation by constraining the synchrotron spectrum. We combine Planck and WMAP data to make the highest signal-to-noise ratio maps yet of the intensity of the all-sky polarized synchrotron emission at frequencies above a few GHz. Most of the high-latitude polarized emission is associated with distinct large-scale loops and spurs, and we re-discuss their structure. We argue that nearly all the emission at 40deg > l > \u221290deg is part of the Loop I structure, and show that the emission extends much further in to the southern Galactic hemisphere than previously recognised, giving Loop I an ovoid rather than circular outline. However, it does not continue as far as the \"Fermi bubble/microwave haze\", making it less probable that these are part of the same structure. We identify a number of new faint features in the polarized sky, including a dearth of polarized synchrotron emission directly correlated with a narrow, roughly 20deg long filament seen in H\u03b1 at high Galactic latitude. Finally, we look for evidence of polarized AME, however many AME regions are significantly contaminated by polarized synchrotron emission, and we find a 2\u03c3 upper limit of 1.6% in the Perseus region.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A25", "id_number": "CaltechAUTHORS:20150918-100209126", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-100209126", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft (MPG)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "European Research Council (ERC)", "grant_number": "307209" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L000768/1" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201526803", "primary_object": { "basename": "1506.06660v1.pdf", "url": "https://authors.library.caltech.edu/records/2mwb8-crd22/files/1506.06660v1.pdf" }, "related_objects": [ { "basename": "aa26803-15.pdf", "url": "https://authors.library.caltech.edu/records/2mwb8-crd22/files/aa26803-15.pdf" } ], "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/sqgt0-nz529", "eprint_id": 60286, "eprint_status": "archive", "datestamp": "2023-08-20 13:56:58", "lastmod": "2023-10-24 16:23:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XIX. Constraints on primordial magnetic fields", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 ESO. \n\nReceived: 5 February 2015; Accepted: 19 February 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231. Some of the results in this paper have been derived using the HEALPix package.\n\nPublished - aa25821-15.pdf
Submitted - 1502.01594v1.pdf
", "abstract": "We compute and investigate four types of imprint of a stochastic background of primordial magnetic fields (PMFs) on the cosmic microwave background (CMB) anisotropies: the impact of PMFs on the CMB temperature and polarization spectra, which is related to their contribution to cosmological perturbations; the effect on CMB polarization induced by Faraday rotation; the impact of PMFs on the ionization history; magnetically-induced non-Gaussianities and related non-zero bispectra; and the magnetically-induced breaking of statistical isotropy. We present constraints on the amplitude of PMFs that are derived from different Planck data products, depending on the specific effect that is being analysed. Overall, Planck data constrain the amplitude of PMFs to less than a few nanoGauss, with different bounds that depend on the considered model. In particular, individual limits coming from the analysis of the CMB angular power spectra, using the Planck likelihood, are B_(1 Mpc) < 4.4 nG (where B_(1 Mpc) is the comoving field amplitude at a scale of 1\u2009Mpc) at 95% confidence level, assuming zero helicity. By considering the Planck likelihood, based only on parity-even angular power spectra, we obtain B_(1 Mpc) < 5.6 nG for a maximally helical field. For nearly scale-invariant PMFs we obtain B_(1 Mpc) < 2.0\u2009nG and B_(1 Mpc) < 0.9\u2009nG if the impact of PMFs on the ionization history of the Universe is included in the analysis. From the analysis of magnetically-induced non-Gaussianity, we obtain three different values, corresponding to three applied methods, all below 5\u2009nG. The constraint from the magnetically-induced passive-tensor bispectrum is B_(1 Mpc) < 2.8\u2009nG. A search for preferred directions in the magnetically-induced passive bispectrum yields B_(1 Mpc) < 4.5\u2009nG, whereas the compensated-scalar bispectrum gives B_(1 Mpc) < 3\u2009nG. The analysis of the Faraday rotation of CMB polarization by PMFs uses the Planck power spectra in EE and BB at 70\u2009GHz and gives B_(1 Mpc) < 1380\u2009nG. In our final analysis, we consider the harmonic-space correlations produced by Alfv\u00e9n waves, finding no significant evidence for the presence of these waves. Together, these results comprise a comprehensive set of constraints on possible PMFs with Planck data.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A19", "id_number": "CaltechAUTHORS:20150916-145551601", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150916-145551601", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft (MPG)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525821", "primary_object": { "basename": "1502.01594v1.pdf", "url": "https://authors.library.caltech.edu/records/sqgt0-nz529/files/1502.01594v1.pdf" }, "related_objects": [ { "basename": "aa25821-15.pdf", "url": "https://authors.library.caltech.edu/records/sqgt0-nz529/files/aa25821-15.pdf" } ], "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/f0qyk-mnn69", "eprint_id": 60320, "eprint_status": "archive", "datestamp": "2023-08-20 13:58:03", "lastmod": "2023-10-24 16:25:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "C." }, "orcid": "0000-0002-5627-5471" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XXVI. The Second Planck Catalogue of Compact Sources", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs / cosmology: observations / radio continuum: general / submillimeter: general", "note": "\u00a9 2016 ESO. \n\nReceived: 8 July 2015; Accepted: 28 January 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and, RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. We are grateful to the H-ATLAS Executive Committee and primarily to the PIs, S. Eales and L. Dunne, for permission to use the unpublished H-ATLAS catalogue for the validation of the present catalogue. This research has made use of the \"Aladin sky atlas\" (Bonnarel et al. 2000), developed at CDS, Strasbourg Observatory, France. Part of this work was performed using the Darwin Supercomputer of the University of Cambridge High Performance Computing Service (http://www.hpc.cam.ac.uk/), provided by Dell Inc. using Strategic Research Infrastructure Funding from the HEFCE and funding from the STFC. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nPublished - aa26914-15.pdf
Submitted - 1507.02058v1.pdf
", "abstract": "The Second Planck Catalogue of Compact Sources is a list of discrete objects detected in single-frequency maps from the full duration of the Planck mission and supersedes previous versions. It consists of compact sources, both Galactic and extragalactic, detected over the entire sky. Compact sources detected in the lower frequency channels are assigned to the PCCS2, while at higher frequencies they are assigned to one of two subcatalogues, the PCCS2 or PCCS2E, depending on their location on the sky. The first of these (PCCS2) covers most of the sky and allows the user to produce subsamples at higher reliabilities than the target 80% integral reliability of the catalogue. The second (PCCS2E) contains sources detected in sky regions where the diffuse emission makes it difficult to quantify the reliability of the detections. Both the PCCS2 and PCCS2E include polarization measurements, in the form of polarized flux densities, or upper limits, and orientation angles for all seven polarization-sensitive Planck channels. The improved data-processing of the full-mission maps and their reduced noise levels allow us to increase the number of objects in the catalogue, improving its completeness for the target 80% reliability as compared with the previous versions, the PCCS and the Early Release Compact Source Catalogue (ERCSC).", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A26", "id_number": "CaltechAUTHORS:20150918-104502219", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-104502219", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "Higher Education Funding Council for England (HEFCE)" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201526914", "primary_object": { "basename": "aa26914-15.pdf", "url": "https://authors.library.caltech.edu/records/f0qyk-mnn69/files/aa26914-15.pdf" }, "related_objects": [ { "basename": "1507.02058v1.pdf", "url": "https://authors.library.caltech.edu/records/f0qyk-mnn69/files/1507.02058v1.pdf" } ], "pub_year": "2016", "author_list": "Ade, P. A. R.; Beichman, C.; et el." }, { "id": "https://authors.library.caltech.edu/records/x1rn2-33y63", "eprint_id": 60313, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:30", "lastmod": "2023-10-24 16:25:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XIII. Cosmological parameters", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations / cosmology: theory / cosmic background radiation / cosmological parameters", "note": "\u00a9 2016 ESO. \n\nReceived: 6 February 2015; Accepted: 4 June 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. Some of the results in this paper have been derived using the HEALPix package. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007\u22122013)/ERC Grant Agreement No. [616170] and from the UK Science and Technology Facilities Council [grant number ST/L000652/1]. Part of this work was undertaken on the STFC DiRAC HPC Facilities at the University of Cambridge, funded by UK BIS National E-infrastructure capital grants, and on the Andromeda cluster of the University of Geneva. A large set of cosmological parameter constraints from different data combinations, and including many separate extensions to the 6-parameter base \u039bCDM model, are available at http://pla.esac.esa.int/pla/#cosmology.\n\nPublished - aa25830-15.pdf
Submitted - 1502.01589v2.pdf
", "abstract": "This paper presents cosmological results based on full-mission Planck observations of temperature and polarization anisotropies of the cosmic microwave background (CMB) radiation. Our results are in very good agreement with the 2013 analysis of the Planck nominal-mission temperature data, but with increased precision. The temperature and polarization power spectra are consistent with the standard spatially-flat 6-parameter \u039bCDM cosmology with a power-law spectrum of adiabatic scalar perturbations (denoted \"base \u039bCDM\" in this paper). From the Planck temperature data combined with Planck lensing, for this cosmology we find a Hubble constant, H_0 = (67.8 \u00b1 0.9) km s^(-1)Mpc^(-1), a matter density parameter \u03a9_m = 0.308 \u00b1 0.012, and a tilted scalar spectral index with n_s = 0.968 \u00b1 0.006, consistent with the 2013 analysis. Note that in this abstract we quote 68% confidence limits on measured parameters and 95% upper limits on other parameters. We present the first results of polarization measurements with the Low Frequency Instrument at large angular scales. Combined with the Planck temperature and lensing data, these measurements give a reionization optical depth of \u03c4 = 0.066 \u00b1 0.016, corresponding to a reionization redshift of Z_(re) = 8.8^(+1.7)_(-1.4). These results are consistent with those from WMAP polarization measurements cleaned for dust emission using 353-GHz polarization maps from the High Frequency Instrument. We find no evidence for any departure from base \u039bCDM in the neutrino sector of the theory; for example, combining Planck observations with other astrophysical data we find N_(eff) = 3.15 \u00b1 0.23 for the effective number of relativistic degrees of freedom, consistent with the value N_(eff) = 3.046 of the Standard Model of particle physics. The sum of neutrino masses is constrained to \u2211 m_\u03bd < 0.23 eV. The spatial curvature of our Universe is found to be very close to zero, with | \u03a9_K | < 0.005. Adding a tensor component as a single-parameter extension to base \u039bCDM we find an upper limit on the tensor-to-scalar ratio of r_(0.002)< 0.11, consistent with the Planck 2013 results and consistent with the B-mode polarization constraints from a joint analysis of BICEP2, Keck Array, and Planck (BKP) data. Adding the BKP B-mode data to our analysis leads to a tighter constraint of r_(0.002) < 0.09 and disfavours inflationarymodels with a V(\u03c6) \u221d \u03c6^2 potential. The addition of Planck polarization data leads to strong constraints on deviations from a purely adiabatic spectrum of fluctuations. We find no evidence for any contribution from isocurvature perturbations or from cosmic defects. Combining Planck data with other astrophysical data, including Type Ia supernovae, the equation of state of dark energy is constrained to w = \u22121.006 \u00b1 0.045, consistent with the expected value for a cosmological constant. The standard big bang nucleosynthesis predictions for the helium and deuterium abundances for the best-fit Planck base \u039bCDM cosmology are in excellent agreement with observations. We also constraints on annihilating dark matter and on possible deviations from the standard recombination history. In neither case do we find no evidence for new physics. The Planck results for base \u039bCDM are in good agreement with baryon acoustic oscillation data and with the JLA sample of Type Ia supernovae. However, as in the 2013 analysis, the amplitude of the fluctuation spectrum is found to be higher than inferred from some analyses of rich cluster counts and weak gravitational lensing. We show that these tensions cannot easily be resolved with simple modifications of the base \u039bCDM cosmology. Apart from these tensions, the base \u039bCDM cosmology provides an excellent description of the Planck CMB observations and many other astrophysical data sets.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A13", "id_number": "CaltechAUTHORS:20150918-070918069", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-070918069", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "European Research Council (ERC)", "grant_number": "616170" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L000652/1" }, { "agency": "UK BIS National E-Infrastructure" }, { "agency": "University of Geneva" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525830", "primary_object": { "basename": "1502.01589v2.pdf", "url": "https://authors.library.caltech.edu/records/x1rn2-33y63/files/1502.01589v2.pdf" }, "related_objects": [ { "basename": "aa25830-15.pdf", "url": "https://authors.library.caltech.edu/records/x1rn2-33y63/files/aa25830-15.pdf" } ], "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/nvrhy-wp979", "eprint_id": 60323, "eprint_status": "archive", "datestamp": "2023-08-20 13:58:18", "lastmod": "2023-10-24 16:25:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Pelkonen-Veli-Matti", "name": { "family": "Pelkonen", "given": "V.-M." }, "orcid": "0000-0002-8898-1047" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XXVIII. The Planck Catalogue of Galactic Cold Clumps", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: clouds / ISM: structure / local insterstellar matter / stars: formation", "note": "\u00a9 2016 ESO. \n\nReceived: 5 February 2015; Accepted: 16 August 2015; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration.\n\nPublished - aa25819-15.pdf
Submitted - 1502.01599v1.pdf
", "abstract": "We present the Planck Catalogue of Galactic Cold Clumps (PGCC), an all-sky catalogue of Galactic cold clump candidates detected by Planck. This catalogue is the full version of the Early Cold Core (ECC) catalogue, which was made available in 2011 with the Early Release Compact Source Catalogue (ERCSC) and which contained 915 high signal-to-noise sources. It is based on the Planck 48-month mission data that are currently being released to the astronomical community. The PGCC catalogue is an observational catalogue consisting exclusively of Galactic cold sources. The three highest Planck bands (857, 454, and 353 GHz) have been combined with IRAS data at 3\u2009THz to perform a multi-frequency detection of sources colder than their local environment. After rejection of possible extragalactic contaminants, the PGCC catalogue contains 13188 Galactic sources spread across the whole sky, i.e., from the Galactic plane to high latitudes, following the spatial distribution of the main molecular cloud complexes. The median temperature of PGCC sources lies between 13 and 14.5\u2009K, depending on the quality of the flux density measurements, with a temperature ranging from 5.8 to 20\u2009K after removing the sources with the top 1% highest temperature estimates. Using seven independent methods, reliable distance estimates have been obtained for 5574 sources, which allows us to derive their physical properties such as their mass, physical size, mean density, and luminosity.The PGCC sources are located mainly in the solar neighbourhood, but also up to a distance of 10.5\u2009kpc in the direction of the Galactic centre, and range from low-mass cores to large molecular clouds. Because of this diversity and because the PGCC catalogue contains sources in very different environments, the catalogue is useful for investigating the evolution from molecular clouds to cores. Finally, it also includes 54 additional sources located in the Small and Large Magellanic Clouds.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. 28", "id_number": "CaltechAUTHORS:20150918-112734674", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-112734674", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525819", "primary_object": { "basename": "1502.01599v1.pdf", "url": "https://authors.library.caltech.edu/records/nvrhy-wp979/files/1502.01599v1.pdf" }, "related_objects": [ { "basename": "aa25819-15.pdf", "url": "https://authors.library.caltech.edu/records/nvrhy-wp979/files/aa25819-15.pdf" } ], "pub_year": "2016", "author_list": "Ade, P. A. R.; Crill, B. P.; et el." }, { "id": "https://authors.library.caltech.edu/records/eyhw3-dfk52", "eprint_id": 60315, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:44", "lastmod": "2023-10-24 16:25:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XVII. Constraints on primordial non-Gaussianity", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation / cosmology: observations / cosmology: theory / early Universe / inflation / methods: data analysis", "note": "\u00a9 2016 ESO. \n\nReceived: 6 February 2015; Accepted: 27 January 2016;\nPublished online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. Some of the results in this paper have been derived using the HEALPix package. Part of this work was undertaken on the STFC COSMOS@DiRAC HPC Facility at the University of Cambridge, funded by UK BIS NEI grants. We gratefully acknowledge IN2P3 Computer Center (http://cc.in2p3.fr) for providing a significant amount of the computing resources and services needed for the analysis with the binned bispectrum estimator. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. We also acknowledge the IAP magique3 computer facilities. Some computations were performed on the GPC cluster at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, and the University of Toronto.\n\nPublished - aa25836-15.pdf
Submitted - 1502.01592v1.pdf
", "abstract": "The Planck full mission cosmic microwave background (CMB) temperature and E-mode polarization maps are analysed to obtain constraints on primordial non-Gaussianity (NG). Using three classes of optimal bispectrum estimators \u2013 separable template-fitting (KSW), binned, and modal \u2013 we obtain consistent values for the primordial local, equilateral, and orthogonal bispectrum amplitudes, quoting as our final result from temperature alone \u0192^(local)_(NL) = 2.5 \u00b1 5.7, \u0192^(equil)_(NL)= -16 \u00b1 70, , and \u0192^(ortho)_(NL) = -34 \u00b1 32 (68% CL, statistical). Combining temperature and polarization data we obtain \u0192^(local)_(NL) = 0.8 \u00b1 5.0, \u0192^(equil)_(NL)= -4 \u00b1 43, and \u0192^(ortho)_(NL) = -26 \u00b1 21 (68% CL, statistical). The results are based on comprehensive cross-validation of these estimators on Gaussian and non-Gaussian simulations, are stable across component separation techniques, pass an extensive suite of tests, and are consistent with estimators based on measuring the Minkowski functionals of the CMB. The effect of time-domain de-glitching systematics on the bispectrum is negligible. In spite of these test outcomes we conservatively label the results including polarization data as preliminary, owing to a known mismatch of the noise model in simulations and the data. Beyond estimates of individual shape amplitudes, we present model-independent, three-dimensional reconstructions of the Planck CMB bispectrum and derive constraints on early universe scenarios that generate primordial NG, including general single-field models of inflation, axion inflation, initial state modifications, models producing parity-violating tensor bispectra, and directionally dependent vector models. We present a wide survey of scale-dependent feature and resonance models, accounting for the \"look elsewhere\" effect in estimating the statistical significance of features. We also look for isocurvature NG, and find no signal, but we obtain constraints that improve significantly with the inclusion of polarization. The primordial trispectrum amplitude in the local model is constrained to be g^(local)_(NL) = (\u22129.0\u00b17.7)\u00d710^4 (68% CL statistical), and we perform an analysis of trispectrum shapes beyond the local case. The global picture that emerges is one of consistency with the premises of the \u039bCDM cosmology, namely that the structure we observe today was sourced by adiabatic, passive, Gaussian, and primordial seed perturbations.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A17", "id_number": "CaltechAUTHORS:20150918-082428843", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-082428843", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "UK BIS NEI Grants" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Compute Canada" }, { "agency": "Government of Ontario" }, { "agency": "University of Toronto" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525836", "primary_object": { "basename": "aa25836-15.pdf", "url": "https://authors.library.caltech.edu/records/eyhw3-dfk52/files/aa25836-15.pdf" }, "related_objects": [ { "basename": "1502.01592v1.pdf", "url": "https://authors.library.caltech.edu/records/eyhw3-dfk52/files/1502.01592v1.pdf" } ], "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/dbvx7-g5555", "eprint_id": 74520, "eprint_status": "archive", "datestamp": "2023-08-20 14:05:51", "lastmod": "2023-10-24 22:43:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Adam-R", "name": { "family": "Adam", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. VIII. High Frequency Instrument data processing: Calibration and maps", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations / cosmic background radiation / surveys / methods: data analysis", "note": "\u00a9 2016 ESO. \n\nReceived: 5 February 2015; Accepted: 10 September 2015; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration\n\nPublished - aa25820-15.pdf
Submitted - 1502.01587.pdf
", "abstract": "This paper describes the processing applied to the cleaned, time-ordered information obtained from the Planck High Frequency Instrument (HFI) with the aim of producing photometrically calibrated maps in temperature and (for the first time) in polarization. The data from the entire 2.5-year HFI mission include almost five full-sky surveys. HFI observes the sky over a broad range of frequencies, from 100 to 857\u2009GHz. To obtain the best accuracy on the calibration over such a large range, two different photometric calibration schemes have been used. The 545 and 857\u2009GHz data are calibrated using models of planetary atmospheric emission. The lower frequencies (from 100 to 353\u2009GHz) are calibrated using the time-variable cosmological microwave background dipole, which we call the orbital dipole. This source of calibration only depends on the satellite velocity with respect to the solar system. Using a CMB temperature of T_(CMB) = 2.7255 \u00b1 0.0006 K, it permits an independent measurement of the amplitude of the CMB solar dipole (3364.3 \u00b1 1.5 \u03bcK), which is approximatively 1\u03c3 higher than the WMAP measurement with a direction that is consistent between the two experiments. We describe the pipeline used to produce the maps ofintensity and linear polarization from the HFI timelines, and the scheme used to set the zero level of the maps a posteriori. We also summarize the noise characteristics of the HFI maps in the 2015 Planck data release and present some null tests to assess their quality. Finally, we discuss the major systematic effects and in particular the leakage induced by flux mismatch between the detectors that leads to spurious polarization signal.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A8", "id_number": "CaltechAUTHORS:20170224-082939025", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170224-082939025", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525820", "primary_object": { "basename": "1502.01587.pdf", "url": "https://authors.library.caltech.edu/records/dbvx7-g5555/files/1502.01587.pdf" }, "related_objects": [ { "basename": "aa25820-15.pdf", "url": "https://authors.library.caltech.edu/records/dbvx7-g5555/files/aa25820-15.pdf" } ], "pub_year": "2016", "author_list": "Adam, R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/xrdg8-83809", "eprint_id": 74467, "eprint_status": "archive", "datestamp": "2023-08-20 14:05:35", "lastmod": "2023-10-24 22:40:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XX. Constraints on inflation", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation / cosmology: theory / early Universe / inflation", "note": "\u00a9 2016 ESO. \n\nReceived: 14 February 2015; Accepted: 3 March 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231. Part of this work was undertaken at the STFC DiRAC HPC Facilities at the University of Cambridge, funded by UK BIS National E-infrastructure capital grants. We gratefully acknowledge the IN2P3 Computer Center (http://cc.in2p3.fr) for providing a significant amount of the computing resources and services needed for this work.\n\nPublished - aa25898-15.pdf
Submitted - 1502.02114.pdf
", "abstract": "We present the implications for cosmic inflation of the Planck measurements of the cosmic microwave background (CMB) anisotropies in both temperature and polarization based on the full Planck survey, which includes more than twice the integration time of the nominal survey used for the 2013 release papers. The Planck full mission temperature data and a first release of polarization data on large angular scales measure the spectral index of curvature perturbations to be ns = 0.968 \u00b1 0.006 and tightly constrain its scale dependence to dns/ dlnk = \u22120.003 \u00b1 0.007 when combined with the Planck lensing likelihood. When the Planck high-\u2113 polarization data are included, the results are consistent and uncertainties are further reduced. The upper bound on the tensor-to-scalar ratio is r_(0.002)< 0.11 (95% CL). This upper limit is consistent with the B-mode polarization constraint r< 0.12 (95% CL) obtained from a joint analysis of the BICEP2/Keck Array and Planck data. These results imply that V(\u03c6) \u221d \u03c6^2 and natural inflation are now disfavoured compared to models predicting a smaller tensor-to-scalar ratio, such as R^2 inflation. We search for several physically motivated deviations from a simple power-law spectrum of curvature perturbations, including those motivated by a reconstruction of the inflaton potential not relying on the slow-roll approximation. We find that such models are not preferred, either according to a Bayesian model comparison or according to a frequentist simulation-based analysis. Three independent methods reconstructing the primordial power spectrum consistently recover a featureless and smooth P_R(k) over the range of scales 0.008 Mpc^(-1) \u2272 k \u2272 0.1 Mpc^(-1). At large scales, each method finds deviations from a power law, connected to a deficit at multipoles \u2113 \u2248 20\u221240 in the temperature power spectrum, but at an uncompelling statistical significance owing to the large cosmic variance present at these multipoles. By combining power spectrum and non-Gaussianity bounds, we constrain models with generalized Lagrangians, including Galileon models and axion monodromy models. The Planck data are consistent with adiabatic primordial perturbations, and the estimated values for the parameters of the base \u039b cold dark matter (\u039bCDM) model are not significantly altered when more general initial conditions are admitted. In correlated mixed adiabatic and isocurvature models, the 95% CL upper bound for the non-adiabatic contribution to the observed CMB temperature variance is | \u03b1_(non \u2013 adi) | < 1.9%, 4.0%, and 2.9% for CDM, neutrino density, and neutrino velocity isocurvature modes, respectively. We have tested inflationary models producing an anisotropic modulation of the primordial curvature power spectrum findingthat the dipolar modulation in the CMB temperature field induced by a CDM isocurvature perturbation is not preferred at a statistically significant level. We also establish tight constraints on a possible quadrupolar modulation of the curvature perturbation. These results are consistent with the Planck 2013 analysis based on the nominal mission data and further constrain slow-roll single-field inflationary models, as expected from the increased precision of Planck data using the full set of observations.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A20", "id_number": "CaltechAUTHORS:20170222-105731785", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170222-105731785", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "UK BIS National E-Infrastructure" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525898", "primary_object": { "basename": "aa25898-15.pdf", "url": "https://authors.library.caltech.edu/records/xrdg8-83809/files/aa25898-15.pdf" }, "related_objects": [ { "basename": "1502.02114.pdf", "url": "https://authors.library.caltech.edu/records/xrdg8-83809/files/1502.02114.pdf" } ], "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/59bq5-d0583", "eprint_id": 69978, "eprint_status": "archive", "datestamp": "2023-08-22 18:39:30", "lastmod": "2023-10-20 21:18:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Masters-D-C", "name": { "family": "Masters", "given": "Daniel" }, "orcid": "0000-0001-5382-6138" }, { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "Andreas" }, "orcid": "0000-0002-9382-9832" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" } ] }, "title": "A Tight Relation between N/O Ratio and Galaxy Stellar Mass Can Explain the Evolution of Strong Emission Line Ratios with Redshift", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: ISM; galaxies: abundances; HII regions; ISM: abundances", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 May 12; revised 2016 June 29; accepted 2016 July 5; published 2016 August 24. \n\nWe thank the anonymous referee for a thoughtful and constructive report that improved this paper. D.M. is grateful to Alaina Henry, Samir Salim, Charles Steinhardt, John Silverman, Lin Yan, Jin Koda, and Louis Abramson for helpful and enjoyable conversations. D.M. acknowledges the organizers and participants of the \"First Carnegie Symposium in Honor of Leonard Searle\", held at the Carnegie Observatories in July 2015, for many enlightening talks and conversations. A.F. acknowledges support from the Swiss National Science Foundation.\n\nPublished - apj_828_1_18.pdf
Submitted - 1605.04314v1.pdf
", "abstract": "The offset of high-redshift star-forming galaxies in the [O III]/H\u03b2 versus [N II]/H\u03b1 (O3N2) diagram in comparison with the local star-forming galaxy sequence is now well established. The physical origin of the shift is the subject of some debate and has important implications for metallicity measurements based on strong lines at all redshifts. To investigate the origin of the O3N2 offset, we use a sample of ~100,000 star-forming galaxies from the Sloan Digital Sky Survey DR12 to understand how measurable galaxy physical properties (\u03a3_(SFR), ionization parameter, nitrogen-to-oxygen (N/O) ratio, and stellar mass) drive galaxy position in two key diagnostic diagrams: O3N2 and [O III]/H\u03b2 versus [S II]/H\u03b1 (O3S2). At fixed [O III]/H\u03b2, galaxies close to the high-redshift locus in O3N2 have higher \u03a3_(SFR), stellar mass, and N/O ratio. We conclude that higher N/O ratios at fixed [O III]/H\u03b2 are the proximate cause of the O3N2 shift. We also find a tight correspondence in the distributions of stellar mass and N/O in the diagnostic diagrams. This relation, spanning a range of galaxy evolutionary states, suggests that the N/O\u2013M* relation is more fundamental than the relation between N/O and O/H. We argue that a more fundamental N/O\u2013M* relation is well-motivated physically. Because the mass\u2013metallicity relation evolves more rapidly with redshift than N/O\u2013M*, the N/O ratios of high-redshift galaxies are elevated in comparison with local galaxies with the same gas-phase O/H. The O3N2 shift and elevated N/O ratios observed in high-redshift galaxies, therefore, come about as a natural consequence of the N/O\u2013M* relation combined with the evolution of the mass\u2013metallicity relation.", "date": "2016-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "828", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 18", "id_number": "CaltechAUTHORS:20160826-132511755", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160826-132511755", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swiss National Science Foundation (SNSF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/0004-637X/828/1/18", "primary_object": { "basename": "1605.04314v1.pdf", "url": "https://authors.library.caltech.edu/records/59bq5-d0583/files/1605.04314v1.pdf" }, "related_objects": [ { "basename": "apj_828_1_18.pdf", "url": "https://authors.library.caltech.edu/records/59bq5-d0583/files/apj_828_1_18.pdf" } ], "pub_year": "2016", "author_list": "Masters, Daniel; Faisst, Andreas; et el." }, { "id": "https://authors.library.caltech.edu/records/y0vbh-pwx93", "eprint_id": 69372, "eprint_status": "archive", "datestamp": "2023-08-22 18:26:07", "lastmod": "2023-10-20 16:50:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hung-Chao-Ling", "name": { "family": "Hung", "given": "Chao-Ling" }, "orcid": "0000-0002-6879-3639" }, { "id": "Casey-C-M", "name": { "family": "Casey", "given": "Caitlin M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Chiang-Yi-Kuan", "name": { "family": "Chiang", "given": "Yi-Kuan" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Cowley-M-J", "name": { "family": "Cowley", "given": "Michael J." } }, { "id": "Darvish-B", "name": { "family": "Darvish", "given": "Behnam" }, "orcid": "0000-0003-4919-9017" }, { "id": "Kacprzak-G-G", "name": { "family": "Kacprzak", "given": "Glenn G." } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "Simon J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Nanayakkara-Themiya", "name": { "family": "Nanayakkara", "given": "Themiya" } }, { "id": "Spitler-L-R", "name": { "family": "Spitler", "given": "Lee R." } }, { "id": "Tran-Kim-Vy-H", "name": { "family": "Tran", "given": "Kim-Vy H." } }, { "id": "Yuan-Tiantian", "name": { "family": "Yuan", "given": "Tiantian" } } ] }, "title": "Large scale structure around a z = 2.1 cluster", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general; galaxies: starburst; large-scale structure of universe", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 March 9; revised 2016 May 17; accepted 2016 May 20; published 2016 July 27. \n\nC.-L.H. thanks J. R. Mart\u00ednez-Galarza for helpful discussion on SED fitting. C.-L.H. acknowledges support from the Harlan J. Smith Fellowship. C.M.C. thanks the University of Texas at Austin, College of Natural Science for support. G.G.K. acknowledges the support of the Australian Research Council through the award of a Future Fellowship (FT140100933). The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Some of the data presented here were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration and made possible by financial support of the W.M. Keck Foundation. \n\nPart of the data presented in this paper has been made available by the COSMOS team (http://cosmos.astro.caltech. edu). COSMOS is based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc, under NASA contract NAS 5-26555; also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc; and the Canada\u2013France\u2013Hawaii Telescope operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France and the University of Hawaii.\n\nPublished - apj_826_2_130.pdf
Submitted - 1605.07176v1.pdf
", "abstract": "The most prodigious starburst galaxies are absent in massive galaxy clusters today, but their connection with large-scale environments is less clear at z \u2273 2. We present a search of large-scale structure around a galaxy cluster core at z = 2.095 using a set of spectroscopically confirmed galaxies. We find that both color-selected star-forming galaxies (SFGs) and dusty star-forming galaxies (DSFGs) show significant overdensities around the z = 2.095 cluster. A total of eight DSFGs (including three X-ray luminous active galactic nuclei, AGNs) and 34 SFGs are found within a 10' radius (corresponds to ~15 cMpc at z ~ 2.1) from the cluster center and within a redshift range of \u0394z = 0.02, which leads to galaxy overdensities of \u03b4_(DSFG) ~ 12.3$ and \u03b4_(SFG) ~ 2.8. The cluster core and the extended DSFG- and SFG-rich structures together demonstrate an active cluster formation phase, in which the cluster is accreting a significant amount of material from large-scale structure while the more mature core may begin to virialize. Our finding of this DSFG-rich structure, along with a number of other protoclusters with excess DSFGs and AGNs found to date, suggest that the overdensities of these rare sources indeed trace significant mass overdensities. However, it remains puzzling how these intense star formers are triggered concurrently. Although an increased probability of galaxy interactions and/or enhanced gas supply can trigger the excess of DSFGs, our stacking analysis based on 850 \u03bcm images and morphological analysis based on rest-frame optical imaging do not show such enhancements of merger fraction and gas content in this structure.", "date": "2016-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "826", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 130", "id_number": "CaltechAUTHORS:20160802-073409566", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160802-073409566", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council", "grant_number": "FT140100933" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "ESA Member States" }, { "agency": "European Southern Observatory (ESO)" }, { "agency": "Kitt Peak National Observatory" }, { "agency": "Cerro Tololo Inter-American Observatory" }, { "agency": "National Optical Astronomy Observatory (NOAO)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "doi": "10.3847/0004-637X/826/2/130", "primary_object": { "basename": "1605.07176v1.pdf", "url": "https://authors.library.caltech.edu/records/y0vbh-pwx93/files/1605.07176v1.pdf" }, "related_objects": [ { "basename": "apj_826_2_130.pdf", "url": "https://authors.library.caltech.edu/records/y0vbh-pwx93/files/apj_826_2_130.pdf" } ], "pub_year": "2016", "author_list": "Hung, Chao-Ling; Casey, Caitlin M.; et el." }, { "id": "https://authors.library.caltech.edu/records/f9vwt-34y95", "eprint_id": 70417, "eprint_status": "archive", "datestamp": "2023-08-22 18:17:52", "lastmod": "2023-10-20 22:56:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Darvish-B", "name": { "family": "Darvish", "given": "Behnam" }, "orcid": "0000-0003-4919-9017" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Sobral-D", "name": { "family": "Sobral", "given": "David" }, "orcid": "0000-0001-8823-4845" }, { "id": "Rettura-A", "name": { "family": "Rettura", "given": "Alessandro" }, "orcid": "0000-0002-5615-256X" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "Andreas" }, "orcid": "0000-0002-9382-9832" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" } ] }, "title": "The Effects of the Local Environment and Stellar Mass on Galaxy Quenching to z ~ 3", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; large-scale structure of universe", "note": "\u00a9 2016 The American Astronomical Society. Received 2016 January 19; revised 2016 April 19; accepted 2016 May 9; published 2016 July 8.\n\nWe are grateful to the anonymous referee for reading the manuscript and providing very useful comments which significantly improved the quality of this work. B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. B.D. wishes to thank Brian Siana, Gabriela Canalizo, and Chang Hoon Hahn for their helpful comments and discussions. D.S. acknowledges financial support from the Netherlands Organization for Scientific Research (NWO) through a Veni Fellowship, from FCT through an FCT Investigator Starting Grant and Startup Grant (IF/01154/2012/CP0189/CT0010), and from FCT grant PEst-OE/FIS/UI2751/2014. A.F. acknowledges support from the Swiss National Science Foundation. This work extensively uses COSMOS UltraVISTA data that are based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO program ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.\n\nPublished - apj_825_2_113.pdf
Submitted - 1605.03182v1.pdf
", "abstract": "We study the effects of the local environment and stellar mass on galaxy properties using a mass complete sample of quiescent and star-forming systems in the COSMOS field at z \u227e 3. We show that at z \u227e 1 the median star formation rate (SFR) and specific SFR (sSFR) of all galaxies depend on the environment, but they become independent of the environment at z \u2273 1. However, we find that only for star-forming galaxies, the median SFR and sSFR are similar in different environments regardless of redshift and stellar mass. We find that the quiescent fraction depends on the environment at z \u227e 1 and on stellar mass out to z ~ 3. We show that at z \u227e 1 galaxies become quiescent faster in denser environments and that the overall environmental quenching efficiency increases with cosmic time. Environmental and mass quenching processes depend on each other. At z \u227e 1 denser environments more efficiently quench galaxies with higher masses (log(M/M_\u2609) \u2273 10.7), possibly due to a higher merger rate of massive galaxies in denser environments. We also show that mass quenching is more efficient in denser regions. We show that the overall mass quenching efficiency (\u0454_(mass) for more massive galaxies (log(M/M_\u2609) \u2273 10.2) rises with cosmic time until z ~ 1 and then flattens out. However, for less massive galaxies, the rise in \u0454_(mass) continues to the present time. Our results suggest that environmental quenching is only relevant at z \u227e 1 and is likely a fast process, whereas mass quenching is the dominant mechanism at z \u2273 1 with a possible stellar feedback physics.", "date": "2016-07-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "825", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No.113", "id_number": "CaltechAUTHORS:20160919-090850444", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160919-090850444", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX12AE20G" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT) (Portugal)", "grant_number": "IF/01154/2012/CP0189/CT0010" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT) (Portugal)", "grant_number": "PEst-OE/FIS/UI2751/2014" }, { "agency": "Swiss National Science Foundation (SNSF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/0004-637X/825/2/113", "primary_object": { "basename": "1605.03182v1.pdf", "url": "https://authors.library.caltech.edu/records/f9vwt-34y95/files/1605.03182v1.pdf" }, "related_objects": [ { "basename": "apj_825_2_113.pdf", "url": "https://authors.library.caltech.edu/records/f9vwt-34y95/files/apj_825_2_113.pdf" } ], "pub_year": "2016", "author_list": "Darvish, Behnam; Mobasher, Bahram; et el." }, { "id": "https://authors.library.caltech.edu/records/z9jbx-wka69", "eprint_id": 68889, "eprint_status": "archive", "datestamp": "2023-09-15 05:29:45", "lastmod": "2023-10-23 21:18:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steinhardt-C-L", "name": { "family": "Steinhardt", "given": "Charles. L." }, "orcid": "0000-0003-3780-6801" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "Dan" }, "orcid": "0000-0001-5382-6138" }, { "id": "Speagle-J-S", "name": { "family": "Speagle", "given": "Josh S." }, "orcid": "0000-0002-5065-9896" } ] }, "title": "The Impossibly Early Galaxy Problem", "ispublished": "pub", "full_text_status": "public", "keywords": "dark matter \u2013 galaxies: evolution \u2013 galaxies: formation", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 June 3; accepted 2016 April 8; published 2016 June 6. \n\nThe authors would like to thank Michaela Bagley, Peter Behroozi, Rychard Bouwens, Andreas Faisst, Steven Finkelstein, Hendrik Hildebrandt, Alexander Karim, Olivier Le Fevre, Nick Lee, Surhud More, Dave Sanders, Johannes Staguhn, and Dominic Yurk for helpful comments.\n\nPublished - apj_824_1_21.pdf
Submitted - 1506.01377v2.pdf
", "abstract": "The current hierarchical merging paradigm and \u039bCDM predict that the z ~ 4 \u2013 8 universe should be a time in which the most massive galaxies are transitioning from their initial halo assembly to the later baryonic evolution seen in star-forming galaxies and quasars. However, no evidence of this transition has been found in many high-redshift galaxy surveys including CFHTLS, Cosmic Assembly Near-infrared Deep Extragalactic Survey (CANDELS), and Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH), which were the first studies to probe the high-mass end at these redshifts. Indeed, if halo mass to stellar mass ratios estimated at lower-redshift continue to z ~ 6 - 8, CANDELS and SPLASH report several orders of magnitude more M ~ 10^(12-13)M\u2299 halos than is possible to have been formed by those redshifts, implying that these massive galaxies formed impossibly early. We consider various systematics in the stellar synthesis models used to estimate physical parameters and possible galaxy formation scenarios in an effort to reconcile observation with theory. Although known uncertainties can greatly reduce the disparity between recent observations and cold dark matter merger simulations, there remains considerable tension with current theory even if taking the most conservative view of the observations.", "date": "2016-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "824", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 21", "id_number": "CaltechAUTHORS:20160707-104137561", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160707-104137561", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "SPLASH" } ] }, "doi": "10.3847/0004-637X/824/1/21", "primary_object": { "basename": "1506.01377v2.pdf", "url": "https://authors.library.caltech.edu/records/z9jbx-wka69/files/1506.01377v2.pdf" }, "related_objects": [ { "basename": "apj_824_1_21.pdf", "url": "https://authors.library.caltech.edu/records/z9jbx-wka69/files/apj_824_1_21.pdf" } ], "pub_year": "2016", "author_list": "Steinhardt, Charles. L.; Capak, Peter; et el." }, { "id": "https://authors.library.caltech.edu/records/7ykez-j9p93", "eprint_id": 78669, "eprint_status": "archive", "datestamp": "2023-08-20 12:01:47", "lastmod": "2023-10-26 00:17:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Roberts-Borsani-G-W", "name": { "family": "Roberts-Borsani", "given": "G. W." } }, { "id": "Bouwens-R-J", "name": { "family": "Bouwens", "given": "R. J." }, "orcid": "0000-0002-4989-2471" }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P. A." }, "orcid": "0000-0001-5851-6649" }, { "id": "Labb\u00e9-I", "name": { "family": "Labb\u00e9", "given": "I." }, "orcid": "0000-0002-2057-5376" }, { "id": "Smit-Renske", "name": { "family": "Smit", "given": "R." }, "orcid": "0000-0001-8034-7802" }, { "id": "Illingworth-G-D", "name": { "family": "Illingworth", "given": "G. D." }, "orcid": "0000-0002-8096-2837" }, { "id": "van-Dokkum-P-G", "name": { "family": "van Dokkum", "given": "P. G." }, "orcid": "0000-0002-8282-9888" }, { "id": "Holden-B-P", "name": { "family": "Holden", "given": "B." }, "orcid": "0000-0002-6153-3076" }, { "id": "Gonzalez-V", "name": { "family": "Gonzalez", "given": "V." }, "orcid": "0000-0002-3120-0510" }, { "id": "Stefanon-M", "name": { "family": "Stefanon", "given": "M." }, "orcid": "0000-0001-7768-5309" }, { "id": "Holwerda-B-W", "name": { "family": "Holwerda", "given": "B." }, "orcid": "0000-0002-4884-6756" }, { "id": "Wilkins-S", "name": { "family": "Wilkins", "given": "S." } } ] }, "title": "z\u2273 7 galaxies with red Spitzer/IRAC [3.6]-[4.5] colors in the full CANDELS data set: The brightest-known galaxies at z~ 7-9 and a probable spectroscopic confirmation at z = 7.48", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2016. The American Astronomical Society.", "abstract": "We identify four unusually bright (H ${}_{160,{AB}}$ < 25.5) galaxies from Hubble Space Telescope (HST) and Spitzer CANDELS data with probable redshifts z ~ 7\u20139. These identifications include the brightest-known galaxies to date at z gsim 7.5. As Y-band observations are not available over the full CANDELS program to perform a standard Lyman-break selection of z > 7 galaxies, we employ an alternate strategy using deep Spitzer/IRAC data. We identify z ~ 7.1\u20139.1 galaxies by selecting z gsim 6 galaxies from the HST CANDELS data that show quite red IRAC [3.6]\u2212[4.5] colors, indicating strong [O iii]+H\u03b2 lines in the 4.5 \u03bcm band. This selection strategy was validated using a modest sample for which we have deep Y-band coverage, and subsequently used to select the brightest z \u2265 7 sources. Applying the IRAC criteria to all HST-selected optical dropout galaxies over the full ~900 arcmin2 of the CANDELS survey revealed four unusually bright z ~ 7.1, 7.6, 7.9, and 8.6 candidates. The median [3.6]\u2212[4.5] color of our selected z ~ 7.1\u20139.1 sample is consistent with rest-frame [O iii]+H\u03b2 EWs of ~1500 \u00c5 in the [4.5] band. Keck/MOSFIRE spectroscopy has been independently reported for two of our selected sources, showing Ly\u03b1 at redshifts of 7.7302 \u00b1 0.0006 and ${8.683}_{-0.004}^{+0.001}$, respectively. We present similar Keck/MOSFIRE spectroscopy for a third selected galaxy with a probable 4.7\u03c3 Ly\u03b1 line at z spec = 7.4770 \u00b1 0.0008. All three have H160-band magnitudes of ~25 mag and are ~0.5 mag more luminous (M 1600 ~ \u221222.0) than any previously discovered z ~ 8 galaxy, with important implications for the UV luminosity function (LF). Our three brightest and highest redshift z > 7 galaxies all lie within the CANDELS-EGS field, providing a dramatic illustration of the potential impact of field-to-field variance", "date": "2016-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "823", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 143", "id_number": "CaltechAUTHORS:20170628-142851441", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170628-142851441", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "SPLASH" }, { "id": "COSMOS" } ] }, "doi": "10.3847/0004-637X/823/2/143", "pub_year": "2016", "author_list": "Roberts-Borsani, G. W.; Bouwens, R. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/pd4gk-kjc16", "eprint_id": 70427, "eprint_status": "archive", "datestamp": "2023-08-22 18:05:41", "lastmod": "2023-10-20 22:57:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Laigle-C", "name": { "family": "Laigle", "given": "C." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The COSMOS2015 Catalog: Exploring the 1 < z < 6 Universe with Half a Million Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: evolution; galaxies: high-redshift; galaxies: photometry; methods: observational; techniques: photometric", "note": "\u00a9 2016 The American Astronomical Society. Received 2015 September 30; accepted 2016 February 23; published 2016 June 8.\n\nC.L. is supported by the ILP LABEX (under reference ANR-10-LABX-63 and ANR-11-IDEX-0004-02). This work is partially supported by the Spin(e) grants ANR-13-BS05-0005 of the French Agence Nationale de la Recherche. H.J.M.C.C. acknowledges financial support form the \"Programme national cosmologie et galaxies\" (PNCG). O.I. acknowledges the funding of the French Agence Nationale de la Recherche for the project \"SAGACE\". J.D.S. is supported by JSPS KAKENHI grant No. 26400221, the World Premier International Research Center Initiative (WPI), MEXT, Japan and by CREST, JST. B.M.J. and J.P.U.F. acknowledge support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the DNRF. S.T. and M.S. acknowledge support from the ERC Consolidator Grant funding scheme (project ConTExt, grant No. 648179). This research is also partly supported by the Centre National dEtudes Spatiales (CNES). This work is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. V.S. acknowledges the European Union's Seventh Framework program under grant agreement 337595.\n\nPublished - apjs_224_2_24.pdf
Submitted - 1604.02350v1.pdf
", "abstract": "We present the COSMOS2015 catalog, which contains precise photometric redshifts and stellar masses for more than half a million objects over the 2deg^2 COSMOS field. Including new YJHK_s images from the UltraVISTA-DR2 survey, Y-band images from Subaru/Hyper-Suprime-Cam, and infrared data from the Spitzer Large Area Survey with the Hyper-Suprime-Cam Spitzer legacy program, this near-infrared-selected catalog is highly optimized for the study of galaxy evolution and environments in the early universe. To maximize catalog completeness for bluer objects and at higher redshifts, objects have been detected on a \u03c7^2 sum of the YJHK_s and z^(++) images. The catalog contains ~6 x 10^5 objects in the 1.5 deg^2 UltraVISTA-DR2 region and ~ 1.5 x 10^5 objects are detected in the \"ultra-deep stripes\" (0.62 deg^2) at K_s \u2a7d 24.7 (3\u03c3, 3\", AB magnitude). Through a comparison with the zCOSMOS-bright spectroscopic redshifts, we measure a photometric redshift precision of \u03c3_\u0394z/(1+_s) = 0.007 and a catastrophic failure fraction of \u03b7 = 0.5%. At 3 < z < 6, using the unique database of spectroscopic redshifts in COSMOS, we find \u03c3_\u0394z/(1+z_s) = 0.021 and \u03b7 = 13.2%. The deepest regions reach a 90% completeness limit of 10^10 M_\u2299 to z = 4. Detailed comparisons of the color distributions, number counts, and clustering show excellent agreement with the literature in the same mass ranges. COSMOS2015 represents a unique, publicly available, valuable resource with which to investigate the evolution of galaxies within their environment back to the earliest stages of the history of the universe. The COSMOS2015 catalog is distributed via anonymous ftp and through the usual astronomical archive systems (CDS, ESO Phase 3, IRSA).", "date": "2016-06", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "224", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 24", "id_number": "CaltechAUTHORS:20160919-104756275", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160919-104756275", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agence Nationale de la Recherche (ANR)", "grant_number": "ANR-10-LABX-63" }, { "agency": "Agence Nationale de la Recherche (ANR)", "grant_number": "ANR-11-IDEX-0004-02" }, { "agency": "Agence Nationale de la Recherche (ANR)", "grant_number": "ANR-13-BS05-0005" }, { "agency": "Programme National Cosmologie et Galaxies (PNCG)" }, { "agency": "Agence Nationale de la Recherche (ANR) SAGACE" }, { "agency": "Japan Society for the Promotion of Science (JSPS) KAKENHI", "grant_number": "26400221" }, { "agency": "World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan" }, { "agency": "Japan Science and Technology Agency (JST) CREST" }, { "agency": "European Research Council (ERC)", "grant_number": "278202" }, { "agency": "Danish National Research Foundation (DNRF)" }, { "agency": "European Research Council (ERC)", "grant_number": "648179" }, { "agency": "Centre National dEtudes Spatiales (CNES)" }, { "agency": "European Research Council (European Union)", "grant_number": "337595" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "SPLASH" } ] }, "doi": "10.3847/0067-0049/224/2/24", "primary_object": { "basename": "1604.02350v1.pdf", "url": "https://authors.library.caltech.edu/records/pd4gk-kjc16/files/1604.02350v1.pdf" }, "related_objects": [ { "basename": "apjs_224_2_24.pdf", "url": "https://authors.library.caltech.edu/records/pd4gk-kjc16/files/apjs_224_2_24.pdf" } ], "pub_year": "2016", "author_list": "Laigle, C.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/0sr5s-4h724", "eprint_id": 68636, "eprint_status": "archive", "datestamp": "2023-08-22 17:56:58", "lastmod": "2023-10-19 22:23:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "A. L." }, "orcid": "0000-0002-9382-9832" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Davidzon-I", "name": { "family": "Davidzon", "given": "I." }, "orcid": "0000-0002-2951-7519" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "C." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Onodera-Masato", "name": { "family": "Onodera", "given": "M." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Kakazu-Yuko", "name": { "family": "Kakazu", "given": "Y." } }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "D." }, "orcid": "0000-0001-5382-6138" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Rest-UV Absorption Lines as Metallicity Estimator: the Metal Content of Star-Forming Galaxies at z ~ 5", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: abundances; galaxies: evolution; galaxies: high-redshift; galaxies: ISM", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 November 19; accepted 2016 February 13; published 2016 May 2. \n\nWe would like to acknowledge the support of the Keck Observatory staff who made these observations possible as well as Micaela Bagley, Janice Lee, and David Sobral for valuable discussions. We also would like to thank the referee for valuable comments that have improved this paper. A.F. acknowledges support from the Swiss National Science Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\n\nPublished - apj_822_1_29.pdf
Submitted - 1512.00018v1.pdf
", "abstract": "We measure a relation between the depth of four prominent rest-UV absorption complexes and metallicity for local galaxies and verify it up to z ~ 3. We then apply this relation to a sample of 224 galaxies at 3.5 < z < 6.0 ( \u3008z\u3009 = 4.8) in the Cosmic Evolution Survey (COSMOS), for which unique UV spectra from the Deep Imaging Multi-object Spectrograph (DEIMOS) and accurate stellar masses from the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH) are available. The average galaxy population at z ~ 5 and log(M/M_\u2609) > 9 is characterized by 0.3\u20130.4 dex (in units of 12 + log O/H lower metallicities than at z ~ 2, but comparable to z ~ 3.5. We find galaxies with weak or no Ly\u03b1 emission to have metallicities comparable to z ~ 2 galaxies and therefore may represent an evolved subpopulation of z ~ 5 galaxies. We find a correlation between metallicity and dust in good agreement with local galaxies and an inverse trend between metallicity and star-formation rate consistent with observations at z ~ 2. The relation between stellar mass and metallicity (MZ relation) is similar to z ~ 3.5, but there are indications of it being slightly shallower, in particular for the young, Ly\u03b1-emitting galaxies. We show that, within a \"bathtub\" approach, a shallower MZ relation is expected in the case of a fast (exponential) build-up of stellar mass with an e-folding time of 100\u2013200 Myr. Because of this fast evolution, the process of dust production and metal enrichment as a function of mass could be more stochastic in the first billion years of galaxy formation compared to later times.", "date": "2016-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "822", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 29", "id_number": "CaltechAUTHORS:20160623-120349827", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160623-120349827", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swiss National Science Foundation (SNSF)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" }, { "id": "SPLASH" } ] }, "doi": "10.3847/0004-637X/822/1/29", "primary_object": { "basename": "1512.00018v1.pdf", "url": "https://authors.library.caltech.edu/records/0sr5s-4h724/files/1512.00018v1.pdf" }, "related_objects": [ { "basename": "apj_822_1_29.pdf", "url": "https://authors.library.caltech.edu/records/0sr5s-4h724/files/apj_822_1_29.pdf" } ], "pub_year": "2016", "author_list": "Faisst, A. L.; Capak, P. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/xxrdp-jpc38", "eprint_id": 68647, "eprint_status": "archive", "datestamp": "2023-08-22 17:49:22", "lastmod": "2023-10-19 22:24:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "A. L." }, "orcid": "0000-0002-9382-9832" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Hsieh-Bau-Ching", "name": { "family": "Hsieh", "given": "B. C." }, "orcid": "0000-0001-5615-4904" }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "C." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Tasca-L", "name": { "family": "Tasca", "given": "L." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Davidzon-I", "name": { "family": "Davidzon", "given": "I." }, "orcid": "0000-0002-2951-7519" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "D." }, "orcid": "0000-0001-5382-6138" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Steinhardt-C-L", "name": { "family": "Steinhardt", "given": "C." }, "orcid": "0000-0003-3780-6801" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "de-Barros-S", "name": { "family": "de Barros", "given": "S." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "A Coherent Study of Emission Lines from Broadband Photometry: Specific Star Formation Rates and [O III]/H\u03b2 Ratio at 3 < z < 6", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: star formation", "note": "\u00a9 2016 The American Astronomical Society. Received 2016 January 15; accepted 2016 March 7; published 2016 April 20.\n\nWe would like to thank Josh Speagle, Micaela Bagley, and\nBahram Mobasher for valuable discussions. We also would like\nto thank the referee for valuable comments that have improved this paper. A.F. acknowledges support from the Swiss National Science Foundation. C.L. is supported by the ILP LABEX\n(under reference ANR-10-LABX-63 and ANR-11-IDEX-0004-\n02). J.D.S. is supported by JSPS KAKENHI Grant Number\n26400221, the World Premier International Research Center\nInitiative (WPI), MEXT, Japan and by CREST, JST. Part of\nthis work is based on data obtained with the European Southern\nObservatory Very Large Telescope, Paranal, Chile, under\nLarge Programs 175.A-0839 and 185.A-0791. This work is\nsupported by funding from the European Research Council\nAdvanced Grant ERC-2010-AdG-268107-EARLY. Based on\ndata products from observations made with ESO Telescopes at\nthe La Silla Paranal Observatory under ESO programme ID\n179.A-2005 and on data products produced by TERAPIX and\nthe Cambridge Astronomy Survey Unit on behalf of the\nUltraVISTA consortium. Also, the authors wish to recognize\nand acknowledge the very significant cultural role and\nreverence that the summit of Mauna Kea has always had\nwithin the indigenous Hawaiian community. We are most\nfortunate to have the opportunity to conduct observations from\nthis mountain.\n\nPublished - apj_821_2_122.pdf
Submitted - 1601.07173v1.pdf
", "abstract": "We measure the H\u03b1 and [O III] emission line properties as well as specific star formation rates (sSFRs) of spectroscopically confirmed 3 < z < 6 galaxies in COSMOS from their observed colors versus redshift evolution. Our model describes consistently the ensemble of galaxies including intrinsic properties (age, metallicity, star formation history), dust attenuation, and optical emission lines. We forward-model the measured H\u03b1 equivalent widths (EW) to obtain the sSFR out to z ~ 6 without stellar mass fitting. We find a strongly increasing rest-frame H\u03b1 EW that is flattening off above z ~ 2.5 with average EWs of 300\u2013600 \u00c5 at z ~ 6. The sSFR is increasing proportionally to (1+z)^(2.4) at z < 2.2 and to (1+z)^(1.5) at higher redshifts, indicative of a fast build-up of mass in high-z galaxies within e-folding times of 100\u2013200 Myr at z ~ 6. The redshift evolution at z > 3 cannot be fully explained in a picture of growth driven by cold accretion. We find a progressively increasing [O III]\u03bb5007/H\u03b2 ratio out to z ~ 6, consistent with the ratios in local galaxies selected by increasing H\u03b1 EW (i.e., sSFR). This demonstrates the potential of using \"local high-z analogs\" to investigate the spectroscopic properties and relations of galaxies in the re-ionization epoch.", "date": "2016-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "821", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 122", "id_number": "CaltechAUTHORS:20160624-075417558", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160624-075417558", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-10-LABX-63" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-11-IDEX-0004-02" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "26400221" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Japan Science and Technology Agency (JST) CREST" }, { "agency": "European Research Council (ERC)", "grant_number": "ERC-2010-AdG-268107-EARLY" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" }, { "id": "SPLASH" } ] }, "doi": "10.3847/0004-637X/821/2/122", "primary_object": { "basename": "1601.07173v1.pdf", "url": "https://authors.library.caltech.edu/records/xxrdp-jpc38/files/1601.07173v1.pdf" }, "related_objects": [ { "basename": "apj_821_2_122.pdf", "url": "https://authors.library.caltech.edu/records/xxrdp-jpc38/files/apj_821_2_122.pdf" } ], "pub_year": "2016", "author_list": "Faisst, A. L.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/rxn8y-8en22", "eprint_id": 58899, "eprint_status": "archive", "datestamp": "2023-08-20 11:10:00", "lastmod": "2023-10-23 15:25:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Vanden-Bout-P-A", "name": { "family": "Vanden Bout", "given": "P." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Casey-C-M", "name": { "family": "Casey", "given": "C. M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Murchikova-L", "name": { "family": "Murchikova", "given": "L." } }, { "id": "Koda-Jin", "name": { "family": "Koda", "given": "J." }, "orcid": "0000-0002-8762-7863" }, { "id": "\u00c1lvarez-M\u00e1rquez-J", "name": { "family": "\u00c1lvarez-M\u00e1rquez", "given": "J." }, "orcid": "0000-0002-7093-1877" }, { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "N." } }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Pope-Alexandra", "name": { "family": "Pope", "given": "A." }, "orcid": "0000-0001-8592-2706" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Chu-Jason", "name": { "family": "Chu", "given": "J." }, "orcid": "0000-0003-3955-2470" }, { "id": "Toft-S", "name": { "family": "Toft", "given": "S." }, "orcid": "0000-0003-3631-7176" }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Manohar-S", "name": { "family": "Manohar", "given": "S." } } ] }, "title": "ISM masses and the star formation law at Z = 1 to 6: ALMA observations of dust continuum in 145 galaxies in the COSMOS survey field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 galaxies: evolution \u2013 galaxies: ISM", "note": "\u00a9 2016 The American Astronomical Society. Received 2015 May 7; accepted 2016 February 10; published 2016 March 22. We thank Zara Scoville for proof reading the manuscript and Sue Madden for suggesting use of the SPIRE fluxes for calibration. This paper makes use of the following ALMA data: ADS/JAO.ALMA# 2013.1.00034.S. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00111. S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. R.J.I. acknowledges support from ERC in the form of the Advanced Investigator Programme, 321302, COSMICISM.\n\nPublished - apj_820_2_83.pdf
Submitted - 1505.02159v1.pdf
Submitted - 1511.05149.pdf
Erratum - apj_824_1_63_er.pdf
", "abstract": "ALMA Cycle 2 observations of long-wavelength dust emission in 145 star-forming galaxies are used to probe the evolution of the star-forming interstellar medium (ISM). We also develop a physical basis and empirical calibration (with 72 low-z and z ~ 2 galaxies) for using the dust continuum as a quantitative probe of ISM masses. The galaxies with the highest star formation rates (SFRs) at = 2.2 and 4.4 have gas masses up to 100 times that of the Milky Way and gas mass fractions reaching 50%\u201380%, i.e., gas masses 1-4\u00d7 their stellar masses. We find a single high-z star formation law: SFR = 35 M^(0.89)_(mol) x (1 + z)^(0.95)_(z=2) x (sSFR)^(0.23)_(MS) M\u2299yr^(\u22121)\u2014an approximately linear dependence on the ISM mass and an increased star formation efficiency per unit gas mass at higher redshift. Galaxies above the main sequence (MS) have larger gas masses but are converting their ISM into stars on a timescale only slightly shorter than those on the MS; thus, these \"starbursts\" are largely the result of having greatly increased gas masses rather than an increased efficiency of converting gas to stars. At z > 1, the entire population of star-forming galaxies has ~2\u20135 times shorter gas depletion times than low-z galaxies. These shorter depletion times indicate a different mode of star formation in the early universe\u2014most likely dynamically driven by compressive, high-dispersion gas motions\u2014a natural consequence of the high gas accretion rates.", "date": "2016-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "820", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 83", "id_number": "CaltechAUTHORS:20150715-154118222", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150715-154118222", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "321302" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/0004-637X/820/2/83", "primary_object": { "basename": "1505.02159v1.pdf", "url": "https://authors.library.caltech.edu/records/rxn8y-8en22/files/1505.02159v1.pdf" }, "related_objects": [ { "basename": "1511.05149.pdf", "url": "https://authors.library.caltech.edu/records/rxn8y-8en22/files/1511.05149.pdf" }, { "basename": "apj_820_2_83.pdf", "url": "https://authors.library.caltech.edu/records/rxn8y-8en22/files/apj_820_2_83.pdf" }, { "basename": "apj_824_1_63_er.pdf", "url": "https://authors.library.caltech.edu/records/rxn8y-8en22/files/apj_824_1_63_er.pdf" } ], "pub_year": "2016", "author_list": "Scoville, N.; Sheth, K.; et el." }, { "id": "https://authors.library.caltech.edu/records/gqthk-5h760", "eprint_id": 67195, "eprint_status": "archive", "datestamp": "2023-08-20 11:11:50", "lastmod": "2023-10-18 20:56:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hathi-N-P", "name": { "family": "Hathi", "given": "N. P." }, "orcid": "0000-0001-6145-5090" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The VIMOS Ultra Deep Survey: Ly\u03b1 emission and stellar populations of star-forming galaxies at 2 < z < 2.5", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: formation, galaxies: high-redshift", "note": "\u00a9 2016 ESO. \n\nReceived 3 March 2015. Accepted 11 December 2015. \n\nWe thank the referee for helpful comments and suggestions that significantly improved this paper. This work is supported by funding from the European Research Council Advanced Grant ERC-2010-AdG-268107-EARLY and by INAF Grants PRIN 2010, PRIN 2012 and PICS 2013. A.C., O.C., M.T. and V.S. acknowledge the grant MIUR PRIN 2010\u20132011. This work is based on data products made available at the CESAM data center, Laboratoire d'Astrophysique de Marseille. This work partly uses observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS.\n\nPublished - aa26012-15.pdf
Submitted - 1503.01753v2.pdf
", "abstract": "The aim of this paper is to investigate spectral and photometric properties of 854 faint (i_(AB)\u2009\u2272\u200925 mag) star-forming galaxies (SFGs) at 2\u2009<\u2009z\u2009<\u20092.5 using the VIMOS Ultra-Deep Survey (VUDS) spectroscopic data and deep multi-wavelength photometric data in three extensively studied extragalactic fields (ECDFS, VVDS, COSMOS). These SFGs were targeted for spectroscopy as a result of their photometric redshifts. The VUDS spectra are used to measure the UV spectral slopes (\u03b2) as well as Ly\u03b1 equivalent widths (EW). On average, the spectroscopically measured \u03b2 (\u20131.36 \u00b1 0.02), is comparable to the photometrically measured \u03b2 (\u20131.32 \u00b1 0.02), and has smaller measurement uncertainties. The positive correlation of \u03b2 with the spectral energy distribution (SED)-based measurement of dust extinction E_s(B\u2212V) emphasizes the importance of \u03b2 as an alternative dust indicator at high redshifts. To make a proper comparison, we divide these SFGs into three subgroups based on their rest-frame Ly\u03b1 EW: SFGs with no Ly\u03b1 emission (SFG_N; EW\u2009\u2264\u20090 \u00c5), SFGs with Ly\u03b1 emission (SFG_L; EW\u2009>\u20090 \u00c5), and Ly\u03b1 emitters (LAEs; EW\u2009\u2265\u200920 \u00c5). The fraction of LAEs at these redshifts is ~10%, which is consistent with previous observations. We compared best-fitSED-estimated stellar parameters of the SFG_N, SFG_L and LAE samples. For the luminosities probed here (~ L^\u2217), we find that galaxies with and without Ly\u03b1 in emission have small but significant differences in their SED-based properties. We find that LAEs have less dust, and lower star-formation rates (SFR) compared to non-LAEs. We also find that LAEs are less massive compared to non-LAEs, though the difference is smaller and less significant compared to the SFR and Es(B\u2212V). When we divide the LAEs according to their Spitzer/IRAC 3.6 \u03bcm fluxes, we find that the fraction of IRAC-detected (m_(3.6)\u2009\u2272\u200925 mag) LAEs is much higher than the fraction of IRAC-detected narrow band (NB)-selected LAEs at z\u2009\u2243\u20092\u20133. This could imply that UV-selected LAEs host a more evolved stellar population, which represents a later stage of galaxy evolution, compared to NB-selected LAEs.", "date": "2016-04-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "588", "publisher": "EDP Sciences", "pagerange": "Art. No. A26", "id_number": "CaltechAUTHORS:20160520-072846490", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160520-072846490", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "ERC-2010-AdG-268107-EARLY" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2010" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2012" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PICS 2013" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 della Ricerca (MIUR)", "grant_number": "PRIN 2010\u20132011" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201526012", "primary_object": { "basename": "aa26012-15.pdf", "url": "https://authors.library.caltech.edu/records/gqthk-5h760/files/aa26012-15.pdf" }, "related_objects": [ { "basename": "1503.01753v2.pdf", "url": "https://authors.library.caltech.edu/records/gqthk-5h760/files/1503.01753v2.pdf" } ], "pub_year": "2016", "author_list": "Hathi, N. P.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/8w96h-04689", "eprint_id": 66225, "eprint_status": "archive", "datestamp": "2023-08-20 10:47:24", "lastmod": "2023-10-18 17:16:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "F. A." }, "orcid": "0000-0003-2992-8024" }, { "id": "Stern-D", "name": { "family": "Stern", "given": "D." }, "orcid": "0000-0003-2686-9241" } ] }, "title": "The Chandra COSMOS Legacy survey: overview and point source catalog", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2015 July 31; accepted 2015 December 24; published 2016 February 29. \n\nThe authors thank the referee for the useful comments. F. C. and M. C. U. gratefully thank Debra Fine for her support to women in science and the Chandra EPO team, in particular J. De Pasquale, for creating the true-color X-ray image. This research has made use of data obtained from the Chandra Data Archive and software provided by the Chandra X-ray Center (CXC) in the CIAO application package. \n\nThis work was supported in part by NASA Chandra grant number GO7-8136A (F.C., S.M., V.A., M.E., H.S.); PRIN-INAF 2014 \"Windy Black Holes combing galaxy evolution\" (A.C., M.B., G.L. and C.V.); the FP7 Career Integration Grant \"eEASy\": \"Supermassive blackholes through cosmic time: from current surveys to eROSITA-Euclid Synergies\"(CIG 321913; M.B. and G.L.); UNAM-DGAPA Grant PAPIIT IN104113 and CONACyT Grant Cient\u00edfica B\u00e1sica #179662 (T.M.); Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (A.K.); NASA contract NAS8-03060 (T.A., A.F., K.G.); the Greek General Secretariat of Research and Technology in the framework of the Programme of Support of Postdoctoral Researchers (P.R.); NASA award NNX15AE61G (R.G.); the Science and Technology Facilities Council through grant code ST/I001573/1 (D.M.A.); the Swiss National Science Foundation Grant PP00P2_138979/1 (K.S.); the Center of Excellence in Astrophysics and Associated Technologies (PFB 06), by the FONDECYT regular grant 1120061 and by the CONICYT Anillo project ACT1101 (E.T.); the European Union's Seventh Framework Programme under grant agreements 337595 (ERC Starting Grant, \"CoSMass\") and 333654 (CIG, AGN feedback; V.S.). S.T. is part of The Dark Cosmology Centre, funded by the Danish National Research Foundation. B.T. is a Zwicky Fellow.\n\nPublished - apj_819_1_62.pdf
Submitted - 1601.00941v1.pdf
", "abstract": "The COSMOS-Legacy survey is a 4.6 Ms Chandra program that has imaged 2.2 deg2 of the COSMOS field with an effective exposure of \u2243 160 ks over the central 1.5 deg^2 and of \u2243 80 ks in the remaining area. The survey is the combination of 56 new observations obtained as an X-ray Visionary Project with the previous C-COSMOS survey. We describe the reduction and analysis of the new observations and the properties of 2273 point sources detected above a spurious probability of 2 \u00d7 10^(\u22125). We also present the updated properties of the C-COSMOS sources detected in the new data. The whole survey includes 4016 point sources (3814, 2920 and 2440 in the full, soft, and hard band). The limiting depths are 2.2 \u00d7 10^(\u221216), 1.5 \u00d7 10^(\u221215), and 8.9 \u00d7 10^(\u221216) erg cm^(-2)s^(-1) in the 0.5\u20132, 2\u201310, and 0.5\u201310 keV bands, respectively. The observed fraction of obscured active galactic nuclei with a column density >10^(22) cm^(\u22122) from the hardness ratio (HR) is 50_(-16)^(+17)%. Given the large sample we compute source number counts in the hard and soft bands, significantly reducing the uncertainties of 5%\u201310%. For the first time we compute number counts for obscured (HR > \u22120.2) and unobscured (HR < \u22120.2) sources and find significant differences between the two populations in the soft band. Due to the unprecedent large exposure, COSMOS-Legacy area is three times larger than surveys at similar depths and its depth is three times fainter than surveys covering similar areas. The area-flux region occupied by COSMOS-Legacy is likely to remain unsurpassed for years to come.", "date": "2016-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "819", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 62", "id_number": "CaltechAUTHORS:20160418-074725693", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160418-074725693", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO7-8136A" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Marie Curie Fellowship", "grant_number": "CIG 321913" }, { "agency": "UNAM-DGAPA", "grant_number": "PAPIIT IN104113" }, { "agency": "Consejo Nacional de Ciencia y Tecnologia (CONACyT)", "grant_number": "179662" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "Collaborative Research Council 956" }, { "agency": "NASA", "grant_number": "NAS8-03060" }, { "agency": "General Secretariat of Research and Technology (GSRT)" }, { "agency": "NASA", "grant_number": "NNX15AE61G" }, { "agency": "Science & Technology Facilities Council (STFC)", "grant_number": "ST/I001573/1" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "PP00P2_138979/1" }, { "agency": "Center of Excellence in Astrophysics and Associated Technologies", "grant_number": "PFB 06" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1120061" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "ACT1101" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "European Research Council (ERC)", "grant_number": "333654" }, { "agency": "Danish National Research Foundation" }, { "agency": "ETH Zurich" } ] }, "other_numbering_system": { "items": [ { "id": "2016-17", "name": "Space Radiation Laboratory" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "SPLASH" }, { "id": "Space-Radiation-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/0004-637X/819/1/62", "primary_object": { "basename": "apj_819_1_62.pdf", "url": "https://authors.library.caltech.edu/records/8w96h-04689/files/apj_819_1_62.pdf" }, "related_objects": [ { "basename": "1601.00941v1.pdf", "url": "https://authors.library.caltech.edu/records/8w96h-04689/files/1601.00941v1.pdf" } ], "pub_year": "2016", "author_list": "Civano, F.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/3d3e1-92766", "eprint_id": 78670, "eprint_status": "archive", "datestamp": "2023-08-20 10:47:49", "lastmod": "2023-10-26 00:17:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Parsa-S", "name": { "family": "Parsa", "given": "Shaghayegh" } }, { "id": "Dunlop-J-S", "name": { "family": "Dunlop", "given": "James S." } }, { "id": "McLure-R-J", "name": { "family": "McLure", "given": "Ross J." } }, { "id": "Mortlock-A", "name": { "family": "Mortlock", "given": "Alice" } } ] }, "title": "The galaxy UV luminosity function at z\u2243 2\u20134; new results on faint-end slope and the evolution of luminosity density", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 The Authors. Published for the Royal Astronomical Society by Oxford University Press.\n\nPublished - stv2857.pdf
", "abstract": "We present a new, robust measurement of the evolving rest-frame ultraviolet (UV) galaxy luminosity function (LF) over the key redshift range from z \u2243 2 to z \u2243 4. Our results are based on the high dynamic range provided by combining the Hubble Ultra Deep Field (HUDF), CANDELS/GOODS-South, and UltraVISTA/COSMOS surveys. We utilize the unparalleled multifrequency photometry available in this survey 'wedding cake' to compile complete galaxy samples at z \u2243 2, 3, 4 via photometric redshifts (calibrated against the latest spectroscopy) rather than colour\u2013colour selection, and to determine accurate rest-frame UV absolute magnitudes (M1500) from spectral energy distribution (SED) fitting. Our new determinations of the UV LF extend from M1500 \u2243 \u221222 (AB mag) down to M1500 = \u221214.5, \u221215.5 and \u221216 at z \u2243 2, 3 and 4, respectively (thus, reaching \u2243 3\u20134 mag fainter than previous blank-field studies at z \u2243 2,3). At z \u2243 2, 3, we find a much shallower faint-end slope (\u03b1 = \u22121.32 \u00b1 0.03) than reported in some previous studies (\u03b1 \u2243 \u22121.7), and demonstrate that this new measurement is robust. By z \u2243 4, the faint-end slope has steepened slightly, to \u03b1 = \u22121.43 \u00b1 0.04, and we show that these measurements are consistent with the overall evolutionary trend from z = 0 to 8. Finally, we find that while characteristic number density (\u03d5*) drops from z \u2243 2 to z \u2243 4, characteristic luminosity (M*) brightens by \u2243 1 mag. This, combined with the new flatter faint-end slopes, has the consequence that UV luminosity density (and hence unobscured star formation density) peaks at z \u2243 2.5\u20133, when the Universe was \u2243 2.5 Gyr old.", "date": "2016-03-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "456", "number": "3", "publisher": "Oxford University Press", "pagerange": "3194-3211", "id_number": "CaltechAUTHORS:20170628-143424767", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170628-143424767", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "SPLASH" }, { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stv2857", "primary_object": { "basename": "stv2857.pdf", "url": "https://authors.library.caltech.edu/records/3d3e1-92766/files/stv2857.pdf" }, "pub_year": "2016", "author_list": "Parsa, Shaghayegh; Dunlop, James S.; et el." }, { "id": "https://authors.library.caltech.edu/records/7n0ck-xn688", "eprint_id": 66486, "eprint_status": "archive", "datestamp": "2023-08-22 17:29:32", "lastmod": "2023-10-18 18:08:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Baronchelli-I", "name": { "family": "Baronchelli", "given": "I." }, "orcid": "0000-0003-0556-2929" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Mei-Simona", "name": { "family": "Mei", "given": "S." }, "orcid": "0000-0002-2849-559X" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H. I." }, "orcid": "0000-0002-7064-5424" }, { "id": "Colbert-J", "name": { "family": "Colbert", "given": "J." } }, { "id": "Kovacs-A", "name": { "family": "Kovacs", "given": "A." } }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Kirkpatrick-J-D", "name": { "family": "Kirkpatrick", "given": "J. D." }, "orcid": "0000-0003-4269-260X" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The Spitzer-IRAC/MIPS Extragalactic survey (SIMES) in the South Ecliptic Pole field", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: evolution; infrared: galaxies; submillimeter: galaxies; surveys", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 September 18; accepted 2016 January 2; published 2016 March 7.\n\nWe thank the referee for the useful comments that improved\nthe presentation of the paper. I.B. and G.R. acknowledge\nsupport from ASI (Herschel Science Contract 2011aI/005/\n011/0). C.S. and I.B. acknowledge support from NASA JPL/\nSpitzer grant RSA 1449911, provided for the SIMES project.\nS.M. acknowledges financial support from the Institut\nUniversitaire de France (IUF), of which she is senior member. M.V. acknowledges support from the European Commission Research Executive Agency (FP7-SPACE-2013-1 GA 607254) and the Italian Ministry for Foreign Affairs and International Cooperation (PGR GA ZA14GR02). This research has made use of data from the HerMES project (http://hermes.\nsussex.ac.uk/). HerMES is a Herschel Key Program using\nGuaranteed Time from the SPIRE instrument team, ESAC\nscientists, and a mission scientist. The HerMES data were\naccessed through the Herschel Database in Marseille (HeDaM\n\u2014http://hedam.lam.fr), operated by CeSAM and hosted by the\nLaboratoire d'Astrophysique de Marseille. This research has\nmade use of the NASA/IPAC Infrared Science Archive, which\nis operated by the Jet Propulsion Laboratory, California\nInstitute of Technology, under contract with the National\nAeronautics and Space Administration. M.V. acknowledges\nsupport from the European Commission Research Executive\nAgency (FP7-SPACE-2013-1 GA 607254) and the Italian\nMinistry for Foreign Affairs and International Cooperation\n(PGR GA ZA14GR02).\n\nPublished - apjs_223_1_1.pdf
Submitted - 1602.00892v1.pdf
", "abstract": "We present the Spitzer-IRAC/MIPS Extragalactic survey (SIMES) in the South Ecliptic Pole field. The large area covered (7.7 deg^2), together with one of the lowest Galactic cirrus emissions in the entire sky and a very extensive coverage by Spitzer, Herschel, Akari, and GALEX, make the SIMES field ideal for extragalactic studies. The elongated geometry of the SIMES area (\u22484:1), allowing for significant cosmic variance reduction, further improves the quality of statistical studies in this field. Here we present the reduction and photometric measurements of the Spitzer/IRAC data. The survey reaches depths of 1.93 and 1.75 \u03bcJy (1\u03c3) at 3.6 and 4.5 \u03bcm, respectively. We discuss the multiwavelength IRAC-based catalog, completed with optical, mid-, and far-IR observations. We detect 341,000 sources with F_(3.6\u00b5m) \u2a7e3\u03c3. Of these, 10% have an associated 24 \u03bcm counterpart, while 2.7% have an associated SPIRE source. We release the catalog through the NASA/IPAC Infrared Science Archive. Two scientific applications of these IRAC data are presented in this paper. First, we compute integral number counts at 3.6 \u03bcm. Second, we use the [3.6]\u2013[4.5] color index to identify galaxy clusters at z > 1.3. We select 27 clusters in the full area, a result consistent with previous studies at similar depth.", "date": "2016-03", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "223", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 1", "id_number": "CaltechAUTHORS:20160426-132926892", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160426-132926892", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "2011aI/005/ 011/0" }, { "agency": "Spitzer", "grant_number": "RSA 1449911" }, { "agency": "Institut Universitaire de France (IUF)" }, { "agency": "European Commission Research Executive Agency", "grant_number": "FP7-SPACE-2013-1 GA 607254" }, { "agency": "Ministry for Foreign Affairs and International Cooperation (Italy)", "grant_number": "PGR GA ZA14GR02" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/0067-0049/223/1/1", "primary_object": { "basename": "1602.00892v1.pdf", "url": "https://authors.library.caltech.edu/records/7n0ck-xn688/files/1602.00892v1.pdf" }, "related_objects": [ { "basename": "apjs_223_1_1.pdf", "url": "https://authors.library.caltech.edu/records/7n0ck-xn688/files/apjs_223_1_1.pdf" } ], "pub_year": "2016", "author_list": "Baronchelli, I.; Capak, P. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/vmbwv-x6t12", "eprint_id": 65055, "eprint_status": "archive", "datestamp": "2023-08-20 10:11:01", "lastmod": "2023-10-17 23:09:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lin-Lihwai", "name": { "family": "Lin", "given": "Lihwai" }, "orcid": "0000-0001-7218-7407" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "C." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Hsieh-Bau-Ching", "name": { "family": "Hsieh", "given": "Bau-Ching" }, "orcid": "0000-0001-5615-4904" }, { "id": "Jian-Hung-Yu", "name": { "family": "Jian", "given": "Hung-Yu" } }, { "id": "Lemaux-B-C", "name": { "family": "Lemaux", "given": "B. C." }, "orcid": "0000-0002-1428-7036" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Coupon-J", "name": { "family": "Coupon", "given": "Jean" } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The SPLASH Survey: Quiescent Galaxies Are More Strongly Clustered but Are Not Necessarily Located in High-density Environments", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: high-redshift \u2013 large-scale structure of universe", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 February 28; accepted 2015 November 2; published 2016 January 26. \n\nWe thank the anonymous referee for constructive suggestions that significantly improved the clarity of this paper. We also thank C.-C. Lai for useful discussions. The work is supported by the Ministry of Science and Technology (MoST) in Taiwan under the grant MOST 103-2112-M-001-031-MY3. C.L. is supported by the ILP LABEX (ANR-10-LABX-63 and ANR- 11-IDEX-0004-02). The UltraVISTA data are based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO program ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.\n\nPublished - Lin_2016p97.pdf
Submitted - 1511.03734v2.pdf
", "abstract": "We use the stellar-mass-selected catalog from the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH) in the COSMOS field to study the environments of galaxies via galaxy density and clustering analyses up to z ~ 2.5. The clustering strength of quiescent galaxies exceeds that of star-forming galaxies, implying that quiescent galaxies are preferentially located in more massive halos. When using local density measurement, we find a clear positive quiescent fraction\u2013density relation at z < 1, consistent with earlier results. However, the quiescent fraction\u2013density relation reverses its trend at intermediate redshifts (1 < z < 1.5) with marginal significance (<1.8\u03c3) and is found to be scale dependent (1.6\u03c3). The lower fraction of quiescent galaxies seen in large-scale dense environments, if confirmed to be true, may be associated with the fact that the star formation can be more easily sustained via cold stream accretion in \"large-scale\" high-density regions, preventing galaxies from permanent quenching. Finally, at z > 1.5, the quiescent fraction depends little on the local density, even though clustering shows that quiescent galaxies are in more massive halos. We argue that at high redshift the typical halo size falls below 10^(13)M\u2299, where intrinsically the local density measurements are so varied that they do not trace the halo mass. Our results thus suggest that in the high-redshift universe, halo mass may be the key in quenching the star formation in galaxies, rather than the conventionally measured galaxy density.", "date": "2016-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "817", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 97", "id_number": "CaltechAUTHORS:20160303-154315200", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160303-154315200", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "MOST 103-2112-M-001-031-MY3" }, { "agency": "Agence Nationale de la Recherche (ANR)", "grant_number": "ANR-10-LABX-63" }, { "agency": "Agence Nationale de la Recherche (ANR)", "grant_number": "ANR-11-IDEX-0004-02" }, { "agency": "agence" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "SPLASH" } ] }, "doi": "10.3847/0004-637X/817/2/97", "primary_object": { "basename": "1511.03734v2.pdf", "url": "https://authors.library.caltech.edu/records/vmbwv-x6t12/files/1511.03734v2.pdf" }, "related_objects": [ { "basename": "Lin_2016p97.pdf", "url": "https://authors.library.caltech.edu/records/vmbwv-x6t12/files/Lin_2016p97.pdf" } ], "pub_year": "2016", "author_list": "Lin, Lihwai; Capak, P. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/d8sgj-pxp72", "eprint_id": 78673, "eprint_status": "archive", "datestamp": "2023-08-20 09:58:09", "lastmod": "2023-10-26 00:17:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Marchesi-S", "name": { "family": "Marchesi", "given": "S." }, "orcid": "0000-0001-5544-0749" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Gilli-R", "name": { "family": "Gilli", "given": "R." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Lanzuisi-G", "name": { "family": "Lanzuisi", "given": "G." }, "orcid": "0000-0001-9094-0984" }, { "id": "Miyaji-Takamitsu", "name": { "family": "Miyaji", "given": "T." } }, { "id": "Treister-E", "name": { "family": "Treister", "given": "E." }, "orcid": "0000-0001-7568-6412" }, { "id": "Urry-C-M", "name": { "family": "Urry", "given": "C. M." }, "orcid": "0000-0002-0745-9792" }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "C." }, "orcid": "0000-0002-8853-9611" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Allevato-V", "name": { "family": "Allevato", "given": "V." } }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "N." } }, { "id": "Cardamone-C-N", "name": { "family": "Cardamone", "given": "C." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Griffiths-R-E", "name": { "family": "Griffiths", "given": "R. E." } }, { "id": "Kari-A", "name": { "family": "Karim", "given": "A." } }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "C." } }, { "id": "LaMassa-S-M", "name": { "family": "LaMassa", "given": "S. M." }, "orcid": "0000-0002-5907-3330" }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "K." }, "orcid": "0000-0003-3804-2137" }, { "id": "Ranalli-P", "name": { "family": "Ranalli", "given": "P." } }, { "id": "Schawinski-K", "name": { "family": "Schawinski", "given": "K." }, "orcid": "0000-0001-5464-0888" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Suh-Hyewon", "name": { "family": "Suh", "given": "H." }, "orcid": "0000-0002-2536-1633" }, { "id": "Trakhtenbrot-B", "name": { "family": "Trakhtenbrot", "given": "B." }, "orcid": "0000-0002-3683-7297" } ] }, "title": "The CHANDRA COSMOS Legacy Survey: Optical / IR Identifications", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2016 The American Astronomical Society.", "abstract": "We present the catalog of optical and infrared counterparts of the Chandra COSMOS-Legacy Survey, a 4.6 Ms Chandra program on the 2.2 deg2 of the COSMOS field, combination of 56 new overlapping observations obtained in Cycle 14 with the previous C-COSMOS survey. In this Paper we report the i, K, and 3.6 \u03bcm identifications of the 2273 X-ray point sources detected in the new Cycle 14 observations. We use the likelihood ratio technique to derive the association of optical/infrared (IR) counterparts for 97% of the X-ray sources. We also update the information for the 1743 sources detected in C-COSMOS, using new K and 3.6 \u03bcm information not available when the C-COSMOS analysis was performed. The final catalog contains 4016 X-ray sources, 97% of which have an optical/IR counterpart and a photometric redshift, while sime54% of the sources have a spectroscopic redshift. The full catalog, including spectroscopic and photometric redshifts and optical and X-ray properties described here in detail, is available online. We study several X-ray to optical (X/O) properties: with our large statistics we put better constraints on the X/O flux ratio locus, finding a shift toward faint optical magnitudes in both soft and hard X-ray band. We confirm the existence of a correlation between X/O and the the 2\u201310 keV luminosity for Type 2 sources. We extend to low luminosities the analysis of the correlation between the fraction of obscured AGNs and the hard band luminosity, finding a different behavior between the optically and X-ray classified obscured fraction.", "date": "2016-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "817", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art No 34", "id_number": "CaltechAUTHORS:20170628-144219700", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170628-144219700", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "SPLASH" }, { "id": "COSMOS" } ] }, "doi": "10.3847/0004-637X/817/1/34", "pub_year": "2016", "author_list": "Marchesi, S.; Civano, F.; et el." }, { "id": "https://authors.library.caltech.edu/records/gnpnv-nwa41", "eprint_id": 65337, "eprint_status": "archive", "datestamp": "2023-08-20 09:30:12", "lastmod": "2023-10-18 14:33:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Grazian-A", "name": { "family": "Grazian", "given": "A." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The Lyman continuum escape fraction of galaxies at z = 3.3 in the VUDS-LBC/COSMOS field", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2015 ESO. \n\nReceived 23 April 2015. Accepted 2 August 2015. Published online December 16 2015. \n\nWe thank the anonymous referee for her/his useful suggestions and comments that help us to improve this paper. We acknowledge financial contribution from the agreement ASI-INAF I/009/10/0. The LBT is an international collaboration among institutions in the United States, Italy, and Germany. LBT Corporation partners are The University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max-Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; The Ohio State University; and The Research Corporation, on behalf of The University of Notre Dame, University of Minnesota, and University of Virginia. This work is supported by funding from the European Research Council Advanced Grant ERC-2010-AdG-268107-EARLY and by INAF Grants PRIN 2010, PRIN 2012 and PICS 2013. A.C., O.C., M.T. and V.S. acknowledge the grant MIUR PRIN 2010\u20132011. D.M. gratefully acknowledges LAM hospitality during the initial phases of the project. This work is based on data products made available at the CESAM data center, Laboratoire d'Astrophysique de Marseille. This work partly uses observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on observations made with ESO Telescopes at the La Silla or Paranal Observatories under programme ID 175.A-0839. A.G. and E.V. warmly thank A. K. Inoue for providing the updated IGM transmission used in this paper. A.F. and J.S.D. acknowledge the contribution of the EC FP7 SPACE project ASTRODEEP (Ref. No: 312725).\n\nPublished - aa26396-15.pdf
Submitted - 1509.01101v1.pdf
", "abstract": "Context. The ionizing Lyman continuum flux escaping from high-redshift galaxies into the intergalactic medium is a fundamental quantity to understand the physical processes involved in the reionization epoch. However, from an observational point of view, direct detections of HI ionizing photons at high redshifts are feasible for galaxies mainly in the interval z ~ 3\u22124.\n\nAims. We have investigated a sample of star-forming galaxies at z ~ 3.3 to search for possible detections of Lyman continuum ionizing photons escaping from galaxy halos.\n\nMethods. We used deep ultraviolet (UV) imaging in the COSMOS field, obtained with the prime focus camera LBC at the LBT telescope, along with a catalogue of spectroscopic redshifts obtained by the VIMOS Ultra Deep Survey (VUDS) to build a sample of 45 galaxies at z ~ 3.3 with L > 0.5 L^\u2217. We obtained deep LBC images of galaxies with spectroscopic redshifts in the interval 3.27 < z < 3.40 both in the R- and deep U-bands (magnitude limit U ~ 29.7 at S/N = 1). At these redshifts, the R-band samples the non-ionizing 1500 \u00c5 rest-frame luminosity and the U-band samples the rest-frame spectral region just short-ward of the Lyman edge at 912 \u00c5. Their flux ratio is related to the ionizing escape fraction after statistical removal of the absorption by the intergalactic medium along the line of sight.\n\nResults. A subsample of ten galaxies apparently shows escape fractions >28%, but a detailed analysis of their properties reveals that, with the exception of two marginal detections (S/N ~ 2) in the U-band, all the other eight galaxies are most likely contaminated by the UV flux of low-redshift interlopers located close (in angular position) to the high-z targets. The average escape fraction derived from the stacking of the cleaned sample was constrained to f_(esc)^(rel) < 2%. The implied hydrogen photoionization rate is a factor two lower than that needed to keep the intergalactic medium ionized at z ~ 3, as observed in the Lyman-\u03b1 forest of high-z quasar spectra or by the proximity effect.\n\nConclusions. These results support a scenario where high redshift, relatively bright (L \u2265 0.5L^\u2217) star-forming galaxies alone are unable to sustain the level of ionization observed in the cosmic intergalactic medium at z ~ 3. Star-forming galaxies at higher redshift and at fainter luminosities (L \u226a L^\u2217) can only be major contributors to the reionization of the Universe if their physical properties are subject to rapid changes from z ~ 3 to z ~ 6\u201310. Alternatively, ionizing sources could be discovered looking for fainter sources among the active galactic nuclei population at high redshift.", "date": "2015-12-16", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "585", "publisher": "EDP Sciences", "pagerange": "Art. No. A48", "id_number": "CaltechAUTHORS:20160314-122019767", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160314-122019767", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/009/10/0" }, { "agency": "European Research Council (ERC)", "grant_number": "ERC-2010-AdG-268107-EARLY" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2010" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2012" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PICS 2013" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)", "grant_number": "PRIN 2010\u20132011" }, { "agency": "European Research Council (ERC)", "grant_number": "312725 ASTRODEEP" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201526396", "primary_object": { "basename": "1509.01101v1.pdf", "url": "https://authors.library.caltech.edu/records/gnpnv-nwa41/files/1509.01101v1.pdf" }, "related_objects": [ { "basename": "aa26396-15.pdf", "url": "https://authors.library.caltech.edu/records/gnpnv-nwa41/files/aa26396-15.pdf" } ], "pub_year": "2015", "author_list": "Grazian, A.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/bswe6-e1m70", "eprint_id": 63732, "eprint_status": "archive", "datestamp": "2023-08-20 09:16:13", "lastmod": "2023-10-17 15:30:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Carniani-S", "name": { "family": "Carniani", "given": "S." } }, { "id": "Maiolino-R", "name": { "family": "Maiolino", "given": "R." } }, { "id": "De-Zotti-G", "name": { "family": "De Zotti", "given": "G." }, "orcid": "0000-0003-2868-2595" }, { "id": "Negrello-M", "name": { "family": "Negrello", "given": "M." } }, { "id": "Marconi-A", "name": { "family": "Marconi", "given": "A." } }, { "id": "Bothwell-M-S", "name": { "family": "Bothwell", "given": "M. S." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Castellano-M", "name": { "family": "Castellano", "given": "M." } }, { "id": "Cristiani-S", "name": { "family": "Cristiani", "given": "S." } }, { "id": "Ferrara-A", "name": { "family": "Ferrara", "given": "A." }, "orcid": "0000-0002-9400-7312" }, { "id": "Fontana-A", "name": { "family": "Fontana", "given": "A." } }, { "id": "Gallerani-S", "name": { "family": "Gallerani", "given": "S." } }, { "id": "Jones-G", "name": { "family": "Jones", "given": "G." } }, { "id": "Ohta-K", "name": { "family": "Ohta", "given": "K." } }, { "id": "Ota-K", "name": { "family": "Ota", "given": "K." } }, { "id": "Pentericci-L", "name": { "family": "Pentericci", "given": "L." } }, { "id": "Santini-P", "name": { "family": "Santini", "given": "P." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Vallini-L", "name": { "family": "Vallini", "given": "L." }, "orcid": "0000-0002-3258-3672" }, { "id": "Vanzella-E", "name": { "family": "Vanzella", "given": "E." } }, { "id": "Wagg-J", "name": { "family": "Wagg", "given": "J." } }, { "id": "Williams-R-J", "name": { "family": "Williams", "given": "R. J." } } ] }, "title": "ALMA constraints on the faint millimetre source number counts and their contribution to the cosmic infrared background", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: high-redshift \u2013 galaxies: formation", "note": "\u00a9 ESO, 2015. \n\nReceived 1 February 2015 / Accepted 2 September 2015. \n\nWe thank the anonymous referee for comments and suggestions that improved the paper. We thank Paola Andreani, Matthew Auger and Valentina Calvi for comments and discussions. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.1.00115.S, ADS/JAO.ALMA#2011.1.00243.S, ADS/JAO.ALMA#2011.1.00767.S, ADS/JAO.ALMA#2012.1.00142.S, ADS/JAO.ALMA#2012.1.00374.S, ADS/JAO.ALMA#2012.1.00523.S, ADS/JAO.ALMA#2012.1.00719.S and ADS/JAO.ALMA#2012.A.00040.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. G.D.Z. and M.N. acknowledge financial support from ASI/INAF Agreement 2014-024-R.0 for the Planck LFI activity of Phase E2.\n\nPublished - aa25780-15.pdf
", "abstract": "We have analysed 18 ALMA continuum maps in Bands 6 and 7, with rms down to 7.8 \u03bcJy, to derive differential number counts down to 60 \u03bcJy and 100 \u03bcJy at \u03bb = 1.3 mm and \u03bb = 1.1 mm, respectively. Furthermore, the non-detection of faint sources in the deepest ALMA field enabled us to set tight upper limits on the number counts down to 30 \u03bcJy. This is a factor of four deeper than the currently most stringent upper limit. The area covered by the combined fields is 9.5 \u00d7 10^(-4) deg^2 at 1.1 mm and 6.6 \u00d7 10^(-4) deg^2 at 1.3 mm. With respect to previous works, we improved the source extraction method by requiring that the dimension of the detected sources be consistent with the beam size. This method enabled us to remove spurious detections that have plagued the purity of the catalogues in previous studies. We detected 50 faint sources (at fluxes <1 mJy) with signal-to-noise (S/N) >3.5 down to 60 \u03bcJy, hence improving the statistics by a factor of four relative to previous studies. The inferred differential number counts are dN/ d(Log_(10)S) = 1 \u00d7 10^5 deg^2 at a 1.1 mm flux S_\u03bb = 1.1 mm = 130 \u03bcJy, and dN/ d(Log_(10)S) = 1.1 \u00d7 10^5 deg^2 at a 1.3 mm flux S_\u03bb = 1.3 mm = 60 \u03bcJy. At the faintest flux limits probed by our data, i.e. 30 \u03bcJy and 40 \u03bcJy, we obtain upper limits on the differential number counts of dN/ d(Log_(10)S) < 7 \u00d7 10^5 deg^2 and dN/ d(Log_(10)S) < 3 \u00d7 10^5 deg^2, respectively. Determining the fraction of cosmic infrared background (CIB) resolved by the ALMA observations was hampered by the large uncertainties plaguing the CIB measurements (a factor of four in flux). However, our results provide a new lower limit to CIB intensity of 17.2 Jy\u2009deg^(-2) at 1.1 mm and of 12.9 Jy deg^(-2) at 1.3 mm. Moreover, the flattening of the integrated number counts at faint fluxes strongly suggests that we are probably close to the CIB intensity. Our data imply that galaxies with star formation rate (SFR) < 40 M_\u2299/yr certainly contribute less than 50% to the CIB (and probably a much lower percentage) while more than 50% of the CIB must be produced by galaxies with SFR> 40 M_\u2299/yr. The differential number counts are in nice agreement with recent semi-analytical models of galaxy formation even as low as our faint fluxes. Consequently, this supports the galaxy evolutionary scenarios and assumptions made in these models.", "date": "2015-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "584", "publisher": "EDP Sciences", "pagerange": "Art. No. A78", "id_number": "CaltechAUTHORS:20160115-165135620", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160115-165135620", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "2014-024-R.0" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201525780", "primary_object": { "basename": "aa25780-15.pdf", "url": "https://authors.library.caltech.edu/records/bswe6-e1m70/files/aa25780-15.pdf" }, "pub_year": "2015", "author_list": "Carniani, S.; Maiolino, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/xtsfp-1t480", "eprint_id": 63722, "eprint_status": "archive", "datestamp": "2023-08-20 09:15:51", "lastmod": "2023-10-17 15:29:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Yoshiaki" }, "orcid": "0000-0003-2247-3741" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The Subaru COSMOS 20: Subaru optical imaging of the HST COSMOS field with 20 filters", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2015 The Author. Published by Oxford University Press on behalf of the Astronomical Society of Japan. \n\nReceived January 30, 2015. Accepted October 2, 2015. Advance Access Publication Date: 2015 November 10. \n\nThe HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at \u3008http://www.astro.caltech.edu/\u223ccosmos\u3009. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS datasets. We are deeply grateful to the referee for his/her useful comments and excellent refereeing, which helped us to improve this paper very much. We would also like to thank the staff at the Subaru Telescope for their invaluable help. In particular, we would like to thank Hisanori Furusawa because his professional help as a support scientist made our Suprime-Cam observations successful. Data analysis was in part carried out on the common use data analysis computer system at the Astronomy Data Center, ADC, of the National Astronomical Observatory of Japan. This work was financially supported in part by JSPS (YT: 15340059, 17253001, 19340046, 23244031; TN: 23654068 and 25707010) and by the Yamada Science Foundation (TN).\n\nSubmitted - 1510.00550v1.pdf
", "abstract": "We present both the observations and the data reduction procedures of the Subaru COSMOS 20 project, an optical imaging survey of the HST COSMOS field, carried out by using Suprime-Cam on the Subaru Telescope with the following 20 optical filters: six broad-band (B, g\u2032, V, r\u2032, i\u2032, and z\u2032), two narrow-band (NB711 and NB816), and 12 intermediate-band filters (IA427, IA464, IA484, IA505, IA527, IA574, IA624, IA679, IA709, IA738, IA767, and IA827). Part of this project is described in Taniguchi et al. (2007, ApJS, 172, 9) and Capak et al. (2007, ApJS, 172, 99) for the six broad-band and one narrow-band (NB816) filter data. In this paper, we present details of the observations and data reduction for the remaining 13 filters (the 12 IA filters and NB711). In particular, we describe the accuracy of both the photometry and astrometry in all the filter bands. We also present the optical properties of the Suprime-Cam IA filter system in appendices.", "date": "2015-12", "date_type": "published", "publication": "Publications of the Astronomical Society of Japan", "volume": "67", "number": "6", "publisher": "Astronomical Society of Japan", "pagerange": "Art. No. 104", "id_number": "CaltechAUTHORS:20160115-144520331", "issn": "0004-6264", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160115-144520331", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15340059" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17253001" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19340046" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23244031" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23244031" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "25707010" }, { "agency": "Yamada Science Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/pasj/psv106", "primary_object": { "basename": "1510.00550v1.pdf", "url": "https://authors.library.caltech.edu/records/xtsfp-1t480/files/1510.00550v1.pdf" }, "pub_year": "2015", "author_list": "Taniguchi, Yoshiaki; Capak, Peter L.; et el." }, { "id": "https://authors.library.caltech.edu/records/xtjyd-zkh02", "eprint_id": 63729, "eprint_status": "archive", "datestamp": "2023-08-20 09:16:04", "lastmod": "2023-10-17 15:30:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Miettinen-O", "name": { "family": "Miettinen", "given": "O." } }, { "id": "Novak-Mladen", "name": { "family": "Novak", "given": "M." }, "orcid": "0000-0001-8695-825X" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Sargent-M", "name": { "family": "Sargent", "given": "M." }, "orcid": "0000-0003-1033-9684" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" }, { "id": "Bondi-M", "name": { "family": "Bondi", "given": "M." } }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } } ] }, "title": "(Sub)millimetre interferometric imaging of a sample of COSMOS/AzTEC submillimetre galaxies. II. The spatial extent of the radio-emitting regions", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: formation \u2013 galaxies: starburst \u2013 galaxies: star formation \u2013 radio continuum: galaxies \u2013 submillimeter: galaxies", "note": "\u00a9 ESO, 2015. \n\nReceived 23 May 2015 / Accepted 22 September 2015. \n\nWe thank the referee for constructive comments that helped to improve this paper. This research was funded by the European Union's Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). M.A. acknowledges partial support from FONDECYT through grant 1140099. A.K. acknowledges support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2012.1.00978.S and ADS/JAO.ALMA#2013.1.00118.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This research has made use of NASA's Astrophysics Data System, and the NASA/IPAC Infrared Science Archive, which is operated by the JPL, California Institute of Technology, under contract with the NASA. We greatfully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/~cosmos\n\nPublished - aa26589-15.pdf
", "abstract": "Radio emission at centimetre wavelengths from highly star-forming galaxies, like submillimetre galaxies (SMGs), is dominated by synchrotron radiation arising from supernova activity. Hence, radio continuum imaging has the potential to determine the spatial extent of star formation in these types of galaxies. Using deep, high-resolution (1\u03c3 = 2.3 \u03bcJy beam^(-1); 0\".75 75) centimetre radio-continuum observations taken by the Karl G. Jansky Very Large Array (VLA)-COSMOS 3 GHz Large Project, we studied the radio-emitting sizes of a flux-limited sample of SMGs in the COSMOS field. The target SMGs were originally discovered in a 1.1 mm continuum survey carried out with the AzTEC bolometer, and followed up with higher resolution interferometric (sub)millimetre continuum observations. Of the 39 SMGs studied here, 3 GHz emission was detected towards 18 of them (~46 \u00b1 11%) with signal-to-noise ratios in the range of S/N = 4.2\u201337.4. Towards four SMGs (AzTEC2, 5, 8, and 11), we detected two separate 3 GHz sources with projected separations of ~1''\u03235\u20136''\u03236, but they might be physically related in only one or two cases (AzTEC2 and 11). Using two-dimensional elliptical Gaussian fits, we derived a median deconvolved major axis FWHM size of 0''\u032354\u00b10''\u032311 for our 18 SMGs detected at 3 GHz. For the 15 SMGs with known redshift we derived a median linear major axis FWHM of 4.2 \u00b1 0.9 kpc. No clear correlation was found between the radio-emitting size and the 3 GHz or submm flux density, or the redshift of the SMG. However, there is a hint of larger radio sizes at z ~ 2.5\u20135 compared to lower redshifts. The sizes we derived are consistent with previous SMG sizes measured at 1.4 GHz and in mid-J CO emission, but significantly larger than those seen in the (sub)mm continuum emission (typically probing the rest-frame far-infrared with median FWHM sizes of only ~1.5\u20132.5 kpc). One possible scenario is that SMGs have i) an extended gas component with a low dust temperature, which can be traced by low- to mid-J CO line emission and radio continuum emission; and ii) a warmer, compact starburst region giving rise to the high-excitation line emission of CO, which could dominate the dust continuum size measurements. Because of the rapid cooling of cosmic-ray electrons in dense starburst galaxies (~10^4\u201310^5 yr), the more extended synchrotron radio-emitting size being a result of cosmic-ray diffusion seems unlikely. Instead, if SMGs are driven by galaxy mergers \u2013 a process where the galactic magnetic fields can be pulled out to larger spatial scales \u2013 the radio synchrotron emission might arise from more extended magnetised interstellar medium around the starburst region.", "date": "2015-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "584", "publisher": "EDP Sciences", "pagerange": "Art. No. A32", "id_number": "CaltechAUTHORS:20160115-162134996", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160115-162134996", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "CoSMass 337595" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1140099" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "Collaborative Research Council 956" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201526589", "primary_object": { "basename": "aa26589-15.pdf", "url": "https://authors.library.caltech.edu/records/xtjyd-zkh02/files/aa26589-15.pdf" }, "pub_year": "2015", "author_list": "Miettinen, O.; Novak, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/mcf5q-sea44", "eprint_id": 58879, "eprint_status": "archive", "datestamp": "2023-08-20 08:04:36", "lastmod": "2023-10-23 19:50:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K. I." }, "orcid": "0000-0001-8183-1460" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Fynbo-J-P-U", "name": { "family": "Fynbo", "given": "J." }, "orcid": "0000-0002-8149-8298" }, { "id": "Milvang-Jensen-B", "name": { "family": "Milvang-Jensen", "given": "B." }, "orcid": "0000-0002-2281-2785" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" } ] }, "title": "Spitzer bright, UltraVISTA faint sources in COSMOS: the contribution to the overall population of massive galaxies at z = 3-7", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: galaxies - galaxies: high-redshift - galaxies: evolution", "note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2015 May 18; accepted 2015 July 27; published 2015 September 1.\n\nBased on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO program ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations carried out with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA; the NASA/ESA Hubble Space Telescope, obtained and archived at the Space Telescope Science Institute; and the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. O.I. acknowledges funding from the French Agence Nationale de la Recherche (ANR) for the project SAGACE. B.M.-J. and J.F. acknowledge support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the DNRF. We thank Kenneth Duncan, Yu Lu, and Paola Santini for providing us data in electronic format; Rebecca Bowler for performing photometric tests; and Yu Lu for useful discussions. We also thank an anonymous referee for a constructive report.\n\nPublished - Caputi_2015.pdf
Submitted - 1505.05721v1.pdf
", "abstract": "We have analysed a sample of 574 Spitzer 4.5 \u03bcm-selected galaxies with [4.5] < 23 and K_s^(auto) > 24 (AB) over the UltraVISTA ultra-deep COSMOS field. Our aim is to investigate whether these mid-IR bright, near-IR faint sources contribute significantly to the overall population of massive galaxies at redshifts z \u2265 3. By performing a spectral energy distribution (SED) analysis using up to 30 photometric bands, we have determined that the redshift distribution of our sample peaks at redshifts z \u2248 2.5 \u2212 3.0, and ~ 32% of the galaxies lie at z \u2265 3. We have studied the contribution of these sources to the galaxy stellar mass function (GSMF) at high redshifts. We found that the [4.5] < 23, K_s^(auto) > 24 galaxies produce a negligible change to the GSMF previously determined for K_s^(auto) < 24 sources at 3 \u2264 z < 4, but their contribution is more important at 4 \u2264 z < 5, accounting for > \u2273 50% of the galaxies with stellar masses M_(st) \u2273 6 \u00d7 10^(10)M\u2299. We also constrained the GSMF at the highest-mass end (M_(st) \u2273 2 \u00d7 10^(11)M\u2299) at z \u2265 5. From their presence at 5 \u2264 z < 6, and virtual absence at higher redshifts, we can pinpoint quite precisely the moment of appearance of the first most massive galaxies as taking place in the ~ 0.2Gyr of elapsed time between z ~ 6 and z ~ 5. Alternatively, if very massive galaxies existed earlier in cosmic time, they should have been significantly dust-obscured to lie beyond the detection limits of current, large-area, deep near-IR surveys.", "date": "2015-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "810", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 73", "id_number": "CaltechAUTHORS:20150714-110504040", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150714-110504040", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agence Nationale pour la Recherche (ANR)" }, { "agency": "European Research Council (ERC)", "grant_number": "278202" }, { "agency": "Danish National Research Foundation" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/810/1/73", "primary_object": { "basename": "1505.05721v1.pdf", "url": "https://authors.library.caltech.edu/records/mcf5q-sea44/files/1505.05721v1.pdf" }, "related_objects": [ { "basename": "Caputi_2015.pdf", "url": "https://authors.library.caltech.edu/records/mcf5q-sea44/files/Caputi_2015.pdf" } ], "pub_year": "2015", "author_list": "Caputi, K. I.; Ilbert, O.; et el." }, { "id": "https://authors.library.caltech.edu/records/qdgwp-12v12", "eprint_id": 60728, "eprint_status": "archive", "datestamp": "2023-08-22 16:18:23", "lastmod": "2023-10-24 21:08:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Riguccini-L", "name": { "family": "Riguccini", "given": "L." } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Mullaney-J-R", "name": { "family": "Mullaney", "given": "J. R." }, "orcid": "0000-0002-3126-6712" }, { "id": "Men\u00e9ndez-Delmestre-K", "name": { "family": "Men\u00e9ndez-Delmestre", "given": "K." }, "orcid": "0000-0003-3153-5123" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Berta-S", "name": { "family": "Berta", "given": "S." }, "orcid": "0000-0002-0320-1532" }, { "id": "Calanog-J-A", "name": { "family": "Calanog", "given": "J." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Magnelli-B", "name": { "family": "Magnelli", "given": "B." }, "orcid": "0000-0002-6777-6490" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S." }, "orcid": "0000-0001-7862-1032" }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Treister-E", "name": { "family": "Treister", "given": "E." }, "orcid": "0000-0001-7568-6412" } ] }, "title": "The composite nature of Dust-Obscured Galaxies (DOGs) at z \u223c 2\u20133 in the COSMOS field \u2013 I. A far-infrared view", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; cosmology: observations; infrared: galaxies", "note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 June 8. Received 2015 May 15. In original form 2014 September 23. First published online July 3, 2015. \n\nCOSMOS is based on observations with the NASA/ESA HST, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555; also based on data collected at: the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities,Inc; and the Canada\u2013France\u2013Hawaii Telescope, operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France, and the University of Hawaii. \n\nPACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). \n\nSPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada), NAOC (China), CEA, LAM (France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK), Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).\n\nPublished - MNRAS-2015-Riguccini-470-85.pdf
", "abstract": "Dust-Obscured Galaxies (DOGs) are bright 24\u2009\u03bcm-selected sources with extreme obscuration at optical wavelengths. They are typically characterized by a rising power-law continuum of hot dust (T_D \u223c 200\u20131000 K) in the near-IR indicating that their mid-IR luminosity is dominated by an active galactic nucleus (AGN). DOGs with a fainter 24\u2009\u03bcm flux display a stellar bump in the near-IR and their mid-IR luminosity appears to be mainly powered by dusty star formation. Alternatively, it may be that the mid-IR emission arising from AGN activity is dominant but the torus is sufficiently opaque to make the near-IR emission from the AGN negligible with respect to the emission from the host component. In an effort to characterize the astrophysical nature of the processes responsible for the IR emission in DOGs, this paper exploits Herschel data (PACS + SPIRE) on a sample of 95 DOGs within the COSMOS field. We derive a wealth of far-IR properties (e.g. total IR luminosities; mid-to-far-IR colours; dust temperatures and masses) based on spectral energy distribution fitting. Of particular interest are the 24\u2009\u03bcm-bright DOGs (F_(24)\u2009\u03bcm > 1 mJy). They present bluer far-IR/mid-IR colours than the rest of the sample, unveiling the potential presence of an AGN. The AGN contribution to the total 8\u20131000\u2009\u03bcm flux increases as a function of the rest-frame 8\u2009\u03bcm-luminosity irrespective of the redshift. This confirms that faint DOGs (L_8\u2009\u03bcm < 10^(12) L_\u2299) are dominated by star formation while brighter DOGs show a larger contribution from an AGN.", "date": "2015-09-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "452", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "470-485", "id_number": "CaltechAUTHORS:20151002-142311846", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151002-142311846", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Association of Universities for Research in Astronomy (AURA)" }, { "agency": "NSF" }, { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" }, { "agency": "Ministry of Science and Technology (MCyT)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stv1297", "primary_object": { "basename": "MNRAS-2015-Riguccini-470-85.pdf", "url": "https://authors.library.caltech.edu/records/qdgwp-12v12/files/MNRAS-2015-Riguccini-470-85.pdf" }, "pub_year": "2015", "author_list": "Riguccini, L.; Le Floc'h, E.; et el." }, { "id": "https://authors.library.caltech.edu/records/aws27-pjf86", "eprint_id": 62518, "eprint_status": "archive", "datestamp": "2023-08-20 08:01:21", "lastmod": "2023-10-25 17:13:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The FMOS-COSMOS Survey of Star-forming Galaxies at z ~ 1.6. III. Survey Design, Performance, and Sample Characteristics", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: general \u2013 galaxies: high-redshift \u2013 galaxies: ISM \u2013 surveys \u2013 techniques: spectroscopic", "note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2014 September 8; accepted 2015 July 29; published 2015 September 11.\n\nJ.D.S. is supported by JSPS KAKENHI grant Number 26400221 and the World Premier International Research Center Initiative (WPI), MEXT, Japan. D.K. receives support through the Grant-in-Aid for JSPS Fellows (No. 26-3216). A.R. acknowledges support by a grant PRIN-INAF 2012. \n\nFacility: Subaru(FMOS).\n\nPublished - Silverman_2015p12.pdf
Submitted - 1409.0447v2.pdf
", "abstract": "We present a spectroscopic survey of galaxies in the COSMOS field using the Fiber Multi-object Spectrograph (FMOS), a near-infrared instrument on the Subaru Telescope. Our survey is specifically designed to detect the H\u03b1 emission line that falls within the H-band (1.6\u20131.8 \u03bcm) spectroscopic window from star-forming galaxies with 1.4 < z < 1.7 and M_(stellar) \u2273 10^(10) M\u2299. With the high multiplex capability of FMOS, it is now feasible to construct samples of over 1000 galaxies having spectroscopic redshifts at epochs that were previously challenging. The high-resolution mode (R ~ 2600) effectively separates H\u03b1 and [N ii]\u03bb6585, thus enabling studies of the gas-phase metallicity and photoionization state of the interstellar medium. The primary aim of our program is to establish how star formation depends on stellar mass and environment, both recognized as drivers of galaxy evolution at lower redshifts. In addition to the main galaxy sample, our target selection places priority on those detected in the far-infrared by Herschel/PACS to assess the level of obscured star formation and investigate, in detail, outliers from the star formation rate (SFR)\u2014stellar mass relation. Galaxies with H\u03b1 detections are followed up with FMOS observations at shorter wavelengths using the J-long (1.11\u20131.35 \u03bcm) grating to detect H\u03b2 and [O iii]\u03bb5008 which provides an assessment of the extinction required to measure SFRs not hampered by dust, and an indication of embedded active galactic nuclei. With 460 redshifts measured from 1153 spectra, we assess the performance of the instrument with respect to achieving our goals, discuss inherent biases in the sample, and detail the emission-line properties. Our higher-level data products, including catalogs and spectra, are available to the community.", "date": "2015-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "220", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 12", "id_number": "CaltechAUTHORS:20151201-150113650", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151201-150113650", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "26400221" }, { "agency": "World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "26-3216" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0067-0049/220/1/12", "primary_object": { "basename": "1409.0447v2.pdf", "url": "https://authors.library.caltech.edu/records/aws27-pjf86/files/1409.0447v2.pdf" }, "related_objects": [ { "basename": "Silverman_2015p12.pdf", "url": "https://authors.library.caltech.edu/records/aws27-pjf86/files/Silverman_2015p12.pdf" } ], "pub_year": "2015", "author_list": "Silverman, J. D.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/e2zgm-4n810", "eprint_id": 61790, "eprint_status": "archive", "datestamp": "2023-08-20 08:00:37", "lastmod": "2023-10-25 15:44:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L. A. M." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The evolving star formation rate: M\u22c6 relation and sSFR since z \u2243 5 from the VUDS spectroscopic survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: star formation \u2013 galaxies: formation \u2013 galaxies: high-redshift", "note": "\u00a9 2015 ESO. Article published by EDP Sciences. \n\nReceived 20 November 2014; Accepted 20 June 2015; Published online 01 September 2015. \n\nBased on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Program 185.A\u22120791. \n\nWe thank the ESO staff for their continuous support for the VUDS survey, particularly the Paranal staff conducting the observations and Marina Rejkuba and the ESO user support group in Garching. This work is supported by funding from the European Research Council Advanced Grant ERC-2010-AdG-268107-EARLY and by INAF Grants PRIN 2010, PRIN 2012 and PICS 2013. A.C., O.C., M.T. and V.S. acknowledge the grant MIUR PRIN 2010\u20132011. This work is based on data products made available at the CESAM data center, Laboratoire d'Astrophysique de Marseille. This work partly uses observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS.\n\nPublished - aa25379-14.pdf
Submitted - 1411.5687v1.pdf
", "abstract": "We study the evolution of the star formation rate (SFR) \u2013 stellar mass (M\u22c6) relation and specific star formation rate (sSFR) of star-forming galaxies (SFGs) since a redshift z \u2243 5.5 using 2435 (4531) galaxies with highly reliable spectroscopic redshifts in the VIMOS Ultra-Deep Survey (VUDS). It is the first time that these relations can be followed over such a large redshift range from a single homogeneously selected sample of galaxies with spectroscopic redshifts. The log\u2009(SFR) \u2212 log\u2009(M\u22c6) relation for SFGs remains roughly linear all the way up to z = 5, but the SFR steadily increases at fixed mass with increasing redshift. We find that for stellar masses M\u22c6 \u2265 3.2 \u00d7 10^9M\u2299 the SFR increases by a factor of ~13 between z = 0.4 and z = 2.3. Weextend this relation up to z = 5, finding an additional increase in SFR by a factor of 1.7 from z = 2.3 to z = 4.8 for masses M\u22c6 \u2265 10^(10)M\u2299. We observe a turn-off in the SFR\u2013M\u22c6 relation at the highest mass end up to a redshift z ~ 3.5. We interpret this turn-off as the signature of a strong on-going quenching mechanism and rapid mass growth. The sSFR increases strongly up to z ~ 2, but it grows much less rapidly in 2", "date": "2015-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "581", "publisher": "EDP Sciences", "pagerange": "Art. No. A54", "id_number": "CaltechAUTHORS:20151103-090349586", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151103-090349586", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "ERC-2010-AdG-268107-EARLY" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2010" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2012" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PICS 2013" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)", "grant_number": "PRIN 2010-2011" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201425379", "primary_object": { "basename": "aa25379-14.pdf", "url": "https://authors.library.caltech.edu/records/e2zgm-4n810/files/aa25379-14.pdf" }, "related_objects": [ { "basename": "1411.5687v1.pdf", "url": "https://authors.library.caltech.edu/records/e2zgm-4n810/files/1411.5687v1.pdf" } ], "pub_year": "2015", "author_list": "Tasca, L. A. M.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/nqy0y-ps267", "eprint_id": 61290, "eprint_status": "archive", "datestamp": "2023-08-20 07:50:21", "lastmod": "2023-10-25 14:42:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ikeda-Hideyuki", "name": { "family": "Ikeda", "given": "H." } }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "T." }, "orcid": "0000-0002-7402-5441" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Matsuoka-Kenta", "name": { "family": "Matsuoka", "given": "K." }, "orcid": "0000-0002-2689-4634" }, { "id": "Kajisawa-Masaru", "name": { "family": "Kajisawa", "given": "M." }, "orcid": "0000-0002-1732-6387" }, { "id": "Akiyama-Masayuki", "name": { "family": "Akiyama", "given": "M." } }, { "id": "Miyaji-Takamitsu", "name": { "family": "Miyaji", "given": "T." } }, { "id": "Kashikawa-Nobunari", "name": { "family": "Kashikawa", "given": "N." } }, { "id": "Morokuma-Tomoki", "name": { "family": "Morokuma", "given": "T." } }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Enoki-Motohiro", "name": { "family": "Enoki", "given": "M." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "D." }, "orcid": "0000-0001-5382-6138" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The Quasar-LBG Two-point Angular Cross-correlation Function at z~4 in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active \u2013 large-scale structure of universe \u2013 quasars: general", "note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2014 August 21; accepted 2015 July 13; published 2015 August 18.\n\nWe would like to thank the Subaru staff for their invaluable help and all members of the COSMOS team. We thank Philip Hopkins for providing the data of the predicted bias factor, which are calculated by his models. We also thank the referee for useful suggestions and comments that helped us to improve this paper. This work was financially supported in part by the Japan Society for the Promotion of Science (JSPS; grant Nos. 23244031 and 25707010), and also by the Yamada Science Foundation. T.M. is supported by UNAM-DGAPA grant PAPIIT IN104113 and CONACyT Grant Cient\u00edfica B\u00e1sica 179662. H.I. and K.M. are financially supported by the JSPS through the JSPS Research Fellowship.\n\nPublished - Ikeda_2015.pdf
Submitted - 1507.05292v2.pdf
", "abstract": "In order to investigate the origin of quasars, we estimate the bias factor for low-luminosity quasars at high redshift for the first time. In this study, we use the two-point angular cross-correlation function (CCF) for both low-luminosity quasars at -24 < M_(1450) < -22 and Lyman-break galaxies (LBGs). Our sample consists of both 25 low-luminosity quasars (16 objects are spectroscopically confirmed low-luminosity quasars) in the redshift range 3.1 < z < 4.5 and 835 color-selected LBGs with z'_(LBG) < 25.0 at z ~ 4 in the COSMOS field. We have performed our analysis for the following two quasar samples: (1) the spectroscopic sample (the 16 quasars confirmed by spectroscopy), and (2) the total sample (the 25 quasars including 9 quasars with photometric redshifts). The bias factor for low-luminosity quasars at z ~ 4 is derived by utilizing the quasar-LBG CCF and the LBG auto-correlation function. We then obtain the 86% upper limits of the bias factors for low-luminosity quasars, which are 5.63 and 10.50 for the total and the spectroscopic samples, respectively. These bias factors correspond to the typical dark matter halo masses, log (M_(DM)/(h^(-1)M\u2299)) = 12.7 and 13.5, respectively. This result is not inconsistent with the predicted bias for quasars that is estimated by the major merger models.", "date": "2015-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "809", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 138", "id_number": "CaltechAUTHORS:20151019-152143500", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151019-152143500", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23244031" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "25707010" }, { "agency": "Yamada Science Foundation" }, { "agency": "UNAM-DGAPA", "grant_number": "PAPIIT IN104113" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "179662" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/809/2/138", "primary_object": { "basename": "1507.05292v2.pdf", "url": "https://authors.library.caltech.edu/records/nqy0y-ps267/files/1507.05292v2.pdf" }, "related_objects": [ { "basename": "Ikeda_2015.pdf", "url": "https://authors.library.caltech.edu/records/nqy0y-ps267/files/Ikeda_2015.pdf" } ], "pub_year": "2015", "author_list": "Ikeda, H.; Nagao, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/zv4bs-jzt56", "eprint_id": 60057, "eprint_status": "archive", "datestamp": "2023-08-22 16:10:04", "lastmod": "2023-10-24 14:51:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Yoshiaki" }, "orcid": "0000-0003-2247-3741" }, { "id": "Kajisawa-Masaru", "name": { "family": "Kajisawa", "given": "Masaru" }, "orcid": "0000-0002-1732-6387" }, { "id": "Kobayashi-Masakazu-A-R", "name": { "family": "Kobayashi", "given": "Masakazu A. R." } }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "Tohru" }, "orcid": "0000-0002-7402-5441" }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Yasuhiro" } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "David B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Toft-S", "name": { "family": "Toft", "given": "Sune" }, "orcid": "0000-0003-3631-7176" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "Henry J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "Olivier" }, "orcid": "0000-0001-5891-2596" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "Lidia" } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "Alvio" }, "orcid": "0000-0002-7093-7355" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "Simon" }, "orcid": "0000-0002-6423-3597" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "Marcella C." }, "orcid": "0000-0003-1624-7609" }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "Katarina" } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Fu-Hai", "name": { "family": "Fu", "given": "Hai" }, "orcid": "0000-0001-9608-6395" }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "Laurence" } }, { "id": "Griffiths-R-E", "name": { "family": "Griffiths", "given": "Richard E." } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "Francesca" }, "orcid": "0000-0002-2115-1137" } ] }, "title": "Discovery of Massive, Mostly Star Formation Quenched Galaxies with Extremely Large Ly\u03b1 Equivalent Widths at z ~ 3", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; early universe; galaxies: evolution; galaxies: formation; galaxies: high-redshift", "note": "\u00a9 2015 American Astronomical Society. Received 2015 May 25; accepted 2015 July 14; published 2015 August 5.\n\nWe would like to thank both the Subaru and HST staff for\ntheir invaluable help, as well as all members of the COSMOS\nteam. We would also like to thank the anonymous referee for\nvaluable suggestions and comments. We also thank Alex\nHagen for kindly providing us with the information of their\nLAEs. This work was financially supported in part by JSPS (Y. T.: 15340059, 17253001, 19340046, and 23244031; T.N.:\n23654068 and 25707010). Data analysis was in part carried out on the common use data analysis computer system at the\nAstronomy Data Center, ADC, of the National Astronomical\nObservatory of Japan.\n\nPublished - 2041-8205_809_1_L7.pdf
Submitted - 1507.04439v1.pdf
", "abstract": "We report a discovery of six massive galaxies with both extremely large Ly\u03b1 equivalent widths (EWs) and evolved stellar populations at z ~ 3. These MAssive Extremely STrong Ly\u03b1 emitting Objects (MAESTLOs) have been discovered in our large-volume systematic survey for strong Ly\u03b1 emitters (LAEs) with 12 optical intermediate-band data taken with Subaru/Suprime-Cam in the COSMOS field. Based on the spectral energy distribution fitting analysis for these LAEs, it is found that these MAESTLOs have (1) large rest-frame EWs of EW_0 (Ly\u03b1) ~ 100\u2013300 \u00c5, (2) M_\u2605 ~ 10^(10.5)\u201310^(11.1) M_\u2299, and (3) relatively low specific star formation rates of SFR/M_\u2605 ~ 0.03\u20131 Gyr^(\u22121). Three of the six MAESTLOs have extended Ly\u03b1 emission with a radius of several kiloparsecs, although they show very compact morphology in the HST/ACS images, which correspond to the rest-frame UV continuum. Since the MAESTLOs do not show any evidence for active galactic nuclei, the observed extended Ly\u03b1 emission is likely to be caused by a star formation process including the superwind activity. We suggest that this new class of LAEs, MAESTLOs, provides a missing link from star-forming to passively evolving galaxies at the peak era of the cosmic star formation history.", "date": "2015-08-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "809", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L7", "id_number": "CaltechAUTHORS:20150903-140209397", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150903-140209397", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15340059" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17253001" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19340046" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23244031" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23654068" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "25707010" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/2041-8205/809/1/L7", "primary_object": { "basename": "1507.04439v1.pdf", "url": "https://authors.library.caltech.edu/records/zv4bs-jzt56/files/1507.04439v1.pdf" }, "related_objects": [ { "basename": "2041-8205_809_1_L7.pdf", "url": "https://authors.library.caltech.edu/records/zv4bs-jzt56/files/2041-8205_809_1_L7.pdf" } ], "pub_year": "2015", "author_list": "Taniguchi, Yoshiaki; Kajisawa, Masaru; et el." }, { "id": "https://authors.library.caltech.edu/records/cf4mf-5ys83", "eprint_id": 59987, "eprint_status": "archive", "datestamp": "2023-08-20 07:41:09", "lastmod": "2023-10-24 14:47:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Casey-C-M", "name": { "family": "Casey", "given": "C. M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Fu-Hai", "name": { "family": "Fu", "given": "H." }, "orcid": "0000-0001-9608-6395" }, { "id": "Kova\u010d-K", "name": { "family": "Kovac", "given": "K." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Treister-E", "name": { "family": "Treister", "given": "E." }, "orcid": "0000-0001-7568-6412" } ] }, "title": "A Massive, Distant Proto-Cluster at z = 2.47 Caught in a Phase of Rapid Formation", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general \u2013 galaxies: starburst \u2013 large-scale structure of universe \u2013 quasars: general", "note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 May 8; accepted 2015 June 4; published 2015 July 24.\n\nWe thank the anonymous referee for constructive comments\nwhich have improved the manuscript. Some of the data\npresented herein were obtained at the W. M. Keck Observatory,\nwhich is operated as a scientific partnership among the\nCalifornia Institute of Technology, the University of California, and the National Aeronautics and Space Administration and\nmade possible by financial support of the W. M. Keck\nFoundation. We also thank the Joint Astornomy Centre (run by\nSTFC, NSERC, and NOSR) for operation of the JCMT and\nSCUBA-2 instrument. Mahalo nui loa to the kama'aina of\nHawai'i for use of the cultural site of Maunakea for\nastronomical observing. Based in part on NASA/ESA HST\ndata, operated by STScI of AURA Inc, under NASA contract\nNAS 5-26555. Other observations obtained from the European\nSouthern Observatory, Chile. C.M.C. acknowledges generous\nsupport of a McCue Fellowship from the UC Irvine Center for\nCosmology. A.C. and C.M.C. acknowledge support from NSF\nAST-1313319, NSF CAREER 0645427, and NASA Herschel\nScience Center.\n\nPublished - 2041-8205_808_2_L33.pdf
Submitted - 1506.01715v2.pdf
", "abstract": "Numerical simulations of cosmological structure formation show that the universe's most massive clusters, and the galaxies living in those clusters, assemble rapidly at early times (2.5 < z < 4). While more than 20 proto-clusters have been observed at z \u2273 2 based on associations of 5\u201340 galaxies around rare sources, the observational evidence for rapid cluster formation is weak. Here we report observations of an asymmetric filamentary structure at z = 2.47 containing 7 starbursting, submillimeter-luminous galaxies and 5 additional active galactic nuclei (AGNs) within a comoving volume of 15,000 Mpc3. As the expected lifetime of both the luminous AGN and starburst phase of a galaxy is ~100 Myr, we conclude that these sources were likely triggered in rapid succession by environmental factors or, alternatively, the duration of these cosmologically rare phenomena is much longer than prior direct measurements suggest. The stellar mass already built up in the structure is ~10^(12) M\u2299 and we estimate that the cluster mass will exceed that of the Coma supercluster at z ~ 0. The filamentary structure is in line with hierarchical growth simulations that predict that the peak of cluster activity occurs rapidly at z > 2.", "date": "2015-08-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "808", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L33", "id_number": "CaltechAUTHORS:20150831-104640271", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150831-104640271", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "University of California Irvine" }, { "agency": "NSF", "grant_number": "AST-1313319" }, { "agency": "NSF", "grant_number": "AST-0645427" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/2041-8205/808/2/L33", "primary_object": { "basename": "1506.01715v2.pdf", "url": "https://authors.library.caltech.edu/records/cf4mf-5ys83/files/1506.01715v2.pdf" }, "related_objects": [ { "basename": "2041-8205_808_2_L33.pdf", "url": "https://authors.library.caltech.edu/records/cf4mf-5ys83/files/2041-8205_808_2_L33.pdf" } ], "pub_year": "2015", "author_list": "Casey, C. M.; Cooray, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/dbgee-r0a97", "eprint_id": 61292, "eprint_status": "archive", "datestamp": "2023-08-20 07:36:07", "lastmod": "2023-10-25 14:42:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Petric-A-O", "name": { "family": "Petric", "given": "Andreea O." }, "orcid": "0000-0003-4030-3455" }, { "id": "Ho-Luis-C", "name": { "family": "Ho", "given": "Luis C." }, "orcid": "0000-0001-6947-5846" }, { "id": "Flagey-N-J-M", "name": { "family": "Flagey", "given": "Nicolas J. M." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Herschel Survey of the Palomar-Green QSOs at Low Redshift", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 quasars: general", "note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2014 December 30; accepted 2015 May 13; published 2015 August 6. \n\nL.C.H. acknowledges support by the Chinese Academy of Science through grant No. XDB09030102 (Emergence of Cosmological Structures) from the Strategic Priority Research Program and by the National Natural Science Foundation of China through grant No. 11473002. We thank the anonymous referee for providing valuable comments and help in improving the contents of this paper. This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. The authors would like to thank Nicolas Billot for help preparing the observations, and Roberta Paladini for numerous and very helpful consultations about Herschel data reduction and HIPE. A.P. would like to thank Mia U. and Maya Angelou for their lives and words \"You may encounter many defeats, but you must not be defeated. In fact, it may be necessary to encounter the defeats, so you can know who you are, what you can rise from, how you can still come out of it\" (M.A.).\n\nPublished - Petric_2015.pdf
Submitted - 1505.05273v1.pdf
", "abstract": "We investigate the global cold dust properties of 85 nearby (z \u2a7d 0.5) QSOs, chosen from the Palomar-Green sample of optically luminous quasars. We determine their infrared spectral energy distributions and estimate their rest-frame luminosities by combining Herschel data from 70 to 500 \u03bcm with near-infrared and mid-infrared measurements from the 2MASS and the Wide-Field Infrared Survey Explorer. In most sources the far-infrared (FIR) emission can be attributed to thermally heated dust. Single temperature modified blackbody fits to the FIR photometry give an average dust temperature for the sample of 33 K, with a standard deviation of 8 K, and an average dust mass of 7 x 10^6 M\u2299 with a standard deviation of 9 x 10^6 M\u2299. Estimates of star formation rates that are based on the FIR continuum emission correlate with those based on the 11.3 \u03bcm polycyclic aromatic hydrocarbon (PAH) feature, however, the star formation rates estimated from the FIR continuum are higher than those estimated from the 11.3 \u03bcm PAH emission. We attribute this result to a variety of factors including the possible destruction of the PAHs and that, in some sources, a fraction of the FIR originates from dust heated by the active galactic nucleus and by old stars.", "date": "2015-08", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "219", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 22", "id_number": "CaltechAUTHORS:20151019-155256159", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151019-155256159", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Chinese Academy of Science", "grant_number": "XDB09030102" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11473002" }, { "agency": "NASA" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0067-0049/219/2/22", "primary_object": { "basename": "1505.05273v1.pdf", "url": "https://authors.library.caltech.edu/records/dbgee-r0a97/files/1505.05273v1.pdf" }, "related_objects": [ { "basename": "Petric_2015.pdf", "url": "https://authors.library.caltech.edu/records/dbgee-r0a97/files/Petric_2015.pdf" } ], "pub_year": "2015", "author_list": "Petric, Andreea O.; Ho, Luis C.; et el." }, { "id": "https://authors.library.caltech.edu/records/z9wsg-1xa67", "eprint_id": 58878, "eprint_status": "archive", "datestamp": "2023-08-22 15:48:54", "lastmod": "2023-10-23 19:50:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "S." } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "B\u00e9thermin-Matthieu", "name": { "family": "B\u00e9thermin", "given": "M." }, "orcid": "0000-0002-3915-2015" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Hsieh-B-C", "name": { "family": "Hsieh", "given": "B.-C." } }, { "id": "Kajisawa-Masaru", "name": { "family": "Kajisawa", "given": "M." }, "orcid": "0000-0002-1732-6387" }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "N." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Michel-Dansac-L", "name": { "family": "Michel-Dansac", "given": "L." } }, { "id": "Moutard-T", "name": { "family": "Moutard", "given": "T." } }, { "id": "Renzini-M-A", "name": { "family": "Renzini", "given": "M. A." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } } ] }, "title": "Evolution of the specific star formation rate function at z < 1.4 Dissecting the mass-SFR plane in COSMOS and GOODS", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: luminosity function, mass function; galaxies: stellar content; galaxies: star formation; galaxies: statistics; galaxies: formation", "note": "\u00a9 2015 ESO.\nArticle published by EDP Sciences.\n\nReceived 17 October 2014; Accepted 2 March 2015;\nPublished online 19 June 2015.\n\nWe are grateful to the referee for the careful reading of the\nmanuscript and his/her useful suggestions. We thank Samuel Boissier, V\u00e9ronique\nBuat, Andrea Cattaneo, Jared Gabor, Sylvain De La Torre and Mark Sargent\nfor useful discussions. We thank Carlota Gruppioni for providing her data.\nWe gratefully acknowledge the contributions of the entire COSMOS collaboration\nconsisting of more than 100 scientists. The HST COSMOS program\nwas supported through NASA grant HST-GO-09822. More information on the\nCOSMOS survey is available at http://www.astro.caltech.edu/cosmos.\nThis paper is based on observations made with ESO Telescopes at the La Silla\nParanal Observatory under ESO programme ID 179.A-2005 and on data products\nproduced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf\nof the UltraVISTA consortium. LMD acknowledges support from the Lyon\nInstitute of Origins under grant ANR-10-LABX-66. A.K. acknowledges support\nby the Collaborative Research Council 956, sub-project A1, funded by the\nDeutsche Forschungsgemeinschaft (DFG).\n\nPublished - aa25176-14.pdf
Submitted - 1410.4875v3.pdf
", "abstract": "The relation between the stellar mass (M\u22c6) and the star formation rate (SFR) characterizes how the instantaneous star formation is determined by the galaxy past star formation history and by the growth of the dark matter structures. We deconstruct the M\u22c6-SFR plane by measuring the specific SFR functions in several stellar mass bins from z = 0.2 out to z = 1.4 (specific SFR = SFR/M\u22c6, noted sSFR). Our analysis is primary based on a 24 \u03bcm selected catalogue combining the COSMOS and GOODS surveys. We estimate the SFR by combining mid- and far-infrared data for 20500 galaxies. The sSFR functions are derived in four stellar mass bins within the range 9.5 < log\u2009(M\u22c6 /M\u2299) < 11.5. First, we demonstrate the importance of taking into account selection effects when studying the M\u22c6-SFR relation. Secondly, we find a mass-dependent evolution of the median sSFR with redshift varying as sSFR \u221d (1 + z)^b, with b increasing from b = 2.88^(\u00b10.12) to b = 3.78^(\u00b1 0.60) between M\u22c6 = 10^(9.75) M\u2299 and M\u22c6 = 10^(11.1) M\u2299, respectively. At low masses, this evolution is consistent with the cosmological accretion rate and predictions from semi-analytical models (SAM). This agreement breaks down for more massive galaxies showing the need for a more comprehensive description of the star formation history in massive galaxies. Third, we obtain that the shape of the sSFR function is invariant with time at z< 1.4 but depends on the mass. We observe a broadening of the sSFR function ranging from 0.28 dex at M\u22c6 = 10^(9.75) M\u2299 to 0.46 dex at M\u22c6 = 10^(11.1) M\u2299. Such increase in the intrinsic scatter of the M\u22c6-SFR relation suggests an increasing diversity ofstar formation histories (SFHs) as the stellar mass increases. Finally, we find a gradual decline of the sSFR with stellar mass as log\u2009_(10)(sSFR) \u221d \u22120.17M\u22c6. We discuss the numerous physical processes, as gas exhaustion in hot gas halos or secular evolution, which can gradually reduce the sSFR and increase the SFH diversity.", "date": "2015-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "579", "publisher": "EDP Sciences", "pagerange": "Art. No. A2", "id_number": "CaltechAUTHORS:20150714-105208366", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150714-105208366", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "Lyon Institute of Origins", "grant_number": "ANR-10-LABX-66" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "956" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "SPLASH" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201425176", "primary_object": { "basename": "1410.4875v3.pdf", "url": "https://authors.library.caltech.edu/records/z9wsg-1xa67/files/1410.4875v3.pdf" }, "related_objects": [ { "basename": "aa25176-14.pdf", "url": "https://authors.library.caltech.edu/records/z9wsg-1xa67/files/aa25176-14.pdf" } ], "pub_year": "2015", "author_list": "Ilbert, O.; Arnouts, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/8tqp2-xy148", "eprint_id": 56856, "eprint_status": "archive", "datestamp": "2023-08-20 07:01:06", "lastmod": "2023-10-23 16:03:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C." }, "orcid": "0000-0001-6647-3861" }, { "id": "Jones-G", "name": { "family": "Jones", "given": "G." } }, { "id": "Casey-C-M", "name": { "family": "Casey", "given": "C. M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" } ] }, "title": "Galaxies at redshifts 5 to 6 with systematically low dust content and high [C II] emission", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2015 Macmillan Publishers Limited. \n\nReceived 20 November 2014; accepted 23 April 2015. \n\nSupport for this work was provided by NASA through an award issued by JPL/Caltech. We thank the ALMA staff for facilitating the observations and aiding in the calibration and reduction process. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This work is based in part on observations made with the Spitzer Space Telescope and the W.M. Keck Observatory, along with archival data from the NASA/ESA Hubble Space Telescope, the Subaru Telescope, the Canada-France-Hawaii-Telescope and the ESO Vista telescope obtained from the NASA/IPAC Infrared Science Archive. V.S. acknowledges funding by the European Union's Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, 'CoSMass'). \n\nContributions: P.L.C. proposed and carried out the observations, conducted the analysis in this paper, and authored the majority of the text. C.C., G.J. and K.S. carried out the reduction and direct analysis of the ALMA data. C.M.C. consulted on the spectral energy distribution fitting and interpretation of the data, and also conducted a blind test of the FIR luminosity, [C II] line luminosity, and \u03b2 measurements, along with testing for sample selection effects. D.R. conducted the spectral line analysis and carried out an independent blind check of the ALMA data reduction. O.I. carried out the spectral energy distribution fitting and consulted on their interpretation. C.M.C., A.K., O.L., S.L., N.S., V.S. and L.Y. contributed to the overall interpretation of the results and various aspects of the analysis. \n\nThe authors declare no competing financial interests. \n\nThis paper makes use of ALMA data: ADS/JAO.ALMA#2012.1.00523.S. ALMA.\n\nSubmitted - 1503.07596.pdf
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", "abstract": "The rest-frame ultraviolet properties of galaxies during the first three billion years of cosmic time (redshift z > 4) indicate a rapid evolution in the dust obscuration of such galaxies. This evolution implies a change in the average properties of the interstellar medium, but the measurements are systematically uncertain owing to untested assumptions and the inability to detect heavily obscured regions of the galaxies. Previous attempts to measure the interstellar medium directly in normal galaxies at these redshifts have failed for a number of reasons, with two notable exceptions. Here we report measurements of the forbidden C II emission (that is, [C II]) from gas, and the far-infrared emission from dust, in nine typical star-forming galaxies about one billion years after the Big Bang (z \u2248 5\u20136). We find that these galaxies have thermal emission that is less than 1/12 that of similar systems about two billion years later, and enhanced [C II] emission relative to the far-infrared continuum, confirming a strong evolution in the properties of the interstellar medium in the early Universe. The gas is distributed over scales of one to eight kiloparsecs, and shows diverse dynamics within the sample. These results are consistent with early galaxies having significantly less dust than typical galaxies seen at z < 3 and being comparable in dust content to local low-metallicity systems.", "date": "2015-06-25", "date_type": "published", "publication": "Nature", "volume": "522", "number": "7557", "publisher": "Nature Publishing Group", "pagerange": "455-458", "id_number": "CaltechAUTHORS:20150422-092810804", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150422-092810804", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1038/nature14500", "primary_object": { "basename": "nature14500-sf3.jpg", "url": "https://authors.library.caltech.edu/records/8tqp2-xy148/files/nature14500-sf3.jpg" }, "related_objects": [ { "basename": "nature14500-sf4.jpg", "url": "https://authors.library.caltech.edu/records/8tqp2-xy148/files/nature14500-sf4.jpg" }, { "basename": "nature14500-st1.jpg", "url": "https://authors.library.caltech.edu/records/8tqp2-xy148/files/nature14500-st1.jpg" }, { "basename": "nature14500-st3.jpg", "url": "https://authors.library.caltech.edu/records/8tqp2-xy148/files/nature14500-st3.jpg" }, { "basename": "nature14500-st5.jpg", "url": "https://authors.library.caltech.edu/records/8tqp2-xy148/files/nature14500-st5.jpg" }, { "basename": "1503.07596.pdf", "url": "https://authors.library.caltech.edu/records/8tqp2-xy148/files/1503.07596.pdf" }, { "basename": "nature14500-sf2.jpg", "url": "https://authors.library.caltech.edu/records/8tqp2-xy148/files/nature14500-sf2.jpg" }, { "basename": "nature14500-st2.jpg", "url": "https://authors.library.caltech.edu/records/8tqp2-xy148/files/nature14500-st2.jpg" }, { "basename": "nature14500-st4.jpg", "url": "https://authors.library.caltech.edu/records/8tqp2-xy148/files/nature14500-st4.jpg" }, { "basename": "nature14500-sf1.jpg", "url": "https://authors.library.caltech.edu/records/8tqp2-xy148/files/nature14500-sf1.jpg" } ], "pub_year": "2015", "author_list": "Capak, P. L.; Carilli, C.; et el." }, { "id": "https://authors.library.caltech.edu/records/zn5v4-r5r85", "eprint_id": 58979, "eprint_status": "archive", "datestamp": "2023-08-20 06:58:05", "lastmod": "2023-10-23 19:56:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "Jeyhan S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Kashino-Daichi", "name": { "family": "Kashino", "given": "D." }, "orcid": "0000-0001-9044-1747" }, { "id": "Chu-J", "name": { "family": "Chu", "given": "J." } }, { "id": "Zahid-H-J", "name": { "family": "Zahid", "given": "H." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Kewley-L-J", "name": { "family": "Kewley", "given": "L. J." }, "orcid": "0000-0001-8152-3943" }, { "id": "Matsuoka-Kenta", "name": { "family": "Matsuoka", "given": "K." }, "orcid": "0000-0002-2689-4634" }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "T." }, "orcid": "0000-0002-7402-5441" }, { "id": "Riguccini-L", "name": { "family": "Riguccini", "given": "L." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Schawinski-K", "name": { "family": "Schawinski", "given": "K." }, "orcid": "0000-0001-5464-0888" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Treister-E", "name": { "family": "Treister", "given": "E." }, "orcid": "0000-0001-7568-6412" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "Ohta-K", "name": { "family": "Ohta", "given": "K." } } ] }, "title": "Rest-frame Optical Emission Lines in Far-infrared-selected Galaxies at z < 1.7 from the FMOS-COSMOS Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 galaxies: active \u2013 galaxies: evolution \u2013 galaxies: high-redshift \u2013 infrared: galaxies \u2013 surveys", "note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2014 November 25; accepted 2015 May 9; published 2015 June 22.\n\nPublished - 2041-8205_806_2_L35.pdf
Submitted - 1505.03527v2.pdf
", "abstract": "We have used FMOS on Subaru to obtain near-infrared spectroscopy of 123 far-infrared-selected galaxies in COSMOS and the key rest-frame optical emission lines. This is the largest sample of infrared galaxies with near-infrared spectroscopy at these redshifts. The far-infrared selection results in a sample of galaxies that are massive systems that span a range of metallicities in comparison with previous optically selected surveys, and thus has a higher active galactic nucleus (AGN) fraction and better samples the AGN branch. We establish the presence of AGNs and starbursts in this sample of (U)LIRGs selected as Herschel-PACS and Spitzer-MIPS detections in two redshift bins (z ~ 0.7 and z ~ 1.5) and test the redshift dependence of diagnostics used to separate AGNs from star formation dominated galaxies. In addition, we construct a low-redshift (z ~ 0.1) comparison sample of infrared-selected galaxies and find that the evolution from z ~ 1.5 to today is consistent with an evolving AGN selection line and a range of ISM conditions and metallicities from the models of Kewley et al. We find that a large fraction of (U)LIRGs are BPT-selected AGNs using their new redshift-dependent classification line. We compare the position of known X-ray-detected AGNs (67 in total) with the BPT selection and find that the new classification line accurately selects most of these objects (>70%). Furthermore, we identify 35 new (likely obscured) AGNs not selected as such by their X-ray emission. Our results have direct implications for AGN selection at higher redshift with either current (MOSFIRE, KMOS) or future (PFS, MOONS) spectroscopic efforts with near-infrared spectral coverage.", "date": "2015-06-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "806", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L35", "id_number": "CaltechAUTHORS:20150722-100206292", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150722-100206292", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/2041-8205/806/2/L35", "primary_object": { "basename": "1505.03527v2.pdf", "url": "https://authors.library.caltech.edu/records/zn5v4-r5r85/files/1505.03527v2.pdf" }, "related_objects": [ { "basename": "2041-8205_806_2_L35.pdf", "url": "https://authors.library.caltech.edu/records/zn5v4-r5r85/files/2041-8205_806_2_L35.pdf" } ], "pub_year": "2015", "author_list": "Kartaltepe, Jeyhan S.; Sanders, D. B.; et el." }, { "id": "https://authors.library.caltech.edu/records/rm438-2xy91", "eprint_id": 58942, "eprint_status": "archive", "datestamp": "2023-09-15 05:04:22", "lastmod": "2023-10-23 21:13:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Darvish-B", "name": { "family": "Darvish", "given": "Behnam" }, "orcid": "0000-0003-4919-9017" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Sobral-D", "name": { "family": "Sobral", "given": "David" }, "orcid": "0000-0001-8823-4845" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas" }, "orcid": "0000-0002-0438-3323" }, { "id": "Aragon-Calvo-M", "name": { "family": "Aragon-Calvo", "given": "Miguel" } } ] }, "title": "A Comparative Study of Density Field Estimation for Galaxies: New Insights into the Evolution of Galaxies with Environment in COSMOS out to z ~ 3", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; large-scale structure of universe; methods: data analysis", "note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2015 January 26; accepted 2015 March 27; published 2015 May 27.\n\nWe gratefully thank the anonymous referee for thoroughly\nreading the original manuscript and providing very useful\ncomments that improved the quality of the work. B.D.\ngratefully acknowledges Lucia Pozzetti for providing the data for this study. D.S. acknowledges financial support from LKBF, the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship, from FCT through an FCT Investigator Starting Grant, a Start-up Grant (IF/01154/2012/CP0189/CT0010), and the grant PEst-OE/FIS/UI2751/2014. This study used the COSMOS data based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc., under NASA contract NAS 5-26555, and the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. It is also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory under Large Program 175.A-01279, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; and the Canada\u2013France\u2013Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the NRC and CADC of Canada, the CNRS of France, TERAPIX, and the University of Hawaii.\n\nPublished - 0004-637X_805_2_121.pdf
Submitted - 1503.07879v1.pdf
", "abstract": "It is well-known that a galaxy's environment has a fundamental influence in shaping its properties. We study the environmental effects on galaxy evolution, with an emphasis on the environment defined as the local number density of galaxies. The density field is estimated with different estimators (weighted adaptive kernel smoothing, 10th and 5th nearest neighbors, Voronoi and Delaunay tessellation) for a K_s < 24 sample of ~190,000 galaxies in the COSMOS field at 0.1 < z < 3.1. The performance of each estimator is evaluated with extensive simulations. We show that overall there is a good agreement between the estimated density fields using different methods over ~2 dex in overdensity values. However, our simulations show that adaptive kernel and Voronoi tessellation outperform other methods. Using the Voronoi tessellation method, we assign surface densities to a mass complete sample of quiescent and star-forming galaxies out to z ~ 3. We show that at a fixed stellar mass, the median color of quiescent galaxies does not depend on their host environment out to z ~ 3. We find that the number and stellar mass density of massive (>10^11 M_\u2299) star-forming galaxies have not significantly changed since z ~ 3, regardless of their environment. However, for massive quiescent systems at lower redshifts (z \u2272 1.3), we find a significant evolution in the number and stellar mass densities in denser environments compared to lower density regions. Our results suggest that the relation between stellar mass and local density is more fundamental than the color\u2013density relation and that environment plays a significant role in quenching star-formation activity in galaxies at z \u2272 1.", "date": "2015-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "805", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 121", "id_number": "CaltechAUTHORS:20150720-101002370", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150720-101002370", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "LKBF" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "IF/01154/2012/ CP0189/CT0010" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "PEst-OE/FIS/UI2751/2014" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NASA", "grant_number": "1407" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/805/2/121", "primary_object": { "basename": "0004-637X_805_2_121.pdf", "url": "https://authors.library.caltech.edu/records/rm438-2xy91/files/0004-637X_805_2_121.pdf" }, "related_objects": [ { "basename": "1503.07879v1.pdf", "url": "https://authors.library.caltech.edu/records/rm438-2xy91/files/1503.07879v1.pdf" } ], "pub_year": "2015", "author_list": "Darvish, Behnam; Mobasher, Bahram; et el." }, { "id": "https://authors.library.caltech.edu/records/zkdnd-97519", "eprint_id": 58605, "eprint_status": "archive", "datestamp": "2023-08-22 15:34:05", "lastmod": "2023-10-23 19:31:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kabayashi-Masato-I-N", "name": { "family": "Kobayashi", "given": "Masato I. N." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "More-S", "name": { "family": "More", "given": "Surhud" } }, { "id": "Okabe-Nobuhiro", "name": { "family": "Okabe", "given": "Nobuhiro" } }, { "id": "Laigle-C", "name": { "family": "Laigle", "given": "Clotilde" } }, { "id": "Rhodes-J", "name": { "family": "Rhodes", "given": "Jason" } }, { "id": "Takeuchi-T-T", "name": { "family": "Takeuchi", "given": "Tsutomu T." } } ] }, "title": "Can we use weak lensing to measure total mass profiles of galaxies on 20 kpc scales?", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: weak; galaxies: haloes; galaxies: stellar content; galaxies: structure; cosmology: observations; large-scale structure of Universe", "note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2015 February 24. Received 2015 February 19; in original form 2014 December 3.\n\nFirst published online March 30, 2015.\n\nWe are grateful to the referee for a careful reading of the manuscript and for providing thoughtful comments. We thank Robert Lupton for useful discussions during the preparation of this paper and Naoshi Sugiyama for practical advice during the data analysis. This work, AL, and SM are supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. MINK acknowledges the financial support from N. Sugiyama (25287057) by Grants-in-Aid from the Ministry of Education, Culture, Sports, Science, and Technology of Japan. NO (26800097) is supported by Grants-in-Aid from the Ministry of Education, Culture, Sports, Science, and Technology of Japan. CL is supported by the ILP LABEX (under reference ANR-10-LABX-63 and ANR-11-IDEX-0004-02). JR was supported by JPL, run under a contract for NASA by Caltech. TTT has been supported by the Grant-in-Aid for the Scientific Research Fund (23340046), for the Global COE Program Request for Fundamental Principles in the Universe: from Particles to the Solar system and the Cosmos, and for the JSPS Strategic Young Researcher Overseas Visits Program for Accelerating Brain Circulation, commissioned by the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan.\n\nPublished - MNRAS-2015-Kobayashi-2128-43.pdf
Submitted - 1502.06604v1.pdf
", "abstract": "Current constraints on dark matter density profiles from weak lensing are typically limited to radial scales greater than 50\u2013100 kpc. In this paper, we explore the possibility of probing the very inner regions of galaxy/halo density profiles by measuring stacked weak lensing on scales of only a few tens of kpc. Our forecasts focus on scales smaller than the 'equality radius' (R_eq), where the stellar component and the dark matter component contribute equally to the lensing signal. We compute the evolution of R_eq as a function of lens stellar mass and redshift and show that R_eq = 7\u201334 kpc for galaxies with M* = 10^(9.5)\u201310^11.5 M_\u2299. Unbiased shear measurements will be challenging on these scales. We introduce a simple metric to quantify how many source galaxies overlap with their neighbours and for which shear measurements will be challenging. Rejecting source galaxies with close-by companions results in an \u223c20 per cent decrease in the overall source density. Despite this decrease, we show that Euclid and Wide Field Infrared Survey Telescope will be able to constrain galaxy/halo density profiles at Req with S/N >20 for M_* > 10^10\u2009M_\u2299. Weak lensing measurements at Req, in combination with stellar kinematics on smaller scales, will be a powerful means by which to constrain both the inner slope of the dark matter density profile as well as the mass and redshift dependence of the stellar initial mass function.", "date": "2015-05-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "449", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "2128-2143", "id_number": "CaltechAUTHORS:20150625-114959500", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150625-114959500", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "25287057" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "26800097" }, { "agency": "ILP LABEX", "grant_number": "ANR-10-LABX-63" }, { "agency": "ILP LABEX", "grant_number": "ANR-11-IDEX- 0004-02" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Scientific Research Fund Grant-in-Aid", "grant_number": "23340046" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stv424", "primary_object": { "basename": "1502.06604v1.pdf", "url": "https://authors.library.caltech.edu/records/zkdnd-97519/files/1502.06604v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2015-Kobayashi-2128-43.pdf", "url": "https://authors.library.caltech.edu/records/zkdnd-97519/files/MNRAS-2015-Kobayashi-2128-43.pdf" } ], "pub_year": "2015", "author_list": "Kobayashi, Masato I. N.; Leauthaud, Alexie; et el." }, { "id": "https://authors.library.caltech.edu/records/3mywj-d2h08", "eprint_id": 78697, "eprint_status": "archive", "datestamp": "2023-08-20 06:15:46", "lastmod": "2023-10-26 00:18:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Coupon-J", "name": { "family": "Coupon", "given": "J." } }, { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "S." } }, { "id": "van-Waerbeke-L", "name": { "family": "van Waerbeke", "given": "L." } }, { "id": "Moutard-T", "name": { "family": "Moutard", "given": "T." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "van-Uitert-E", "name": { "family": "van Uitert", "given": "E." } }, { "id": "Erben-T", "name": { "family": "Erben", "given": "T." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Heymans-C", "name": { "family": "Heymans", "given": "C." } }, { "id": "Hildebrandt-H", "name": { "family": "Hildebrandt", "given": "H." } }, { "id": "Hoekstra-H", "name": { "family": "Hoekstra", "given": "H." } }, { "id": "Kilbinger-M", "name": { "family": "Kilbinger", "given": "M." } }, { "id": "Kitching-T", "name": { "family": "Kitching", "given": "T." } }, { "id": "Mellier-Y", "name": { "family": "Mellier", "given": "Y." } }, { "id": "Miller-L", "name": { "family": "Miller", "given": "L." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Bonnett-C", "name": { "family": "Bonnett", "given": "C." } }, { "id": "Branchini-E", "name": { "family": "Branchini", "given": "E." } }, { "id": "Davidzon-I", "name": { "family": "Davidzon", "given": "I." }, "orcid": "0000-0002-2951-7519" }, { "id": "De-Lucia-G", "name": { "family": "De Lucia", "given": "G." } }, { "id": "Fritz-A", "name": { "family": "Fritz", "given": "A." } }, { "id": "Fu-L", "name": { "family": "Fu", "given": "L." } }, { "id": "Hudelot-P", "name": { "family": "Hudelot", "given": "P." } }, { "id": "Hudson-M-J", "name": { "family": "Hudson", "given": "M. J." } }, { "id": "Kuijken-K", "name": { "family": "Kuijken", "given": "K." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Moscardini-L", "name": { "family": "Moscardini", "given": "L." } }, { "id": "Rowe-B-T-P", "name": { "family": "Rowe", "given": "B. T. P." } }, { "id": "Schrabback-T", "name": { "family": "Schrabback", "given": "T." } }, { "id": "Sembolini-E", "name": { "family": "Semboloni", "given": "E." } }, { "id": "Velander-M", "name": { "family": "Velander", "given": "M." } } ] }, "title": "The galaxy-halo connection from a joint lensing, clustering and abundance analysis in the CFHTLenS/VIPERS field", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted Version - 1502.02867.pdf
", "abstract": "We present new constraints on the relationship between galaxies and their host dark matter haloes, measured from the location of the peak of the stellar-to-halo mass ratio (SHMR), up to the most massive galaxy clusters at redshift z \u223c 0.8 and over a volume of nearly 0.1 Gpc3. We use a unique combination of deep observations in the CFHTLenS/VIPERS field from the near-UV to the near-IR, supplemented by \u223c60\u2009000 secure spectroscopic redshifts, analysing galaxy clustering, galaxy\u2013galaxy lensing and the stellar mass function. We interpret our measurements within the halo occupation distribution (HOD) framework, separating the contributions from central and satellite galaxies. We find that the SHMR for the central galaxies peaks at \nMh,peak=1.9+0.2\u22120.1\u00d71012M\u2299\nMh,peak=1.9\u22120.1+0.2\u00d71012M\u2299\n \n with an amplitude of 0.025, which decreases to \u223c0.001 for massive haloes (\nMh>1014M\u2299\nMh>1014M\u2299\n \n). Compared to central galaxies only, the total SHMR (including satellites) is boosted by a factor of 10 in the high-mass regime (cluster-size haloes), a result consistent with cluster analyses from the literature based on fully independent methods. After properly accounting for differences in modelling, we have compared our results with a large number of results from the literature up to z = 1: we find good general agreement, independently of the method used, within the typical stellar-mass systematic errors at low to intermediate mass (\nM\u22c6<1011M\u2299\nM\u22c6<1011M\u2299\n \n) and the statistical errors above. We have also compared our SHMR results to semi-analytic simulations and found that the SHMR is tilted compared to our measurements in such a way that they over- (under-) predict star formation efficiency in central (satellite) galaxies.", "date": "2015-05-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "449", "number": "2", "publisher": "Oxford University Press", "pagerange": "1352-1379", "id_number": "CaltechAUTHORS:20170629-125450062", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170629-125450062", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "SPLASH" }, { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stv276", "primary_object": { "basename": "1502.02867.pdf", "url": "https://authors.library.caltech.edu/records/3mywj-d2h08/files/1502.02867.pdf" }, "pub_year": "2015", "author_list": "Coupon, J.; Arnouts, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/ehvkg-vpq87", "eprint_id": 58634, "eprint_status": "archive", "datestamp": "2023-08-20 06:10:56", "lastmod": "2023-10-23 19:32:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Delvecchio-I", "name": { "family": "Delvecchio", "given": "I." }, "orcid": "0000-0001-8706-2252" }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Berta-S", "name": { "family": "Berta", "given": "S." }, "orcid": "0000-0002-0320-1532" }, { "id": "Rosario-D-J", "name": { "family": "Rosario", "given": "D. J." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Pozzi-F", "name": { "family": "Pozzi", "given": "F." } }, { "id": "Gruppioni-C", "name": { "family": "Gruppioni", "given": "C." }, "orcid": "0000-0002-5836-4056" }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "C." }, "orcid": "0000-0002-8853-9611" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Clements-D-L", "name": { "family": "Clements", "given": "D. L." }, "orcid": "0000-0002-9548-5033" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Lanzuisi-G", "name": { "family": "Lanzuisi", "given": "G." }, "orcid": "0000-0001-9094-0984" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S." }, "orcid": "0000-0001-7862-1032" }, { "id": "Rodighiero-G", "name": { "family": "Rodighiero", "given": "G." }, "orcid": "0000-0002-9415-2296" }, { "id": "Santini-P", "name": { "family": "Santini", "given": "P." } }, { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "M." } } ] }, "title": "Mapping the average AGN accretion rate in the SFR\u2013M_\u2217 plane for Herschel-selected galaxies at 0 < z \u2264 2.5", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution\n galaxies: nuclei\n infrared: galaxies", "note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 January 28. Received 2015 January 26; in original form 2014 November 13. First published online March 17, 2015.\n\nHerschel is an ESA space observatory with science instruments provided\nby European-led Principal Investigator consortia and with important participation\nfrom NASA.\n\nThe authors are grateful to the referee, J. R. Mullaney, for his constructive report. This paper uses data from Herschel's photometers PACS and SPIRE. PACS has been developed by a consortium of institutes led by MPE (Germany) and including: UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy) and IAC (Spain). This development has been supported by the funding agencies BMVIT(Austria),ESA-PRODEX(Belgium),CEA/CNES(France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada);\nNAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy);\nIAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and\nCaltech, JPL, NHSC, Univ. Colorado (USA). This development\nhas been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating\nInstitutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max\nPlanck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University.\nFunding for PRIMUS is provided by NSF (AST-0607701,\nAST-0908246, AST-0908442, AST-0908354) and NASA (Spitzer-\n1356708, 08-ADP08-0019, NNX09AC95G). This research has made use of software provided by the Chandra X-ray Center (CXC) in the application package CIAO (v. 4.6). ID is grateful to Jillian Scudder for useful comments, and to Simonetta\nPuccetti and Nico Cappelluti for providing with X-ray sensitivity maps in the COSMOS field. ID is also thankful to Takamitsu Miyaji for his kind support in using CSTACK, and warmly thanks Fabio Vito for helpful suggestions with X-ray tools and routines to compute intrinsic X-ray luminosities. MB and GL acknowledge support from the FP7 Career Integration Grant 'eEASy' (CIG 321913).\n\nPublished - MNRAS-2015-Delvecchio-373-89.pdf
Submitted - 1501.07602v2.pdf
", "abstract": "We study the relation of AGN accretion, star formation rate (SFR) and stellar mass (M_*) using a sample of \u22488600 star-forming galaxies up to z = 2.5 selected with Herschel imaging in the GOODS and COSMOS fields. For each of them we derive SFR and M_*, both corrected, when necessary, for emission from an active galactic nucleus (AGN), through the decomposition of their spectral energy distributions (SEDs). About 10 per cent of the sample are detected individually in Chandra observations of the fields. For the rest of the sample, we stack the X-ray maps to get average X-ray properties. After subtracting the X-ray luminosity expected from star formation and correcting for nuclear obscuration, we derive the average AGN accretion rate for both detected sources and stacks, as a function of M_*, SFR and redshift. The average accretion rate correlates with SFR and with M_*. The dependence on SFR becomes progressively more significant at z > 0.8. This may suggest that SFR is the original driver of these correlations. We find that average AGN accretion and star formation increase in a similar fashion with offset from the star-forming 'main-sequence'. Our interpretation is that accretion on to the central black hole and star formation broadly trace each other, irrespective of whether the galaxy is evolving steadily on the main-sequence or bursting.", "date": "2015-05-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "449", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "373-389", "id_number": "CaltechAUTHORS:20150626-104052498", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150626-104052498", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia Y Tecnologia (MCYT)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NSF", "grant_number": "AST-0607701" }, { "agency": "NSF", "grant_number": "AST-0908246" }, { "agency": "NSF", "grant_number": "AST-0908442" }, { "agency": "NSF", "grant_number": "AST-0908354" }, { "agency": "NASA", "grant_number": "1356708" }, { "agency": "NASA", "grant_number": "08-ADP08-0019" }, { "agency": "NASA", "grant_number": "NNX09AC95G" }, { "agency": "European Research Council (ERC)", "grant_number": "CIG 321913" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stv213", "primary_object": { "basename": "MNRAS-2015-Delvecchio-373-89.pdf", "url": "https://authors.library.caltech.edu/records/ehvkg-vpq87/files/MNRAS-2015-Delvecchio-373-89.pdf" }, "related_objects": [ { "basename": "1501.07602v2.pdf", "url": "https://authors.library.caltech.edu/records/ehvkg-vpq87/files/1501.07602v2.pdf" } ], "pub_year": "2015", "author_list": "Delvecchio, I.; Lutz, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/hcf9p-8k959", "eprint_id": 58041, "eprint_status": "archive", "datestamp": "2023-08-20 06:03:09", "lastmod": "2023-10-23 18:01:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Miettinen-O", "name": { "family": "Miettinen", "given": "O." } }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Novak-Mladen", "name": { "family": "Novak", "given": "M." }, "orcid": "0000-0001-8695-825X" }, { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "D." }, "orcid": "0000-0001-5382-6138" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D. A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Bussmann-R-S", "name": { "family": "Bussmann", "given": "R. S." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Feruglio-C", "name": { "family": "Feruglio", "given": "C." } }, { "id": "Halliday-C", "name": { "family": "Halliday", "given": "C." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Navarrete-F", "name": { "family": "Navarrete", "given": "F." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" } ] }, "title": "(Sub)millimetre interferometric imaging of a sample of COSMOS/AzTEC submillimetre galaxies. I. Multiwavelength identifications and redshift distribution", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: formation, galaxies: starburst, galaxies: star formation, submillimeter: galaxies", "note": "\u00a9 2015 ESO. \n\nReceived 19 September 2014. Accepted 13 February 2015. Published online: 27 April 2015. \n\nWe thank the referee for providing helpful and constructive comments. We would also like to thank C. M. Casey and S. Toft for their comments and suggestions. This research was funded by the European Union's Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, \"CoS-Mass\"). AK acknowledges support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). We would like to thank the IRAM staff for carrying out the PdBI observations\npresented in this paper. This work is partly based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This research has made use of NASA's Astrophysics Data System, and the NASA/IPAC Infrared Science Archive, which is operated by the JPL, California Institute of Technology, under contract with the NASA. This study also made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com, and TOPCAT, an interactive graphical tool for analysis and manipulation of tabular data available at http://www.star.bristol.ac.uk/~mbt/topcat/ (Taylor (2005)). We greatfully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/~cosmos\n\nPublished - aa25032-14.pdf
Submitted - 1502.05854v1.pdf
", "abstract": "We used the Plateau de Bure Interferometer (PdBI) to map a sample of 15 submillimetre galaxies (SMGs) in the COSMOS field at the wavelength of 1.3 mm. The target SMGs were originally discovered in the James Clerk Maxwell Telescope (JCMT)/AzTEC 1.1 mm continuum survey at S/N_(1.1 mm) = 4\u22124.5. This paper presents, for the first time, interferometric millimetre-wavelength observations of these sources. The angular resolution of our observations, ~1.\"8, allowed us to accurately determine the positions of the target SMGs. Using a detection threshold of S/N_(1.3 mm)> 4.5 regardless of multiwavelength counterpart association, and 4", "date": "2015-05", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "577", "publisher": "EDP Sciences", "pagerange": "Art. No. A29", "id_number": "CaltechAUTHORS:20150605-105722803", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150605-105722803", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "SPLASH" } ] }, "doi": "10.1051/0004-6361/201425032", "primary_object": { "basename": "1502.05854v1.pdf", "url": "https://authors.library.caltech.edu/records/hcf9p-8k959/files/1502.05854v1.pdf" }, "related_objects": [ { "basename": "aa25032-14.pdf", "url": "https://authors.library.caltech.edu/records/hcf9p-8k959/files/aa25032-14.pdf" } ], "pub_year": "2015", "author_list": "Miettinen, O.; Smol\u010di\u0107, V.; et el." }, { "id": "https://authors.library.caltech.edu/records/2hwxy-caq72", "eprint_id": 57572, "eprint_status": "archive", "datestamp": "2023-08-22 15:19:46", "lastmod": "2023-10-23 17:32:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Buchner-J", "name": { "family": "Buchner", "given": "Johannes" }, "orcid": "0000-0003-0426-6634" }, { "id": "Georgakakis-A", "name": { "family": "Georgakakis", "given": "Antonis" } }, { "id": "Nandra-K", "name": { "family": "Nandra", "given": "Kirpal" }, "orcid": "0000-0002-7150-9192" }, { "id": "Brightman-M", "name": { "family": "Brightman", "given": "Murray" }, "orcid": "0000-0002-8147-2602" }, { "id": "Menzel-M-L", "name": { "family": "Menzel", "given": "Marie-Luise" } }, { "id": "Liu-Zhu", "name": { "family": "Liu", "given": "Zhu" }, "orcid": "0000-0002-8968-7050" }, { "id": "Hsu-Li-Ting", "name": { "family": "Hsu", "given": "Li-Ting" } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Rangel-C", "name": { "family": "Rangel", "given": "Cyprian" } }, { "id": "Aird-J-A", "name": { "family": "Aird", "given": "James" }, "orcid": "0000-0003-1908-8463" }, { "id": "Merloni-A", "name": { "family": "Merloni", "given": "Andrea" } }, { "id": "Ross-N-P", "name": { "family": "Ross", "given": "Nicholas" }, "orcid": "0000-0003-1830-6473" } ] }, "title": "Obscuration-dependent Evolution of Active Galactic Nuclei", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; quasars: supermassive black holes; surveys; X-rays: galaxies", "note": "\u00a9 2015 American Astronomical Society. Received 2014 October 7; accepted 2014 December 21; published 2015 March 26.\n\nJ.B. acknowledges financial support through a Max Planck\nsociety stipend. We thank the builders and operators of Chandra X-ray Observatory and XMM-Newton. This research has\nmade use of software provided by the Chandra X-ray Center\n(CXC) in the application package CIAO and Sherpa. Additionally, the CosmoloPy (http://roban.github.com/CosmoloPy/), BXA (https://johannesbuchner.github.io/BXA/), and pymultinest (https://johannesbuchner.github.io/PyMultiNest/) software packages were used. A.G.E. acknowledges the THALES project 383549, which is jointly funded by the European Union and the Greek Government\nin the framework of the program \"Education and Lifelong\nLearning.\"\nFunding for SDSS-III has been provided by the Alfred P.\nSloan Foundation, the Participating Institutions, the National\nScience Foundation, and the U.S. Department of Energy Office\nof Science. The SDSS-III Web site is http://www.sdss3.org/.\nSDSS-III is managed by the Astrophysical Research Consortium\nfor the Participating Institutions of the SDSS-III Collaboration.\n\nPublished - 0004-637X_802_2_89.pdf
Submitted - 1501.02805v2.pdf
", "abstract": "We aim to constrain the evolution of active galactic nuclei (AGNs) as a function of obscuration using an X-ray-selected sample of ~2000 AGNs from a multi-tiered survey including the CDFS, AEGIS-XD, COSMOS, and XMM-XXL fields. The spectra of individual X-ray sources are analyzed using a Bayesian methodology with a physically realistic model to infer the posterior distribution of the hydrogen column density and intrinsic X-ray luminosity. We develop a novel non-parametric method that allows us to robustly infer the distribution of the AGN population in X-ray luminosity, redshift, and obscuring column density, relying only on minimal smoothness assumptions. Our analysis properly incorporates uncertainties from low count spectra, photometric redshift measurements, association incompleteness, and the limited sample size. We find that obscured AGNs with N_H > 10^(22) cm^(\u20132) account for 77^(+4_(-5)% of the number density and luminosity density of the accretion supermassive black hole population with L_X > 10^(43) erg s^(\u20131), averaged over cosmic time. Compton-thick AGNs account for approximately half the number and luminosity density of the obscured population, and 38^(+8)_(-7)% of the total. We also find evidence that the evolution is obscuration dependent, with the strongest evolution around N_H \u2248 10^(23) cm^(\u20132). We highlight this by measuring the obscured fraction in Compton-thin AGNs, which increases toward z ~ 3, where it is 25% higher than the local value. In contrast, the fraction of Compton-thick AGNs is consistent with being constant at \u224835%, independent of redshift and accretion luminosity. We discuss our findings in the context of existing models and conclude that the observed evolution is, to first order, a side effect of anti-hierarchical growth.", "date": "2015-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "802", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 89", "id_number": "CaltechAUTHORS:20150515-151548160", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150515-151548160", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Max Planck Society" }, { "agency": "European Research Council (ERC)", "grant_number": "383549 THALES" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/802/2/89", "primary_object": { "basename": "1501.02805v2.pdf", "url": "https://authors.library.caltech.edu/records/2hwxy-caq72/files/1501.02805v2.pdf" }, "related_objects": [ { "basename": "0004-637X_802_2_89.pdf", "url": "https://authors.library.caltech.edu/records/2hwxy-caq72/files/0004-637X_802_2_89.pdf" } ], "pub_year": "2015", "author_list": "Buchner, Johannes; Georgakakis, Antonis; et el." }, { "id": "https://authors.library.caltech.edu/records/w5vx8-gb152", "eprint_id": 59434, "eprint_status": "archive", "datestamp": "2023-08-20 05:39:57", "lastmod": "2023-10-23 20:35:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Durkalec-A", "name": { "family": "Durkalec", "given": "A." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Stellar mass to halo mass relation from galaxy clustering in VUDS: a high star formation efficiency at z \u2243 3", "ispublished": "pub", "full_text_status": "public", "keywords": "large-scale structure of Universe \u2013 early Universe \u2013 galaxies: evolution \u2013 methods: statistical", "note": "\u00a9 2015 ESO. Article published by EDP Sciences. \n\nReceived 17 December 2014; Accepted 27 February 2015;\nPublished online 23 March 2015. \n\n\nWe thank Jean Coupon and Carlo Schimd for interesting discussions. This work is supported by the European Research Council Advanced Grant ERC-2010-AdG-268107-EARLY, and by INAF Grants PRIN 2010&2012 and PICS 2013. A.C., O.C., M.T. and V.S. acknowledge the grant MIUR PRIN 2010\u20132011. This work is supported by the OCEVU Labex (ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02). A.P. is supported by grant UMO-2012/07/B/ST9/04425 and the Polish-Swiss Astro Project. Research conducted within the scope of the HECOLS International Associated Laboratory, supported in part by the Polish NCN grant Dec-2013/08/M/ST9/00664. This work is based on data products made available at the CESAM data center, Laboratoire d'Astrophysique de Marseille, France.\n\nPublished - aa25532-14.pdf
Submitted - 1412.5584v1.pdf
", "abstract": "The relation between the galaxy stellar mass M\u22c6 and the dark matter halo mass M_h gives important information on the efficiency in forming stars and assembling stellar mass in galaxies. We present measurements of the ratio of stellar mass to halo mass (SMHR) at redshifts 2 < z < 5, obtained from the VIMOS Ultra Deep Survey. We use halo occupation distribution (HOD) modelling of clustering measurements on ~3000 galaxies with spectroscopic redshifts to derive the dark matter halo mass M_h, and spectral energy density fitting over a large set of multi-wavelength data to derive the stellar mass M\u22c6 and compute the SMHR = M\u22c6/M_h. We find that the SMHR ranges from 1% to 2.5% for galaxies with M\u22c6 = 1.3 \u00d7 10^9 M\u2299 to M\u22c6 = 7.4 \u00d7 10^9 M\u2299 in DM halos with M_h = 1.3 \u00d7 10^(11) M\u2299 to M_h = 3 \u00d7 10^(11) M\u2299. We derive the integrated star formation efficiency (ISFE) of these galaxies and find that the star formation efficiency is a moderate 6\u22129% for lower mass galaxies, while it is relatively high at 16% for galaxies with the median stellar mass of the sample ~ 7 \u00d7 10^9 M\u2299. The lower ISFE at lower masses may indicate that some efficient means of suppressing star formation is at work (like SNe feedback), while the high ISFE for the average galaxy at z ~ 3 indicates that these galaxies efficiently build up their stellar mass at a key epoch in the mass assembly process. Based on our results, we propose a possible scenario in which the average massive galaxy at z ~ 3 begins to experience truncation of its star formation within a few million years.", "date": "2015-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "576", "publisher": "EDP Sciences", "pagerange": "Art. No. L7", "id_number": "CaltechAUTHORS:20150812-083009200", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150812-083009200", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "ERC-2010-AdG-268107-EARLY" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2010" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2012" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PICS 2013" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)", "grant_number": "PRIN 2010\u20132011" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-11-LABX-0060" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-11-IDEX-0001-02" }, { "agency": "National Science Center", "grant_number": "UMO-2012/07/B/ST9/04425" }, { "agency": "Polish-Swiss Astro Project" }, { "agency": "Polish NCN", "grant_number": "Dec-2013/08/M/ST9/00664" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201425532", "primary_object": { "basename": "1412.5584v1.pdf", "url": "https://authors.library.caltech.edu/records/w5vx8-gb152/files/1412.5584v1.pdf" }, "related_objects": [ { "basename": "aa25532-14.pdf", "url": "https://authors.library.caltech.edu/records/w5vx8-gb152/files/aa25532-14.pdf" } ], "pub_year": "2015", "author_list": "Durkalec, A.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/qvk7b-b2b57", "eprint_id": 59351, "eprint_status": "archive", "datestamp": "2023-08-22 15:17:37", "lastmod": "2023-10-23 20:28:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Cooper-M-C", "name": { "family": "Cooper", "given": "M." }, "orcid": "0000-0003-1371-6019" }, { "id": "Allevato-V", "name": { "family": "Allevato", "given": "V." } }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "N." } }, { "id": "Choi-A", "name": { "family": "Choi", "given": "A." } }, { "id": "Heymans-C", "name": { "family": "Heymans", "given": "C." } }, { "id": "Bauer-F-E", "name": { "family": "Bauer", "given": "F. E." }, "orcid": "0000-0002-8686-8737" }, { "id": "Ziparo-F", "name": { "family": "Ziparo", "given": "F." } }, { "id": "Ranalli-P", "name": { "family": "Ranalli", "given": "P." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Brandt-W-N", "name": { "family": "Brandt", "given": "W. N." }, "orcid": "0000-0002-0167-2453" }, { "id": "Xue-Y-Q", "name": { "family": "Xue", "given": "Y. Q." } }, { "id": "Mulchaey-J-S", "name": { "family": "Mulchaey", "given": "J." } }, { "id": "Howes-Louise", "name": { "family": "Howes", "given": "L." }, "orcid": "0000-0003-0117-0231" }, { "id": "Schmid-C", "name": { "family": "Schmid", "given": "C." } }, { "id": "Wilman-D", "name": { "family": "Wilman", "given": "D." } }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Luo-Bin", "name": { "family": "Luo", "given": "B." }, "orcid": "0000-0002-9036-0063" }, { "id": "Tozzi-P", "name": { "family": "Tozzi", "given": "P." } }, { "id": "Rosati-P", "name": { "family": "Rosati", "given": "P." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Popesso-P", "name": { "family": "Popesso", "given": "P." } } ] }, "title": "Ultra-deep catalog of X-ray groups in the Extended Chandra Deep Field South", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: weak; X-rays: galaxies: clusters; large-scale structure of Universe", "note": "\u00a9 2015 ESO. Article published by EDP Sciences. \n\nReceived 14 November 2013; Accepted 31 January 2015; Published online 17 April 2015. \n\nThis work has been partially supported through a SAO grant SP1-12006B to UMBC. W.N.B. thanks Chandra grant SP1-12007A and NASA ADP grant NNX10AC99G. A.F. and V.A. wish to acknowledge Finnish Academy award, decision 266918. M.T. acknowledges support by KAKENHI No. 23740144. P.R. acknowledges a grant from the Greek General Secretariat of Research and Technology in the framework of the programme Support of Postdoctoral Researchers. A.C. and C.H. acknowledge support from the European Research Council under the EC FP7 grant number 240185. J.S.M. acknowledges partial support from Chandra grant SP1-12006A. C.S. acknowledges support by DLR grants 50QR1103 and 50QR0803. Y.Q.X. acknowledges support of the Thousand Young Talents program (KJ2030220004), the 973 Program (2015CB857004), the USTC startup funding (ZC9850290195), the National Natural Science Foundation of China (NSFC-11473026, 11421303), and the Strategic Priority Research Program \"The Emergence of Cosmological Structures\" of the Chinese Academy of Sciences (XDB09000000). F.E.B. acknowledges support from Basal-CATA PFB-06/2007, CONICYT-Chile (FONDECYT 1141218, ALMA-CONICYT 31100004, Gemini-CONICYT 32120003, \"EMBIGGEN\" Anillo ACT1101), and Project IC120009 \"Millennium Institute of Astrophysics (MAS)\" of Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo.\n\nPublished - aa23053-13.pdf
Submitted - 1501.03506v2.pdf
", "abstract": "Aims. We present the detection, identification and calibration of extended sources in the deepest X-ray dataset to date, the Extended Chandra Deep Field South (ECDF-S).\nMethods. Ultra-deep observations of ECDF-S with Chandra and XMM-Newton enable a search for extended X-ray emission down to an unprecedented flux of 2 \u00d7 10^(-16) ergs\u2009s^(-1) cm^(-2). By using simulations and comparing them with the Chandra and XMM data, we show that it is feasible to probe extended sources of this flux level, which is 10\u2009000 times fainter than the first X-ray group catalogs of the ROSAT all sky survey. Extensive spectroscopic surveys at the VLT and Magellan have been completed, providing spectroscopic identification of galaxy groups to high redshifts. Furthermore, available HST imaging enables a weak-lensing calibration of the group masses.\nResults. We present the search for the extended emission on spatial scales of 32\u2032\u2032 in both Chandra and XMM data, covering 0.3 square degrees and model the extended emission on scales of arcminutes. We present a catalog of 46 spectroscopically identified groups, reaching a redshift of 1.6. We show that the statistical properties of ECDF-S, such as log\u2009 N \u2212 log\u2009 S and X-ray luminosity function are broadly consistent with LCDM, with the exception that dn/dz/d\u03a9 test reveals that a redshift range of 0.2 < z < 0.5 in ECDF-S is sparsely populated. The lack of nearby structure, however, makes studies of high-redshift groups particularly easier both in X-rays and lensing, due to a lower level of clustered foreground. We present one and two point statistics of the galaxy groups as well as weak-lensing analysis to show that the detected low-luminosity systems are indeed low-mass systems. We verify the applicability of the scaling relations between the X-ray luminosity and the total mass of the group, derived for the COSMOS survey to lower masses and higher redshifts probed by ECDF-S by means of stacked weak lensing and clustering analysis, constraining any possible departures to be within 30% in mass.\nConclusions. Ultra-deep X-ray surveys uniquely probe the low-mass galaxy groups across a broad range of redshifts. These groups constitute the most common environment for galaxy evolution. Together with the exquisite data set available in the best studied part of the Universe, the ECDF-S group catalog presented here has an exceptional legacy value.", "date": "2015-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "576", "publisher": "EDP Sciences", "pagerange": "Art. No. A130", "id_number": "CaltechAUTHORS:20150810-103143722", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150810-103143722", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Smithsonian Astrophysical Observatory", "grant_number": "SP1-12006B" }, { "agency": "NASA", "grant_number": "SP1-12007A" }, { "agency": "NASA", "grant_number": "NNX10AC99G" }, { "agency": "Academy of Finland", "grant_number": "266918" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23740144" }, { "agency": "General Secretariat of Research and Technology (GSRT)" }, { "agency": "European Research Council (ERC)", "grant_number": "240185" }, { "agency": "NASA", "grant_number": "SP1-12006A" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50QR1103" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50QR0803" }, { "agency": "Thousand Young Talents program", "grant_number": "KJ2030220004" }, { "agency": "National Basic Research Program of China 973 Program", "grant_number": "2015CB857004" }, { "agency": "USTC", "grant_number": "ZC9850290195" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11473026" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11421303" }, { "agency": "Chinese Academy of Sciences", "grant_number": "XDB09000000" }, { "agency": "Basal-CATA", "grant_number": "PFB-06/2007" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1141218" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "31100004" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "32120003" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "ACT1101" }, { "agency": "Iniciativa Cient\u00edfica Milenio (ICM) del Ministerio de Econom\u00eda", "grant_number": "IC120009" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201323053", "primary_object": { "basename": "1501.03506v2.pdf", "url": "https://authors.library.caltech.edu/records/qvk7b-b2b57/files/1501.03506v2.pdf" }, "related_objects": [ { "basename": "aa23053-13.pdf", "url": "https://authors.library.caltech.edu/records/qvk7b-b2b57/files/aa23053-13.pdf" } ], "pub_year": "2015", "author_list": "Finoguenov, A.; Tanaka, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/ha955-qhs96", "eprint_id": 55824, "eprint_status": "archive", "datestamp": "2023-08-20 05:35:34", "lastmod": "2023-10-20 23:15:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The VIMOS Ultra-Deep Survey: \u223c10 000 galaxies with spectroscopic redshifts to study galaxy assembly at early epochs 2 < z \u2243 6", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxies: evolution, Galaxies: formation, Galaxies: high redshift, Cosmology: observations, Cosmology: large-scale\nstructure of Universe, Astronomical Databases: surveys", "note": "\u00a9 2015 ESO.\nArticle published by EDP Sciences.\n\nBased on data obtained with the European Southern Observatory\nVery Large Telescope, Paranal, Chile, under Large Program 185.A-0791.\n\nWe thank the ESO staff for their continuous support for the\nVUDS survey, particularly the Paranal staff, who conduct the observations, and\nMarina Rejkuba and the ESO user support group in Garching. This work is supported\nby funding from the European Research Council Advanced Grant ERC-\n2010-AdG-268107-EARLY and by INAF Grants PRIN 2010, PRIN 2012 and\nPICS 2013. A.C., O.C., M.T. and V.S. acknowledge the grant MIUR PRIN 2010\u2013\n2011. D.M. gratefully acknowledges LAM hospitality during the initial phases of\nthe project. This work is based on data products made available at the CESAM\ndata center, Laboratoire d'Astrophysique de Marseille. This work partly uses observations obtained with MegaPrime/MegaCam, a joint project of CFHT and\nCEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated\nby the National Research Council (NRC) of Canada, the Institut National\ndes Sciences de l'Univers of the Centre National de la Recherche Scientifique\n(CNRS) of France, and the University of Hawaii. This work is based in part on\ndata products produced at TERAPIX and the Canadian Astronomy Data Centre\nas part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative\nproject of NRC and CNRS.\n\nPublished - aa23829-14.pdf
Submitted - 1403.3938v1.pdf
", "abstract": "We present the VIMOS Ultra Deep Survey (VUDS), a spectroscopic redshift survey of \u223c10 000 very faint galaxies to study the major phase of galaxy assembly 2 < z \u2243 6. The survey covers 1 deg^2 in 3 separate fields: COSMOS, ECDFS and VVDS-02h, with targets selection based on an inclusive combination of photometric redshifts and color properties. Spectra covering 3650 < \u03bb < 9350\u00c5 are\nobtained with VIMOS on the ESO-VLT with integration times of 14h. Here we present the survey strategy, the target selection, the data processing, as well as the redshift measurement process, emphasizing the specific methods adapted to this high redshift range. The spectra quality and redshift reliability are discussed, and we derive a completeness in redshift measurement of 91%, or 74% for\nthe most reliable measurements, down to i_(AB) = 25, and measurements are performed all the way down to i_(AB) = 27. The redshift distribution of the main sample peaks at z = 3 \u2212 4 and extends over a large redshift range mainly in 2 < z < 6. At 3 < z < 5, the galaxies cover a large range of luminosities \u221223 < M_(NUV) < \u221220.5, stellar mass 10^9M_\u2299 < M_\u2217 < 10^(11)M_\u2299, and star formation rates 1 M_\u2299/yr< S FR < 10^3M_\u2299/yr. We discuss the spectral properties of galaxies using individual as well as stacked spectra. The comparison between spectroscopic and photometric redshifts as well as color selection demonstrate the effectiveness of our selection scheme. With \u223c 6000 galaxies with reliable spectroscopic redshifts in 2 < z < 6 expected when complete, this survey is the largest at these redshifts and offers the opportunity for unprecedented studies of the star-forming galaxy population and its distribution in large scale structures during the major phase of galaxy assembly.", "date": "2015-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "576", "publisher": "EDP Sciences", "pagerange": "Art. No. A79", "id_number": "CaltechAUTHORS:20150317-075810913", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150317-075810913", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council", "grant_number": "ERC-2010-AdG-268107-EARLY" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-2010" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2012" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PICS-2013" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 della Ricerca (MIUR)", "grant_number": "PRIN 2010\u20132011" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201423829", "primary_object": { "basename": "1403.3938v1.pdf", "url": "https://authors.library.caltech.edu/records/ha955-qhs96/files/1403.3938v1.pdf" }, "related_objects": [ { "basename": "aa23829-14.pdf", "url": "https://authors.library.caltech.edu/records/ha955-qhs96/files/aa23829-14.pdf" } ], "pub_year": "2015", "author_list": "Le F\u00e8vre, O.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/hx5w8-a1c68", "eprint_id": 58900, "eprint_status": "archive", "datestamp": "2023-08-20 05:39:17", "lastmod": "2023-10-23 19:51:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Bourke-S-A", "name": { "family": "Bourke", "given": "S." } }, { "id": "Hallinan-G", "name": { "family": "Hallinan", "given": "G." }, "orcid": "0000-0002-7083-4049" }, { "id": "Mooley-Kunal-Prakash", "name": { "family": "Mooley", "given": "K." }, "orcid": "0000-0002-2557-5180" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" } ] }, "title": "Physical properties of z > 4 submillimeter galaxies in the COSMOS field", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys \u2013 galaxies: high-redshift \u2013 galaxies: starburst \u2013 radio continuum: galaxies \u2013 submillimeter: galaxies", "note": "\u00a9 2015 ESO. Article published by EDP Sciences. \n\nReceived 16 September 2014; Accepted 3 December 2014; Published online 17 April 2015. \n\nWe thank the referee for insightful comments on the manuscript. This research was funded by the European Union's Seventh Framework program under grant agreement 337595 (ERC Starting Grant, \"CoSMass\"). A.K. acknowledges support by the Collaborative Research Council 956, subproject A1, funded by the Deutsche Forschungsgemeinschaft (DFG). The Dark Cosmology Centre is funded by the Danish National Research Foundation. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nPublished - aa24996-14.pdf
Submitted - 1412.3799v3.pdf
", "abstract": "We investigate the physical properties of a sample of six submillimeter galaxies (SMGs) in the COSMOS field, spectroscopically confirmed to lie at redshifts z> 4. While the redshifts for four of these SMGs were previously known, we present here two newly discovered z_(spec)> 4 SMGs. For our analysis we employ the rich (X-ray to radio) COSMOS multi-wavelength datasets. In particular, we use new data from the Giant Meterwave Radio Telescope (GMRT) 325 MHz and 3 GHz Jansky Very Large Array (VLA) to probe the rest-frame 1.4 GHz emission at z = 4, and to estimate the sizes of the star formation regions of these sources, respectively. We find that only oneSMG is clearly resolved at a resolution of 0''\u03236 \u00d7 0''\u03237 at 3 GHz, two may be marginally resolved, while the remaining three SMGs are unresolved at this resolution. Combining this with sizes from high-resolution (sub-)mm observations available in the literature for AzTEC 1 and AzTEC 3 we infer a median radio-emitting size for our z> 4 SMGs of (0''\u032363 \u00b1 0''\u032312) \u00d7 (0''\u032335 \u00b1 0''\u032305) or 4.1 \u00d7 2.3 kpc^2 (major \u00d7 minor axis; assuming z = 4.5) or lower if we take the two marginally resolved SMGs as unresolved. This is consistent with the sizes of star formation regions in lower-redshift SMGs, and local normal galaxies, yet higher than the sizes of star formation regions of local ultraluminous infrared galaxies (ULIRGs). Our SMG sample consists of a fair mix of compact and more clumpy systems with multiple, perhaps merging, components. With an average formation time of ~280 Myr, as derived through modeling of the UV IR spectral energy distributions, the studied SMGs are young systems. The average stellar mass, dust temperature, and IR luminosity we derive are M\u22c6 ~ 1.4 \u00d7 10^(11) M\u2299, T_(dust) ~ 43 K, and L_(IR) ~ 1.3 \u00d7 10^(13)L\u2299, respectively. The average L_(IR) is up to an order of magnitude higher than for SMGs at lower redshifts. Our SMGs follow the correlation between dust temperature and IR luminosity as derived for Herschel-selected 0.1 4 SMGs put them at the high end of the L_(IR)\u2013T_(dust) distribution of SMGs, and that our SMGs form a morphologically heterogeneous sample. Thus, additional in-depth analyses of large, statistical samples of high-redshift SMGs are needed to fully understand their role in galaxy formation and evolution.", "date": "2015-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "576", "publisher": "EDP Sciences", "pagerange": "Art. No. A127", "id_number": "CaltechAUTHORS:20150715-155646132", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150715-155646132", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "Collaborative Research Council 956" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "Danish National Research Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201424996", "primary_object": { "basename": "1412.3799v3.pdf", "url": "https://authors.library.caltech.edu/records/hx5w8-a1c68/files/1412.3799v3.pdf" }, "related_objects": [ { "basename": "aa24996-14.pdf", "url": "https://authors.library.caltech.edu/records/hx5w8-a1c68/files/aa24996-14.pdf" } ], "pub_year": "2015", "author_list": "Smol\u010di\u0107, V.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/1pkq4-kz545", "eprint_id": 56955, "eprint_status": "archive", "datestamp": "2023-08-22 15:11:58", "lastmod": "2023-10-23 16:10:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Diener-C", "name": { "family": "Diener", "given": "C." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Ledoux-C", "name": { "family": "Ledoux", "given": "C." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Murphy-D-N-A", "name": { "family": "Murphy", "given": "D. N. A." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" } ] }, "title": "A Protocluster at z = 2.45", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general; galaxies: high-redshift", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2014 November 3; accepted 2014 December 29; published 2015 March 18. \n\nThis research has been supported by the Swiss National Science Foundation (SNF) and the European Southern Observatory (ESO). It is based on observations undertaken at the ESO Very Large Telescope (VLT) under Program 290.A-5160(A). It also uses data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO program ID 179.A-2005 and data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. The Millennium simulation databases used in this paper and the Web application providing online access to them were constructed as part of the activities of the German Astrophysical Virtual Observatory.\n\nPublished - 0004-637X_802_1_31.pdf
Submitted - 1411.0649v2.pdf
", "abstract": "We present the spectroscopic confirmation of a z = 2.45 protocluster. Its member galaxies lie within a radius of 1.4 Mpc (physical) on the sky and within \u0394v \u00b1 700 km^(-1) along the line of sight. We estimate an overdensity of 10, suggesting that the structure has made the turnaround but is not assembled yet. A comparison to the Millennium simulation suggests that analogous structures evolve into 10^(14)\u201310^(15) M_\u2299h^(\u22121) type dark matter halos by z = 0, qualifying the notion of \"protocluster.\" The search for the complete census of mock progenitor galaxies at z ~ 2.5 of these massive z = 0 mock clusters reveals that they are widely spread over areas with a diameter of 3\u201320 Mpc. This suggests that the optical selection of such protoclusters can result in a rich diversity regarding their z = 0 descendants. We also searched for signs of environmental differentiation in this protocluster. While we see a weak trend for more massive and more quiescent galaxies within the protocluster, this is not statistically significant.", "date": "2015-03-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "802", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 31", "id_number": "CaltechAUTHORS:20150424-115610914", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150424-115610914", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "European Southern Observatory" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/802/1/31", "primary_object": { "basename": "0004-637X_802_1_31.pdf", "url": "https://authors.library.caltech.edu/records/1pkq4-kz545/files/0004-637X_802_1_31.pdf" }, "related_objects": [ { "basename": "1411.0649v2.pdf", "url": "https://authors.library.caltech.edu/records/1pkq4-kz545/files/1411.0649v2.pdf" } ], "pub_year": "2015", "author_list": "Diener, C.; Lilly, S. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/febp6-b3526", "eprint_id": 56727, "eprint_status": "archive", "datestamp": "2023-08-22 15:09:02", "lastmod": "2023-10-23 15:46:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "Nicholas" } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Casey-C-M", "name": { "family": "Casey", "given": "Caitlin M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Toft-S", "name": { "family": "Toft", "given": "Sune" }, "orcid": "0000-0003-3631-7176" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Hung-Chao-Ling", "name": { "family": "Hung", "given": "Chao-Ling" }, "orcid": "0000-0002-6879-3639" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "Emeric" } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Zahid-H-J", "name": { "family": "Zahid", "given": "H. Jabran" } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "Herve" }, "orcid": "0000-0002-1371-5705" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "Jeyhan S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Kewley-L-J", "name": { "family": "Kewley", "given": "Lisa J." }, "orcid": "0000-0001-8152-3943" }, { "id": "Li-Yanxia", "name": { "family": "Li", "given": "Yanxia" } }, { "id": "Schawinski-K", "name": { "family": "Schawinski", "given": "Kevin" }, "orcid": "0000-0001-5464-0888" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Xiao-Quanbao", "name": { "family": "Xiao", "given": "Quanbao" } } ] }, "title": "A Turnover in the Galaxy Main Sequence of Star Formation at M_* ~ 10^(10) M_\u2609 for Redshifts z < 1.3", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: star formation", "note": "\u00a9 2015 American Astronomical Society. Received 2014 July 29; accepted 2015 January 5; published 2015 March 5.\n\nD.B.S. and C.M.C. acknowledge the hospitality of the Aspen Center for Physics, which is supported by the National Science Foundation grant No. PHY-1066293. C.M.C. acknowledges generous support from a McCue Fellowship through the University of California, Irvine's Center for Cosmology. K.S. gratefully acknowledges support from Swiss National Science Foundation Grant PP00P2_138979/1. K.S. acknowledges support from the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. COSMOS is based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc, under NASA contract NAS 5-26555; also based on data collected at: the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc;\nand the Canada\u2013France\u2013Hawaii Telescope operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France and the University of Hawaii. The Dark Cosmology Centre is funded by the Danish National Research Foundation.\n\nPublished - 0004-637X_801_2_80.pdf
Submitted - 1501.01080v1.pdf
", "abstract": "The relationship between galaxy star formation rates (SFRs) and stellar masses (M_*) is reexamined using a mass-selected sample of ~62,000 star-forming galaxies at z \u2264 1.3 in the COSMOS 2 deg^2 field. Using new far-infrared photometry from Herschel-PACS and SPIRE and Spitzer-MIPS 24 \u03bcm, along with derived infrared luminosities from the NRK method based on galaxies' locations in the restframe color-color diagram (NUV \u2013 r) versus (r \u2013 K), we are able to more accurately determine total SFRs for our complete sample. At all redshifts, the relationship between median SFR and M_* follows a power law at low stellar masses, and flattens to nearly constant SFR at high stellar masses. We describe a new parameterization that provides the best fit to the main sequence and characterizes the low mass power-law slope, turnover mass, and overall scaling. The turnover in the main sequence occurs at a characteristic mass of about M_0 ~ 10^(10) M_\u2609 at all redshifts. The low mass power-law slope ranges from 0.9-1.3 and the overall scaling rises in SFR as a function of (1 + z)^(4.12\u00b10.10). A broken power-law fit below and above the turnover mass gives relationships of SFR \u221d M_*^(0.88\u00b10.06) below the turnover mass and SFR \u221d M_*^(0.27\u00b10.04) above the turnover mass. Galaxies more massive than M_* \u2273 10^(10) M_\u2609 have a much lower average specific star formation rate (sSFR) than would be expected by simply extrapolating the traditional linear fit to the main sequence found for less massive galaxies.", "date": "2015-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "801", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 80", "id_number": "CaltechAUTHORS:20150416-115610730", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150416-115610730", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "University of California, Irvine" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "PP00P2_138979/1" }, { "agency": "National Radio Astronomy Observatory" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "ESA Member States" }, { "agency": "European Southern Observatory (Chile)" }, { "agency": "Kitt Peak National Observatory" }, { "agency": "Cerro Tololo Inter-American Observatory" }, { "agency": "National Optical Astronomy Observatory" }, { "agency": "Danish National Research Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "SPLASH" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/801/2/80", "primary_object": { "basename": "0004-637X_801_2_80.pdf", "url": "https://authors.library.caltech.edu/records/febp6-b3526/files/0004-637X_801_2_80.pdf" }, "related_objects": [ { "basename": "1501.01080v1.pdf", "url": "https://authors.library.caltech.edu/records/febp6-b3526/files/1501.01080v1.pdf" } ], "pub_year": "2015", "author_list": "Lee, Nicholas; Sanders, D. B.; et el." }, { "id": "https://authors.library.caltech.edu/records/pydxa-b2h96", "eprint_id": 57774, "eprint_status": "archive", "datestamp": "2023-08-22 15:05:02", "lastmod": "2023-10-23 17:44:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hanish-D-J", "name": { "family": "Hanish", "given": "D. J." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H. I." }, "orcid": "0000-0002-7064-5424" }, { "id": "Desai-V", "name": { "family": "Desai", "given": "V." }, "orcid": "0000-0002-1340-0543" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Brinkworth-C-S", "name": { "family": "Brinkworth", "given": "C." } }, { "id": "Brooke-T-Y", "name": { "family": "Brooke", "given": "T." } }, { "id": "Colbert-J-W", "name": { "family": "Colbert", "given": "J." } }, { "id": "Edwards-L", "name": { "family": "Edwards", "given": "L." } }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Huynh-Minh-T", "name": { "family": "Huynh", "given": "M." } }, { "id": "Lacy-M", "name": { "family": "Lacy", "given": "M." }, "orcid": "0000-0002-3032-1783" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E." }, "orcid": "0000-0001-7089-7325" }, { "id": "Noriega-Crespo-A", "name": { "family": "Noriega-Crespo", "given": "A." }, "orcid": "0000-0002-6296-8960" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Shenoy-S-S", "name": { "family": "Shenoy", "given": "S." } } ] }, "title": "The Spitzer Archival Far-Infrared Extragalactic Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: galaxies; surveys", "note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2013 June 21; accepted 2014 December 15; published 2015 March 24.\n\nSupport for this work was provided by NASA through\ncontract NASA-ADAP NNX10AD52G. This publication makes use of raw data from the Spitzer Space Telescope, operated by the Jet Propulsion Laboratory/California Institute of Technology under NASA contract, as well as data products from the Two Micron All Sky Survey, a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF.\n\nPublished - 0067-0049_217_1_17.pdf
Submitted - 1503.08567v1.pdf
", "abstract": "We present the Spitzer Archival Far-InfraRed Extragalactic Survey (SAFIRES). This program produces refined mosaics and source lists for all far-infrared (FIR) extragalactic data taken during the more than six years of the cryogenic operation of the Spitzer Space Telescope. The SAFIRES products consist of FIR data in two wavelength bands (70 and 160 \u03bcm) across approximately 180 square degrees of sky, with source lists containing far-infrared fluxes for almost 40,000 extragalactic point sources. Thus, SAFIRES provides a large, robust archival far-infrared data set suitable for many scientific goals.", "date": "2015-03", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "217", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 17", "id_number": "CaltechAUTHORS:20150522-100203505", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150522-100203505", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX10AD52G" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0067-0049/217/1/17", "primary_object": { "basename": "0067-0049_217_1_17.pdf", "url": "https://authors.library.caltech.edu/records/pydxa-b2h96/files/0067-0049_217_1_17.pdf" }, "related_objects": [ { "basename": "1503.08567v1.pdf", "url": "https://authors.library.caltech.edu/records/pydxa-b2h96/files/1503.08567v1.pdf" } ], "pub_year": "2015", "author_list": "Hanish, D. J.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/2fvbx-ay656", "eprint_id": 56541, "eprint_status": "archive", "datestamp": "2023-08-20 05:01:48", "lastmod": "2023-10-23 15:32:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Novak-Mladen", "name": { "family": "Novak", "given": "Mladen" }, "orcid": "0000-0001-8695-825X" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "Vernesa" }, "orcid": "0000-0002-3893-8614" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "Francesca" }, "orcid": "0000-0002-2115-1137" }, { "id": "Bondi-Marco", "name": { "family": "Bondi", "given": "Marco" } }, { "id": "Ciliegi-P", "name": { "family": "Ciliegi", "given": "Paolo" } }, { "id": "Wang-Xiawei", "name": { "family": "Wang", "given": "Xiawei" } }, { "id": "Loeb-A", "name": { "family": "Loeb", "given": "Abraham" }, "orcid": "0000-0003-4330-287X" }, { "id": "Banfield-J", "name": { "family": "Banfield", "given": "Julie" } }, { "id": "Bourke-S-A", "name": { "family": "Bourke", "given": "Stephen" } }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "id": "Hallinan-G", "name": { "family": "Hallinan", "given": "Gregg" }, "orcid": "0000-0002-7083-4049" }, { "id": "Intema-H-T", "name": { "family": "Intema", "given": "Huib T." }, "orcid": "0000-0002-5880-2730" }, { "id": "Kl\u00f6ckner-H-R", "name": { "family": "Kl\u00f6ckner", "given": "Hans-Rainer" } }, { "id": "Mooley-Kunal-Prakash", "name": { "family": "Mooley", "given": "Kunal" }, "orcid": "0000-0002-2557-5180" }, { "id": "Navarrete-F", "name": { "family": "Navarrete", "given": "Felipe" } } ] }, "title": "New insights from deep VLA data on the potentially recoiling black hole CID-42 in the COSMOS field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active\n galaxies: individual: CID-42\n galaxies: interactions\n galaxies: nuclei\n radio continuum: galaxies", "note": "\u00a9 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2014 November 20. Received 2014 November 19; in original form 2014 September 25. First published online December 24, 2014.\n\nWe thank the anonymous referee for providing helpful comments which improved the paper. This research was funded by the European Union's Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, CoSMass). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nPublished - MNRAS-2015-Novak-1282-8.pdf
Submitted - 1412.0004v1.pdf
", "abstract": "We present deep 3-GHz Karl G. Jansky Very Large Array (VLA) observations of the potentially recoiling black hole CID-42 in the Cosmic Evolution Survey (COSMOS) field. This galaxy shows two optical nuclei in the Hubble Space Telescope/Advanced Camera for Surveys (HST/ACS) image and a large velocity offset of \u22481300 km s^(\u22121) between the broad and narrow H\u03b2 emission line although the spectrum is not spacially resolved (Civano et al. 2010). The new 3 GHz VLA data have a bandwidth of 2 GHz and to correctly interpret the flux densities imaging was done with two different methods: multiscale multifrequency (MSMF) synthesis and spectral windows (SPWs) stacking. The final resolutions and sensitivities of these maps are 0.7 arcsec with rms = 4.6\u2009\u03bcJy beam^(\u22121) and 0.9 arcsec with rms = 4.8\u2009\u03bcJy beam^(\u22121), respectively. With a 7\u03c3 detection, we find that the entire observed 3-GHz radio emission can be associated with the south-eastern component of CID-42, coincident with the detected X-ray emission. We use our 3 GHz data combined with other radio data from the literature ranging from 320 MHz to 9 GHz, which include the VLA, Very Long Baseline Array (VLBA) and Giant Metrewave Radio Telescope (GMRT) data, to construct a radio synchrotron spectrum of CID-42. The radio spectrum suggests a type I unobscured radio-quiet flat-spectrum active galactic nucleus (AGN) in the south-eastern component which may be surrounded by a more extended region of old synchrotron electron population or shocks generated by the outflow from the supermassive black hole (SMBH). Our data are consistent with the recoiling black hole picture but cannot rule out the presence of an obscured and radio-quiet SMBH in the north-western component.", "date": "2015-02-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "447", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1282-1288", "id_number": "CaltechAUTHORS:20150409-133259758", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150409-133259758", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "337595" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stu2473", "primary_object": { "basename": "1412.0004v1.pdf", "url": "https://authors.library.caltech.edu/records/2fvbx-ay656/files/1412.0004v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2015-Novak-1282-8.pdf", "url": "https://authors.library.caltech.edu/records/2fvbx-ay656/files/MNRAS-2015-Novak-1282-8.pdf" } ], "pub_year": "2015", "author_list": "Novak, Mladen; Smol\u010di\u0107, Vernesa; et el." }, { "id": "https://authors.library.caltech.edu/records/deaqf-62664", "eprint_id": 55987, "eprint_status": "archive", "datestamp": "2023-08-22 14:59:39", "lastmod": "2023-10-20 23:31:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "Andreas" }, "orcid": "0000-0002-9382-9832" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Kakazu-Yuko", "name": { "family": "Kakazu", "given": "Yuko" } }, { "id": "Li-Gongjie", "name": { "family": "Li", "given": "Gongjie" }, "orcid": "0000-0001-8308-0808" }, { "id": "Steinhardt-C-L", "name": { "family": "Steinhardt", "given": "Charles L." }, "orcid": "0000-0003-3780-6801" } ] }, "title": "Dust Attenuation in High Redshift Galaxies: \"Diamonds in the Sky\"", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; dust, extinction; Galaxy: evolution; galaxies: high-redshift; ISM: clouds", "note": "\u00a9 2015 American Astronomical Society. Received 2014 October 27; accepted 2014 December 27; published 2015 February 18.\n\nWe thank the referee for suggestions and Martin Elvis for\ncomments on an early draft. We also thank Zara Scoville for\nproofreading the manuscript. A.F. acknowledges support from\nthe Swiss National Science Foundation and thanks Caltech for\nhospitality while working on this article.\n\nPublished - 0004-637X_800_2_108.pdf
Submitted - 1412.8219v1.pdf
", "abstract": "We use observed optical to near-infrared spectral energy distributions (SEDs) of 266 galaxies in the COSMOS survey to derive the wavelength dependence of the dust attenuation at high redshift. All of the galaxies have spectroscopic redshifts in the range z = 2-6.5. The presence of the C IV absorption feature, indicating that the rest-frame UV-optical SED is dominated by OB stars, is used to select objects for which the intrinsic, unattenuated spectrum has a well-established shape. Comparison of this intrinsic spectrum with the observed broadband photometric SED then permits derivation of the wavelength dependence of the dust attenuation. The derived dust attenuation curve is similar in overall shape to the Calzetti curve for local starburst galaxies. We also see the 2175 \u00c5 bump feature which is present in the Milky Way and Large Magellanic Cloud extinction curves but not seen in the Calzetti curve. The bump feature is commonly attributed to graphite or polycyclic aromatic hydrocarbons. No significant dependence is seen with redshift between sub-samples at z = 2-4 and z = 4-6.5. The \"extinction\" curve obtained here provides a firm basis for color and extinction corrections of high redshift galaxy photometry.", "date": "2015-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "800", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 108", "id_number": "CaltechAUTHORS:20150323-145007978", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150323-145007978", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swiss National Science Foundation (SNSF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "SPLASH" } ] }, "doi": "10.1088/0004-637X/800/2/108", "primary_object": { "basename": "0004-637X_800_2_108.pdf", "url": "https://authors.library.caltech.edu/records/deaqf-62664/files/0004-637X_800_2_108.pdf" }, "related_objects": [ { "basename": "1412.8219v1.pdf", "url": "https://authors.library.caltech.edu/records/deaqf-62664/files/1412.8219v1.pdf" } ], "pub_year": "2015", "author_list": "Scoville, Nick; Faisst, Andreas; et el." }, { "id": "https://authors.library.caltech.edu/records/20jsw-vgw93", "eprint_id": 56368, "eprint_status": "archive", "datestamp": "2023-08-20 04:56:51", "lastmod": "2023-10-23 15:21:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cheung-Edmund", "name": { "family": "Cheung", "given": "Edmond" } }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "Jonathan R." } }, { "id": "Athanassoula-E", "name": { "family": "Athanassoula", "given": "E." } }, { "id": "Bamford-S-P", "name": { "family": "Bamford", "given": "Steven P." }, "orcid": "0000-0001-7821-7195" }, { "id": "Bell-E-F", "name": { "family": "Bell", "given": "Eric F." } }, { "id": "Bosma-A", "name": { "family": "Bosma", "given": "A." } }, { "id": "Cardamone-C-N", "name": { "family": "Cardamone", "given": "Carolin N." } }, { "id": "Casteels-K-R", "name": { "family": "Casteels", "given": "Kevin R." } }, { "id": "Faber-S-M", "name": { "family": "Faber", "given": "S. M." }, "orcid": "0000-0003-4996-214X" }, { "id": "Fang-Jerome-J", "name": { "family": "Fang", "given": "Jerome J." } }, { "id": "Fortson-L-F", "name": { "family": "Fortson", "given": "Lucy F." }, "orcid": "0000-0002-1067-8558" }, { "id": "Kocevski-D-D", "name": { "family": "Kocevski", "given": "Dale D." } }, { "id": "Koo-David-C", "name": { "family": "Koo", "given": "David C." }, "orcid": "0000-0003-3385-6799" }, { "id": "Laine-S-J", "name": { "family": "Laine", "given": "Seppo" }, "orcid": "0000-0003-1250-8314" }, { "id": "Lintott-C-J", "name": { "family": "Lintott", "given": "Chris" }, "orcid": "0000-0001-5578-359X" }, { "id": "Masters-K-L", "name": { "family": "Masters", "given": "Karen L." }, "orcid": "0000-0003-0846-9578" }, { "id": "Melvin-T", "name": { "family": "Melvin", "given": "Thomas" } }, { "id": "Nichol-R-C", "name": { "family": "Nichol", "given": "Robert C." } }, { "id": "Schawinski-K", "name": { "family": "Schawinski", "given": "Kevin" }, "orcid": "0000-0001-5464-0888" }, { "id": "Simmons-B-D", "name": { "family": "Simmons", "given": "Brooke" }, "orcid": "0000-0001-5882-3323" }, { "id": "Smethurst-R-J", "name": { "family": "Smethurst", "given": "Rebecca" } }, { "id": "Willett-K-W", "name": { "family": "Willett", "given": "Kyle W." }, "orcid": "0000-0002-3654-3504" } ] }, "title": "Galaxy Zoo: Are bars responsible for the feeding of active galactic nuclei at 0.2 < z < 1.0?", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution\n galaxies: general\n galaxies: Seyfert\n galaxies: structure", "note": "\u00a9 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 November 20. Received 2014 November 13. In original form 2014 September 18. First published online December 18, 2014.\n\nAuthors from UC Santa Cruz acknowledge financial support from the NSF Grant AST 08-08133. KS gratefully acknowledges support from Swiss National Science Foundation Grant PP00P2_138979/1. JRT acknowledges support by NASA through Hubble Fellowship grant HST-HF-51330.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. EA and AB acknowledge financial support to the DAGAL network from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme FP7/2007-2013/ under REA grant agreement number PITN-GA-2011-289313. They also acknowledge financial support from the CNES (Centre National d'Etudes Spatiales \u2013 France). RCN acknowledges\nSTFC Rolling Grant ST/I001204/1 'Survey Cosmology and Astrophysics'. BS gratefully acknowledges support from the Oxford Martin School and from the Henry Skynner Junior Research Fellowship at Balliol College, Oxford. LFF and KWW acknowledge support from the UMN GIA programme. EC thanks Ramin A. Skibba, Michael Williams, Sugata Kaviraj, Yicheng Guo, Hassen Yesuf, and Guillermo Barro for useful discussions. The JavaScript Cosmology Calculator (Wright 2006) and TOPCAT (Taylor 2005) were used in the preparation of this paper. We also thank the anonymous referee for a helpful report.\n\nPublished - MNRAS-2015-Cheung-506-16.pdf
Submitted - 1409.5434v2.pdf
", "abstract": "We present a new study investigating whether active galactic nuclei (AGN) beyond the local universe are preferentially fed via large-scale bars. Our investigation combines data from Chandra and Galaxy Zoo: Hubble (GZH) in the AEGIS (All-wavelength Extended Groth strip International Survey), COSMOS (Cosmological Evolution Survey), and (Great Observatories Origins Deep Survey-South) GOODS-S surveys to create samples of face-on, disc galaxies at 0.2 < z < 1.0. We use a novel method to robustly compare a sample of 120 AGN host galaxies, defined to have 10^(42)\u2009erg\u2009s^(\u22121) < LX < 10^(44)\u2009erg\u2009s^(\u22121), with inactive control galaxies matched in stellar mass, rest-frame colour, size, S\u00e9rsic index, and redshift. Using the GZH bar classifications of each sample, we demonstrate that AGN hosts show no statistically significant enhancement in bar fraction or average bar likelihood compared to closely-matched inactive galaxies. In detail, we find that the AGN bar fraction cannot be enhanced above the control bar fraction by more than a factor of 2, at 99.7\u2009per\u2009cent confidence. We similarly find no significant difference in the AGN fraction among barred and non-barred galaxies. Thus we find no compelling evidence that large-scale bars directly fuel AGN at 0.2 < z < 1.0. This result, coupled with previous results at z = 0, implies that moderate-luminosity AGN have not been preferentially fed by large-scale bars since z = 1. Furthermore, given the low bar fractions at z > 1, our findings suggest that large-scale bars have likely never directly been a dominant fuelling mechanism for supermassive black hole growth.", "date": "2015-02-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "447", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "506-516", "id_number": "CaltechAUTHORS:20150406-084820885", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150406-084820885", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 08-08133" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "PP00P2_138979/1" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51330.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Marie Curie Fellowship", "grant_number": "PITN-GA-2011-289313" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I001204/1" }, { "agency": "Oxford Martin School" }, { "agency": "Balliol College" }, { "agency": "University of Minnesota" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stu2462", "primary_object": { "basename": "MNRAS-2015-Cheung-506-16.pdf", "url": "https://authors.library.caltech.edu/records/20jsw-vgw93/files/MNRAS-2015-Cheung-506-16.pdf" }, "related_objects": [ { "basename": "1409.5434v2.pdf", "url": "https://authors.library.caltech.edu/records/20jsw-vgw93/files/1409.5434v2.pdf" } ], "pub_year": "2015", "author_list": "Cheung, Edmond; Trump, Jonathan R.; et el." }, { "id": "https://authors.library.caltech.edu/records/9q4pk-w7b30", "eprint_id": 55766, "eprint_status": "archive", "datestamp": "2023-08-22 14:55:45", "lastmod": "2023-10-20 23:09:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lentati-L-T", "name": { "family": "Lentati", "given": "L." } }, { "id": "Wagg-Jeff", "name": { "family": "Wagg", "given": "J." } }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "F." }, "orcid": "0000-0003-4793-7880" }, { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" }, { "id": "da-Cunha-E", "name": { "family": "da Cunha", "given": "E." }, "orcid": "0000-0001-9759-4797" }, { "id": "Hodge-J-A", "name": { "family": "Hodge", "given": "J. A." }, "orcid": "0000-0001-6586-8845" }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Smail-Ian-R", "name": { "family": "Smail", "given": "I." }, "orcid": "0000-0003-3037-257X" }, { "id": "Sharon-C-E", "name": { "family": "Sharon", "given": "C." }, "orcid": "0000-0002-6250-5608" }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "Decarli-R", "name": { "family": "Decarli", "given": "R." }, "orcid": "0000-0002-2662-8803" }, { "id": "Dickinson-Mark-E", "name": { "family": "Dickinson", "given": "M." }, "orcid": "0000-0001-5414-5131" }, { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M." }, "orcid": "0000-0003-1033-9684" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" } ] }, "title": "COLDz: Karl G. Jansky Very Large Array Discovery of a Gas-rich Galaxy in COSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: star formation; radio lines: galaxies", "note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 1 August 2014; accepted for publication 1 December 2014; Published 10 February 2015. \n\nWe thank all those involved in the VLA project. These data were obtained as part of VLA observing program 13A-398 (PI: Riechers). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. I.R.S. acknowledges support from STFC (ST/L00075X/1), the ERC advanced investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson Merit Award. R.J.I. acknowledges support from the European Research Council (ERC) in the form of Advanced Grant, COSMICISM. D.R., F.W., E.dC., J.A.H., I.R.S., and V.S. acknowledge the Aspen Center for Physics and NSF grant 1066293 for hospitality during the preparation of this study. V.S. acknowledges funding by the European Union's Seventh Framework program under grant agreement 337595 (ERC Starting Grant, \"CoSMass\").\n\nPublished - 0004-637X_800_1_67.pdf
Submitted - 1412.1262v1.pdf
", "abstract": "The broad spectral bandwidth at millimeter and centimeter wavelengths provided by the recent upgrades to the Karl G. Jansky Very Large Array (VLA) has made it possible to conduct unbiased searches for molecular CO line emission at redshifts, z > 1.31. We present the discovery of a gas-rich, star-forming galaxy at z = 2.48 through the detection of CO J = 1\u20130 line emission in the COLDz survey and through a sensitive, Ka-band (31\u201339\u2009GHz) VLA survey of a 6.5 arcmin^2 region of the COSMOS field. We argue that the broad line (FWHM ~ 570\u2009 \u00b1 \u200980\u2009km\u2009s^\u22121) is most likely to be CO J = 1\u20130 at z = 2.48, as the integrated emission is spatially coincident with an infrared-detected galaxy with a photometric redshift estimate of z_phot = 3.2 \u00b1 0.4. The CO J = 1\u20130 line luminosity is L'_CO = (2.2\u00b10.3)\u00d7 10^10\u2009\u2009K\u2009km\u2009s^\u22121 pc^2, suggesting a cold molecular gas mass of M_gas ~ (2\u20138) \u00d7 10^10\u2009M_\u2609 depending on the assumed value of the molecular gas mass to CO luminosity ratio \u03b1_CO. The estimated infrared luminosity from the (rest-frame) far-infrared spectral energy distribution (SED) is L_IR = 2.5 \u00d7 10^12\u2009L^\u2609 and the star formation rate is ~250\u2009M^\u2609 yr^\u22121, with the SED shape indicating substantial dust obscuration of the stellar light. The infrared to CO line luminosity ratio is ~114\u2009 \u00b1 \u200919\u2009L_\u2609/(K\u2009km\u2009s^\u22121 pc^2), similar to galaxies with similar SFRs selected at UV/optical to radio wavelengths. This discovery confirms the potential for molecular emission line surveys as a route to study populations of gas-rich galaxies in the future.", "date": "2015-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "800", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 67", "id_number": "CaltechAUTHORS:20150316-084501175", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150316-084501175", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L00075X/1" }, { "agency": "European Research Council (ERC)", "grant_number": "321334" }, { "agency": "Royal Society" }, { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/800/1/67", "primary_object": { "basename": "0004-637X_800_1_67.pdf", "url": "https://authors.library.caltech.edu/records/9q4pk-w7b30/files/0004-637X_800_1_67.pdf" }, "related_objects": [ { "basename": "1412.1262v1.pdf", "url": "https://authors.library.caltech.edu/records/9q4pk-w7b30/files/1412.1262v1.pdf" } ], "pub_year": "2015", "author_list": "Lentati, L.; Wagg, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/pvan1-cnv54", "eprint_id": 52309, "eprint_status": "archive", "datestamp": "2023-08-20 04:34:48", "lastmod": "2023-10-18 19:45:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "Benson-A-J", "name": { "family": "Benson", "given": "Andrew J." }, "orcid": "0000-0001-5501-6008" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "Francesca" }, "orcid": "0000-0002-2115-1137" }, { "id": "Coil-A-L", "name": { "family": "Coil", "given": "Alison L." } }, { "id": "Bundy-K-A", "name": { "family": "Bundy", "given": "Kevin" }, "orcid": "0000-0001-9742-3138" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "Richard" }, "orcid": "0000-0002-6085-3780" }, { "id": "Schramm-M", "name": { "family": "Schramm", "given": "Malte" } }, { "id": "Schulze-A", "name": { "family": "Schulze", "given": "Andreas" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "id": "Kulier-A", "name": { "family": "Kulier", "given": "Andrea" } }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" } ] }, "title": "The Dark Matter Halos of Moderate Luminosity X-ray AGN as Determined fromWeak Gravitational Lensing and Host Stellar Masses", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: abundances galaxies: active galaxies: haloes galaxies: Seyfert galaxies: stellar content", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2014 October 21. Received 2014 September 30. In original form 2014 August 10. First published online November 21, 2014. \n\nWe thank Phil Hopkins, Surhud More, and John Silverman for insightful discussions while preparing this paper. We also thank Ed Turner for valuable discussions related to statistical methods. We are grateful to Ian Harnett for editing this manuscript. We also thank Nikos Fanidakis for clarifications regarding halo mass values in Fanidakis et al. (2013). This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. AK is supported by the National Science Foundation Graduate Research Fellowship, grant no. DGE-1148900. FC acknowledges financial support by the NASA grant AR1-12012X. RM is supported by a Royal Society University Research Fellowship. JR was supported by JPL, which is run by Caltech under a contract for NASA. ALC acknowledge support from NSF CAREER award AST-1055081.\n\nPublished - MNRAS-2015-Leauthaud-1874-88.pdf
Submitted - 1410.5817v1.pdf
", "abstract": "Understanding the relationship between galaxies hosting active galactic nuclei (AGN) and the dark matter haloes in which they reside is key to constraining how black hole fuelling is triggered and regulated. Previous efforts have relied on simple halo mass estimates inferred from clustering, weak gravitational lensing, or halo occupation distribution modelling. In practice, these approaches remain uncertain because AGN, no matter how they are identified, potentially live a wide range of halo masses with an occupation function whose general shape and normalization are poorly known. In this work, we show that better constraints can be achieved through a rigorous comparison of the clustering, lensing, and cross-correlation signals of AGN hosts to the fiducial stellar-to-halo mass relation (SHMR) derived for all galaxies, irrespective of nuclear activity. Our technique exploits the fact that the global SHMR can be measured with much higher accuracy than any statistic derived from AGN samples alone. Using 382 moderate luminosity X-ray AGN at z < 1 from the COSMOS field, we report the first measurements of weak gravitational lensing from an X-ray-selected sample. Comparing this signal to predictions from the global SHMR, we find that, contrary to previous results, most X-ray AGN do not live in medium size groups \u2013 nearly half reside in relatively low mass haloes with M_(200b) \u223c 10^(12.5) M_\u2299. The AGN occupation function is well described by the same form derived for all galaxies but with a lower normalization \u2013 the fraction of haloes with AGN in our sample is a few per cent. The number of AGN satellite galaxies scales as a power law with host halo mass with a power-law index \u03b1 = 1. By highlighting the relatively 'normal' way in which moderate luminosity X-ray AGN hosts occupy haloes, our results suggest that the environmental signature of distinct fuelling modes for luminous quasars compared to moderate luminosity X-ray AGN is less obvious than previously claimed.", "date": "2015-01-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "446", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1874-1888", "id_number": "CaltechAUTHORS:20141203-090456560", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141203-090456560", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1148900" }, { "agency": "NASA", "grant_number": "AR1-12012X" }, { "agency": "Royal Society" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "AST-1055081" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stu2210", "primary_object": { "basename": "1410.5817v1.pdf", "url": "https://authors.library.caltech.edu/records/pvan1-cnv54/files/1410.5817v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2015-Leauthaud-1874-88.pdf", "url": "https://authors.library.caltech.edu/records/pvan1-cnv54/files/MNRAS-2015-Leauthaud-1874-88.pdf" } ], "pub_year": "2015", "author_list": "Leauthaud, Alexie; Benson, Andrew J.; et el." }, { "id": "https://authors.library.caltech.edu/records/s0jb3-1xn23", "eprint_id": 56029, "eprint_status": "archive", "datestamp": "2023-08-20 04:25:23", "lastmod": "2023-10-20 23:34:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The VIMOS Ultra-Deep Survey (VUDS): fast increase in the fraction of strong Lyman-\u03b1 emitters from z = 2 to z = 6", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: formation, galaxies: high-redshift, galaxies: fundamental parameters, cosmology: observations", "note": "\u00a9 2014 ESO. Received 17 March 2014. Accepted 15 September 2014. Published online 09 December 2014.\n\n\nBased on data obtained with the European Southern\nObservatory Very Large Telescope, Paranal, Chile, under Large\nProgram 185.A-0791.\n\nWe thank ESO staff for their continuous support for the VUDS survey, particularly the Paranal staff conducting the observations and Marina Rejkuba and the ESO user support group in Garching. This work is supported by funding from the European Research Council Advanced Grant ERC-2010-AdG-268107-EARLY and by INAF Grants PRIN 2010, PRIN 2012 and PICS 2013. A.C., O.C., M.T. and V.S. acknowledge the grant MIUR PRIN 2010\u20132011. D.M. gratefully acknowledges LAM hospitality during the initial phases of the project. This work is based on data products made available at the CESAM data center, Laboratoire d'Astrophysique de Marseille. This work partly uses observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS.\n\nPublished - aa23824-14.pdf
Submitted - 1403.3693v2.pdf
", "abstract": "Aims. The aim of this work is to constrain the evolution of the fraction of strong Ly\u03b1 emitters among UV selected star-forming galaxies at 2 25 \u00c5 to increase from ~5% at z ~ 2 to ~30% at z ~ 6, with the increase being stronger beyond z ~ 4. We observe no difference, for the narrow range of UV luminosities explored in this work, between the fraction of strong Ly\u03b1 emitters among galaxies fainter or brighter than M^*_(FUV), although the fraction for the faint galaxies evolves faster, at 2", "date": "2015-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "573", "publisher": "EDP Sciences", "pagerange": "Art. No. A24", "id_number": "CaltechAUTHORS:20150324-120025853", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150324-120025853", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council", "grant_number": "ERC-2010-AdG-268107-EARLY" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2010" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2012" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PICS 2013" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)", "grant_number": "PRIN 2010-2011" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201423824", "primary_object": { "basename": "1403.3693v2.pdf", "url": "https://authors.library.caltech.edu/records/s0jb3-1xn23/files/1403.3693v2.pdf" }, "related_objects": [ { "basename": "aa23824-14.pdf", "url": "https://authors.library.caltech.edu/records/s0jb3-1xn23/files/aa23824-14.pdf" } ], "pub_year": "2015", "author_list": "Cassata, P.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/wdpqv-cqs79", "eprint_id": 53811, "eprint_status": "archive", "datestamp": "2023-08-22 14:28:14", "lastmod": "2023-10-19 22:14:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Erfanianfar-G", "name": { "family": "Erfanianfar", "given": "G." } }, { "id": "Fadda-D", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" } ] }, "title": "The evolution of star formation activity in galaxy groups", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogues; galaxies: evolution; cosmology: observations; large-scale structure of Universe; infrared: galaxies", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2014 September 9. Received 2014 September 9; in original form 2013 December 17.\n\nGE acknowledges the support from and participation in the International Max-Planck Research School on Astrophysics at the Ludwig-Maximilians University. MLB acknowledges financial support from an NSERC Discovery Grant, and from NWO and NOVA grants that supported his sabbatical at the University of Leiden, where this work was completed. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy), and CICYT/MCYT (Spain).\n\nThis research has made use of NASA's Astrophysics Data System, of NED, which is operated by JPL/Caltech, under contract with NASA, and of SDSS, which has been funded by the Sloan Foundation, NSF, the US Department of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council of England. The SDSS is managed by the participating institutions (www.sdss.org/collaboration/credits.html).\n\nWe gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information about the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. This project has been supported by the DLR grant 50OR1013 to MPE.\n\nPublished - MNRAS-2014-Erfanianfar-2725-45.pdf
Submitted - 1409.5795v1.pdf
", "abstract": "We study the evolution of the total star formation (SF) activity, total stellar mass (\u03a3M*) and halo occupation distribution (HOD) in massive haloes by using one of the largest X-ray selected sample of galaxy groups with secure spectroscopic identification in the major blank field surveys (ECDFS, CDFN, COSMOS, AEGIS). We provide an accurate measurement of star formation rate (SFR) for the bulk of the star-forming galaxies using very deep mid-infrared Spitzer MIPS and far-infrared Herschel PACS observations. For undetected IR sources, we provide a well-calibrated SFR from spectral energy distribution (SED) fitting. We observe a clear evolution in the level of SF activity in galaxy groups. The total SF activity in the high-redshift groups (0.5 < z < 1.1) is higher with respect to the low-redshift (0.15 < z < 0.5) sample at any mass by 0.8 \u00b1 0.12 dex. A milder difference (0.35 \u00b1 0.1 dex) is observed between the low-redshift bin and the groups at z \u223c 0. We show that the level of SF activity is declining more rapidly in the more massive haloes than in the more common lower mass haloes. We do not observe any evolution in the HOD and total stellar mass\u2013halo mass relations in groups. The picture emerging from our findings suggests that the galaxy population in the most massive systems is evolving faster than galaxies in lower mass haloes, consistently with a 'halo downsizing' scenario.", "date": "2014-12-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "445", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2725-2745", "id_number": "CaltechAUTHORS:20150116-095302650", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150116-095302650", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "International Max-Planck Research School on Astrophysics" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "NWO" }, { "agency": "NOVA" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50OR1013" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "COSMOS Collaboration" ] }, "doi": "10.1093/mnras/stu1883", "primary_object": { "basename": "MNRAS-2014-Erfanianfar-2725-45.pdf", "url": "https://authors.library.caltech.edu/records/wdpqv-cqs79/files/MNRAS-2014-Erfanianfar-2725-45.pdf" }, "related_objects": [ { "basename": "1409.5795v1.pdf", "url": "https://authors.library.caltech.edu/records/wdpqv-cqs79/files/1409.5795v1.pdf" } ], "pub_year": "2014", "author_list": "Erfanianfar, G. and Fadda, D." }, { "id": "https://authors.library.caltech.edu/records/wjena-vfj20", "eprint_id": 53075, "eprint_status": "archive", "datestamp": "2023-08-22 14:25:44", "lastmod": "2023-10-19 14:30:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "Dominik A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "Christopher L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "Vernesa" }, "orcid": "0000-0002-3893-8614" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "Min" }, "orcid": "0000-0001-7095-7543" }, { "id": "Cox-Pierre", "name": { "family": "Cox", "given": "Pierre" }, "orcid": "0000-0003-2027-8221" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "Frank" }, "orcid": "0000-0002-1707-1775" }, { "id": "Karim-A", "name": { "family": "Karim", "given": "Alexander" }, "orcid": "0000-0002-8414-9579" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" } ] }, "title": "ALMA Imaging of Gas and Dust in a Galaxy Protocluster at Redshift 5.3: [C II] Emission in \"Typical\" Galaxies and Dusty Starbursts \u2248 1 Billion Years after the Big Bang", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: formation; galaxies: high-redshift; galaxies: starburst; radio lines: galaxies", "note": "\u00a9 2014 American Astronomical Society. Received 2014 April 28; accepted 2014 October 15; published 2014 November 10.\n\nWe thank the anonymous referee for a helpful and constructive report, Jim Braatz for assistance with setting up the observations, Mark Lacy for taking on the QA2 check of the data, and Alex Conley for help with the SED fitting. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO.ALMA# 2011.0.00064.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. F.B. and A.K. acknowledge support from Collaborative Research Centre 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). V.S. acknowledges support by the European Union's Seventh Framework program under grant agreement 337595 (ERC Starting Grant, \"Cos-Mass\"). Additional support for this work was provided by the NSF through award SOSPA0-002 from the NRAO.\n\nPublished - 0004-637X_796_2_84.pdf
Submitted - 1404.7159v2.pdf
", "abstract": "We report interferometric imaging of [C II](^2 P_(3/2)\u2192^2 P_(1/2)) and OH(^2\u03a0_(1/2)J = 3/2\u21921/2) emission toward the center of the galaxy protocluster associated with the z = 5.3 submillimeter galaxy (SMG) AzTEC-3, using the Atacama Large (sub)Millimeter Array (ALMA). We detect strong [C II], OH, and rest-frame 157.7 \u03bcm continuum emission toward the SMG. The [C II](^2 P_(3/2)\u2192^2 P_(1/2)) emission is distributed over a scale of 3.9 kpc, implying a dynamical mass of 9.7 \u00d7 10^(10) M_\u2609, and a star formation rate (SFR) surface density of \u03a3_(SFR) = 530 M_\u2609 yr^(\u20131) kpc^(\u20132). This suggests that AzTEC-3 forms stars at \u03a3^(SFR) approaching the Eddington limit for radiation pressure supported disks. We find that the OH emission is slightly blueshifted relative to the [C II] line, which may indicate a molecular outflow associated with the peak phase of the starburst. We also detect and dynamically resolve [C II](^2 P_(3/2)\u2192^2 P_(1/2)) emission over a scale of 7.5 kpc toward a triplet of Lyman-break galaxies with moderate UV-based SFRs in the protocluster at ~95 kpc projected distance from the SMG. These galaxies are not detected in the continuum, suggesting far-infrared SFRs of <18-54 M_\u2609 yr^(\u20131), consistent with a UV-based estimate of 22 M_\u2609 yr^(\u20131). The spectral energy distribution of these galaxies is inconsistent with nearby spiral and starburst galaxies, but resembles those of dwarf galaxies. This is consistent with expectations for young starbursts without significant older stellar populations. This suggests that these galaxies are significantly metal-enriched, but not heavily dust-obscured, \"normal\" star-forming galaxies at z > 5, showing that ALMA can detect the interstellar medium in \"typical\" galaxies in the very early universe.", "date": "2014-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "796", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 84", "id_number": "CaltechAUTHORS:20141222-091844381", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141222-091844381", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "Collaborative Research Centre 956" }, { "agency": "European Research Council (ERC)", "grant_number": "337595" }, { "agency": "NSF", "grant_number": "SOSPA0-002" }, { "agency": "National Radio Astronomy Observatory" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/796/2/84", "primary_object": { "basename": "0004-637X_796_2_84.pdf", "url": "https://authors.library.caltech.edu/records/wjena-vfj20/files/0004-637X_796_2_84.pdf" }, "related_objects": [ { "basename": "1404.7159v2.pdf", "url": "https://authors.library.caltech.edu/records/wjena-vfj20/files/1404.7159v2.pdf" } ], "pub_year": "2014", "author_list": "Riechers, Dominik A.; Carilli, Christopher L.; et el." }, { "id": "https://authors.library.caltech.edu/records/akywc-jzq88", "eprint_id": 53073, "eprint_status": "archive", "datestamp": "2023-08-22 14:25:38", "lastmod": "2023-10-18 21:55:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Casey-C-M", "name": { "family": "Casey", "given": "C. M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "N." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Finkelstein-S-L", "name": { "family": "Finkelstein", "given": "S. L." }, "orcid": "0000-0001-8519-1130" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Conley-A", "name": { "family": "Conley", "given": "A." } }, { "id": "De-Zotti-G", "name": { "family": "de Zotti", "given": "G." }, "orcid": "0000-0003-2868-2595" }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Fu-Hai", "name": { "family": "Fu", "given": "H." }, "orcid": "0000-0001-9608-6395" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Takeuchi-Tsutomu-T", "name": { "family": "Takeuchi", "given": "T. T." } } ] }, "title": "Are Dusty Galaxies Blue? Insights on UV Attenuation from Dust-selected Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimeter: galaxies", "note": "\u00a9 2014 American Astronomical Society.\n\nReceived 2014 June 23; accepted 2014 September 25; published 2014 November 12.\n\nCOSMOS is based on observations with the NASA/ESA\nHubble Space Telescope, obtained at the Space Telescope\nScience Institute, which is operated by AURA Inc, under\nNASA contract NAS 5-26555; also based on data collected\nat: the Subaru Telescope, which is operated by the National\nAstronomical Observatory of Japan; XMM-Newton, an ESA\nscience mission with instruments and contributions directly\nfunded by ESA Member States and NASA; the European\nSouthern Observatory, Chile; Kitt Peak National Observatory,\nCerro Tololo Inter-American Observatory, and the National\nOptical Astronomy Observatory, which are operated by the\nAssociation of Universities for Research in Astronomy, Inc.\n(AURA) under cooperative agreement with theNational Science\nFoundation; the National Radio Astronomy Observatory, which\nis a facility of the National Science Foundation operated\nunder cooperative agreement by Associated Universities, Inc;\nand the Canada\u2013France\u2013Hawaii Telescope operated by the\nNational Research Council of Canada, the Centre National de la Recherche Scientifique de France, and the University of Hawaii. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, HNSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). This research has made use of data from the HerMES project (http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists and a mission scientist. The data presented in this paper will be released through the HerMES Database in Marseille,HeDaM (http://hedam.oamp.fr/HerMES/). We would also like to recognize the use of the Glue Visualization tool (www.glueviz.org) in the initial analysis of this data set.\nC.M.C. acknowledges support from a McCue Fellowship\nthrough the University of California, Irvine's Center for Cosmology. A.C. acknowledges support from NSF AST-1313319.\nR.J.I. acknowledges support from ERC AdG, COSMICISM.\nT.T.T. has been supported by the Grant-in-Aid for the Scientific Research Fund (24111707) commissioned by the Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan. T.T.T. has also been partially supported from Strategic Young Researches OverseasVisits Program forAccelerating Brain Circulation from the MEXT. We are grateful to the anonymous referee for productive comments that improved the paper. We would also like to thank Naveen Reddy, Brian Siana, Mara Salvato, and Douglas Scott for helpful conversations during the manuscript's preparation.\n\nPublished - 0004-637X_796_2_95.pdf
Submitted - 1410.0702v1.pdf
", "abstract": "Galaxies' rest-frame ultraviolet (UV) properties are often used to directly infer the degree to which dust obscuration affects the measurement of star formation rates (SFRs). While much recent work has focused on calibrating dust attenuation in galaxies selected at rest-frame ultraviolet wavelengths, locally and at high-z, here we investigate attenuation in dusty, star forming galaxies (DSFGs) selected at far-infrared wavelengths. By combining multiwavelength coverage across 0.15-500 \u03bcm in the COSMOS field, in particular making use of Herschel imaging, and a rich data set on local galaxies, we find an empirical variation in the relationship between the rest-frame UV slope (\u03b2) and the ratio of infrared-to-ultraviolet emission (L_IR/L_UV \u2261 IRX) as a function of infrared luminosity, or total SFR. Both locally and at high-z, galaxies above SFR \u2273 50 M_\u2609 yr^\u20131 deviate from the nominal IRX-\u03b2 relation toward bluer colors by a factor proportional to their increasing IR luminosity. We also estimate contamination rates of DSFGs on high-z dropout searches of \u226a1% at z \u2272 4-10, providing independent verification that contamination from very dusty foreground galaxies is low in Lyman-break galaxy searches. Overall, our results are consistent with the physical interpretation that DSFGs, e.g., galaxies with >50 M_\u2609 yr^\u20131, are dominated at all epochs by short-lived, extreme burst events, producing many young O and B stars that are primarily, yet not entirely, enshrouded in thick dust cocoons. The blue rest-frame UV slopes of DSFGs are inconsistent with the suggestion that most DSFGs at z ~ 2 exhibit steady-state star formation in secular disks.", "date": "2014-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "796", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 95", "id_number": "CaltechAUTHORS:20141222-091108670", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141222-091108670", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "ESA Member States" }, { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia Y Tecnologia (MCYT)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "McCue Fellowship" }, { "agency": "University of California, Irvine" }, { "agency": "NSF", "grant_number": "AST-1313319" }, { "agency": "European Research Council (ERC)" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "24111707" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/796/2/95", "primary_object": { "basename": "0004-637X_796_2_95.pdf", "url": "https://authors.library.caltech.edu/records/akywc-jzq88/files/0004-637X_796_2_95.pdf" }, "related_objects": [ { "basename": "1410.0702v1.pdf", "url": "https://authors.library.caltech.edu/records/akywc-jzq88/files/1410.0702v1.pdf" } ], "pub_year": "2014", "author_list": "Casey, C. M.; Scoville, N. Z.; et el." }, { "id": "https://authors.library.caltech.edu/records/40494-p7922", "eprint_id": 53828, "eprint_status": "archive", "datestamp": "2023-08-22 14:21:26", "lastmod": "2023-10-19 22:15:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lemaux-B-C", "name": { "family": "Lemaux", "given": "B. C." }, "orcid": "0000-0002-1428-7036" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "VIMOS Ultra-Deep Survey (VUDS): Witnessing the assembly of a massive cluster at z ~ 3.3", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: active; galaxies: clusters: general; techniques: spectroscopic; techniques: photometric", "note": "\u00a9 2014 ESO. Received 17 March 2014. Accepted 29 July 2014. Published online 26 November 2014.\n\nWe thank ESO staff for their continuous support for the\nVUDS survey, particularly the Paranal staff conducting the observations and Marina Rejkuba and the ESO user support group in Garching. This work is supported by funding from the European Research Council Advanced Grant ERC-2010-AdG-268107-EARLY and by INAF Grants PRIN 2010, PRIN 2012 and\nPICS 2013. A.C., O.C., M.T. and V.S. acknowledge the grant MIUR PRIN 2010\u20132011. D.M. gratefully acknowledges LAM hospitality during the initial phases of the project. B.C.L. gratefully acknowledges the kindness, support, and salty muffins of Debora Pelliccia provided, even at the most unreasonable of hours, throughout the course of this work. This work is based on data products made available at the CESAM data center, Laboratoire d'Astrophysique de Marseille. This work partly uses observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada,\nthe Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian\nAstronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. A portion of the spectroscopic data presented herein were obtained at the W. M. Keck Observatory. We wish to thank the indigenous Hawaiian community for allowing us to be guests on their sacred mountain; we are most fortunate to be able to conduct observations from this site.\n\nPublished - aa23828-14.pdf
Submitted - 1403.4230v4.pdf
", "abstract": "Using new spectroscopic observations obtained as part of the VIMOS Ultra-Deep Survey (VUDS), we performed a systematic search for overdense environments in the early universe (z > 2) and report here on the discovery of C1 J0227-0421, a massive protocluster at z = 3.29. This protocluster is characterized by both the large overdensity of spectroscopically confirmed members, \u03b4_(gal) = 10.5 \u00b1 2.8, and a significant overdensity in photometric redshift members. The halo mass of this protocluster is estimated by a variety of methods to be ~3 x 10^(14) M_\u2609 at z ~ 3.3, which, evolved to z = 0 results in a halo mass rivaling or exceeding that of the Coma cluster. The properties of 19 spectroscopically confirmed member galaxies are compared with a large sample of VUDS/VVDS galaxies in lower density field environments at similar redshifts. We find tentative evidence for an excess of redder, brighter, and more massive galaxies within the confines of the protocluster relative to the field population, which suggests that we may be observing the beginning of environmentally induced quenching. The properties of these galaxies are investigated, including a discussion of the brightest protocluster galaxy, which appears to be undergoing vigorous coeval nuclear and starburst activity. The remaining member galaxies appear to have characteristics that are largely similar to the field population. Though we find weaker evidence of the suppression of the median star formation rates among and differences in the stacked spectra of member galaxies with respect to the field, we defer any conclusions about these trends to future work with the ensemble of protostructures that are found in the full VUDS sample.", "date": "2014-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "572", "publisher": "EDP Sciences", "pagerange": "Art. No. A41", "id_number": "CaltechAUTHORS:20150116-112603880", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150116-112603880", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Counci", "grant_number": "ERC-2010-AdG-268107-EARLY" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-2010" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2012" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PICS 2013" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)", "grant_number": "PRIN 2010\u20132011" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201423828", "primary_object": { "basename": "1403.4230v4.pdf", "url": "https://authors.library.caltech.edu/records/40494-p7922/files/1403.4230v4.pdf" }, "related_objects": [ { "basename": "aa23828-14.pdf", "url": "https://authors.library.caltech.edu/records/40494-p7922/files/aa23828-14.pdf" } ], "pub_year": "2014", "author_list": "Lemaux, B. C.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/4qje5-y2496", "eprint_id": 53041, "eprint_status": "archive", "datestamp": "2023-08-22 14:19:39", "lastmod": "2023-10-18 21:53:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lackner-C-N", "name": { "family": "Lackner", "given": "C. N." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Halliday-C", "name": { "family": "Halliday", "given": "C." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "K." }, "orcid": "0000-0003-3804-2137" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "N." } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Liu-Charles-T", "name": { "family": "Liu", "given": "C. T." }, "orcid": "0000-0002-4314-8713" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Toft-S", "name": { "family": "Toft", "given": "S." }, "orcid": "0000-0003-3631-7176" } ] }, "title": "Late-Stage Galaxy Mergers in Cosmos to z ~ 1", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: formation; galaxies: interactions; techniques: image processing", "note": "\u00a9 2014 American Astronomical Society.\n\nReceived 2014 February 2; accepted 2014 August 24; published 2014 November 13.\n\nWe thank the referee for insightful comments that greatly\nimproved this work. We also thank Richard Massey and Kevin\nBundy for helpful comments on a draft. This work was\nsupported by the World Premier International Research Center\nInitiative (WPI Initiative), MEXT, Japan. S.T. acknowledges\nsupport from the Lundbeck Foundation. The Dark Cosmology\nCentre is funded by the Danish National Research Foundation.\nThis research has made use of the NASA/IPAC Infrared\nScience Archive, which is operated by the Jet Propulsion\nLaboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com\n\nPublished - 1538-3881_148_6_137.pdf
Submitted - 1406.2327v1.pdf
", "abstract": "The role of major mergers in galaxy and black hole formation is not well-constrained. To help address this, we develop an automated method to identify late-stage galaxy mergers before coalescence of the galactic cores. The resulting sample of mergers is distinct from those obtained using pair-finding and morphological indicators. Our method relies on median-filtering of high-resolution images to distinguish two concentrated galaxy nuclei at small separations. This method does not rely on low surface brightness features to identify mergers, and is therefore reliable to high redshift. Using mock images, we derive statistical contamination and incompleteness corrections for the fraction of late-stage mergers. The mock images show that our method returns an uncontaminated (<10%) sample of mergers with projected separations between 2.2 and 8 kpc out to z ~ 1. We apply our new method to a\nmagnitude-limited (m_(FW 814) < 23) sample of 44,164 galaxies from the COSMOS HST/ACS catalog. Using a mass-complete sample with log M_* M_\u2299 > 10.6 and 0.25 < z \u2a7d 1.00, we find ~5% of systems are late-stage mergers. Correcting for incompleteness and contamination, the fractional merger rate increases strongly with redshift as\nRmerge \u03bc (1 + z)^(3.8\u00b10.9), in agreement both with earlier studies and with dark matter halo merger rates. Separating\nthe sample into star-forming and quiescent galaxies shows that the merger rate for star-forming galaxies increases\nstrongly with redshift, (1 + z)^(4.5\u00b11.3), while the merger rate for quiescent galaxies is consistent with no evolution,\n(1 + z)^(1.1\u00b11.2). The merger rate also becomes steeper with decreasing stellar mass. Limiting our sample to galaxies with spectroscopic redshifts from zCOSMOS, we find that the star formation rates and X-ray selected active galactic nucleus (AGN) activity in likely late-stage mergers are higher by factors of ~2 relative to those of a\ncontrol sample. Combining our sample with more widely separated pairs, we find that 8 \u00b1 5% of star formation\nand 20 \u00b1 8% of AGN activity are triggered by close encounters (<143 kpc) or mergers, providing additional\nevidence that major mergers are not the only channels for star formation and black hole growth.", "date": "2014-12", "date_type": "published", "publication": "Astronomical Journal", "volume": "148", "number": "6", "publisher": "American Astronomical Society", "pagerange": "Art. No. 137", "id_number": "CaltechAUTHORS:20141219-112207981", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141219-112207981", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan" }, { "agency": "Lundbeck Foundation" }, { "agency": "Danish National Research Foundation" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-6256/148/6/137", "primary_object": { "basename": "1538-3881_148_6_137.pdf", "url": "https://authors.library.caltech.edu/records/4qje5-y2496/files/1538-3881_148_6_137.pdf" }, "related_objects": [ { "basename": "1406.2327v1.pdf", "url": "https://authors.library.caltech.edu/records/4qje5-y2496/files/1406.2327v1.pdf" } ], "pub_year": "2014", "author_list": "Lackner, C. N.; Silverman, J. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/vnmdg-ts905", "eprint_id": 52598, "eprint_status": "archive", "datestamp": "2023-08-22 14:15:04", "lastmod": "2023-10-18 21:00:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Darvish-B", "name": { "family": "Darvish", "given": "B." }, "orcid": "0000-0003-4919-9017" }, { "id": "Sobral-D", "name": { "family": "Sobral", "given": "D." }, "orcid": "0000-0001-8823-4845" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B" } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Best-P-N", "name": { "family": "Best", "given": "P." } }, { "id": "Sales-L-V", "name": { "family": "Sales", "given": "L. V." } }, { "id": "Smail-I", "name": { "family": "Smail", "given": "I." }, "orcid": "0000-0003-3037-257X" } ] }, "title": "Cosmic Web and Star Formation Activity in Galaxies at z ~ 1", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general; galaxies: evolution; galaxies: star formation; large-scale structure of universe", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2014 August 27; accepted 2014 September 25; published 2014 November 4. \n\nWe gratefully thank the referee for thoroughly reading the original manuscript and providing very useful comments that improved the quality of this work. D.S. acknowledges financial support from LKBF, the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship, from FCT through an FCT Investigator Starting Grant, a Start-up Grant (IF/01154/2012/CP0189/CT0010), and the grant PEst-OE/FIS/UI2751/2014. B.D. thanks Miguel Arag\u03ccn-Calvo for his useful comments on an earlier draft. I.S. acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334, and a Royal Society/Wolfson Merit Award.\n\nPublished - 0004-637X_796_1_51.pdf
Submitted - 1409.7695v1.pdf
", "abstract": "We investigate the role of the delineated cosmic web/filaments on star formation activity by exploring a sample of 425 narrow-band selected H\u03b1 emitters, as well as 2846 color-color selected underlying star-forming galaxies for a large-scale structure at z = 0.84 in the COSMOS field from the HiZELS survey. Using the scale-independent Multi-scale Morphology Filter algorithm, we are able to quantitatively describe the density field and disentangle it into its major components: fields, filaments, and clusters. We show that the observed median star formation rate (SFR), stellar mass, specific SFR, the mean SFR-mass relation, and its scatter for both H\u03b1 emitters and underlying star-forming galaxies do not strongly depend on different classes of environment, in agreement with previous studies. However, the fraction of H\u03b1 emitters varies with environment and is enhanced in filamentary structures at z ~ 1. We propose mild galaxy-galaxy interactions as the possible physical agent for the elevation of the fraction of H\u03b1 star-forming galaxies in filaments. Our results show that filaments are the likely physical environments that are often classed as the \"intermediate\" densities and that the cosmic web likely plays a major role in galaxy formation and evolution which has so far been poorly investigated.", "date": "2014-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "796", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 51", "id_number": "CaltechAUTHORS:20141211-104915111", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141211-104915111", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "LKBF" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "IF/01154/2012/CP0189/CT0010" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "PEst-OE/FIS/UI2751/2014" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L00075X/1" }, { "agency": "European Research Council (ERC)", "grant_number": "DUSTYGAL 321334" }, { "agency": "Royal Society" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/796/1/51", "primary_object": { "basename": "0004-637X_796_1_51.pdf", "url": "https://authors.library.caltech.edu/records/vnmdg-ts905/files/0004-637X_796_1_51.pdf" }, "related_objects": [ { "basename": "1409.7695v1.pdf", "url": "https://authors.library.caltech.edu/records/vnmdg-ts905/files/1409.7695v1.pdf" } ], "pub_year": "2014", "author_list": "Darvish, B.; Sobral, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/bn80x-2da43", "eprint_id": 52418, "eprint_status": "archive", "datestamp": "2023-08-22 13:48:23", "lastmod": "2023-10-18 19:50:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Speagle-J-S", "name": { "family": "Speagle", "given": "J. S." }, "orcid": "0000-0002-5065-9896" }, { "id": "Steinhardt-C-L", "name": { "family": "Steinhardt", "given": "C. L." }, "orcid": "0000-0003-3780-6801" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" } ] }, "title": "A Highly Consistent Framework for the Evolution of the Star-Forming \"Main Sequence\" from z~0-6", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: star formation; radio continuum: galaxies; surveys", "note": "\u00a9 2014 American Astronomical Society. Received 2014 April 9; accepted 2014 June 24; published 2014 September 18.\n\nThe authors thank the anonymous referee for thorough and\ninsightful comments that greatly improved the quality of this work. The authors also thank Martin Elvis, Daniel Masters, David Sanders, and David Sobral for their input and helpful comments, as well as Douglas Finkbeiner for advising the junior thesis course where much of this work was completed. In addition, the authors thank Herv\u00b4e Aussel, Kevin Bundy, Brian Feldstein, Olivier Ilbert, Emil Khabiboulline, Alex Krolewski, John Moustakas, Alvio Renzini, and Michael Strauss for useful discussions and/or comments. In addition, we thank Stephane Arnouts, Rychard Bouwens, Alison Coil, Loretta Dunne, Alex Karim, Mariska Kriek, Kyoungsoo Lee, Sam Leitner, Georgios Magdis, John Moustakas, EricMurphy, Kai Noeske, Seb Oliver, Samir Salim, Paola Santini, Hyunjin Shim, and David Sobral for providing us with data and/or answering questions about their work. We especially thank Alex Karim, Eric Murphy, and Olivier Ilbert for insightful discussions about stacking and radio SFR observations. JSS thanks Rebecca Bleich for all her\nsupport. JSS was partially supported by grants from the Harvard Office of Career Services' Weismann International Internship Program and the Harvard College Research Program.\n\nPublished - 0067-0049_214_2_15.pdf
Submitted - 1405.2041v2.pdf
", "abstract": "Using a compilation of 25 studies from the literature, we investigate the evolution of the star-forming galaxy (SFG) main sequence (MS) in stellar mass and star formation rate (SFR) out to z ~ 6. After converting all observations to a common set of calibrations, we find a remarkable consensus among MS observations (~0.1 dex 1\u03c3 interpublication scatter). By fitting for time evolution of the MS in bins of constant mass, we deconvolve the observed scatter about the MS within each observed redshift bin. After accounting for observed scatter between different SFR indicators, we find the width of the MS distribution is ~0.2 dex and remains constant over cosmic time. Our best fits indicate the slope of the MS is likely time-dependent, with our best-fit log SFR(M_*, t) = (0.84 \u00b1 0.02 \u2013 0.026 \u00b1 0.003 \u00d7 t)log M_* \u2013 (6.51 \u00b1 0.24 \u2013 0.11 \u00b1 0.03 \u00d7 t), where t is the age of the universe in Gyr. We use our fits to create empirical evolutionary tracks in order to constrain MS galaxy star formation histories (SFHs), finding that (1) the most accurate representations of MS SFHs are given by delayed-\u03c4 models, (2) the decline in fractional stellar mass growth for a \"typical\" MS galaxy today is approximately linear for most of its lifetime, and (3) scatter about the MS can be generated by galaxies evolving along identical evolutionary tracks assuming an initial 1\u03c3 spread in formation times of ~1.4 Gyr.", "date": "2014-10", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "214", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 15", "id_number": "CaltechAUTHORS:20141205-080407335", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141205-080407335", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Harvard Office of Career Services' Weismann International Internship Program" }, { "agency": "Harvard College Research Program" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0067-0049/214/2/15", "primary_object": { "basename": "0067-0049_214_2_15.pdf", "url": "https://authors.library.caltech.edu/records/bn80x-2da43/files/0067-0049_214_2_15.pdf" }, "related_objects": [ { "basename": "1405.2041v2.pdf", "url": "https://authors.library.caltech.edu/records/bn80x-2da43/files/1405.2041v2.pdf" } ], "pub_year": "2014", "author_list": "Speagle, J. S.; Steinhardt, C. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/v9v8t-95h16", "eprint_id": 52444, "eprint_status": "archive", "datestamp": "2023-08-20 03:07:57", "lastmod": "2023-10-18 19:52:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Discovery of a rich proto-cluster at z = 2.9 and associated diffuse cold gas in the VIMOS Ultra-Deep Survey (VUDS)", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift, large-scale structure of Universe, cosmology: observations", "note": "\u00a9 2014 ESO. \nArticle published by EDP Sciences.\n\nReceived 14 March 2014. Accepted 23 July 2014.\nPublished online 07 October 2014.\n\nBased on data obtained with the European Southern Observatory\nVery Large Telescope, Paranal, Chile, under Large Program\n185.A-0791.\n\nWe thank the referee for the useful comments that improved\nthe paper. We thank Nico Cappelluti for his help with X-ray data and Mauro Roncarelli for helpful discussion. We thank ESO staff for their continuous support of the VUDS survey, particularly the Paranal staff conducting the observations and Marina Rejkuba and the ESO user support group in Garching. This work is supported by funding from the European Research Council Advanced Grant ERC-2010-AdG-268107-EARLY and by INAF Grants PRIN 2010, PRIN 2012, and PICS 2013. A.C., O.C., M.T., and V.S. acknowledge\nthe grants MIUR PRIN 2010\u20132011 and ASI n.I/023/12/0 \"Attivit\u00e0 relative alla fase B2/C per la missione Euclid\". D.M. gratefully acknowledges LAM hospitality during the initial phases of the project. This work is based on data products made available at the CESAM data centre, Laboratoire d'Astrophysique de Marseille. This work partly uses observations obtained with MegaPrime/MegaCam, a joint project of the CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National\nResearch Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of the NRC and CNRS.\n\nPublished - aa23811-14.pdf
Submitted - 1403.3691v2.pdf
", "abstract": "High-density environments are crucial places for studying the link between hierarchical structure formation and stellar mass growth in galaxies. In this work, we characterise a massive proto-cluster at z = 2.895 that we found in the COSMOS field using the spectroscopic sample of the VIMOS Ultra-Deep Survey (VUDS). This is one of the rare structures at z ~ 3 not identified around an active galactic nucleus (AGN) or a radio galaxy, thus it represents an ideal laboratory for investigating the formation of galaxies in dense environments. The structure comprises 12 galaxies with secure spectroscopic redshift in an area of ~ 7\u2032 \u00d7 8\u2032, in a total z range of \u0394z = 0.016. The measured galaxy number overdensity is \u03b4_g = 12 \u00b1 2. This overdensity has a total mass of M ~ 8.1 \u00d7 10^(14) M_\u2299 in a volume of 13 \u00d7 15 \u00d7 17 Mpc^3. Simulations indicate that such an overdensity at z ~ 2.9 is a proto-cluster, which will collapse in a cluster of total mass M_(z = 0) ~ 2.5 \u00d7 10^(15) M_\u2299 at z = 0, i.e. a massive cluster in the local Universe. We analysed the properties of the galaxies within the overdensity, and we compared them with acontrol sample at the same redshift but outside the overdensity. We could not find any statistically significant difference between the properties (stellar mass, star formation rate, specific star formation rate, NUV-r and r \u2212 K colours) of the galaxies inside and outside the overdensity, but this result might be due to the lack of statistics or possibly to the specific galaxy population sampled by VUDS, which could be less affected by environment than the other populations not probed by the survey. The stacked spectrum of galaxies in the background of the overdensity shows a significant absorption feature at the wavelength of Ly\u03b1 redshifted at z = 2.895 (\u03bb = 4736 \u00c5), with a rest frame equivalent width (EW) of 4 \u00b1 1.4 \u00c5. Stacking only background galaxies without intervening sources at z ~ 2.9 along their line of sight, we find that this absorption feature has a rest frame EW of 10.8 \u00b1 3.7 \u00c5, with a detection S/N of ~4. We verify that this measurement is not likely to be due to noise fluctuations. These EW values imply a high column density (N(HI) ~ 3\u221220 \u00d7 10^(19) cm^(-2)), consistent with a scenario where such absorption is due to intervening cold streams of gas that are falling into the halo potential wells of the proto-cluster galaxies. Nevertheless, we cannot rule out the hypothesis that this absorption line is related to the diffuse gas within the overdensity.", "date": "2014-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "570", "publisher": "EDP Sciences", "pagerange": "Art. No. A16", "id_number": "CaltechAUTHORS:20141205-150242657", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141205-150242657", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council Advanced Grant", "grant_number": "ERC-2010-AdG-268107-EARLY" }, { "agency": "INAF", "grant_number": "PRIN 2010" }, { "agency": "INAF", "grant_number": "PRIN 2012" }, { "agency": "INAF", "grant_number": "PICS 2013" }, { "agency": "MIUR", "grant_number": "PRIN 2010\u20132011" }, { "agency": "ASI", "grant_number": "I/023/12/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201423811", "primary_object": { "basename": "1403.3691v2.pdf", "url": "https://authors.library.caltech.edu/records/v9v8t-95h16/files/1403.3691v2.pdf" }, "related_objects": [ { "basename": "aa23811-14.pdf", "url": "https://authors.library.caltech.edu/records/v9v8t-95h16/files/aa23811-14.pdf" } ], "pub_year": "2014", "author_list": "Cucciati, O.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/68ba2-61r07", "eprint_id": 58917, "eprint_status": "archive", "datestamp": "2023-08-20 02:59:03", "lastmod": "2023-10-23 19:52:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smol\u010di\u0107-Vernesa", "name": { "family": "Smol\u010di\u0107", "given": "Vernesa" }, "orcid": "0000-0002-3893-8614" }, { "id": "Ciliegi-Paolo", "name": { "family": "Ciliegi", "given": "Paolo" } }, { "id": "Jeli\u0107-Vibor", "name": { "family": "Jeli\u0107", "given": "Vibor" } }, { "id": "Bondi-Marco", "name": { "family": "Bondi", "given": "Marco" } }, { "id": "Schinnerer-Eva", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Carilli-Chris-L", "name": { "family": "Carilli", "given": "Chris L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Riechers-Domink-A", "name": { "family": "Riechers", "given": "Dominik A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Brkovi\u0107-Alen", "name": { "family": "Brkovi\u0107", "given": "Alen" } }, { "id": "Capak-Peter", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Karim-Alexander", "name": { "family": "Karim", "given": "Alexander" }, "orcid": "0000-0002-8414-9579" }, { "id": "McCracken-Henry-J", "name": { "family": "McCracken", "given": "Henry J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The VLA-COSMOS Survey - V. 324 MHz continuum observations", "ispublished": "pub", "full_text_status": "public", "keywords": "radiation mechanisms: general \u2013 surveys \u2013 radio continuum: galaxies", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2014 July 1. Received 2014 June 23; in original form 2014 April 1. First published online August 4, 2014.\n\nVS acknowledges the European Unions Seventh Frame-work\nprogramme grant agreement 333654 (CIG, 'AGN feedback')\nand the Australian Group of Eight European Fellowship 2013.\nThe National Radio Astronomy Observatory is a facility of the\nNational Science Foundation operated under cooperative agreement\nby Associated Universities, Inc. AK acknowledges support by the\nCollaborative Research Council 956, sub-project A1, funded by the\nDeutsche Forschungsgemeinschaft (DFG).\n\nPublished - MNRAS-2014-Smol_i_-2590-8.pdf
Submitted - 1407.4844v1.pdf
", "abstract": "We present 90 cm Very Large Array imaging of the COSMOS field, comprising a circular area of 3.14 square degrees at 8.0 arcsec \u00d7 6.0 arcsec angular resolution with an average rms of 0.5 mJy beam\u207b\u00b9. The extracted catalogue contains 182 sources (down to 5.5\u03c3), 30 of which are multicomponent sources. Using Monte Carlo artificial source simulations, we derive the completeness of the catalogue, and we show that our 90 cm source counts agree very well with those from previous studies. Using X-ray, NUV\u2013NIR and radio COSMOS data to investigate the population mix of our 90 cm radio sample, we find that our sample is dominated by active galactic nuclei. The average 90\u201320 cm spectral index (S_\u03bd\u2009\u221d\u2009\u03bd^\u03b1, where S_\u03bd is the flux density at frequency \u03bd and \u03b1 the spectral index) of our 90 cm selected sources is \u22120.70, with an interquartile range from \u22120.90 to \u22120.53. Only a few ultra-steep-spectrum sources are present in our sample, consistent with results in the literature for similar fields. Our data do not show clear steepening of the spectral index with redshift. Nevertheless, our sample suggests that sources with spectral indices steeper than \u22121 all lie at z \u2273 1, in agreement with the idea that ultra-steep-spectrum radio sources may trace intermediate-redshift galaxies (z \u2273 1).", "date": "2014-09-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "443", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2590-2598", "id_number": "CaltechAUTHORS:20150717-093344696", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150717-093344696", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "333654" }, { "agency": "Australian Group of Eight European Fellowship" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "956" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stu1331", "primary_object": { "basename": "MNRAS-2014-Smol_i_-2590-8.pdf", "url": "https://authors.library.caltech.edu/records/68ba2-61r07/files/MNRAS-2014-Smol_i_-2590-8.pdf" }, "related_objects": [ { "basename": "1407.4844v1.pdf", "url": "https://authors.library.caltech.edu/records/68ba2-61r07/files/1407.4844v1.pdf" } ], "pub_year": "2014", "author_list": "Smol\u010di\u0107, Vernesa; Ciliegi, Paolo; et el." }, { "id": "https://authors.library.caltech.edu/records/dgm9h-1rd30", "eprint_id": 50029, "eprint_status": "archive", "datestamp": "2023-08-22 13:36:18", "lastmod": "2023-10-17 22:27:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zahid-H-J", "name": { "family": "Zahid", "given": "H. J." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The FMOS-Cosmos Survey of Star-Forming Galaxies at z ~ 1.6 II. The Mass-Metallicity Relation and the Dependence on Star Formation Rate and Dust Extinction", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: abundances; galaxies: evolution; galaxies: fundamental parameters; galaxies: ISM", "note": "\u00a9 2014 American Astronomical Society. Received 2013 October 18; accepted 2014 July 8; published 2014 August 18.\n\nWe thank the anonymous referee for a careful reading and\nfor many useful suggestions that greatly improved this paper. This work is possible through the important contribution of Kentaro Aoki and the Subaru Telescope staff who assisted in acquiring much of the data presented in this work. This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. This work has been partially supported by the Grant-in-Aid for the Scientific Research Fund under grant Nos. 22340056: N.S., 23224005: N.A., 25707010 and Program for Leading Graduate Schools PhD Professional: Gateway to Success in Frontier Asia commissioned by the Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan. We are also grateful to INAF for regular support through grant \"PRIN-2010.\" We acknowledge the importance of Mauna Kea within the indigenous Hawaiian community and with all respect say mahalo for the use of this sacred site.\n\nPublished - 0004-637X_792_1_75.pdf
Submitted - 1310.4950v3.pdf
", "abstract": "We investigate the relationships between stellar mass, gas-phase oxygen abundance (metallicity), star formation rate (SFR), and dust content of star-forming galaxies at z ~ 1.6 using Subaru/FMOS spectroscopy in the COSMOS field. The mass-metallicity (MZ) relation at z ~ 1.6 is steeper than the relation observed in the local universe. The steeper MZ relation at z ~ 1.6 is mainly due to evolution in the stellar mass where the MZ relation begins to turnover and flatten. This turnover mass is 1.2 dex larger at z ~ 1.6. The most massive galaxies at z ~ 1.6 (~10^(11) M_\u2609) are enriched to the level observed in massive galaxies in the local universe. The MZ relation we measure at z ~ 1.6 supports the suggestion of an empirical upper metallicity limit that does not significantly evolve with redshift. We find an anti-correlation between metallicity and SFR for galaxies at a fixed stellar mass at z ~ 1.6, which is similar to trends observed in the local universe. We do not find a relation between stellar mass, metallicity, and SFR that is independent of redshift; rather, our data suggest that there is redshift evolution in this relation. We examine the relation between stellar mass, metallicity, and dust extinction, and find that at a fixed stellar mass, dustier galaxies tend to be more metal rich. From examination of the stellar masses, metallicities, SFRs, and dust extinctions, we conclude that stellar mass is most closely related to dust extinction.", "date": "2014-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "792", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 75", "id_number": "CaltechAUTHORS:20140925-105920968", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140925-105920968", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan" }, { "agency": "Grant-in-Aid for the Scientific Research Fund", "grant_number": "22340056" }, { "agency": "Grant-in-Aid for the Scientific Research Fund", "grant_number": "23224005" }, { "agency": "Grant-in-Aid for the Scientific Research Fund", "grant_number": "25707010" }, { "agency": "INAF", "grant_number": "PRIN-2010" }, { "agency": "Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "COSMOS Team" ] }, "doi": "10.1088/0004-637X/792/1/75", "primary_object": { "basename": "0004-637X_792_1_75.pdf", "url": "https://authors.library.caltech.edu/records/dgm9h-1rd30/files/0004-637X_792_1_75.pdf" }, "related_objects": [ { "basename": "1310.4950v3.pdf", "url": "https://authors.library.caltech.edu/records/dgm9h-1rd30/files/1310.4950v3.pdf" } ], "pub_year": "2014", "author_list": "Zahid, H. J.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/4601w-8rw65", "eprint_id": 50178, "eprint_status": "archive", "datestamp": "2023-08-20 02:35:18", "lastmod": "2023-10-17 22:49:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steinhardt-C-L", "name": { "family": "Steinhardt", "given": "Charles L." }, "orcid": "0000-0003-3780-6801" }, { "id": "Speagle-J-S", "name": { "family": "Speagle", "given": "Josh S." }, "orcid": "0000-0002-5065-9896" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "John D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "Marcella C." }, "orcid": "0000-0003-1624-7609" }, { "id": "Dunlop-J-S", "name": { "family": "Dunlop", "given": "James" } }, { "id": "Hashimoto-Yasuhiro", "name": { "family": "Hashimoto", "given": "Yasuhiro" } }, { "id": "Hsieh-Bau-Ching", "name": { "family": "Hsieh", "given": "Bau-Ching" }, "orcid": "0000-0001-5615-4904" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "Olivier" }, "orcid": "0000-0001-5891-2596" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "Emeric" } }, { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "Nicholas" } }, { "id": "Lin-Lihwai", "name": { "family": "Lin", "given": "Lihwai" }, "orcid": "0000-0001-7218-7407" }, { "id": "Lin-Yen-Ting", "name": { "family": "Lin", "given": "Yen-Ting" } }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "Dan" }, "orcid": "0000-0001-5382-6138" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "Henry J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "Tohru" }, "orcid": "0000-0002-7402-5441" }, { "id": "Petric-A-O", "name": { "family": "Petric", "given": "Andreea" }, "orcid": "0000-0003-4030-3455" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "Dave" }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Strauss-M-A", "name": { "family": "Strauss", "given": "Michael A." }, "orcid": "0000-0002-0106-7755" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Yoshiaki" }, "orcid": "0000-0003-2247-3741" } ] }, "title": "Star Formation at 4 < z < 6 from the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH)", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution", "note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2014 April 7; accepted 2014 June 22; published 2014 August 6.\n\nThe authors would like to thank Steve Bickerton, Sean Carey,\nMartin Elvis, and Brian Feldstein for helpful comments.\n\nPublished - 2041-8205_791_2_L25.pdf
Submitted - 1407.7030v1.pdf
", "abstract": "Using the first 50% of data collected for the Spitzer Large Area Survey with Hyper-Suprime-Cam observations on the 1.8 deg^2 Cosmological Evolution Survey we estimate the masses and star formation rates of 3398 M_* > 10^(10) M_\u2609 star-forming galaxies at 4 < z < 6 with a substantial population up to M_* \u2273 10^(11.5) M_\u2609. We find that the strong correlation between stellar mass and star formation rate seen at lower redshift (the \"main sequence\" of star-forming galaxies) extends to z ~ 6. The observed relation and scatter is consistent with a continued increase in star formation rate at fixed mass in line with extrapolations from lower-redshift observations. It is difficult to explain this continued correlation, especially for the most massive systems, unless the most massive galaxies are forming stars near their Eddington-limited rate from their first collapse. Furthermore, we find no evidence for moderate quenching at higher masses, indicating quenching either has not occurred prior to z ~ 6 or else occurs rapidly, so that few galaxies are visible in transition between star-forming and quenched.", "date": "2014-08-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "791", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L25", "id_number": "CaltechAUTHORS:20141002-133810713", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141002-133810713", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "SPLASH" } ] }, "doi": "10.1088/2041-8205/791/2/L25", "primary_object": { "basename": "1407.7030v1.pdf", "url": "https://authors.library.caltech.edu/records/4601w-8rw65/files/1407.7030v1.pdf" }, "related_objects": [ { "basename": "2041-8205_791_2_L25.pdf", "url": "https://authors.library.caltech.edu/records/4601w-8rw65/files/2041-8205_791_2_L25.pdf" } ], "pub_year": "2014", "author_list": "Steinhardt, Charles L.; Speagle, Josh S.; et el." }, { "id": "https://authors.library.caltech.edu/records/8rhxw-xy327", "eprint_id": 50602, "eprint_status": "archive", "datestamp": "2023-08-20 02:19:58", "lastmod": "2023-10-20 23:09:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Amor\u00edn-Ricardo-O", "name": { "family": "Amor\u00edn", "given": "R." }, "orcid": "0000-0001-5758-1000" }, { "id": "Capak-Peter", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Discovering extremely compact and metal-poor, star-forming dwarf galaxies out to z \u223c 0.9 in the VIMOS Ultra-Deep Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: high-redshift, galaxies: starburst, galaxies: abundances, galaxies: dwarf, galaxies: fundamental parameters", "note": "\u00a9 2014 ESO. Received 15 March 2014. Accepted 2 July 2014. Published online 19 August 2014. \n\nWe thank the anonymous referee for helpful comments that helped to improve this manuscript. We thank the ESO staff for their continuous support for the VUDS survey, particularly the Paranal staff conducting the observations and Marina Rejkuba and the ESO user support group in Garching. This work is supported by funding from the European Research Council Advanced Grant ERC-2010-AdG-268107-EARLY and by INAF Grants PRIN 2010, PRIN 2012 and PICS 2013. RA and AF acknowledge the FP7 SPACE project ASTRODEEP (Ref. No: 312725), supported by the European\nCommission. A.C., O.C., M.T. and V.S. acknowledge the grant MIUR PRIN 2010\u20132011. D.M. gratefully acknowledges LAM hospitality during the initial phases of the project. This work is based on data products made available at the CESAM data center, Laboratoire d'Astrophysique de Marseille. This work partly uses observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which\nis operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based\nin part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS.\n\nPublished - aa23816-14.pdf
Submitted - 1403.3692v1.pdf
", "abstract": "We report the discovery of 31 low-luminosity (\u221214.5 \u2273 M_(AB)(B) \u2273 \u221218.8), extreme emission line galaxies (EELGs) at 0.2 \u2272 z \u2272 0.9 identified by their unusually high rest-frame equivalent widths (100\u2009\u2264\u2009EW[O\u2009iii]\u2009\u2264\u20091700 \u00c5) as part of the VIMOS Ultra Deep Survey (VUDS). VIMOS optical spectra of unprecedented sensitivity (I_(AB)\u2009~\u200925\u2009mag) along with multiwavelength photometry and HST imaging are used to investigate spectrophotometric properties of this unique sample and to explore, for the first time, the very low stellar mass end (M* \u2272 10^8M_\u2299) of the luminosity-metallicity (LZR) and mass-metallicity (MZR) relations at z < 1. Characterized by their extreme compactness (R_50 <\u20091 kpc), low stellar mass and enhanced specific star formation rates (sSFR = SFR/M_* ~ 10^(-9)\u221210^(-7) yr^(-1)), the VUDS EELGs are blue dwarf galaxies likely experiencing the first stages of a vigorous galaxy-wide starburst. Using T_e-sensitive direct and strong-line methods, we find that VUDS EELGs are low-metallicity (7.5 \u2272 12 + log\u2009 (O/H) \u2272 8.3) galaxies with high ionization conditions (log\u2009(q_(ion))\u2009\u2273\u20098\u2009cm\u2009s^(-1)), including at least three EELGs showing Heii\u03bb\u20094686 \u00c5 emission and four extremely metal-poor (\u227210% solar) galaxies. The LZR and MZR followed by VUDS EELGs show relatively large scatter, being broadly consistent with the extrapolation toward low luminosity and mass from previous studies at similar redshift. However, we find evidence that galaxies with younger and more vigorous star formation \u2013 as characterized by their larger EWs, ionization and sSFR \u2013 tend to be more metal poor at a given stellar mass.", "date": "2014-08", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "568", "publisher": "EDP Sciences", "pagerange": "Art. No. L8", "id_number": "CaltechAUTHORS:20141021-101119830", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141021-101119830", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "268107" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2010" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2012" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PICS 2013" }, { "agency": "European Research Council (ERC)", "grant_number": "312725" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201423816", "primary_object": { "basename": "1403.3692v1.pdf", "url": "https://authors.library.caltech.edu/records/8rhxw-xy327/files/1403.3692v1.pdf" }, "related_objects": [ { "basename": "aa23816-14.pdf", "url": "https://authors.library.caltech.edu/records/8rhxw-xy327/files/aa23816-14.pdf" } ], "pub_year": "2014", "author_list": "Amor\u00edn, R.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/ars92-jdh44", "eprint_id": 46400, "eprint_status": "archive", "datestamp": "2023-08-20 01:23:35", "lastmod": "2023-10-26 19:43:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Delaye-L", "name": { "family": "Delaye", "given": "L." } }, { "id": "Huertas-Company-M", "name": { "family": "Huertas-Company", "given": "M." } }, { "id": "Mei-Simona", "name": { "family": "Mei", "given": "S." }, "orcid": "0000-0002-2849-559X" }, { "id": "Lidman-C", "name": { "family": "Lidman", "given": "C." }, "orcid": "0000-0003-1731-0497" }, { "id": "Licitra-R", "name": { "family": "Licitra", "given": "R." } }, { "id": "Newman-A-B", "name": { "family": "Newman", "given": "A. B." }, "orcid": "0000-0001-7769-8660" }, { "id": "Raichoor-A", "name": { "family": "Raichoor", "given": "A." } }, { "id": "Shankar-F", "name": { "family": "Shankar", "given": "F." } }, { "id": "Barrientos-F", "name": { "family": "Barrientos", "given": "F." } }, { "id": "Bernardi-Mariangela", "name": { "family": "Bernardi", "given": "M." } }, { "id": "Cerulo-P", "name": { "family": "Cerulo", "given": "P." } }, { "id": "Couch-W", "name": { "family": "Couch", "given": "W." } }, { "id": "Demarco-R", "name": { "family": "Demarco", "given": "R." }, "orcid": "0000-0003-3921-2177" }, { "id": "Mu\u00f1oz-R", "name": { "family": "Mu\u00f1oz", "given": "R." } }, { "id": "S\u00e1nchez-Janssen-R", "name": { "family": "S\u00e1nchez-Janssen", "given": "R." } }, { "id": "Tanaka-M", "name": { "family": "Tanaka", "given": "M." } } ] }, "title": "Larger sizes of massive quiescent early-type galaxies in clusters than in the field at 0.8 < z < 1.5", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general\n galaxies: elliptical and lenticular\n galaxies: evolution", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2014 March 9. Received 2014 February 28; in original form 2013 May 2. \n\nThe authors would like to thank G. Rousset for pointing out interesting suggestions and E. Daddi, V. Strazzulo, R. Gobat for stimulating discussions. RD gratefully acknowledges the support provided by the BASAL Center for Astrophysics and Associated Technologies (CATA), and by FONDECYT grant no. 1130528.\n\nPublished - MNRAS-2014-Delaye-203-23.pdf
Submitted - 1307.0003v1.pdf
Supplemental Material - tex_table.tex
", "abstract": "We analyse the mass\u2013size relation of \u223c400 quiescent massive ETGs (M_*/M_\u2299 > 3 \u00d7 10^(10)) hosted by massive clusters (M_(200 \u223c 2\u20137) \u00d7 10^(14)M_\u2299) at 0.8 < z < 1.5, compared to those found in the field at the same epoch. Size is parametrized using the mass-normalized B-band rest-frame size, \u03b3=R_e/M^(0.57)_(11). We find that the \u03b3 distributions in both environments peak at the same position, but the distributions in clusters are more skewed towards larger sizes. This tail induces average sizes \u223c30\u201340 per\u2009cent larger for cluster galaxies than for field galaxies of similar stellar mass, while the median sizes are statistically the same with a difference of \u223c10 \u00b1 10 per\u2009cent. Since this size difference is not observed in the local Universe, the evolution of average galaxy size at fixed stellar mass from z \u223c 1.5 for cluster galaxies is less steep at more than 3\u03c3 (\u221d(1 + z)^(\u22120.53 \u00b1 0.04)) than the evolution of field galaxies (\u221d(1 + z)^(\u22120.92 \u00b1 0.04)). The difference in evolution is not measured when the median values of \u03b3 are considered: \u221d(1 + z)^(\u22120.84 \u00b1 0.04) in the field versus \u221d(1 + z)^(\u22120.71 \u00b1 0.05) in clusters. In our sample, the tail of large galaxies is dominated by galaxies with 3 \u00d7 10^(10) < M_*/M_\u2299 < 10^(11). At this low-mass end, the difference in the average size is better explained by the accretion of new galaxies that are quenched more efficiently in clusters and/or by different morphological mixing in the cluster and field environments. If part of the size evolution would be due to mergers, the difference that we see between cluster and field galaxies could be caused by higher merger rates in clusters at higher redshift, when galaxy velocities are lower.", "date": "2014-06-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "441", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "203-223", "id_number": "CaltechAUTHORS:20140620-131059224", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140620-131059224", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "BASAL Center for Astrophysics and Associated Technologies (CATA)" }, { "agency": "FONDECYT", "grant_number": "1130528" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stu496", "primary_object": { "basename": "1307.0003v1.pdf", "url": "https://authors.library.caltech.edu/records/ars92-jdh44/files/1307.0003v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2014-Delaye-203-23.pdf", "url": "https://authors.library.caltech.edu/records/ars92-jdh44/files/MNRAS-2014-Delaye-203-23.pdf" }, { "basename": "tex_table.tex", "url": "https://authors.library.caltech.edu/records/ars92-jdh44/files/tex_table.tex" } ], "pub_year": "2014", "author_list": "Delaye, L.; Huertas-Company, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/n3gmy-84z77", "eprint_id": 47097, "eprint_status": "archive", "datestamp": "2023-08-22 12:56:45", "lastmod": "2023-10-26 20:18:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "A. L." }, "orcid": "0000-0002-9382-9832" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Spectroscopic Observation of Ly\u03b1 Emitters at z ~ 7.7 and Implications on Re-ionization", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; dark ages, reionization, first stars; galaxies: formation; galaxies: high-redshift; line: identification", "note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2014 February 12; accepted 2014 April 23; published 2014 May 23.\n\nWe would like to acknowledge the support of the Keck\nObservatory staff who made these observations possible as well as B. Trakhtenbrot and W. Hartley for valuable discussions. We also thank Nick Konidaris for providing and supporting the MOSFIRE reduction pipeline and Gwen Rudie for providing the MOSFIRE exposure time calculator. A.F. acknowledges support from the Swiss National Science Foundation. A.F. also thanks Caltech for hospitality while working on this article. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always\nhad within the indigenous Hawaiian community. We are most\nfortunate to have the opportunity to conduct observations from this mountain.\nFacility: Keck:I (MOSFIRE)\n\nPublished - 0004-637X_788_1_87.pdf
", "abstract": "We present spectroscopic follow-up observations on two bright Ly\u03b1 emitter (LAE) candidates originally found by Krug et al. at a redshift of z ~ 7.7 using the Multi-Object Spectrometer for Infra-Red Exploration at Keck. We rule out any line emission at the >5\u03c3 level for both objects, putting on solid ground a previous null result for one of the objects. The limits inferred from the non-detections rule out the previous claim of no or even reversed evolution between 5.7 < z < 7.7 in the Ly\u03b1 luminosity function (LF) and suggest a drop in the Ly\u03b1 LF consistent with that seen in Lyman break galaxy (LBG) samples. We model the redshift evolution of the LAE LF using the LBG UV-continuum LF and the observed rest-frame equivalent width distribution. From the comparison of our empirical model with the observed LAE distribution, we estimate lower limits of the neutral hydrogen fraction to be 50%\u201370% at z ~ 7.7. Together with this, we find a strong evolution in the Ly\u03b1 optical depth characterized by (1 + z)^(2.2 \u00b1 0.5) beyond z = 6, indicative of a strong evolution of the intergalactic medium. Finally, we extrapolate the LAE LF to z ~ 9 using our model and show that it is unlikely that large area surveys, like UltraVISTA or Euclid, pick up LAEs at this redshift assuming the current depths and area.", "date": "2014-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "788", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 87", "id_number": "CaltechAUTHORS:20140709-092326688", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140709-092326688", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swiss National Science Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/788/1/87", "primary_object": { "basename": "0004-637X_788_1_87.pdf", "url": "https://authors.library.caltech.edu/records/n3gmy-84z77/files/0004-637X_788_1_87.pdf" }, "pub_year": "2014", "author_list": "Faisst, A. L.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/fnerk-g7875", "eprint_id": 47083, "eprint_status": "archive", "datestamp": "2023-08-22 12:56:33", "lastmod": "2023-10-26 20:18:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shibuya-Takatoshi", "name": { "family": "Shibuya", "given": "Takatoshi" } }, { "id": "Ouchi-Masami", "name": { "family": "Ouchi", "given": "Masami" }, "orcid": "0000-0002-1049-6658" }, { "id": "Nakajima-Kimihiko", "name": { "family": "Nakajima", "given": "Kimihiko" } }, { "id": "Hashimoto-Takuya", "name": { "family": "Hashimoto", "given": "Takuya" } }, { "id": "Ono-Yoshiaki", "name": { "family": "Ono", "given": "Yoshiaki" } }, { "id": "Rauch-M", "name": { "family": "Rauch", "given": "Michael" } }, { "id": "Gauthier-J-R", "name": { "family": "Gauthier", "given": "Jean-Ren\u00e9" } }, { "id": "Shimasaku-Kazuhiro", "name": { "family": "Shimasaku", "given": "Kazuhiro" } }, { "id": "Goto-Ryosuke", "name": { "family": "Goto", "given": "Ryosuke" } }, { "id": "Mori-Masao", "name": { "family": "Mori", "given": "Masao" } }, { "id": "Umemura-Masayuki", "name": { "family": "Umemura", "given": "Masayuki" } } ] }, "title": "What is the Physical Origin of Strong Ly\u03b1 Emission? II. Gas Kinematics and Distribution of Ly\u03b1 Emitters", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; early universe; galaxies: formation; galaxies: high-redshift", "note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2014 February 2; accepted 2014 April 28; published 2014 May 22.\n\nBased on data obtained with the Subaru Telescope operated by the National\nAstronomical Observatory of Japan.\n\nWe thank Anne Verhamme, Zheng Zheng, Lennox L. Cowie,\nEsther M. Hu, and James E. Rhoads for useful discussions,\nand an anonymous referee, Mark Dijkstra, and Lucia Guaita\nfor constructive comments. This paper is based on data collected\nwith the Subaru Telescope, which is operated by the\nNational Astronomical Observatory of Japan. Some of the data\npresented herein were obtained at the W.M. Keck Observatory,\nwhich is operated as a scientific partnership among the California\nInstitute of Technology, the University of California, and the\nNational Aeronautics and Space Administration. The Observatory\nwas made possible by the generous financial support of the\nW.M. Keck Foundation. The reduction pipeline used to reduce\nthe LRIS data was developed at UC Berkeley with support from\nNSF grant AST-0071048. This work is based on observations\ntaken by the CANDELS Multi-Cycle Treasury Program with\nthe NASA/ESA HST, which is operated by the Association\nof Universities for Research in Astronomy, Inc., under NASA\ncontract NAS5-26555. The NB387 data used in this work were\ncollected at the Subaru Telescope, which is operated by the National\nAstronomical Observatory of Japan. This work is based\nin part on observations made with the Spitzer Space Telescope,\nwhich is operated by the Jet Propulsion Laboratory, California\nInstitute of Technology, under a contract with NASA. Support\nfor this work was provided by NASA through an award issued\nby JPL/Caltech. This work was supported by World Premier International\nResearch Center Initiative (WPI Initiative), MEXT,\nJapan. This work was supported by KAKENHI (23244025) and\n(21244013) Grant-in-Aid for Scientific Research (A) through\nJapan Society for the Promotion of Science (JSPS). M.R. was\nsupported by NSF grant AST-1108815.\nFacilities: Subaru (Suprime-Cam, FMOS), Keck:I (LRIS),\nMagellan:Baade (IMACS).\n\nPublished - 0004-637X_788_1_74.pdf
Submitted - 1402.1168v2.pdf
", "abstract": "We present a statistical study of velocities of Ly\u03b1, interstellar (IS) absorption, and nebular lines and gas covering fraction for Ly\u03b1 emitters (LAEs) at z \u2243 2. We make a sample of 22 LAEs with a large Ly\u03b1 equivalent width (EW) of \u227350 \u00c5 based on our deep Keck/Low Resolution Imaging Spectrometer (LRIS) observations, in conjunction with spectroscopic data from the Subaru/Fiber Multi Object Spectrograph program and the literature. We estimate the average velocity offset of Ly\u03b1 from a systemic redshift determined with nebular lines to be \u0394v_(Ly\u03b1) = 234 \u00b1 9 km s^(\u20131). Using a Kolmogorov-Smirnov test, we confirm the previous claim of Hashimoto et al. that the average \u0394v Ly\u03b1 of LAEs is smaller than that of Lyman break galaxies (LBGs). Our LRIS data successfully identify blueshifted multiple IS absorption lines in the UV continua of four LAEs on an individual basis. The average velocity offset of IS absorption lines from a systemic redshift is \u0394v_(IS) = 204 \u00b1 27 km s^(\u20131), indicating LAEs' gas outflow with a velocity comparable to typical LBGs. Thus, the ratio R^(Ly\u03b1)_(IS) \u2261 \u0394\u03bd_(Ly\u03b1)/\u0394\u03bd_(IS) of LAEs is around unity, suggestive of low impacts on Ly\u03b1 transmission by resonant scattering of neutral hydrogen in the IS medium. We find an anti-correlation between Ly\u03b1 EW and the covering fraction, f_c, estimated from the depth of absorption lines, where f_c is an indicator of average neutral hydrogen column density, N_(H I) . The results of our study support the idea that N_(H I) is a key quantity determining Ly\u03b1 emissivity.", "date": "2014-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "788", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 74", "id_number": "CaltechAUTHORS:20140708-152853456", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140708-152853456", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NSF", "grant_number": "AST-0071048" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23244025" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21244013" }, { "agency": "NSF", "grant_number": "AST-1108815" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/788/1/74", "primary_object": { "basename": "0004-637X_788_1_74.pdf", "url": "https://authors.library.caltech.edu/records/fnerk-g7875/files/0004-637X_788_1_74.pdf" }, "related_objects": [ { "basename": "1402.1168v2.pdf", "url": "https://authors.library.caltech.edu/records/fnerk-g7875/files/1402.1168v2.pdf" } ], "pub_year": "2014", "author_list": "Shibuya, Takatoshi; Ouchi, Masami; et el." }, { "id": "https://authors.library.caltech.edu/records/jn0gn-s8752", "eprint_id": 78704, "eprint_status": "archive", "datestamp": "2023-08-20 01:00:10", "lastmod": "2023-10-26 00:18:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bowler-R-A-A", "name": { "family": "Bowler", "given": "R. A. A." } }, { "id": "Dunlop-J-S", "name": { "family": "Dunlop", "given": "J. S." } }, { "id": "McLure-R-J", "name": { "family": "McLure", "given": "R. J." } }, { "id": "Rogers-A-B", "name": { "family": "Rogers", "given": "A. B." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Milvang-Jensen-B", "name": { "family": "Milvang-Jensen", "given": "B." }, "orcid": "0000-0002-2281-2785" }, { "id": "Furusawa-H", "name": { "family": "Furusawa", "given": "H." } }, { "id": "Fynbo-J-P-U", "name": { "family": "Fynbo", "given": "J. P. U." }, "orcid": "0000-0002-8149-8298" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Afonso-J", "name": { "family": "Afonso", "given": "J." }, "orcid": "0000-0002-9149-2973" }, { "id": "Bremer-M-N", "name": { "family": "Bremer", "given": "M. N." } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" } ] }, "title": "The bright end of the galaxy luminosity function at z =7: before the onset of mass quenching?", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2014 March 4. Received 2014 March 4; in original form 2013 December 20.", "abstract": "We present the results of a new search for bright star-forming galaxies at redshift z \u2243 7 within the UltraVISTA second data release (DR2) and UKIDSS (UKIRT Infrared Deep Sky Survey) UDS (Ultra Deep Survey) DR10 data, which together provide 1.65 deg^2 of near-infrared imaging with overlapping optical and Spitzer data. Using a full photometric redshift analysis, to identify high-redshift galaxies and reject contaminants, we have selected a sample of 34 luminous (\u221222.7", "date": "2014-05-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "440", "number": "3", "publisher": "Oxford University Press", "pagerange": "2810-2842", "id_number": "CaltechAUTHORS:20170629-131638272", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170629-131638272", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "SPLASH" }, { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stu449", "pub_year": "2014", "author_list": "Bowler, R. A. A.; Dunlop, J. S.; et el." }, { "id": "https://authors.library.caltech.edu/records/038ex-ype66", "eprint_id": 46309, "eprint_status": "archive", "datestamp": "2023-08-22 12:39:34", "lastmod": "2023-10-26 19:39:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Del-Moro-A", "name": { "family": "Del Moro", "given": "A." } }, { "id": "Balokovi\u0107-M", "name": { "family": "Balokovi\u0107", "given": "M." } }, { "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "F. A." }, "orcid": "0000-0003-2992-8024" } ] }, "title": "NuSTAR J033202-2746.8: Direct Constraints on the Compton Reflection in a Heavily Obscured Quasar at z \u2248 2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; infrared: galaxies; quasars: general; quasars: individual (NuSTAR J033202-2746.8); X-rays: galaxies", "note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2013 December 23; accepted 2014 March 9; published 2014 April 10.\n\nWe thank the anonymous referee for careful reading and for\nthe helpful comments, which helped improving this manuscript.\nWe gratefully acknowledge financial support from the UK Science\nand Technology Facilities Council (STFC, ST/I001573/I,\nADM and DMA; ST/K501979/1, GBL; ST/J003697/1, PG)\nand the Leverhulme Trust (D.M.A. and J.R.M.). A.C., C.V.,\nR.G., and P.R. thank the ASI/INAF grant I/037/12/0-011/\n13. F.E.B. acknowledges support from Basal-CATA (PFB-06/\n2007) and CONICYT-Chile (FONDECYT 1101024 and Anillo\ngrant ACT1101) and E.T. acknowledges the FONDECYT grant\n1120061. W.N.B. and B.L. thank Caltech NuSTAR subcontract\n44A-1092750 and NASA ADP grant NNX10AC99G. M.B. acknowledges\nthe International Fulbright Science and Technology\nAward. This work was supported under NASA Contract\nNo. NNG08FD60C, and made use of data from the NuSTAR\nmission, a project led by the California Institute of Technology,\nmanaged by the Jet Propulsion Laboratory, and funded by\nthe National Aeronautics and Space Administration. We thank\nthe NuSTAR Operations, Software and Calibration teams for\nsupport with the execution and analysis of these observations.\nThis research has made use of the NuSTAR Data Analysis Software\n(NuSTARDAS) jointly developed by the ASI Science Data\nCenter (ASDC, Italy) and the California Institute of Technology\n(USA). This work also used observations made with ESO Telescopes\nat the La Silla Paranal Observatory under the program\nID 092.A-0452.\n\nPublished - 0004-637X_786_1_16.pdf
Submitted - 1403.2491v1.pdf
", "abstract": "We report Nuclear Spectroscopic Telescope Array (NuSTAR) observations of NuSTAR J033202-2746.8, a heavily obscured, radio-loud quasar detected in the Extended Chandra Deep Field-South, the deepest layer of the NuSTAR extragalactic survey (~400 ks, at its deepest). NuSTAR J033202-2746.8 is reliably detected by NuSTAR only at E > 8 keV and has a very flat spectral slope in the NuSTAR energy band (\u0393 = 0.55^(+0.62)_(-0.64); 3-30 keV). Combining the NuSTAR data with extremely deep observations by Chandra and XMM-Newton (4 Ms and 3 Ms, respectively), we constrain the broad-band X-ray spectrum of NuSTAR J033202-2746.8, indicating that this source is a heavily obscured quasar (N_H = 5.6^(+0.9)_(-0.8) x 10^(23) cm^(\u20132)) with luminosity L_(10-40 keV) \u22486.4 \u00d7 10^(44) erg s^(\u20131). Although existing optical and near-infrared (near-IR) data, as well as follow-up spectroscopy with the Keck and VLT telescopes, failed to provide a secure redshift identification for NuSTAR J033202-2746.8, we reliably constrain the redshift z = 2.00 \u00b1 0.04 from the X-ray spectral features (primarily from the iron K edge). The NuSTAR spectrum shows a significant reflection component (R = 0.55^(0.44)_(-0.37)), which was not constrained by previous analyses of Chandra and XMM-Newton data alone. The measured reflection fraction is higher than the R ~ 0 typically observed in bright radio-loud quasars such as NuSTAR J033202-2746.8, which has L_(1.4 GHz) \u224810^(27) W Hz^(\u20131). Constraining the spectral shape of active galactic nuclei (AGNs), including bright quasars, is very important for understanding the AGN population, and can have a strong impact on the modeling of the X-ray background. Our results show the importance of NuSTAR in investigating the broad-band spectral properties of quasars out to high redshift.", "date": "2014-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "786", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 16", "id_number": "CaltechAUTHORS:20140617-132453849", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140617-132453849", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I001573/I" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/K501979/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/J003697/1" }, { "agency": "Leverhulme Trust" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/037/12/0-011/13" }, { "agency": "Basal-CATA", "grant_number": "PFB-06/2007" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "FONDECYT 1101024" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "Anillo ACT1101" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1120061" }, { "agency": "Caltech NuSTAR subcontract", "grant_number": "44A-1092750" }, { "agency": "NASA", "grant_number": "NNX10AC99G" }, { "agency": "International Fulbright Science and Technology Award" }, { "agency": "NASA", "grant_number": "NNG08FD60C" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "other_numbering_system": { "items": [ { "id": "2014-58", "name": "Space Radiation Laboratory" } ] }, "local_group": { "items": [ { "id": "NuSTAR" }, { "id": "COSMOS" }, { "id": "Space-Radiation-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/786/1/16", "primary_object": { "basename": "0004-637X_786_1_16.pdf", "url": "https://authors.library.caltech.edu/records/038ex-ype66/files/0004-637X_786_1_16.pdf" }, "related_objects": [ { "basename": "1403.2491v1.pdf", "url": "https://authors.library.caltech.edu/records/038ex-ype66/files/1403.2491v1.pdf" } ], "pub_year": "2014", "author_list": "Del Moro, A.; Balokovi\u0107, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/3tvhd-kyc44", "eprint_id": 46279, "eprint_status": "archive", "datestamp": "2023-08-22 12:39:15", "lastmod": "2023-10-26 19:38:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Murata-K-L", "name": { "family": "Murata", "given": "K. L." } }, { "id": "Kajisawa-Masaru", "name": { "family": "Kajisawa", "given": "M." }, "orcid": "0000-0002-1732-6387" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Kobayashi-M-A-R", "name": { "family": "Kobayashi", "given": "M. A. R." } }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Evolution of the Fraction of Clumpy Galaxies at 0.2 < z < 1.0 in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: irregular; galaxies: star formation", "note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2013 December 12; accepted 2014 March 6; published 2014 April 10.\n\nBased on observations with the NASA/ESA Hubble Space Telescope,\nobtained at the Space Telescope Science Institute, which is operated by\nAURA, Inc., under NASA contract NAS 5-26555. Also based on observations\nmade with the Spitzer Space Telescope, which is operated by the Jet\nPropulsion Laboratory, California Institute of Technology, under NASA\ncontract 1407. Also based on data collected at the Subaru Telescope, which is\noperated by the National Astronomical Observatory of Japan; the\nXMM-Newton, an ESA science mission with instruments and contributions\ndirectly funded by ESA Member States and NASA; the European Southern\nObservatory under Large Program 175.A-0839, Chile; Kitt Peak National\nObservatory, Cerro Tololo Inter-American Observatory and the National\nOptical Astronomy Observatory, which are operated by the Association of\nUniversities for Research in Astronomy, Inc. (AURA), under cooperative\nagreement with the National Science Foundation; and the\nCanada\u2013France\u2013Hawaii Telescope with MegaPrime/MegaCam operated as a\njoint project by the CFHT Corporation, CEA/DAPNIA, the NRC and CADC\nof Canada, the CNRS of France, TERAPIX, and the University of Hawaii.\n\nWe thank the anonymous referee for valuable comments\nand suggestions. We also thank Tsutomu T. Takeuchi at\nNagoya University for his generous support to K.L.M. and\nfor useful discussions. The HST COSMOS Treasury program\nwas supported through NASA grant HST-GO-09822. We\ngreatly acknowledge the contributions of the entire COSMOS collaboration, consisting of more than 70 scientists. This work\nwas financially supported in part by the Japan Society for the\nPromotion of Science (Nos. 17253001, 19340046, 23244031,\nand 23740152).\n\nPublished - 0004-637X_786_1_15.pdf
Submitted - 1403.1496v1.pdf
", "abstract": "Using the Hubble Space Telescope/Advanced Camera for Surveys data in the COSMOS field, we systematically searched clumpy galaxies at 0.2 < z < 1.0 and investigated the fraction of clumpy galaxies and its evolution as a function of stellar mass, star formation rate (SFR), and specific SFR (SSFR). The fraction of clumpy galaxies in star-forming galaxies with M_(star) > 10^(9.5) M\u2609 decreases with time from ~0.35 at 0.8 < z < 1.0 to ~0.05 at 0.2 < z < 0.4, irrespective of the stellar mass, although the fraction tends to be slightly lower for massive galaxies with M_(star) > 10^(10.5) M\u2609 at each redshift. On the other hand, the fraction of clumpy galaxies increases with increasing both SFR and SSFR in all the redshift ranges we investigated. In particular, we found that the SSFR dependences of the fractions are similar among galaxies with different stellar masses, and the fraction at a given SSFR does not depend on the stellar mass in each redshift bin. The evolution of the fraction of clumpy galaxies from z ~ 0.9 to z ~ 0.3 seems to be explained by such SSFR dependence of the fraction and the evolution of SSFRs of star-forming galaxies. The fraction at a given SSFR also appears to decrease with time, but this can be due to the effect of the morphological k correction. We suggest that these results are understood by the gravitational fragmentation model for the formation of giant clumps in disk galaxies, where the gas mass fraction is a crucial parameter.", "date": "2014-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "786", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 15", "id_number": "CaltechAUTHORS:20140616-111641778", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140616-111641778", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17253001" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19340046" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23244031" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23740152" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/786/1/15", "primary_object": { "basename": "0004-637X_786_1_15.pdf", "url": "https://authors.library.caltech.edu/records/3tvhd-kyc44/files/0004-637X_786_1_15.pdf" }, "related_objects": [ { "basename": "1403.1496v1.pdf", "url": "https://authors.library.caltech.edu/records/3tvhd-kyc44/files/1403.1496v1.pdf" } ], "pub_year": "2014", "author_list": "Murata, K. L.; Kajisawa, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/ac1sh-47h89", "eprint_id": 48765, "eprint_status": "archive", "datestamp": "2023-08-22 12:36:49", "lastmod": "2023-10-17 20:25:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mandelbaum-R", "name": { "family": "Mandelbaum", "given": "Rachel" }, "orcid": "0000-0003-2271-1527" }, { "id": "Rhodes-J", "name": { "family": "Rhodes", "given": "Jason" } } ] }, "title": "The Third Gravitational Lensing Accuracy Testing (GREAT3) Challenge Handbook", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: weak; methods: data analysis; methods: statistical; techniques: image processing", "note": "\u00a9 2014 American Astronomical Society.\n\nReceived 2013 August 29; accepted 2014 March 22; published 2014 April 17.\n\nThe authors of this work benefited greatly from discussions\nwith Christopher Hirata, Gary Bernstein, Lance Miller, and Erin Sheldon; the WFIRST project office, including David Content; the Euclid Consortium; and the LSST imSim team, including En-Hsin Peng; and Peter Freeman. We thank the PASCAL-2 network for its sponsorship of the challenge. This work was supported in part by the National Science Foundation under grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics. This project was supported in part by NASA via the Strategic University Research Partnership (SURP) Program of the Jet\nPropulsion Laboratory, California Institute of Technology; and\nby the IST Programme of the European Community, under\nthe PASCAL2 Network of Excellence, IST-2007-216886. This\narticle only reflects the authors' views.\nR.M. was supported in part by program HST-AR-12857.01-\nA, provided by NASA through a grant from the Space Telescope\nScience Institute, which is operated by the Association of Universities\nfor Research in Astronomy, Incorporated, under NASA\ncontractNAS5-26555. B.R. and S.B. acknowledge support from\nthe European Research Council in the form of a Starting Grant\nwith number 240672. H.M. acknowledges support from JSPS\nPostdoctoral Fellowships for Research Abroad. C.H. acknowledges\nsupport from the European Research Council under the\nEC FP7 grant number 240185. F.C. and M.G. are supported by\nthe Swiss National Science Foundation (SNSF).\nCenter for Particle Astrophysics, Fermi National Accelerator\nLaboratory is operated by Fermi Research Alliance, LLC under\ncontract No. De-AC02-07CH11359 with the United States\nDepartment of Energy.\n\nPublished - 0067-0049_212_1_5.pdf
Submitted - 1308.4982v3.pdf
", "abstract": "The GRavitational lEnsing Accuracy Testing 3 (GREAT3) challenge is the third in a series of image analysis challenges, with a goal of testing and facilitating the development of methods for analyzing astronomical images that will be used to measure weak gravitational lensing. This measurement requires extremely precise estimation of very small galaxy shape distortions, in the presence of far larger intrinsic galaxy shapes and distortions due to the blurring kernel caused by the atmosphere, telescope optics, and instrumental effects. The GREAT3 challenge is posed to the astronomy, machine learning, and statistics communities, and includes tests of three specific effects that are of immediate relevance to upcoming weak lensing surveys, two of which have never been tested in a community challenge before. These effects include many novel aspects including realistically complex galaxy models based on high-resolution imaging from space; a spatially varying, physically motivated blurring kernel; and a combination of multiple different exposures. To facilitate entry by people new to the field, and for use as a diagnostic tool, the simulation software for the challenge is publicly available, though the exact parameters used for the challenge are blinded. Sample scripts to analyze the challenge data using existing methods will also be provided. See http://great3challenge.info and http://great3.projects.phys.ucl.ac.uk/leaderboard/ for more information.", "date": "2014-05", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "212", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 5", "id_number": "CaltechAUTHORS:20140821-091048437", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140821-091048437", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHYS-1066293" }, { "agency": "Aspen Center for Physics" }, { "agency": "NASA Strategic University Research Partnership (SURP) Program" }, { "agency": "European Community IST Programme PASCAL2 Network of Excellence", "grant_number": "IST-2007-216886" }, { "agency": "NASA Space Telescope Science Institute", "grant_number": "HST-AR-12857.01- A" }, { "agency": "European Research Council Starting Grant", "grant_number": "240672" }, { "agency": "Japan Society for the Promotion of Science (JSPS)" }, { "agency": "European Research Council EC FP7", "grant_number": "240185" }, { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-07CH11359" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0067-0049/212/1/5", "primary_object": { "basename": "0067-0049_212_1_5.pdf", "url": "https://authors.library.caltech.edu/records/ac1sh-47h89/files/0067-0049_212_1_5.pdf" }, "related_objects": [ { "basename": "1308.4982v3.pdf", "url": "https://authors.library.caltech.edu/records/ac1sh-47h89/files/1308.4982v3.pdf" } ], "pub_year": "2014", "author_list": "Mandelbaum, Rachel and Rhodes, Jason" }, { "id": "https://authors.library.caltech.edu/records/8569e-cyn72", "eprint_id": 46009, "eprint_status": "archive", "datestamp": "2023-08-20 00:34:12", "lastmod": "2023-10-26 18:36:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Huff-E-M", "name": { "family": "Huff", "given": "Eric M." }, "orcid": "0000-0002-9378-3424" }, { "id": "Eifler-T-F", "name": { "family": "Eifler", "given": "Tim" }, "orcid": "0000-0002-1894-3301" }, { "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932" }, { "id": "Mandelbaum-R", "name": { "family": "Mandelbaum", "given": "Rachel" }, "orcid": "0000-0003-2271-1527" }, { "id": "Schlegel-D-J", "name": { "family": "Schlegel", "given": "David" }, "orcid": "0000-0002-5042-5088" }, { "id": "Seljak-U", "name": { "family": "Seljak", "given": "Uro\u0161" } } ] }, "title": "Seeing in the dark \u2013 II. Cosmic shear in the Sloan Digital Sky Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: weak\n surveys\n cosmology: observations", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. First published online: March 23, 2014. Accepted 2014 January 17. Received 2014 January 16; in original form 2011 December 15. \n\nWe thank Alexie Leauthaud for providing faint COSMOS galaxy\npostage-stamp images for simulation purposes. EMH is supported by the US Department of Energy's Office of High Energy Physics (DE-AC02-05CH11231). During the period of work on this paper, CMH was supported by the US Department of Energy's Office of High Energy Physics (DE-FG03-02-ER40701 and DE-SC0006624), the US National Science Foundation (AST-0807337), the Alfred P. Sloan Foundation, and the David & Lucile Packard Foundation. RM was supported for part of the duration of this project by NASA through Hubble Fellowship grant #HST-HF-01199.02-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. US is supported by the DOE, the Swiss National Foundation under contract 200021-116696/1 and WCU grant R32-10130. We thank the PRIMUS team for sharing their redshift catalogue, and thank Alison Coil and John Moustakas for help with using the PRIMUS data set. Funding for PRIMUS has been provided by\nNSF grants AST-0607701, 0908246, 0908442, 0908354, and NASA\ngrant 08-ADP08-0019. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. EMH thanks CCAPP for the hospitality during CCAPP Symposium and participants support provided through NSF grant #1135622. Funding for the DEEP2 survey has been provided by NSF grants AST95-09298, AST-0071048, AST-0071198, AST-0507428, and AST-0507483 as well as NASA LTSA grant NNG04GC89G. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and\nthe National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The DEEP2 team and Keck Observatory acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community and appreciate the opportunity to conduct observations from this mountain.\nFunding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute\nPotsdam, University of Basel, University of Cambridge, Case\nWestern Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University,\nOhio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.\n\nPublished - MNRAS-2014-Huff-1322-44.pdf
Submitted - 1112.3143v1.pdf
", "abstract": "Statistical weak lensing by large-scale structure \u2013 cosmic shear \u2013 is a promising cosmological tool, which has motivated the design of several large upcoming surveys. Here, we present a measurement of cosmic shear using co-added Sloan Digital Sky Survey (SDSS) imaging in 168 square degrees of the equatorial region, with r < 23.5 and i < 22.5, a source number density of 2.2 per arcmin^2 and mean redshift of z_(med) = 0.52. These co-adds were generated using a new method described in the companion Paper I that was intended to minimize systematic errors in the lensing measurement due to coherent point spread function anisotropies that are otherwise prevalent in the SDSS imaging data. We present measurements of cosmic shear out to angular separations of 2\u00b0, along with systematics tests that (combined with those from Paper I on the catalogue generation) demonstrate that our results are dominated by statistical rather than systematic errors. Assuming a cosmological model corresponding to Wilkinson Microwave Anisotropy Probe 7(WMAP7) and allowing only the amplitude of matter fluctuations \u03c3_8 to vary, we find a best-fitting value of \u03c3_8=0.636^(+0.109)_(\u22120.154) (1\u03c3); without systematic errors this would be \u03c3_8=0.636^(+0.099)_(\u22120.137) (1\u03c3). Assuming a flat \u039b cold dark matter model, the combined constraints with WMAP7 are \u03c3_8=0.784^(+0.028)_(\u22120.026)(1\u03c3)^(+0.055)_(\u22120.054)(2\u03c3) and \u03a9_mh^2=0.1303^(+0.0047)_(\u22120.0048)(1\u03c3)^(+0.009)_(\u22120.009)(2\u03c3); the 2\u03c3 error ranges are, respectively, 14 and 17 per\u2009cent smaller than WMAP7 alone.", "date": "2014-05", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "440", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1322-1344", "id_number": "CaltechAUTHORS:20140530-111648679", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140530-111648679", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG03-02-ER40701" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC0006624" }, { "agency": "NSF", "grant_number": "AST-0807337" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-01199.02-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "200021-116696/1" }, { "agency": "WCU", "grant_number": "R32-10130" }, { "agency": "NSF", "grant_number": "AST-0607701" }, { "agency": "NSF", "grant_number": "AST-0908246" }, { "agency": "NSF", "grant_number": "AST-0908442" }, { "agency": "NSF", "grant_number": "AST-0908354" }, { "agency": "NASA", "grant_number": "08-ADP08-0019" }, { "agency": "NSF", "grant_number": "PHY-1135622" }, { "agency": "NSF", "grant_number": "AST95-09298" }, { "agency": "NSF", "grant_number": "AST-0071048" }, { "agency": "NSF", "grant_number": "AST-0071198" }, { "agency": "NSF", "grant_number": "AST-0507428" }, { "agency": "NSF", "grant_number": "AST-0507483" }, { "agency": "NASA", "grant_number": "NNG04GC89G" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stu145", "primary_object": { "basename": "MNRAS-2014-Huff-1322-44.pdf", "url": "https://authors.library.caltech.edu/records/8569e-cyn72/files/MNRAS-2014-Huff-1322-44.pdf" }, "related_objects": [ { "basename": "1112.3143v1.pdf", "url": "https://authors.library.caltech.edu/records/8569e-cyn72/files/1112.3143v1.pdf" } ], "pub_year": "2014", "author_list": "Huff, Eric M.; Eifler, Tim; et el." }, { "id": "https://authors.library.caltech.edu/records/nbd7v-hvw47", "eprint_id": 45990, "eprint_status": "archive", "datestamp": "2023-08-20 00:09:19", "lastmod": "2023-10-26 18:35:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Delvecchio-I", "name": { "family": "Delvecchio", "given": "I." }, "orcid": "0000-0001-8706-2252" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "Tracing the cosmic growth of supermassive black holes to z \u223c 3 with Herschel", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: nuclei, infrared: galaxies.", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 January 16. Received 2013 December 30; in original form 2013 November 14. First published online: February 25, 2014.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation\nfrom NASA.\n\nThis paper uses data from Herschel's photometers PACS and SPIRE. PACS has been developed by a consortium of institutes led by MPE (Germany) and including: UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy) and IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI,Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). ID is deeply grateful to Iary Davidzon, Andrea Negri, Fabio Vito and Alessandro Marconi for inspiring discussions and suggestions. ID also thanks Elisabeta Lusso for useful tests on codes for SED decomposition and Micol Bolzonella for kindly providing a tool to estimate error bars.\n\nPublished - MNRAS-2014-Delvecchio-2736-54.pdf
Submitted - 1401.4503v1.pdf
", "abstract": "We study a sample of Herschel selected galaxies within the Great Observatories Origins Deep Survey-South and the Cosmic Evolution Survey fields in the framework of the Photodetector Array Camera and Spectrometer (PACS) Evolutionary Probe project. Starting from the rich multiwavelength photometric data sets available in both fields, we perform a broad-band spectral energy distribution decomposition to disentangle the possible active galactic nucleus (AGN) contribution from that related to the host galaxy. We find that 37 per cent of the Herschel-selected sample shows signatures of nuclear activity at the 99 per cent confidence level. The probability of revealing AGN activity increases for bright (L_(1\u22121000) > 10^(11) L_\u2299) star-forming galaxies at z > 0.3, becoming about 80 per cent for the brightest (L_(1\u22121000) > 10^(12) L_\u2299) infrared (IR) galaxies at z \u2265 1. Finally, we reconstruct the AGN bolometric luminosity function and the supermassive black hole growth rate across cosmic time up to z \u223c 3 from a far-IR perspective. This work shows general agreement with most of the panchromatic estimates from the literature, with the global black hole growth peaking at z \u223c 2 and reproducing the observed local black hole mass density with consistent values of the radiative efficiency \u03f5_(rad) (\u223c0.07).", "date": "2014-04", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "439", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2736-2754", "id_number": "CaltechAUTHORS:20140530-074307694", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140530-074307694", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "BMVIT (Austria)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "CEA/CNES (France)" }, { "agency": "DLR (Germany)" }, { "agency": "ASI/INAF (Italy)" }, { "agency": "CICYT/MCYT (Spain)" }, { "agency": "CSA (Canada)" }, { "agency": "NAOC (China)" }, { "agency": "CEA (France)" }, { "agency": "CNES (France)" }, { "agency": "CNRS (France)" }, { "agency": "ASI (Italy)" }, { "agency": "MCINN (Spain)" }, { "agency": "SNSB (Sweden)" }, { "agency": "STFC (UK)" }, { "agency": "UKSA (UK)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stu130", "primary_object": { "basename": "1401.4503v1.pdf", "url": "https://authors.library.caltech.edu/records/nbd7v-hvw47/files/1401.4503v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2014-Delvecchio-2736-54.pdf", "url": "https://authors.library.caltech.edu/records/nbd7v-hvw47/files/MNRAS-2014-Delvecchio-2736-54.pdf" } ], "pub_year": "2014", "author_list": "Delvecchio, I. and Bock, J." }, { "id": "https://authors.library.caltech.edu/records/2dn5y-beq54", "eprint_id": 45244, "eprint_status": "archive", "datestamp": "2023-08-22 12:00:38", "lastmod": "2023-10-26 17:53:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kelly-P-L", "name": { "family": "Kelly", "given": "Patrick L." }, "orcid": "0000-0003-3142-997X" }, { "id": "von-der-Linden-A", "name": { "family": "von der Linden", "given": "Anja" } }, { "id": "Applegate-Douglas-E", "name": { "family": "Applegate", "given": "Douglas E." } }, { "id": "Allen-Mark-T", "name": { "family": "Allen", "given": "Mark T." } }, { "id": "Allen-Steven-W", "name": { "family": "Allen", "given": "Steven W." } }, { "id": "Burchat-Patricia-R", "name": { "family": "Burchat", "given": "Patricia R." } }, { "id": "Burke-David-L", "name": { "family": "Burke", "given": "David L." } }, { "id": "Ebeling-Harald", "name": { "family": "Ebeling", "given": "Harald" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Czoske-O", "name": { "family": "Czoske", "given": "Oliver" } }, { "id": "Donovan-David", "name": { "family": "Donovan", "given": "David" } }, { "id": "Mantz-A-B", "name": { "family": "Mantz", "given": "Adam" }, "orcid": "0000-0002-8031-1217" }, { "id": "Morris-R-Glenn", "name": { "family": "Morris", "given": "R. Glenn" } } ] }, "title": "Weighing the Giants \u2013 II. Improved calibration of photometry from stellar colours and accurate photometric redshifts", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: weak; methods: observational; techniques: photometric", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 October 8. Received 2013 October 7; in original form 2013 August 1.\n\nFirst published online: February 4, 2014.\nWe thank F. William High, Jorg Dietrich and Hendrik Hildebrandt for their expert advice and assistance on photometric calibration and redshift estimation. We also appreciate helpful discussions with Thomas Erben, C-J Ma, Daniel Coe and Carlos Cunha. This work is supported in part by the US Department of Energy under contract number DE-AC02-76SF00515. This work was also supported by the National Science Foundation under Grant nos.\nAST-0807458 and AST-1140019. MTA and PRB acknowledge the\nsupport of NSF grant PHY-0969487. AM acknowledges the support of NSF grant AST-0838187. The authors acknowledge support from programmes HST-AR-12654.01-A, HST-GO-12009.02-\nA and HST-GO-11100.02-A provided by NASA through a grant\nfrom the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This work is also supported by the National Aeronautics and Space Administration through Chandra Award Numbers TM1-12010X, GO0-11149X, GO9-0141X and GO8-9119X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. DEA recognizes the support of a\nHewlett Foundation Stanford Graduate Fellowship. Based in part on data collected at Subaru Telescope (University of Tokyo) and obtained from the SMOKA, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the CFHT, which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France and the University\nof Hawaii. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National\nScience Foundation and the US Department of Energy Office\nof Science. The SDSS-III website is http://www.sdss3.org/. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, Caltech, under contract with NASA.\n\nPublished - MNRAS-2014-Kelly-28-47.pdf
Submitted - 1208.0602v3.pdf
", "abstract": "We present improved methods for using stars found in astronomical exposures to calibrate both star and galaxy colours as well as to adjust the instrument flat-field. By developing a spectroscopic model for the Sloan Digital Sky Survey (SDSS) stellar locus in colour\u2013colour space, synthesizing an expected stellar locus, and simultaneously solving for all unknown zero-points when fitting to the instrumental locus, we increase the calibration accuracy of stellar locus matching. We also use a new combined technique to estimate improved flat-field models for the Subaru SuprimeCam camera, forming 'star flats' based on the magnitudes of stars observed in multiple positions or through comparison with available measurements in the SDSS catalogue. These techniques yield galaxy magnitudes with reliable colour calibration (\u22720.01\u20130.02 mag accuracy) that enable us to estimate photometric redshift probability distributions without spectroscopic training samples. We test the accuracy of our photometric redshifts using spectroscopic redshifts z_s for \u223c5000 galaxies in 27cluster fields with at least five bands of photometry, as well as galaxies in the Cosmic Evolution Survey (COSMOS) field, finding \u03c3((z_p \u2212 z_s)/(1 + z_s)) \u2248 0.03 for the most probable redshift z_p. We show that the full posterior probability distributions for the redshifts of galaxies with five-band photometry exhibit good agreement with redshifts estimated from thirty-band photometry in the COSMOS field. The growth of shear with increasing distance behind each galaxy cluster shows the expected redshift\u2013distance relation for a flat \u039b cold dark matter (\u039b-CDM) cosmology. Photometric redshifts and calibrated colours are used in subsequent papers to measure the masses of 51 galaxy clusters from their weak gravitational shear and determine improved cosmological constraints. We make our python code for stellar locus matching publicly available at http://big-macs-calibrate.googlecode.com; the code requires only input catalogues and filter transmission functions.", "date": "2014-03-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "439", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "28-47", "id_number": "CaltechAUTHORS:20140428-102724638", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140428-102724638", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-76SF00515" }, { "agency": "NSF", "grant_number": "AST-0807458" }, { "agency": "NSF", "grant_number": "AST-1140019" }, { "agency": "NSF", "grant_number": "PHY-0969487" }, { "agency": "NSF", "grant_number": "AST-0838187" }, { "agency": "NASA", "grant_number": "HST-AR-12654.01-A" }, { "agency": "NASA", "grant_number": "HST-GO-12009.02- A" }, { "agency": "NASA", "grant_number": "HST-GO-11100.02-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NASA Chandra Award", "grant_number": "TM1-12010X" }, { "agency": "NASA Chandra Award", "grant_number": "GO0-11149X" }, { "agency": "NASA Chandra Award", "grant_number": "GO9-0141X" }, { "agency": "NASA Chandra Award", "grant_number": "GO8-9119X" }, { "agency": "NASA", "grant_number": "NAS8-03060" }, { "agency": "Hewlett Foundation Stanford Graduate Fellowship" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stt1946", "primary_object": { "basename": "1208.0602v3.pdf", "url": "https://authors.library.caltech.edu/records/2dn5y-beq54/files/1208.0602v3.pdf" }, "related_objects": [ { "basename": "MNRAS-2014-Kelly-28-47.pdf", "url": "https://authors.library.caltech.edu/records/2dn5y-beq54/files/MNRAS-2014-Kelly-28-47.pdf" } ], "pub_year": "2014", "author_list": "Kelly, Patrick L.; von der Linden, Anja; et el." }, { "id": "https://authors.library.caltech.edu/records/m19qs-jhy18", "eprint_id": 46296, "eprint_status": "archive", "datestamp": "2023-08-22 11:57:00", "lastmod": "2023-10-26 19:39:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Scott-K-S", "name": { "family": "Scott", "given": "K. S." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Pope-Alexandra", "name": { "family": "Pope", "given": "A." }, "orcid": "0000-0001-8592-2706" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Vanden-Bout-P-A", "name": { "family": "Vanden Bout", "given": "P." } }, { "id": "Manohar-S", "name": { "family": "Manohar", "given": "S." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Robertson-B", "name": { "family": "Robertson", "given": "B." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" } ] }, "title": "The Evolution of Interstellar Medium Mass Probed by Dust Emission: ALMA Observations at z = 0.3-2", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; evolution; galaxies: ISM; galaxies: starburst", "note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2013 September 25; accepted 2014 January 13; published 2014 February 20.\n\nWe thank the referee for a number of useful suggestions. We\nalso thank Zara Scoville for proofreading the manuscript and\nAndreas Schruba for helpful comments. The Aspen Center for\nPhysics is acknowledged for hospitality during the initial writing\nof this paper; NSF grant 1066293 is also acknowledged.\nK.S.S. and K.S. are supported by the National Radio Astronomy\nObservatory, which is a facility of the National Science\nFoundation operated under cooperative agreement by Associated\nUniversities, Inc. This paper makes use of the following\nALMA data: ADS/JAO.ALMA# 2011.0.00097.S. ALMA is\na partnership of ESO (representing its member states), NSF\n(USA), and NINS (Japan), together with NRC (Canada) and\nNSC and ASIAA (Taiwan), in cooperation with the Republic\nof Chile. The Joint ALMA Observatory is operated by ESO,\nAUI/NRAO, and NAOJ.\n\nPublished - 0004-637X_783_2_84.pdf
Submitted - 1401.2987v2.pdf
", "abstract": "The use of submillimeter dust continuum emission to probe the mass of interstellar dust and gas in galaxies is empirically calibrated using samples of local star-forming galaxies, Planck observations of the Milky Way, and high-redshift submillimeter galaxies. All of these objects suggest a similar calibration, strongly supporting the view that the Rayleigh-Jeans tail of the dust emission can be used as an accurate and very fast probe of the interstellar medium (ISM) in galaxies. We present ALMA Cycle 0 observations of the Band 7 (350 GHz) dust emission in 107 galaxies from z = 0.2 to 2.5. Three samples of galaxies with a total of 101 galaxies were stellar-mass-selected from COSMOS to have M* \u2243 10^(11) M\u2609: 37 at z ~ 0.4, 33 at z ~ 0.9, and 31 at z = 2. A fourth sample with six infrared-luminous galaxies at z = 2 was observed for comparison with the purely mass-selected samples. From the fluxes detected in the stacked images for each sample, we find that the ISM content has decreased by a factor ~6 from 1 to 2 \u00d7 10^(10) M\u2609 at both z = 2 and 0.9 down to ~2 \u00d7 10^9 M\u2609 at z = 0.4. The infrared-luminous sample at z = 2 shows a further ~4 times increase in M_(ISM) compared with the equivalent non-infrared-bright sample at the same redshift. The gas mass fractions are ~2% \u00b1 0.5%, 12% \u00b1 3%, 14% \u00b1 2%, and 53% \u00b1 3% for the four subsamples (z = 0.4, 0.9, and 2 and infrared-bright galaxies).", "date": "2014-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "783", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 84", "id_number": "CaltechAUTHORS:20140617-081753735", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140617-081753735", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "National Radio Astronomy Observatory" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/783/2/84", "primary_object": { "basename": "0004-637X_783_2_84.pdf", "url": "https://authors.library.caltech.edu/records/m19qs-jhy18/files/0004-637X_783_2_84.pdf" }, "related_objects": [ { "basename": "1401.2987v2.pdf", "url": "https://authors.library.caltech.edu/records/m19qs-jhy18/files/1401.2987v2.pdf" } ], "pub_year": "2014", "author_list": "Scoville, N.; Aussel, H.; et el." }, { "id": "https://authors.library.caltech.edu/records/bafrx-9f416", "eprint_id": 58836, "eprint_status": "archive", "datestamp": "2023-08-19 23:47:00", "lastmod": "2023-10-23 19:48:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "Olivier" }, "orcid": "0000-0001-5891-2596" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The VIMOS Ultra Deep Survey: 10 000 Galaxies to Study\n the Early Phases of Galaxy Assembly at 2 < z < 6+", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2014 ESO.\n\nPublished - LeFevre_2014p37.pdf
", "abstract": "The VIMOS Ultra Deep Survey (VUDS)\naims to study the early phases of\ngalaxy\nassembly from a large, well-defined\nsample of ~ 10 000 galaxies\nwith spectra obtained from very deep\nVIMOS observations. This sample is\nby far the largest to date, with spectroscopic\nredshifts covering a redshift\nrange 2 < z < ~ 6 and it enables a range\nof fundamental studies to better understand\nthe first major steps in galaxy\nevolution. The first results from the\nVUDS survey are summarised, including\nthe discovery of a galaxy protocluster\nat z = 3.3.", "date": "2014-03", "date_type": "published", "publication": "Messenger", "volume": "155", "publisher": "European Southern Observatory", "pagerange": "37-41", "id_number": "CaltechAUTHORS:20150710-084533060", "issn": "0722-6691", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150710-084533060", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" } ] }, "primary_object": { "basename": "LeFevre_2014p37.pdf", "url": "https://authors.library.caltech.edu/records/bafrx-9f416/files/LeFevre_2014p37.pdf" }, "pub_year": "2014", "author_list": "Le F\u00e8vre, Olivier; Capak, Peter; et el." }, { "id": "https://authors.library.caltech.edu/records/2qmhd-5ed90", "eprint_id": 44213, "eprint_status": "archive", "datestamp": "2023-08-22 11:46:57", "lastmod": "2023-10-26 00:17:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hao-Heng", "name": { "family": "Hao", "given": "Heng" } }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "Francesca" }, "orcid": "0000-0002-2115-1137" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "Gianni" } }, { "id": "Ho-Luis-C", "name": { "family": "Ho", "given": "Luis C." }, "orcid": "0000-0001-6947-5846" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "Andrea" }, "orcid": "0000-0003-3451-9970" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "Marcella" }, "orcid": "0000-0002-5059-6848" }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "Angela" } }, { "id": "Merloni-A-M", "name": { "family": "Merloni", "given": "Anton M." } }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "Jonathan R." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "Chris D." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Lanzuisi-G", "name": { "family": "Lanzuisi", "given": "Giorgio" }, "orcid": "0000-0001-9094-0984" }, { "id": "Celotti-A", "name": { "family": "Celotti", "given": "Annalisa" } }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "Knud" }, "orcid": "0000-0003-3804-2137" }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "Cristian" }, "orcid": "0000-0002-8853-9611" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "John D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Urry-C-M", "name": { "family": "Urry", "given": "C. Megan" }, "orcid": "0000-0002-0745-9792" }, { "id": "Schawinski-K", "name": { "family": "Schawinski", "given": "Kevin" }, "orcid": "0000-0001-5464-0888" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" } ] }, "title": "Spectral energy distributions of type 1 AGN in XMM-COSMOS \u2013 II. Shape evolution", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys; galaxies: evolution; quasars: general", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 November 21; received 2013 November 21; in original form 2012 October 10.\n\nHH thanks Belinda Wilkes and Martin J. Ward for discussion.\nThis work was supported in part by NASA Chandra grant number\nG07-8136A (HH, ME, FC) and the Smithsonian Scholarly Studies\n(FC). Support from the Italian Space Agency (ASI) under the\ncontracts ASI-INAF I/088/06/0 and I/009/10/0 is acknowledged\n(AC and CV). MS acknowledges support by the German Deutsche\nForschungsgemeinschaft,DFG Leibniz Prize (FKZHA1850/28-1).\nKS gratefully acknowledges support from Swiss National Science Foundation Grant PP00P2_138979/1.\n\nPublished - MNRAS-2014-Hao-1288-304.pdf
Submitted - 1210.3033v2.pdf
Supplemental Material - table.zip
", "abstract": "The mid-infrared-to-ultraviolet (0.1\u201310 \u03bcm) spectral energy distribution (SED) shapes of 407 X-ray-selected radio-quiet type 1 active galactic nuclei (AGN) in the wide-field 'Cosmic Evolution Survey' (COSMOS) have been studied for signs of evolution. For a sub-sample of 200 radio-quiet quasars with black hole mass estimates and host galaxy corrections, we studied their mean SEDs as a function of a broad range of redshift, bolometric luminosity, black hole mass and Eddington ratio, and compared them with the Elvis et al. (E94) type 1 AGN mean SED. We found that the mean SEDs in each bin are closely similar to each other, showing no statistical significant evidence of dependence on any of the analysed parameters. We also measured the SED dispersion as a function of these four parameters, and found no significant dependences. The dispersion of the XMM-COSMOS SEDs is generally larger than E94 SED dispersion in the ultraviolet, which might be due to the broader 'window function' for COSMOS quasars, and their X-ray-based selection.", "date": "2014-02-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "438", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1288-1304", "id_number": "CaltechAUTHORS:20140310-095412032", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140310-095412032", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "G07-8136A" }, { "agency": "Smithsonian Institution" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI-INAF I/088/06/0" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/009/10/0" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "HA 1850/28-1" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "PP00P2_138979/1" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stt2274", "primary_object": { "basename": "table.zip", "url": "https://authors.library.caltech.edu/records/2qmhd-5ed90/files/table.zip" }, "related_objects": [ { "basename": "1210.3033v2.pdf", "url": "https://authors.library.caltech.edu/records/2qmhd-5ed90/files/1210.3033v2.pdf" }, { "basename": "MNRAS-2014-Hao-1288-304.pdf", "url": "https://authors.library.caltech.edu/records/2qmhd-5ed90/files/MNRAS-2014-Hao-1288-304.pdf" } ], "pub_year": "2014", "author_list": "Hao, Heng; Elvis, Martin; et el." }, { "id": "https://authors.library.caltech.edu/records/m6xwt-td531", "eprint_id": 45778, "eprint_status": "archive", "datestamp": "2023-08-22 11:45:44", "lastmod": "2023-10-26 18:27:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Toft-S", "name": { "family": "Toft", "given": "S." }, "orcid": "0000-0003-3631-7176" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Magnelli-B", "name": { "family": "Magnelli", "given": "B." }, "orcid": "0000-0002-6777-6490" }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Zirm-A-W", "name": { "family": "Zirm", "given": "A." } }, { "id": "Michalowski-M", "name": { "family": "Michalowski", "given": "M." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Schawinski-K", "name": { "family": "Schawinski", "given": "K." }, "orcid": "0000-0001-5464-0888" }, { "id": "Krogager-J-K", "name": { "family": "Krogager", "given": "J.-K." }, "orcid": "0000-0002-4912-9388" }, { "id": "Wuyts-S", "name": { "family": "Wuyts", "given": "S." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Man-A-W-S", "name": { "family": "Man", "given": "A. W. S." } }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Staguhn-J-G", "name": { "family": "Staguhn", "given": "J." }, "orcid": "0000-0002-8437-0433" }, { "id": "Berta-S", "name": { "family": "Berta", "given": "S." }, "orcid": "0000-0002-0320-1532" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Krpan-J", "name": { "family": "Krpan", "given": "J." } }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" } ] }, "title": "Submillimeter Galaxies as Progenitors of Compact Quiescent Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: high-redshift; galaxies: starburst; Galaxy: formation; submillimeter: galaxies", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2013 September 4; accepted 2013 October 31; published 2014 January 29. \n\nS.T. acknowledges the support of the Lundbeck Foundation and is grateful for the hospitality and support of the Institute for Astronomy, University of Hawaii, during the visit when this work was initiated. The research leading to these results has received funding from the European Union's Seventh Framework programme under grant agreement 229517. K. Schawinski gratefully acknowledges support from the Swiss National Science Foundation Grant PP00P2_138979/1. M.J.M. acknowledges the support of the FWO-Vlaanderen and the Science and Technology Facilities Council. K. Sheth acknowledges support from the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under a cooperative\nagreement by Associated Universities, Inc. J.S. acknowledges\nsupport through NSF ATI grants 1020981 and 1106284.\nWe thank M. Barro for sharing additional information about\nhis compact star-forming galaxies. We thank D. Watson and J.\nHjorth for helpful discussions. The Dark Cosmology Centre is\nfunded by the Danish National Research Foundation.\n\nPublished - 0004-637X_782_2_68.pdf
Submitted - 1401.1510v1.pdf
", "abstract": "Three billion years after the big bang (at redshift z = 2), half of the most massive galaxies were already old, quiescent systems with little to no residual star formation and extremely compact with stellar mass densities at least an order of magnitude larger than in low-redshift ellipticals, their descendants. Little is known about how they formed, but their evolved, dense stellar populations suggest formation within intense, compact starbursts 1-2 Gyr earlier (at 3 < z < 6). Simulations show that gas-rich major mergers can give rise to such starbursts, which produce dense remnants. Submillimeter-selected galaxies (SMGs) are prime examples of intense, gas-rich starbursts. With a new, representative spectroscopic sample of compact, quiescent galaxies at z = 2 and a statistically well-understood sample of SMGs, we show that z = 3-6 SMGs are consistent with being the progenitors of z = 2 quiescent galaxies, matching their formation redshifts and their distributions of sizes, stellar masses, and internal velocities. Assuming an evolutionary connection, their space densities also match if the mean duty cycle of SMG starbursts is 42^(+40)_(-29) Myr (consistent with independent estimates), which indicates that the bulk of stars in these massive galaxies were formed in a major, early surge of star formation. These results suggest a coherent picture of the formation history of the most massive galaxies in the universe, from their initial burst of violent star formation through their appearance as high stellar-density galaxy cores and to their ultimate fate as giant ellipticals.", "date": "2014-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "782", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 68", "id_number": "CaltechAUTHORS:20140515-150334225", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140515-150334225", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Lundbeck Foundation" }, { "agency": "European Research Council (ERC)", "grant_number": "229517" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "PP00P2_138979/1" }, { "agency": "Fonds Wetenschappelijk Onderzoek - Vlaanderen (FWO)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "National Radio Astronomy Observatory" }, { "agency": "NSF", "grant_number": "AST-1020981" }, { "agency": "NSF", "grant_number": "AS-1106284" }, { "agency": "Danish National Research Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/782/2/68", "primary_object": { "basename": "0004-637X_782_2_68.pdf", "url": "https://authors.library.caltech.edu/records/m6xwt-td531/files/0004-637X_782_2_68.pdf" }, "related_objects": [ { "basename": "1401.1510v1.pdf", "url": "https://authors.library.caltech.edu/records/m6xwt-td531/files/1401.1510v1.pdf" } ], "pub_year": "2014", "author_list": "Toft, S.; Smol\u010di\u0107, V.; et el." }, { "id": "https://authors.library.caltech.edu/records/awgsv-r1j57", "eprint_id": 45236, "eprint_status": "archive", "datestamp": "2023-08-19 23:24:08", "lastmod": "2023-10-26 17:53:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jouvel-S", "name": { "family": "Jouvel", "given": "S." } }, { "id": "Zitrin-Adi", "name": { "family": "Zitrin", "given": "A." }, "orcid": "0000-0002-0350-4488" } ] }, "title": "CLASH: Photometric redshifts with 16 HST bands in galaxy cluster fields", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general, galaxies: distances and redshifts", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\nReceived 31 July 2013. Accepted 22 November 2013. \nPublished online 11 February 2014.\nS.J. and O.H. acknowledge at UCL, O.L. acknowledges a Royal Society Wolfson Research Merit Award, a Leverhulme Senior Research Fellowship and an Advanced ERC Grant. S.J. is supported by the Spanish Science Ministry AYA2009-13936\nConsolider-Ingenio CSD2007-00060, project 2009SGR1398 from Generalitat de Catalunya and by the European Commissions Marie Curie Initial Training Network CosmoComp (PITN- GA-2009-238356). The Dark Cosmology Centre is funded by the Danish National Research Foundation. S. Seitz acknowledges\nsupport from the Transregional Collaborative Research Centre TRR 33 \"The Dark Universe\" and from the DFG cluster of excellence \"Origin and Structure of the Universe\". This research is partially supported by PRIN INAF 2010:\n\"Architecture and Tomography of Galaxy Clusters\". A.F. acknowledges support from INAF through PRIN 2008 and 2010 grants. Support for A.Z. is provided by NASA through Hubble Fellowship grant #HST-HF-51334.01-A awarded by\nSTScI. Part of this work was also supported by contract research \"Internationale\nSpitzenforschung II/2-6\" of the Baden W\u00fcrttemberg Stiftung. A.M. acknowledges\nsupport from AYA2006-14056 BES-2007-16280.\n\nPublished - aa22419-13.pdf
Submitted - 1308.0063v2.pdf
", "abstract": "Context. The Cluster Lensing And Supernovae survey with Hubble (CLASH) is a Hubble Space Telescope (HST) Multi-Cycle Treasury programme that observes 25 massive galaxy clusters, 20 of which were X-ray-selected to preferably choose dynamically relaxed clusters, and 5 additional \"high magnification\" clusters, which were selected based on their optical lensing properties. CLASH aims to study the dark matter distribution of the clusters and find magnified high-redshift galaxies behind them. CLASH observations were carried out in 16 bands from UV to NIR to derive accurate and reliable estimates of photometric redshifts.\n\nAims. We present the CLASH photometric redshifts using 16 HST bands and study the photometric redshift accuracy including a detailed comparison between photometric and spectroscopic redshifts for the strong lensing arcs using the measurements from the cluster MACSJ1206.2-0847.\n\nMethods. We used the publicly available Le Phare and BPZ photometric redshift estimation codes on 17 CLASH galaxy clusters for which the full photo-z data processing had been completed at the time of this analysis, and derive an estimate of the CLASH photo-z accuracy.\n\nResults. Using Le Phare code for objects with a S/N \u2265 10, we reach a precision of 3%(1 + z) for the strong lensing arcs, which is reduced to 2.4%(1 + z) after removing outliers. For galaxies in the cluster field, the corresponding values are 4%(1 + z) and 3%(1 + z). Using mock galaxy catalogues, we show that 3%(1 + z) precision is what is expected using the baseline sky substraction algorithm when taking into account extinction from dust, emission lines, and the finite range of SEDs included in the photo-z template library. An improved method for estimating galaxy colours that yields more accurate photometric redshifts will be explored in a forthcoming paper. We study photo-z results for different aperture photometry techniques and find that the SExtractor isophotal photometry works best. We check the robustness of the arcs photo-z results by rederiving the input photometry in the case of MACS1206. We describe and release a photometric redshift catalogue of the MACS1206 cluster we study.\n\nConclusions. Our photo-z codes give similar results for the strong lensing arcs, as well as for galaxies of the cluster field. Results are improved when optimizing the photometric aperture shape that shows an optimal aperture size around 1\u2032\u2032 radius, giving results that are equivalent to isophotal photometry. Tailored photometry of the arcs improves the photo-z results by showing more consistency between the different arcs of the same strong lensing system.", "date": "2014-02", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "562", "publisher": "EDP Sciences", "pagerange": "Art. No. A86", "id_number": "CaltechAUTHORS:20140428-075546682", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140428-075546682", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Royal Society" }, { "agency": "Leverhulme Trust" }, { "agency": "European Research Council (ERC)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)", "grant_number": "AYA2009-13936" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)", "grant_number": "CSD2007-00060" }, { "agency": "Generalitat de Catalunya", "grant_number": "2009SGR1398" }, { "agency": "Marie Curie Fellowship", "grant_number": "PITN- GA-2009-238356" }, { "agency": "Danish National Research Foundation" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "TRR 33" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-2008" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-2010" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51334.01-A" }, { "agency": "Baden W\u00fcrttemberg Stiftung Internationale Spitzenforschung", "grant_number": "II/2-6" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)", "grant_number": "AYA2006-14056BES-2007-16280" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201322419", "primary_object": { "basename": "1308.0063v2.pdf", "url": "https://authors.library.caltech.edu/records/awgsv-r1j57/files/1308.0063v2.pdf" }, "related_objects": [ { "basename": "aa22419-13.pdf", "url": "https://authors.library.caltech.edu/records/awgsv-r1j57/files/aa22419-13.pdf" } ], "pub_year": "2014", "author_list": "Jouvel, S. and Zitrin, A." }, { "id": "https://authors.library.caltech.edu/records/7vp5x-kb465", "eprint_id": 44525, "eprint_status": "archive", "datestamp": "2023-08-22 11:26:35", "lastmod": "2023-10-26 14:22:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Heinis-S", "name": { "family": "Heinis", "given": "S." } }, { "id": "Buat-V", "name": { "family": "Buat", "given": "V." } }, { "id": "B\u00e9thermin-Matthieu", "name": { "family": "B\u00e9thermin", "given": "M." }, "orcid": "0000-0002-3915-2015" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Burgarella-D", "name": { "family": "Burgarella", "given": "D." } }, { "id": "Conley-A", "name": { "family": "Conley", "given": "A." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" } ] }, "title": "HerMES: dust attenuation and star formation activity in ultraviolet-selected samples from z \u223c 4 to \u223c 1.5", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: statistical; galaxies: star formation; infrared: galaxies; ultraviolet: galaxies", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 October 9. Received 2013 October 9; in original form 2013 July 30.\n\nWe thank the referee for useful comments and suggestions. SH\nand VB acknowledge support from the Centre National d'Etudes\nSpatiales. We thank the COSMOS team for sharing data essential to this study. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK) and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille HeDaM\n(http://hedam.oamp.fr/HerMES).\n\nPublished - MNRAS-2014-Heinis-1268-83.pdf
", "abstract": "We study the link between observed ultraviolet (UV) luminosity, stellar mass and dust attenuation within rest-frame UV-selected samples at z \u223c 4,\u2009 \u223c 3 and \u223c1.5. We measure by stacking at 250, 350 and 500\u2009\u03bcm in the Herschel/Spectral and Photometric Imaging Receiver images from the Herschel Multi-Tiered Extragalactic Survey (HerMES) program the average infrared luminosity as a function of stellar mass and UV luminosity. We find that dust attenuation is mostly correlated with stellar mass. There is also a secondary dependence with UV luminosity: at a given UV luminosity, dust attenuation increases with stellar mass, while at a given stellar mass it decreases with UV luminosity. We provide new empirical recipes to correct for dust attenuation given the observed UV luminosity and the stellar mass. Our results also enable us to put new constraints on the average relation between star formation rate (SFR) and stellar mass at z \u223c 4, \u223c3 and \u223c1.5. The SFR\u2013stellar mass relations are well described by power laws (SFR\u221dM^(0.7__\u2217), with the amplitudes being similar at z \u223c 4 and \u223c3, and decreasing by a factor of 4 at z \u223c 1.5 at a given stellar mass. We further investigate the evolution with redshift of the specific SFR. Our results are in the upper range of previous measurements, in particular at z \u223c 3, and are consistent with a plateau at 3 < z < 4. Current model predictions (either analytic, semi-analytic or hydrodynamic) are inconsistent with these values, as they yield lower predictions than the observations in the redshift range we explore. We use these results to discuss the star formation histories of galaxies in the framework of the main sequence of star-forming galaxies. Our results suggest that galaxies at high redshift (2.5 < z < 4) stay around 1 Gyr on the main sequence. With decreasing redshift, this time increases such that z = 1 main-sequence galaxies with 108", "date": "2014-01-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "437", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1268-1283", "id_number": "CaltechAUTHORS:20140326-101000362", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140326-101000362", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National d'Etudes Spatiales (CNES)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stt1960", "primary_object": { "basename": "MNRAS-2014-Heinis-1268-83.pdf", "url": "https://authors.library.caltech.edu/records/7vp5x-kb465/files/MNRAS-2014-Heinis-1268-83.pdf" }, "pub_year": "2014", "author_list": "Heinis, S.; Buat, V.; et el." }, { "id": "https://authors.library.caltech.edu/records/19wpz-re304", "eprint_id": 43430, "eprint_status": "archive", "datestamp": "2023-08-22 11:21:36", "lastmod": "2023-10-25 23:32:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ziparo-F", "name": { "family": "Ziparo", "given": "F." } }, { "id": "Fadda-D", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" } ] }, "title": "Reversal or no reversal: the evolution of the star formation rate\u2013density relation up to z \u223c 1.6", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: groups: general; galaxies: star formation; infrared: galaxies", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 October 3; received 2013 September 22; in original form 2013 April 29.\n\nFirst published online: November 2, 2013.\nWe thank the anonymous referee for her/his constructive comments. FZ acknowledges the support from and participation in the International Max-Planck Research School on Astrophysics at the Ludwig-Maximilians University.\nWe would like to thank Rob Yates for reading the paper and\nproviding useful comments. MT gratefully acknowledges support by KAKENHI no. 23740144. FEB acknowledges support from Basal-CATA (PFB-06/2007), CONICYT-Chile (under grants FONDECYT 1101024, ALMACONICYT 31100004 and Anillo ACT1101), and Chandra X-ray Center grant SAO SP1-12007B. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI,\nOAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); and IAC (Spain).\nThis development has been supported by the funding agencies\nBMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES\n(France), DLR (Germany), ASI (Italy) and CICYT/MCYT (Spain).\nThis research has made use of NASA's Astrophysics Data System, of NED, which is operated by JPL/Caltech, under contract with NASA, and of SDSS, which has been funded by the Sloan Foundation, NSF, the US Department of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council of England. The SDSS is managed by the participating institutions (www.sdss.org/collaboration/credits.html). This work has been partially supported by a SAO grant SP1-12006B grant to UMBC.\n\nPublished - MNRAS-2014-Ziparo-458-74.pdf
Submitted - 1310.1398v2.pdf
", "abstract": "We investigate the evolution of the star formation rate (SFR)\u2013density relation in the Extended Chandra Deep Field South and the Great Observatories Origin Deep Survey fields up to z \u223c 1.6. In addition to the 'traditional method', in which the environment is defined according to a statistical measurement of the local galaxy density, we use a 'dynamical' approach, where galaxies are classified according to three different environment regimes: group, 'filament-like' and field. Both methods show no evidence of an SFR\u2013density reversal. Moreover, group galaxies show a mean SFR lower than other environments up to z \u223c 1, while at earlier epochs group and field galaxies exhibit consistent levels of star formation (SF) activity. We find that processes related to a massive dark matter halo must be dominant in the suppression of the SF below z \u223c 1, with respect to purely density-related processes. We confirm this finding by studying the distribution of galaxies in different environments with respect to the so-called main sequence (MS) of star-forming galaxies. Galaxies in both group and 'filament-like' environments preferentially lie below the MS up to z \u223c 1, with group galaxies exhibiting lower levels of star-forming activity at a given mass. At z > 1, the star-forming galaxies in groups reside on the MS. Groups exhibit the highest fraction of quiescent galaxies up to z \u223c 1, after which group, 'filament-like' and field environments have a similar mix of galaxy types. We conclude that groups are the most efficient locus for SF quenching. Thus, a fundamental difference exists between bound and unbound objects, or between dark matter haloes of different masses.", "date": "2014-01-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "437", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "458-474", "id_number": "CaltechAUTHORS:20140117-113240210", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140117-113240210", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "International Max-Planck Research School on Astrophysics" }, { "agency": "KAKENHI", "grant_number": "23740144" }, { "agency": "Basal-CATA", "grant_number": "PFB-06/2007" }, { "agency": "CONICYT-Chile", "grant_number": "FONDECYT 1101024" }, { "agency": "CONICYT-Chile", "grant_number": "ALMA CONICYT 31100004" }, { "agency": "CONICYT-Chile", "grant_number": "Anillo ACT1101" }, { "agency": "Chandra X-ray Center grant", "grant_number": "SAO SP1-12007B" }, { "agency": "BMVIT (Austria)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "CEA/CNES (France)" }, { "agency": "DLR (Germany)" }, { "agency": "ASI (Italy)" }, { "agency": "CICYT/MCYT (Spain)" }, { "agency": "SAO grant", "grant_number": "SP1-12006B" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stt1901", "primary_object": { "basename": "1310.1398v2.pdf", "url": "https://authors.library.caltech.edu/records/19wpz-re304/files/1310.1398v2.pdf" }, "related_objects": [ { "basename": "MNRAS-2014-Ziparo-458-74.pdf", "url": "https://authors.library.caltech.edu/records/19wpz-re304/files/MNRAS-2014-Ziparo-458-74.pdf" } ], "pub_year": "2014", "author_list": "Ziparo, F. and Fadda, D." }, { "id": "https://authors.library.caltech.edu/records/r2b11-jdy32", "eprint_id": 43229, "eprint_status": "archive", "datestamp": "2023-08-22 11:03:25", "lastmod": "2023-10-25 23:22:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "Nicholas" } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Casey-C-M", "name": { "family": "Casey", "given": "Caitlin M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Hung-Chao-Ling", "name": { "family": "Hung", "given": "Chao-Ling" }, "orcid": "0000-0002-6879-3639" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "Emeric" } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "Herve" }, "orcid": "0000-0002-1371-5705" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "Jeyhan S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "Isaac" } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" }, { "id": "Berta-S", "name": { "family": "Berta", "given": "S." }, "orcid": "0000-0002-0320-1532" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Riguccini-L", "name": { "family": "Riguccini", "given": "L." } }, { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "M." } } ] }, "title": "Multi-wavelength SEDs of Herschel-selected Galaxies in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; infrared: galaxies", "note": "\u00a9 2013 American Astronomical Society. Received 2013 June 24; accepted 2013 September 27; published 2013 November 12. D. B. Sanders and C. M. Casey acknowledge the hospitality\nof the Aspen Center for Physics, which is supported by the\nNational Science Foundation grant No. PHY-1066293. C. M.\nCasey is generously supported by a Hubble Fellowship from\nSpace Telescope Science Institute, grant HST-HF-51268.01-A.\nCOSMOS is based on observations with the NASA/ESA\nHubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555; also based on data collected at: the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc; and the Canada\u2013France\u2013Hawaii Telescope, operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France, and the University of Hawaii. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven,\nCSL, IMEC (Belgium); CEA, LAM (France);MPIA (Germany);\nINAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain).\nSPIRE has been developed by a consortium of institutes led\nby Cardiff University (UK) and including Univ. Lethbridge\n(Canada); NAOC (China); CEA, LAM (France); IFSI, Univ.\nPadua (Italy); IAC (Spain); Stockholm Observatory (Sweden);\nImperial College London, RAL, UCL-MSSL, UKATC, Univ.\nSussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA).\nThis development has been supported by national funding\nagencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS\n(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC\n(UK); and NASA (USA).\n\nPublished - 0004-637X_778_2_131.pdf
Submitted - 1310.0474v1.pdf
", "abstract": "We combine Herschel Photodetector Array Camera and Spectrometer and Spectral and Photometric Imaging Receiver maps of the full 2 deg^2 Cosmic Evolution Survey (COSMOS) field with existing multi-wavelength data to obtain template and model-independent optical-to-far-infrared spectral energy distributions (SEDs) for 4218 Herschel-selected sources with log(L_(IR)/L_\u2609) = 9.4-13.6 and z = 0.02-3.54. Median SEDs are created by binning the optical to far-infrared (FIR) bands available in COSMOS as a function of infrared luminosity. Herschel probes rest-frame wavelengths where the bulk of the infrared radiation is emitted, allowing us to more accurately determine fundamental dust properties of our sample of infrared luminous galaxies. We find that the SED peak wavelength (\u03bbpeak) decreases and the dust mass (M_(dust)) increases with increasing total infrared luminosity (L_(IR)). In the lowest infrared luminosity galaxies (log(L_(IR)/L_\u2609) = 10.0-11.5), we see evidence of polycyclic aromatic hydrocarbon (PAH) features (\u03bb ~ 7-9 \u03bcm), while in the highest infrared luminosity galaxies (L_(IR) > 10^(12) L_\u2609) we see an increasing contribution of hot dust and/or power-law emission, consistent with the presence of heating from an active galactic nucleus (AGN). We study the relationship between stellar mass and star formation rate of our sample of infrared luminous galaxies and find no evidence that Herschel-selected galaxies follow the SFR/M_* \"main sequence\" as previously determined from studies of optically selected, star-forming galaxies. Finally, we compare the mid-infrared to FIR properties of our infrared luminous galaxies using the previously defined diagnostic, IR8 \u2261 L_(IR)/L_8, and find that galaxies with L_(IR) \u2273 10^(11.3) L_\u2609 tend to systematically lie above (\u00d7 3-5) the IR8 \"infrared main sequence,\" suggesting either suppressed PAH emission or an increasing contribution from AGN heating.", "date": "2013-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "778", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 131", "id_number": "CaltechAUTHORS:20140106-131441483", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140106-131441483", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51268.01-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Ministerio de Ciencia Y Tecnologia (MCYT)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/778/2/131", "primary_object": { "basename": "0004-637X_778_2_131.pdf", "url": "https://authors.library.caltech.edu/records/r2b11-jdy32/files/0004-637X_778_2_131.pdf" }, "related_objects": [ { "basename": "1310.0474v1.pdf", "url": "https://authors.library.caltech.edu/records/r2b11-jdy32/files/1310.0474v1.pdf" } ], "pub_year": "2013", "author_list": "Lee, Nicholas; Sanders, D. B.; et el." }, { "id": "https://authors.library.caltech.edu/records/xzqwv-vmp90", "eprint_id": 43226, "eprint_status": "archive", "datestamp": "2023-08-22 11:03:17", "lastmod": "2023-10-25 23:22:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hung-Chao-Ling", "name": { "family": "Hung", "given": "Chao-Ling" }, "orcid": "0000-0002-6879-3639" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Casey-C-M", "name": { "family": "Casey", "given": "C. M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "N." } }, { "id": "Barnes-J-E", "name": { "family": "Barnes", "given": "J. E." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Koss-M-J", "name": { "family": "Koss", "given": "M." }, "orcid": "0000-0002-7998-9581" }, { "id": "Larson-K-L", "name": { "family": "Larson", "given": "K. L." }, "orcid": "0000-0003-3917-6460" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Lockhart-K", "name": { "family": "Lockhart", "given": "K." } }, { "id": "Man-A-W-S", "name": { "family": "Man", "given": "A. W. S." } }, { "id": "Mann-A-W", "name": { "family": "Mann", "given": "A. W." }, "orcid": "0000-0003-3654-1602" }, { "id": "Riguccini-L", "name": { "family": "Riguccini", "given": "L." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "M." } } ] }, "title": "The role of galaxy interaction in the SFR-M_* relation: characterizing morphological properties of Herschel-selected galaxies at 0.2Submitted - 1309.4459v1.pdf
", "abstract": "Galaxy interactions/mergers have been shown to dominate the population of IR-luminous galaxies (L_(IR) \u2273 10^(11.6) L_\u2609) in the local universe (z \u227e 0.25). Recent studies based on the relation between galaxies' star formation rates and stellar mass (the SFR-M_* relation or the \"galaxy main sequence\") have suggested that galaxy interaction/mergers may only become significant when galaxies fall well above the galaxy main sequence. Since the typical SFR at a given M_* increases with redshift, the existence of the galaxy main sequence implies that massive, IR-luminous galaxies at high z may not necessarily be driven by galaxy interactions. We examine the role of galaxy interactions in the SFR-M_* relation by carrying out a morphological analysis of 2084 Herschel-selected galaxies at 0.2 < z < 1.5 in the COSMOS field. Using a detailed visual classification scheme, we show that the fraction of \"disk galaxies\" decreases and the fraction of \"irregular\" galaxies increases systematically with increasing L_(IR) out to z \u227e 1.5 and z \u227e 1.0, respectively. At L_(IR) >10^(11.5) L_\u2609, \u2273 50% of the objects show evident features of strongly interacting/merger systems, where this percentage is similar to the studies of local IR-luminous galaxies. The fraction of interacting/merger systems also systematically increases with the deviation from the SFR-M_* relation, supporting the view that galaxies falling above the main sequence are more dominated by mergers than the main-sequence galaxies. Meanwhile, we find that \u2273 18% of massive IR-luminous \"main-sequence galaxies\" are classified as interacting systems, where this population may not evolve through the evolutionary track predicted by a simple gas exhaustion model.", "date": "2013-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "778", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 129", "id_number": "CaltechAUTHORS:20140106-112331485", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140106-112331485", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51268.01-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "CICYT/MCYT (Spain)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Agentschap voor Innovatie door Wetenschap en Technologie (IWT-Belgium)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/778/2/129", "primary_object": { "basename": "0004-637X_778_2_129.pdf", "url": "https://authors.library.caltech.edu/records/xzqwv-vmp90/files/0004-637X_778_2_129.pdf" }, "related_objects": [ { "basename": "1309.4459v1.pdf", "url": "https://authors.library.caltech.edu/records/xzqwv-vmp90/files/1309.4459v1.pdf" } ], "pub_year": "2013", "author_list": "Hung, Chao-Ling; Sanders, D. B.; et el." }, { "id": "https://authors.library.caltech.edu/records/nmq84-wr523", "eprint_id": 43195, "eprint_status": "archive", "datestamp": "2023-08-22 11:02:27", "lastmod": "2023-10-25 23:21:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tinker-J-L", "name": { "family": "Tinker", "given": "Jeremy L." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "Bundy-K-A", "name": { "family": "Bundy", "given": "Kevin" }, "orcid": "0000-0001-9742-3138" }, { "id": "George-M-R", "name": { "family": "George", "given": "Matthew R." } }, { "id": "Behroozi-P-S", "name": { "family": "Behroozi", "given": "Peter" } }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "Richard" }, "orcid": "0000-0002-6085-3780" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" }, { "id": "Wechsler-R-H", "name": { "family": "Wechsler", "given": "Risa H." }, "orcid": "0000-0003-2229-011X" } ] }, "title": "Evolution of the Stellar-to-dark Matter Relation: Separating Star-forming and Passive Galaxies from z = 1 to 0", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: halos", "note": "\u00a9 2013 American Astronomical Society. Received 2013 June 3; accepted 2013 September 3; published 2013 November 8. We thank the referee for many helpful comments and suggestions\nthat have improved this work. This work was supported\nby World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. The HSTCOSMOS Treasury program\nwas supported through NASA grant HST-GO-09822. We wish to thank Tony Roman, Denise Taylor, and David Soderblom for their assistance in planning and scheduling of the extensive\nCOSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at http://cosmos.astro.caltech.edu/. It is a pleasure the acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman and John Good) in providing online archive and server capabilities for the COSMOS data-sets.\n\nPublished - 0004-637X_778_2_93.pdf
Submitted - 1308.2974v1.pdf
", "abstract": "We use measurements of the stellar mass function, galaxy clustering, and galaxy-galaxy lensing within the COSMOS survey to constrain the stellar-to-halo mass relation (SHMR) of star forming and quiescent galaxies over the redshift range z = [0.2, 1.0]. For massive galaxies, M^* \u2273 10^(10.6) M_\u2609, our results indicate that star-forming galaxies grow proportionately as fast as their dark matter halos while quiescent galaxies are outpaced by dark matter growth. At lower masses, there is minimal difference in the SHMRs, implying that the majority low-mass quiescent galaxies have only recently been quenched of their star formation. Our analysis also affords a breakdown of all COSMOS galaxies into the relative numbers of central and satellite galaxies for both populations. At z = 1, satellite galaxies dominate the red sequence below the knee in the stellar mass function. But the number of quiescent satellites exhibits minimal redshift evolution; all evolution in the red sequence is due to low-mass central galaxies being quenched of their star formation. At M^* ~ 10^(10) M_\u2609, the fraction of central galaxies on the red sequence increases by a factor of 10 over our redshift baseline, while the fraction of quenched satellite galaxies at that mass is constant with redshift. We define a \"migration rate\" to the red sequence as the time derivative of the passive galaxy abundances. We find that the migration rate of central galaxies to the red sequence increases by nearly an order of magnitude from z = 1 to z = 0. These results imply that the efficiency of quenching star formation for centrals is increasing with cosmic time, while the mechanisms that quench the star formation of satellite galaxies in groups and clusters is losing efficiency.", "date": "2013-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "778", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 93", "id_number": "CaltechAUTHORS:20140103-083737842", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140103-083737842", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "NASA", "grant_number": "HST-GO-09822" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/778/2/93", "primary_object": { "basename": "0004-637X_778_2_93.pdf", "url": "https://authors.library.caltech.edu/records/nmq84-wr523/files/0004-637X_778_2_93.pdf" }, "related_objects": [ { "basename": "1308.2974v1.pdf", "url": "https://authors.library.caltech.edu/records/nmq84-wr523/files/1308.2974v1.pdf" } ], "pub_year": "2013", "author_list": "Tinker, Jeremy L.; Leauthaud, Alexie; et el." }, { "id": "https://authors.library.caltech.edu/records/dkd19-ph980", "eprint_id": 43630, "eprint_status": "archive", "datestamp": "2023-08-19 22:23:06", "lastmod": "2023-10-25 23:43:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Casey-C-M", "name": { "family": "Casey", "given": "Caitlin M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Chen-Chian-Chou", "name": { "family": "Chen", "given": "Chian-Chou" }, "orcid": "0000-0002-3805-0789" }, { "id": "Cowie-L-L", "name": { "family": "Cowie", "given": "Lennox L." }, "orcid": "0000-0002-6319-1575" }, { "id": "Barger-A-J", "name": { "family": "Barger", "given": "Amy J." }, "orcid": "0000-0002-3306-1606" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Koss-M-J", "name": { "family": "Koss", "given": "Michael" }, "orcid": "0000-0002-7998-9581" }, { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "Nicholas" } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "Emeric" } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "David B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Williams-J-P", "name": { "family": "Williams", "given": "Jonathan P." }, "orcid": "0000-0001-5058-695X" } ] }, "title": "Characterization of SCUBA-2 450\u03bcm and 850\u03bcm selected galaxies in the COSMOS field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution\n galaxies: high-redshift\n galaxies: starbursts\n infrared: galaxies", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 September 4. Received 2013 August 5; in original form 2013 February 11. First published online: October 22, 2013. We would like to thank the referee for a very thoughtful and helpful report in reviewing this manuscript. CMC is generously supported by a Hubble Fellowship from Space Telescope Science Institute, grant HST-HF-51268.01-A. CCC and LC are generously supported by NSF grant AST 0709356. AB thanks the University of Wisconsin Research Committee with funds granted by the Wisconsin Alumni Research Foundation, and the David and Lucile Packard Foundation. CMC and DBS would like to thank the Aspen Center for Physics and the NSF grant 1066293 for many fruitful conversations with the community regarding this work during 'The Obscured Universe' summer workshop. The JCMT is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the National Research Council of Canada, and (until 2013 March 31) the Netherlands Organization\nfor Scientific Research. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. The authors also wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\n\nPublished - MNRAS-2013-Casey-1919-54.pdf
Submitted - 1302.2619v2.pdf
", "abstract": "We present deep 450\u2009\u03bcm and 850\u2009\u03bcm observations of a large, uniformly covered 394 arcmin2 area in the Cosmic Evolution Survey (COSMOS) field obtained with the Scuba-2 instrument on the James Clerk Maxwell Telescope (JCMT). We achieve root-mean-square noise values of \u03c3_(450) = 4.13\u2009mJy and \u03c3_(850) = 0.80\u2009mJy. The differential and cumulative number counts are presented and compared to similar previous works. Individual point sources are identified at >3.6\u03c3 significance, a threshold corresponding to a 3\u20135 per\u2009cent sample contamination rate. We identify 78 sources at 450\u2009\u03bcm and 99 at 850\u2009\u03bcm, with flux densities S_(450) = 13\u201337\u2009mJy and S_(850) = 2\u201316\u2009mJy. Only 62\u201376 per\u2009cent of 450\u2009\u03bcm sources are 850\u2009\u03bcm detected and 61\u201381 per\u2009cent of 850\u2009\u03bcm sources are 450\u2009\u03bcm detected. The positional uncertainties at 450\u2009\u03bcm are small (1\u20132.5 arcsec) and therefore allow a precise identification of multiwavelength counterparts without reliance on detection at 24\u2009\u03bcm or radio wavelengths; we find that only 44 per\u2009cent of 450\u2009\u03bcm sources and 60 per\u2009cent of 850\u2009\u03bcm sources have 24\u2009\u03bcm or radio counterparts. 450\u2009\u03bcm selected galaxies peak at \u3008z\u3009 = 1.95 \u00b1 0.19 and 850\u2009\u03bcm selected galaxies peak at \u3008z\u3009 = 2.16 \u00b1 0.11. The two samples occupy similar parameter space in redshift and luminosity, while their median SED peak wavelengths differ by \u223c20\u201350\u2009\u03bcm (translating to \u0394T_(dust) = 8\u201312\u2009K, where 450\u2009\u03bcm selected galaxies are warmer). The similarities of the 450\u2009\u03bcm and 850\u2009\u03bcm populations, yet lack of direct overlap between them, suggests that submillimetre surveys conducted at any single far-infrared wavelength will be significantly incomplete (\u227330 per\u2009cent) at censusing infrared-luminous star formation at high z.", "date": "2013-12", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "436", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "1919-1954", "id_number": "CaltechAUTHORS:20140204-071134082", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140204-071134082", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51268.01-A" }, { "agency": "NSF", "grant_number": "AST 0709356" }, { "agency": "University of Wisconsin Research Committee" }, { "agency": "Wisconsin Alumni Research Foundation" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "NSF", "grant_number": "1066293" }, { "agency": "Canada Foundation for Innovation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stt1673", "primary_object": { "basename": "1302.2619v2.pdf", "url": "https://authors.library.caltech.edu/records/dkd19-ph980/files/1302.2619v2.pdf" }, "related_objects": [ { "basename": "MNRAS-2013-Casey-1919-54.pdf", "url": "https://authors.library.caltech.edu/records/dkd19-ph980/files/MNRAS-2013-Casey-1919-54.pdf" } ], "pub_year": "2013", "author_list": "Casey, Caitlin M.; Chen, Chian-Chou; et el." }, { "id": "https://authors.library.caltech.edu/records/57wvd-e1c76", "eprint_id": 43157, "eprint_status": "archive", "datestamp": "2023-08-22 10:54:52", "lastmod": "2023-10-25 23:19:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kettula-K", "name": { "family": "Kettula", "given": "K." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "R." }, "orcid": "0000-0002-6085-3780" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Hoekstra-H", "name": { "family": "Hoekstra", "given": "H." } }, { "id": "Taylor-J-E", "name": { "family": "Taylor", "given": "J. E." } }, { "id": "Spinelli-P-F", "name": { "family": "Spinelli", "given": "P. F." } }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" } ] }, "title": "Weak Lensing Calibrated M-T Scaling Relation of Galaxy Groups in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: groups: general; gravitational lensing: weak", "note": "\u00a9 2013 American Astronomical Society. Received 2013 June 20; accepted 2013 September 25; published 2013 November 6. \n\nBased on observations with the NASA/ESA Hubble Space Telescope,\nobtained at the Space Telescope Science Institute, which is operated by AURA\nInc., under NASA contract NAS 5-26555. Also based on data collected at the\nSubaru Telescope, which is operated by the National Astronomical\nObservatory of Japan; the XMM-Newton, an ESA science mission with\ninstruments and contributions directly funded by ESA Member States and\nNASA; the European Southern Observatory under Large Program 175.A-0839,\nChile; Kitt Peak National Observatory, Cerro Tololo Inter-American\nObservatory, and the National Optical Astronomy Observatory, which are\noperated by the Association of Universities for Research in Astronomy, Inc.\n(AURA) under cooperative agreement with the National Science Foundation;\nthe National Radio Astronomy Observatory, which is a facility of the National\nScience Foundation operated under cooperative agreement by Associated\nUniversities, Inc.; and the Canada\u2013France\u2013Hawaii Telescope (CFHT) with\nMegaPrime/MegaCam operated as a joint project by the CFHT Corporation,\nCEA/DAPNIA, the National Research Council of Canada, the Canadian\nAstronomy Data Centre, the Centre National de la Recherche Scientifique de\nFrance, TERAPIX, and the University of Hawaii.\n\nThe authors thank F. Miniati for useful discussion. K.K. acknowledges support from the Magnus Ehrnrooth Foundation.\nA.F. acknowledges the Academy of Finland (decision 266918).\nR.M. is supported by a Royal Society University Research Fellowship and ERC grant MIRG-CT-208994. J.R. was supported\nby JPL, which is run by Caltech under a contract for NASA. H.H. acknowledges NWO Vidi grant 639.042.814. This research has made use of NASA's Astrophysics Data System.\nFacilities: HST (ACS), XMM (EPIC).\n\nPublished - 0004-637X_778_1_74.pdf
Submitted - 1309.3891v1.pdf
", "abstract": "The scaling between X-ray observables and mass for galaxy clusters and groups is instrumental for cluster-based cosmology and an important probe for the thermodynamics of the intracluster gas. We calibrate a scaling relation between the weak lensing mass and X-ray spectroscopic temperature for 10 galaxy groups in the COSMOS field, combined with 55 higher-mass clusters from the literature. The COSMOS data includes Hubble Space Telescope imaging and redshift measurements of 46 source galaxies per arcminute2, enabling us to perform unique weak lensing measurements of low-mass systems. Our sample extends the mass range of the lensing calibrated M-T relation an order of magnitude lower than any previous study, resulting in a power-law slope of 1.48^(+0.13)_(-0.09). The slope is consistent with the self-similar model, predictions from simulations, and observations of clusters. However, X-ray observations relying on mass measurements derived under the assumption of hydrostatic equilibrium have indicated that masses at group scales are lower than expected. Both simulations and observations suggest that hydrostatic mass measurements can be biased low. Our external weak lensing masses provide the first observational support for hydrostatic mass bias at group level, showing an increasing bias with decreasing temperature and reaching a level of 30%-50% at 1 keV.", "date": "2013-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "778", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 74", "id_number": "CaltechAUTHORS:20131224-072259005", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131224-072259005", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Magnus Ehrnrooth Foundation" }, { "agency": "Academy of Finland", "grant_number": "266918" }, { "agency": "Royal Society" }, { "agency": "European Research Council (ERC)", "grant_number": "MIRG-CT-208994" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "639.042.814" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/778/1/74", "primary_object": { "basename": "0004-637X_778_1_74.pdf", "url": "https://authors.library.caltech.edu/records/57wvd-e1c76/files/0004-637X_778_1_74.pdf" }, "related_objects": [ { "basename": "1309.3891v1.pdf", "url": "https://authors.library.caltech.edu/records/57wvd-e1c76/files/1309.3891v1.pdf" } ], "pub_year": "2013", "author_list": "Kettula, K.; Finoguenov, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/bp1rk-j6k87", "eprint_id": 42734, "eprint_status": "archive", "datestamp": "2023-08-22 10:51:52", "lastmod": "2023-10-23 17:16:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kashino-D", "name": { "family": "Kashino", "given": "D." }, "orcid": "0000-0001-9044-1747" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The FMOS-COSMOS Survey of Star-forming Galaxies at z ~ 1.6. I. H\u03b1-based Star Formation Rates and Dust Extinction", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: general; galaxies: high-redshift; galaxies: ISM; galaxies: star formation", "note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 July 19; accepted 2013 September 16; published 2013 October 11. \n\nWe would like to thank M. Fukugita, T. Nozawa and V. Wild for useful discussions and K. Aoki, F. Iwamuro, and N. Tamura for their invaluable assistance and expertise regarding\nSubaru/FMOS. This work has been partially supported by the\nGrant-in-Aid for the Scientific Research Fund under grant Nos.\n22340056: N.S., 23224005: N.A., and Program for Leading\nGraduate Schools \"PhD Professional: Gateway to Success in\nFrontier Asia\" commissioned by the Ministry of Education,\nCulture, Sports, Science and Technology of Japan, and INAF\nthrough the grant \"PRIN-2010.\"\n\nPublished - 2041-8205_777_1_L8.pdf
Submitted - 1309.4774v1.pdf
Erratum - 2041-8205_785_2_L37.pdf
", "abstract": "We present the first results from a near-IR spectroscopic survey of the COSMOS field, using the Fiber Multi-Object Spectrograph on the Subaru telescope, designed to characterize the star-forming galaxy population at 1.4 < z < 1.7. The high-resolution mode is implemented to detect H\u03b1 in emission between 1.6-1.8 \u03bcm with f H\u03b1 gsim 4 \u00d7 10\u201317 erg cm\u20132 s\u20131. Here, we specifically focus on 271 sBzK-selected galaxies that yield a H\u03b1 detection thus providing a redshift and emission line luminosity to establish the relation between star formation rate and stellar mass. With further J-band spectroscopy for 89 of these, the level of dust extinction is assessed by measuring the Balmer decrement using co-added spectra. We find that the extinction (0.6 lsim A H\u03b1 lsim 2.5) rises with stellar mass and is elevated at high masses compared to low-redshift galaxies. Using this subset of the spectroscopic sample, we further find that the differential extinction between stellar and nebular emission E star(B \u2013 V)/E neb(B \u2013 V) is 0.7-0.8, dissimilar to that typically seen at low redshift. After correcting for extinction, we derive an H\u03b1-based main sequence with a slope (0.81 \u00b1 0.04) and normalization similar to previous studies at these redshifts.", "date": "2013-11-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "777", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L8", "id_number": "CaltechAUTHORS:20131126-092726865", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131126-092726865", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Grant-in-Aid for the Scientific Research Fund", "grant_number": "22340056" }, { "agency": "Grant-in-Aid for the Scientific Research Fund", "grant_number": "23224005" }, { "agency": "INAF grant", "grant_number": "PRIN-2010" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology of Japan" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/2041-8205/777/1/L8", "primary_object": { "basename": "1309.4774v1.pdf", "url": "https://authors.library.caltech.edu/records/bp1rk-j6k87/files/1309.4774v1.pdf" }, "related_objects": [ { "basename": "2041-8205_777_1_L8.pdf", "url": "https://authors.library.caltech.edu/records/bp1rk-j6k87/files/2041-8205_777_1_L8.pdf" }, { "basename": "2041-8205_785_2_L37.pdf", "url": "https://authors.library.caltech.edu/records/bp1rk-j6k87/files/2041-8205_785_2_L37.pdf" } ], "pub_year": "2013", "author_list": "Kashino, D.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/ewb7j-s5n24", "eprint_id": 42853, "eprint_status": "archive", "datestamp": "2023-08-22 10:43:59", "lastmod": "2023-10-25 23:05:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "McLure-R-J", "name": { "family": "McLure", "given": "Ross J." } }, { "id": "Dunlop-J-S", "name": { "family": "Dunlop", "given": "James S." } }, { "id": "Robertson-B-E", "name": { "family": "Robertson", "given": "Brant E." }, "orcid": "0000-0002-4271-0364" }, { "id": "Ono-Yoshiaki", "name": { "family": "Ono", "given": "Yoshiaki" } }, { "id": "Schenker-M-A", "name": { "family": "Schenker", "given": "Matthew A." } }, { "id": "Ouchi-Masami", "name": { "family": "Ouchi", "given": "Masami" }, "orcid": "0000-0002-1049-6658" }, { "id": "Bowler-R-A-A", "name": { "family": "Bowler", "given": "Rebecca A. A." } }, { "id": "Rogers-A-B", "name": { "family": "Rogers", "given": "Alexander B." } }, { "id": "Curtis-Lake-E", "name": { "family": "Curtis-Lake", "given": "Emma" } }, { "id": "Schneider-E", "name": { "family": "Schneider", "given": "Evan" } }, { "id": "Charlot-S", "name": { "family": "Charlot", "given": "St\u00e9phane" } }, { "id": "Stark-D-P", "name": { "family": "Stark", "given": "Daniel P." } }, { "id": "Furlanetto-S-R", "name": { "family": "Furlanetto", "given": "Steven R." }, "orcid": "0000-0002-0658-1243" }, { "id": "Cirasuolo-M", "name": { "family": "Cirasuolo", "given": "Michele" } }, { "id": "Wild-V", "name": { "family": "Wild", "given": "V." } }, { "id": "Targett-T-A", "name": { "family": "Targett", "given": "T." } } ] }, "title": "The 2012 Hubble Ultra Deep Field (UDF12): Observational Overview", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: high-redshift", "note": "\u00a9 2013 American Astronomical Society. Received 2012 December 6; accepted 2013 September 9; published 2013 October 11. We thank the referee for very useful comments that helped to\nimprove this manuscript. We wish to thank the Hubble observing\nteam as well as our Program Coordinator, Shelley Meyett,\nfor help in scheduling and executing this program. Support\nfor HST Program GO-12498 is provided by NASA through\na grant from the Space Telescope Science Institute, which\nis operated by the Association of Universities for Research\nin Astronomy, Incorporated, under NASA contract NAS5-\n26555. J.S.D., R.A.A.B., T.A.T., and V.W. acknowledge the\nsupport of the European Research Council through the award\nof an Advanced Grant to J.S.D. In addition, J.S.D. and R.J.M.\nacknowledge the support of the Royal Society via a Wolfson\nResearch Merit Award and a University Research Fellowship,\nrespectively. A.B.R. and E.F.C.L. acknowledge the support\nof the UK Science and Technology Facilities Council. V.W.\nacknowledges the support of the European Research Council\nthrough the award of a Starting Grant. S.C. acknowledges the\nsupport of the European Commission through the Marie Curie\nInitial Training Network ELIXIR.\nFacility: HST (ACS, WFC3)\n\nPublished - 0067-0049_209_1_3.pdf
Submitted - 1212.1448v1.pdf
", "abstract": "We present the 2012 Hubble Ultra Deep Field campaign (UDF12), a large 128 orbit Cycle 19 Hubble Space Telescope program aimed at extending previous Wide Field Camera 3 (WFC3)/IR observations of the UDF by quadrupling the exposure time in the F105W filter, imaging in an additional F140W filter, and extending the F160W exposure time by 50%, as well as adding an extremely deep parallel field with the Advanced Camera for Surveys (ACS) in the F814W filter with a total exposure time of 128 orbits. The principal scientific goal of this project is to determine whether galaxies reionized the universe; our observations are designed to provide a robust determination of the star formation density at z \u2273 8, improve measurements of the ultraviolet continuum slope at z ~ 7-8, facilitate the construction of new samples of z ~ 9-10 candidates, and enable the detection of sources up to z ~ 12. For this project we committed to combining these and other WFC3/IR imaging observations of the UDF area into a single homogeneous dataset to provide the deepest near-infrared observations of the sky. In this paper we present the observational overview of the project and describe the procedures used in reducing the data as well as the final products that were produced. We present the details of several special procedures that we implemented to correct calibration issues in the data for both the WFC3/IR observations of the main UDF field and our deep 128 orbit ACS/WFC F814W parallel field image, including treatment for persistence, correction for time-variable sky backgrounds, and astrometric alignment to an accuracy of a few milliarcseconds. We release the full, combined mosaics comprising a single, unified set of mosaics of the UDF, providing the deepest near-infrared blank-field view of the universe currently achievable, reaching magnitudes as deep as AB ~ 30 mag in the near-infrared, and yielding a legacy dataset on this field.", "date": "2013-11", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "209", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 3", "id_number": "CaltechAUTHORS:20131205-094419136", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131205-094419136", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-12498.01-A" }, { "agency": "NASA", "grant_number": "NAS5- 26555" }, { "agency": "European Research Council (ERC)" }, { "agency": "Royal Society" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Marie Curie Fellowship" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0067-0049/209/1/3", "primary_object": { "basename": "0067-0049_209_1_3.pdf", "url": "https://authors.library.caltech.edu/records/ewb7j-s5n24/files/0067-0049_209_1_3.pdf" }, "related_objects": [ { "basename": "1212.1448v1.pdf", "url": "https://authors.library.caltech.edu/records/ewb7j-s5n24/files/1212.1448v1.pdf" } ], "pub_year": "2013", "author_list": "Koekemoer, Anton M.; Ellis, Richard S.; et el." }, { "id": "https://authors.library.caltech.edu/records/meban-6md80", "eprint_id": 120760, "eprint_status": "archive", "datestamp": "2023-08-22 10:33:57", "lastmod": "2023-10-18 17:59:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ziparo-Francsco", "name": { "family": "Ziparo", "given": "F." }, "orcid": "0000-0001-6316-1707" }, { "name": { "family": "Popesso", "given": "P." } }, { "name": { "family": "Biviano", "given": "A." }, "orcid": "0000-0002-0857-0732" }, { "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "name": { "family": "Wuyts", "given": "S." } }, { "name": { "family": "Wilman", "given": "D." } }, { "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "name": { "family": "Nandra", "given": "K." }, "orcid": "0000-0002-7150-9192" }, { "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "name": { "family": "Elbaz", "given": "D." }, "orcid": "0000-0002-7631-647X" }, { "name": { "family": "Dickinson", "given": "M." } }, { "name": { "family": "Altieri", "given": "B." }, "orcid": "0000-0003-3936-0284" }, { "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "name": { "family": "Berta", "given": "S." }, "orcid": "0000-0002-0320-1532" }, { "name": { "family": "Cimatti", "given": "A." }, "orcid": "0000-0002-4409-5633" }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "name": { "family": "Genzel", "given": "R." }, "orcid": "0000-0002-2767-9653" }, { "name": { "family": "Le Flo'ch", "given": "E." } }, { "name": { "family": "Magnelli", "given": "B." }, "orcid": "0000-0002-6777-6490" }, { "name": { "family": "Nordon", "given": "R." } }, { "name": { "family": "Poglitsch", "given": "A." } }, { "name": { "family": "Pozzi", "given": "F." }, "orcid": "0000-0002-7412-647X" }, { "name": { "family": "Sanchez Portal", "given": "M." } }, { "name": { "family": "Tacconi", "given": "L." }, "orcid": "0000-0002-1485-9401" }, { "name": { "family": "Bauer", "given": "F. E." }, "orcid": "0000-0002-8686-8737" }, { "name": { "family": "Brandt", "given": "W. N." }, "orcid": "0000-0002-0167-2453" }, { "name": { "family": "Cappelluti", "given": "N." }, "orcid": "0000-0002-1697-186X" }, { "name": { "family": "Cooper", "given": "M. C." }, "orcid": "0000-0003-1371-6019" }, { "name": { "family": "Mulchaey", "given": "J. S." } } ] }, "title": "The lack of star formation gradients in galaxy groups up to z \u223c 1.6", "ispublished": "pub", "full_text_status": "public", "keywords": "Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nWe thank the anonymous referee for her/his constructive comments. \n\nFZ acknowledges the support from and participation in the International Max-Planck Research School on Astrophysics at the Ludwig-Maximilians University. \n\nMT gratefully acknowledges support by KAKENHI No. 23740144. \n\nFEB acknowledges support from Basal-CATA (PFB-06/2007), CONICYT-Chile (under grants FONDECYT 1101024, ALMA-CONICYT 31100004 and Anillo ACT1101) and Chandra X-ray Center grant SAO SP1-12007B. \n\nPACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy) and CICYT/MCYT (Spain). \n\nWe gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information about the COSMOS survey is available at http://www.astro.caltech.edu/\u223ccosmos. \n\nThis research has made use of NASA's Astrophysics Data System, of NED, which is operated by JPL/Caltech, under contract with NASA, and of SDSS, which has been funded by the Sloan Foundation, NSF, the US Department of Energy, NASA, the Japanese Monbukagakusho, the Max-Planck Society and the Higher Education Funding Council of England. The SDSS is managed by the participating institutions (www.sdss.org/collaboration/credits.html). \n\nThis work has been partially supported by a SAO grant SP1-12006B grant to UMBC.\n\nPublished - stt1222.pdf
", "abstract": "In the local Universe, galaxy properties show a strong dependence on environment. In cluster cores, early-type galaxies dominate, whereas star-forming galaxies are more and more common in the outskirts. At higher redshifts and in somewhat less dense environments (e.g. galaxy groups), the situation is less clear. One open issue is that of whether and how the star formation rate (SFR) of galaxies in groups depends on the distance from the centre of mass. To shed light on this topic, we have built a sample of X-ray selected galaxy groups at 0 < z < 1.6 in various blank fields [Extended Chandra Deep Field South (ECDFS), Cosmological Evolution Survey (COSMOS), Great Observatories Origin Deep Survey (GOODS)]. We use a sample of spectroscopically confirmed group members with stellar mass M\u22c6 > 10^(10.3)\u2009M_\u2299 in order to have a high spectroscopic completeness. As we use only spectroscopic redshifts, our results are not affected by uncertainties due to projection effects. We use several SFR indicators to link the star formation (SF) activity to the galaxy environment. Taking advantage of the extremely deep mid-infrared Spitzer MIPS and far-infrared Herschel1 PACS observations, we have an accurate, broad-band measure of the SFR for the bulk of the star-forming galaxies. We use multi-wavelength Spectral Energy Distribution (SED) fitting techniques to estimate the stellar masses of all objects and the SFR of the MIPS and PACS undetected galaxies. We analyse the dependence of the SF activity, stellar mass and specific SFR on the group-centric distance, up to z \u223c 1.6, for the first time. We do not find any correlation between the mean SFR and group-centric distance at any redshift. We do not observe any strong mass segregation either, in agreement with predictions from simulations. Our results suggest that either groups have a much smaller spread in accretion times with respect to the clusters and that the relaxation time is longer than the group crossing time.", "date": "2013-10-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "434", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3089-3103", "id_number": "CaltechAUTHORS:20230411-960204000.2", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230411-960204000.2", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "International Max-Planck Research School on Astrophysics" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23740144" }, { "agency": "Basal-CATA", "grant_number": "PFB-06/2007" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1101024" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "31100004" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "ACT1101" }, { "agency": "Smithsonian Astronomical Observatory", "grant_number": "SAO SP1-12007B" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Funding Council for England" }, { "agency": "Smithsonian Astronomical Observatory", "grant_number": "SAO SP1-12006B" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stt1222", "primary_object": { "basename": "stt1222.pdf", "url": "https://authors.library.caltech.edu/records/meban-6md80/files/stt1222.pdf" }, "pub_year": "2013", "author_list": "Ziparo, F.; Popesso, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/vqazq-wt378", "eprint_id": 43265, "eprint_status": "archive", "datestamp": "2023-08-19 21:41:20", "lastmod": "2023-10-25 23:24:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Moresco-M", "name": { "family": "Moresco", "given": "M." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Spot the difference - Impact of different selection criteria on observed properties of passive galaxies in zCOSMOS-20k sample", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: fundamental parameters, galaxies: statistics, surveys", "note": "\u00a9 2013 ESO. \nArticle published by EDP Sciences.\n\nPublished online 03 October 2013.\nReceived 30 April 2013. Accepted 19 July 2013. \n\n\nBased on data obtained with the European Southern Observatory\nVery Large Telescope, Paranal, Chile, program 175.A-0839.\nM.M. and A.C. acknowledge the grants ASI n.I/023/12/0\n\"Attivit\u00e1 relative alla fase B2/C per la missione Euclid\" and MIUR PRIN 2010-2011 \"The dark Universe and the cosmic evolution of baryons: from current surveys to Euclid\". Part of the work has also been supported by an INAF grant\n\"PRIN-2010\". This analysis is based on zCOSMOS observations, carried out using the Very Large Telescope at the ESO Paranal Observatory under Programme ID: LP175.A-0839. We would like to thank the anonymous referee for the useful\ncomments and suggestions, which helped to improve the paper.\n\nPublished - aa21797-13.pdf
Submitted - 1305.1308v2.pdf
", "abstract": "Aims. We present the analysis of photometric, spectroscopic, and morphological properties for differently selected samples of passive galaxies up to z = 1 extracted from the zCOSMOS-20k spectroscopic survey. This analysis intends toexplore the dependence of galaxy properties on the selection criterion adopted, study the degree of contamination due to star-forming outliers, and provide a comparison between different commonly used selection criteria. This work is a first step to fully investigating the selection effects of passive galaxies for future massive surveys such as Euclid.\nMethods. We extracted from the zCOSMOS-20k catalog six different samples of passive galaxies, based on morphology (3336 \"morphological\" early-type galaxies), optical colors (4889 \"red-sequence\" galaxies and 4882 \"red UVJ\" galaxies), specific star-formation rate (2937 \"quiescent\" galaxies), a best fit to the observed spectral energy distribution (2603 \"red SED\" galaxies), and a criterion that combines morphological, spectroscopic, and photometric information (1530 \"red & passive early-type galaxies\"). For all the samples, we studied optical and infrared colors, morphological properties, specific star-formation rates (SFRs), and the equivalent widths of the residual emission lines; this analysis was performed as a function of redshift and stellar mass to inspect further possible dependencies.\nResults. We find that each passive galaxy sample displays a certain level of contamination due to blue/star-forming/nonpassive outliers. The morphological sample is the one that presents the higher percentage of contamination, with ~12\u221265% (depending on the mass range) of galaxies not located in the red sequence, ~25\u221280% of galaxies with a specific SFR up to ~25 times higher than the adopted definition of passive, and significant emission lines found in the median stacked spectra, at least for log (M/M_\u2299) < 10.25. The red & passive ETGs sample is the purest, with a percentage of contamination in color <10% for stellar masses log (M/M_\u2299) > 10.25, very limited tails in sSFR, a median value ~20% higher than the chosen passive cut, and equivalent widths of emission lines mostly compatible with no star-formation activity. However, it is also the less economic criterion in terms of information used. Among the other criteria, we found that the best performing are the red SED and the quiescent ones, providing a percentage of contamination only slightly higher than the red & passive ETGs criterion (on average of a factor of ~2) but with absolute values of the properties of contaminants still compatible with a red, passively evolving population. We also find a strong dependence of the contamination on the stellar mass and conclude that, almost irrespective of the adopted selection criteria, a cut at log (M/M_\u2299) > 10.75 provides a significantly purer sample in terms of star-forming contaminants. By studying the restframe color-mass and color\u2212color diagrams, we provided two revised definitions of passive galaxies based on these criteria that better reproduce the observed bimodality in the properties of zCOSMOS-20k galaxies. The analysis of the number densities of the various samples shows evidences of mass-assembly \"downsizing\", with galaxies at 10.25 < log\u2009 (M/M_\u2299) < 10.75 increasing their number by a factor ~2\u22124 from z = 0.6 to z = 0.2, by a factor ~2\u22123 from z = 1 to z = 0.2 at 10.75 < log\u2009 (M/M_\u2299) < 11, and by only ~10\u221250% from z = 1 to z = 0.2 at 11 < log\u2009 (M/M_\u2299) < 11.5.", "date": "2013-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "558", "publisher": "EDP Sciences", "pagerange": "Art. No. A61", "id_number": "CaltechAUTHORS:20140108-111022324", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140108-111022324", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/023/12/0" }, { "agency": "MIUR PRIN 2010-2011" }, { "agency": "INAF grant", "grant_number": "PRIN-2010" } ] }, "other_numbering_system": { "items": [ { "id": "LP175.A-0839", "name": "ESO Paranal Observatory Programme ID" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201321797", "primary_object": { "basename": "1305.1308v2.pdf", "url": "https://authors.library.caltech.edu/records/vqazq-wt378/files/1305.1308v2.pdf" }, "related_objects": [ { "basename": "aa21797-13.pdf", "url": "https://authors.library.caltech.edu/records/vqazq-wt378/files/aa21797-13.pdf" } ], "pub_year": "2013", "author_list": "Moresco, M. and Scoville, N." }, { "id": "https://authors.library.caltech.edu/records/wvh9g-dk461", "eprint_id": 43263, "eprint_status": "archive", "datestamp": "2023-08-19 21:41:13", "lastmod": "2023-10-25 23:24:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "S." } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Chevallard-J", "name": { "family": "Chevallard", "given": "J." } }, { "id": "Johnson-B-D", "name": { "family": "Johnson", "given": "B. D." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Treyer-M", "name": { "family": "Treyer", "given": "M." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "B." } }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "L." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" } ] }, "title": "Encoding of the infrared excess in the NUVrK color diagram\n for star-forming galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: galaxies, ultraviolet: galaxies, galaxies: evolution", "note": "\u00a9 2013 ESO. \n\nArticle published by EDP Sciences.\n\nPublished online 04 October 2013.\n\nReceived 25 April 2013. Accepted 25 July 2013. We thank the anonymous referee for his useful comments.\nThis work has been partially supported by the CNRS-INSU and the Progamme National de Cosmologie et Galaxies. J.C. acknowledges the support of the European Commission through the Marie Curie Initial Training Network ELIXIR under contract PITN-GA-2008-214227.\n\nPublished - aa21768-13.pdf
Submitted - 1309.0008v1.pdf
", "abstract": "We present an empirical method of assessing the star formation rate (SFR) of star-forming galaxies based on their locations in the rest-frame color\u2013color diagram (NUV \u2212 r) vs. (r \u2212 K). By using the Spitzer 24\u2009\u2009\u03bcm sample in the COSMOS field (~16\u2009400 galaxies with 0.2 \u2264 z \u2264 1.3) and a local GALEX-SDSS-SWIRE sample (~700 galaxies with z \u2264 0.2), we show that the mean infrared excess \u27e8IRX\u27e9 = \u27e8 L_(IR)/L_(UV)\u27e9 can be described by a single vector, NRK , that combines the two colors. The calibration between \u27e8IRX\u27e9 and NRK allows us to recover the IR luminosity, L_(IR), with an accuracy of \u03c3 ~ 0.21 for the COSMOS sample and 0.27 dex for the local one. The SFRs derived with this method agree with the ones based on the observed (UV+IR) luminosities and on the spectral energy distribution (SED) fitting for the vast majority (~85%) of the star-forming population. Thanks to a library of model galaxy SEDs with realistic prescriptions for the star formation history, we show that we need to include a two-component dust model (i.e., birth clouds and diffuse ISM) and a full distribution of galaxy inclinations in order to reproduce the behavior of the \u27e8IRX\u27e9 stripes in the NUVrK diagram. In conclusion, the NRK method, based only on the rest-frame UV/optical colors available in most of the extragalactic fields, offers a simple alternative of assessing the SFR of star-forming galaxies in the absence of far-IR or spectral diagnostic observations.", "date": "2013-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "558", "publisher": "EDP Sciences", "pagerange": "Art. No. A67", "id_number": "CaltechAUTHORS:20140108-104018487", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140108-104018487", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Progamme National de Cosmologie et Galaxies" }, { "agency": "Marie Curie Fellowship", "grant_number": "PITN-GA-2008-214227" }, { "agency": "Institut national des sciences de l'Univers (INSU)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201321768", "primary_object": { "basename": "1309.0008v1.pdf", "url": "https://authors.library.caltech.edu/records/wvh9g-dk461/files/1309.0008v1.pdf" }, "related_objects": [ { "basename": "aa21768-13.pdf", "url": "https://authors.library.caltech.edu/records/wvh9g-dk461/files/aa21768-13.pdf" } ], "pub_year": "2013", "author_list": "Arnouts, S.; Le Floc'h, E.; et el." }, { "id": "https://authors.library.caltech.edu/records/0f1h8-3ps49", "eprint_id": 42059, "eprint_status": "archive", "datestamp": "2023-08-22 10:23:09", "lastmod": "2023-10-25 15:04:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Calanog-J-A", "name": { "family": "Calanog", "given": "J. A." } }, { "id": "Wardlow-J-L", "name": { "family": "Wardlow", "given": "J." }, "orcid": "0000-0003-2376-8971" }, { "id": "Fu-Hai", "name": { "family": "Fu", "given": "Hai" }, "orcid": "0000-0001-9608-6395" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Assef-R-J", "name": { "family": "Assef", "given": "R. J." }, "orcid": "0000-0002-9508-3667" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Casey-C-M", "name": { "family": "Casey", "given": "C. M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Conley-A", "name": { "family": "Conley", "given": "A." } }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Ibar-Eduardo", "name": { "family": "Ibar", "given": "E." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Magdis-G", "name": { "family": "Magdis", "given": "G." } }, { "id": "Marchetti-L", "name": { "family": "Marchetti", "given": "L." }, "orcid": "0000-0003-3948-7621" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "P\u00e9rez-Fournon-I", "name": { "family": "P\u00e9rez-Fournon", "given": "I." } }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Rigopoulou-D", "name": { "family": "Rigopoulou", "given": "D." }, "orcid": "0000-0001-6854-7545" }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I. G." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "M." } }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: The Far-infrared Emission from Dust-obscured Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: luminosity function, mass function; galaxies: star formation; infrared: galaxies", "note": "\u00a9 2013 American Astronomical Society. Received 2013 April 16, accepted for publication 2013 July 22. Published 2013 September 5. We thank the anonymous referee for useful comments that helped improve this paper. We thank Jason Melbourne for insightful discussions. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including: University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). This research has made use of data from the HerMES project (http://hermes.sussex.ac.uk/). HerMES is a Herschel\nKey Programme utilizing Guaranteed Time from the SPIRE\ninstrument team, ESAC scientists, and a mission scientist.\nThe data presented in this paper will be released through the HerMES Database in Marseille, HeDaM (http://hedam.oamp.fr/HerMES/). We our thankful to the COSMOS collaboration for granting us access to their catalogs and we gratefully acknowledge the contributions of the entire COSMOS team that have made this work possible. More information on the COSMOS survey is available at http://hermes.sussex.ac.uk/. This work is based (in\npart) on observations made with the Spitzer Space Telescope,\nwhich is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We acknowledge support from a GAANN fellowship (to J.A.C.), NSF CAREER AST-0645427 (A.C. and H.F.), and NASA funds to the US HerMES team through JPL. S.O. acknowledges\nsupport from the Science and Technology Facilities Council\n[grant number ST/I000976/1]. Some of the data (spectroscopic redshifts) presented here were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of\nTechnology, the University of California, and the National\nAeronautics and Space Administration. The Observatory was\nmade possible by the generous financial support of the W.\nM. Keck Foundation. The authors wish to recognize and\nacknowledge the very significant cultural role and reverence\nthat the summit of Mauna Kea has always had within the\nindigenous Hawaiian community.We are most fortunate to have\nthe opportunity to conduct observations from this mountain.\nFacilities: Herschel (SPIRE), Spitzer (IRAC, MIPS), Subaru\n(Suprime Cam), Keck:II (DEIMOS)\n\nPublished - 0004-637X_775_1_61.pdf
Submitted - 1307.6967v1.pdf
", "abstract": "Dust-obscured galaxies (DOGs) are an ultraviolet-faint, infrared-bright galaxy population that reside at z ~ 2 and are believed to be in a phase of dusty star-forming and active galactic nucleus (AGN) activity. We present far-infrared (far-IR) observations of a complete sample of DOGs in the 2 deg^2 of the Cosmic Evolution Survey. The 3077 DOGs have \u3008z\u3009 = 1.9 \u00b1 0.3 and are selected from 24 \u03bcm and r^+ observations using a color cut of r^+ \u2013 [24] \u2265 7.5 (AB mag) and S_(24) \u2265 100 \u03bcJy. Based on the near-IR spectral energy distributions, 47% are bump DOGs (star formation dominated) and 10% are power-law DOGs (AGN-dominated). We use SPIRE far-IR photometry from the Herschel Multi-tiered Extragalactic Survey to calculate the IR luminosity and characteristic dust temperature for the 1572 (51%) DOGs that are detected at 250 \u03bcm (\u22653\u03c3). For the remaining 1505 (49%) that are undetected, we perform a median stacking analysis to probe fainter luminosities. Herschel-detected and undetected DOGs have average luminosities of (2.8 \u00b1 0.4) \u00d7 10^(12) L_\u2609 and (0.77 \u00b1 0.08) \u00d7 10^(12) L_\u2609, and dust temperatures of (33 \u00b1 7) K and (37 \u00b1 5) K, respectively. The IR luminosity function for DOGs with S_(24) \u2265 100 \u03bcJy is calculated, using far-IR observations and stacking. DOGs contribute 10%-30% to the total star formation rate (SFR) density of the universe at z = 1.5-2.5, dominated by 250 \u03bcm detected and bump DOGs. For comparison, DOGs contribute 30% to the SFR density for all z = 1.5-2.5 galaxies with S_(24) \u2265 100 \u03bcJy. DOGs have a large scatter about the star formation main sequence and their specific SFRs show that the observed phase of star formation could be responsible for their total observed stellar mass at z ~ 2.", "date": "2013-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "775", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 61", "id_number": "CaltechAUTHORS:20131025-085434310", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131025-085434310", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" }, { "agency": "GAANN fellowship" }, { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/775/1/61", "primary_object": { "basename": "0004-637X_775_1_61.pdf", "url": "https://authors.library.caltech.edu/records/0f1h8-3ps49/files/0004-637X_775_1_61.pdf" }, "related_objects": [ { "basename": "1307.6967v1.pdf", "url": "https://authors.library.caltech.edu/records/0f1h8-3ps49/files/1307.6967v1.pdf" } ], "pub_year": "2013", "author_list": "Calanog, J. A.; Wardlow, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/8thfx-sgg51", "eprint_id": 41456, "eprint_status": "archive", "datestamp": "2023-08-22 10:07:07", "lastmod": "2023-10-24 23:45:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Bschorr-T-J", "name": { "family": "Bschorr", "given": "T. J." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Cibinel-A", "name": { "family": "Cibinel", "given": "A." }, "orcid": "0000-0003-4578-514X" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Onodera-Masato", "name": { "family": "Onodera", "given": "M." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Cameron-E-M", "name": { "family": "Cameron", "given": "E." } }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" } ] }, "title": "Newly Quenched Galaxies as the Cause for the Apparent Evolution in Average Size of the Population", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: fundamental parameters; galaxies: structure", "note": "\u00a9 2013 American Astronomical Society. Received 2013 February 18; accepted 2013 June 7; published 2013 August 1. T.B., A.C., E.C., and M.O. thank the Swiss National Science\nFoundation for financial support. A.R. acknowledges the ETHZ\nInstitute of Astronomy for its kind hospitality at the time when this research was started and this paper first laid down, and the National Institute for Astrophysics for support through the grant INAF-PRIN 2010.\n\nPublished - 0004-637X_773_2_112.pdf
Submitted - 1302.5115v2.pdf
", "abstract": "We use the large COSMOS sample of galaxies to study in an internally self-consistent way the change in the number densities of quenched early-type galaxies (Q-ETGs) of a given size over the redshift interval 0.2 < z < 1 in order to study the claimed size evolution of these galaxies. In a stellar mass bin at 10^(10.5) < M_(galaxy) < 10^(11)\u2009M_\u2609, we see no change in the number density of compact Q-ETGs over this redshift range, while in a higher mass bin at >10^(11)\u2009M_\u2609, where we would expect merging to be more significant, we find a small decrease, by ~30%. In both mass bins, the increase of the median sizes of Q-ETGs with time is primarily caused by the addition to the size function of larger and more diffuse Q-ETGs. At all masses, compact Q-ETGs become systematically redder toward later epochs, with a (U \u2212 V) color difference which is consistent with a passive evolution of their stellar populations, indicating that they are a stable population that does not appreciably evolve in size. We find furthermore, at all epochs, that the larger Q-ETGs (at least in the lower mass bin) have average rest-frame colors that are systematically bluer than those of the more compact Q-ETGs, suggesting that the former are indeed younger than the latter. The idea that new, large, Q-ETGs are responsible for the observed growth in the median size of the population at a given mass is also supported by analysis of the sizes and number of the star-forming galaxies that are expected to be the progenitors of the new Q-ETGs over the same period. In the low mass bin, the new Q-ETGs appear to have ~30% smaller half-light radii than their star-forming progenitors. This is likely due to the fading of their disks after they cease star formation. Comparison with higher redshifts shows that the median size of newly quenched galaxies roughly scales, at constant mass, as (1 + z)^(\u22121). We conclude that the dominant cause of the size evolution seen in the Q-ETG population is that the average sizes and thus stellar densities of individual Q-ETGs roughly scale with the average density of the universe at the time when they were quenched, and that subsequent size changes in individual objects, through merging or other processes, are of secondary importance, especially at masses below 10^(11)\u2009M_\u2609.", "date": "2013-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "773", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 112", "id_number": "CaltechAUTHORS:20130920-152508455", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130920-152508455", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "INAF-PRIN 2010" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/773/2/112", "primary_object": { "basename": "0004-637X_773_2_112.pdf", "url": "https://authors.library.caltech.edu/records/8thfx-sgg51/files/0004-637X_773_2_112.pdf" }, "related_objects": [ { "basename": "1302.5115v2.pdf", "url": "https://authors.library.caltech.edu/records/8thfx-sgg51/files/1302.5115v2.pdf" } ], "pub_year": "2013", "author_list": "Carollo, C. M.; Bschorr, T. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/wyvnz-xzb48", "eprint_id": 41470, "eprint_status": "archive", "datestamp": "2023-08-22 10:07:21", "lastmod": "2023-10-24 23:46:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Alexander-D-M", "name": { "family": "Alexander", "given": "D. M." }, "orcid": "0000-0002-5896-6313" }, { "id": "Grefenstette-B-W", "name": { "family": "Grefenstette", "given": "B. W." }, "orcid": "0000-0002-1984-2932" }, { "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "F. A." }, "orcid": "0000-0003-2992-8024" }, { "id": "Madsen-K-K", "name": { "family": "Madsen", "given": "K. K." }, "orcid": "0000-0003-1252-4891" }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "C. R." } }, { "id": "Miller-S-H", "name": { "family": "Miller", "given": "S. H." } } ] }, "title": "The NuSTAR Extragalactic Survey: A First Sensitive Look at the High-energy Cosmic X-Ray Background Population", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: high-redshift; infrared: galaxies; X-rays: diffuse background; X-rays: general", "note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 June 2; accepted 2013 June 28; published 2013 August 1. \n\nWe acknowledge financial support from the Leverhulme Trust (D.M.A. and J.R.M.), the Science and Technology Facilities\nCouncil (STFC; D.M.A., A.D.M., and G.B.L.), the SAO grant GO2-13164X (M.A.), NASA Postdoctoral Program at the Jet Propulsion Laboratory (R.J.A.), NSF award AST 1008067\n(D.R.B.), Center of Excellence in Astrophysics and Associated Technologies (PFB 06/2007; F.E.B. and E.T.), the Anillo project ACT1101 (F.E.B. and E.T.), FONDECYT Regular 1101024 (F.E.B.), Caltech NuSTAR subcontract 44A-1092750 (W.N.B. and B.L.),NASA ADP grant NNX10AC99G (W.N.B. and B.L.), ASI/INAF grant I/037/12/0 (A.C. and S.P.), CONICYT-Chile under grant FONDECYT 3120198 (C.S.), and FONDECYT regular grant 1120061 (E.T.). We thank the referee for a constructive and positive report. We also thank Michael Koss for the discussion of Swift-BAT results, and Mark Brodwin,Daniel Gettings, John Gizis, Richard Walters, Jingwen Wu, and Dominika Wylezalek for supporting the ground-based follow-up observations. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National\nAeronautics and Space Administration. We thank the NuSTAR\nOperations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - 0004-637X_773_2_125.pdf
Submitted - 1307.1733v1.pdf
", "abstract": "We report on the first 10 identifications of sources serendipitously detected by the Nuclear Spectroscopic Telescope Array (NuSTAR) to provide the first sensitive census of the cosmic X-ray background source population at \u227310 keV. We find that these NuSTAR-detected sources are \u2248100 times fainter than those previously detected at \u227310 keV and have a broad range in redshift and luminosity (z = 0.020-2.923 and L_(10-40 keV) \u2248 4 \u00d7 10^(41)-5 \u00d7 10^(45) erg s^(\u20131)); the median redshift and luminosity are z \u2248 0.7 and L_(10-40 keV) \u2248 3 \u00d7 10^(44) erg s^(\u20131), respectively. We characterize these sources on the basis of broad-band \u22480.5-32 keV spectroscopy, optical spectroscopy, and broad-band ultraviolet-to-mid-infrared spectral energy distribution analyses. We find that the dominant source population is quasars with L_(10-40 keV) > 10^(44) erg s^(\u20131), of which \u224850% are obscured with N_H \u2273 10^(22) cm^(\u20132). However, none of the 10 NuSTAR sources are Compton thick (N_H \u2273 10^(24) cm^(\u20132)) and we place a 90% confidence upper limit on the fraction of Compton-thick quasars (L_(10-40 keV) > 10^(44) erg s^(\u20131)) selected at \u227310 keV of \u227e33% over the redshift range z = 0.5-1.1. We jointly fitted the rest-frame \u224810-40 keV data for all of the non-beamed sources with L_(10-40 keV) > 10^(43) erg s^(\u20131) to constrain the average strength of reflection; we find R < 1.4 for \u0393 = 1.8, broadly consistent with that found for local active galactic nuclei (AGNs) observed at \u227310 keV. We also constrain the host-galaxy masses and find a median stellar mass of \u224810^(11) M_\u2609, a factor \u22485 times higher than the median stellar mass of nearby high-energy selected AGNs, which may be at least partially driven by the order of magnitude higher X-ray luminosities of the NuSTAR sources. Within the low source-statistic limitations of our study, our results suggest that the overall properties of the NuSTAR sources are broadly similar to those of nearby high-energy selected AGNs but scaled up in luminosity and mass.", "date": "2013-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "773", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 125", "id_number": "CaltechAUTHORS:20130923-094035250", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130923-094035250", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Leverhulme Trust" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Smithsonian Astrophysical Observatory", "grant_number": "GO2-13164X" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "NSF", "grant_number": "AST-1008067" }, { "agency": "Basal-CATA", "grant_number": "PFB-06/2007" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "Anillo ACT1101" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1101024" }, { "agency": "Caltech NuSTAR subcontract", "grant_number": "44A-1092750" }, { "agency": "NASA", "grant_number": "NNX10AC99G" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/037/12/0-011/13" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "3120198" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1120061" }, { "agency": "NASA", "grant_number": "NNG08FD60C" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "NuSTAR" }, { "id": "COSMOS" }, { "id": "Space-Radiation-Laboratory" } ] }, "doi": "10.1088/0004-637X/773/2/125", "primary_object": { "basename": "0004-637X_773_2_125.pdf", "url": "https://authors.library.caltech.edu/records/wyvnz-xzb48/files/0004-637X_773_2_125.pdf" }, "related_objects": [ { "basename": "1307.1733v1.pdf", "url": "https://authors.library.caltech.edu/records/wyvnz-xzb48/files/1307.1733v1.pdf" } ], "pub_year": "2013", "author_list": "Alexander, D. M.; Grefenstette, B. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/5fgdh-5w037", "eprint_id": 41489, "eprint_status": "archive", "datestamp": "2023-08-22 10:07:28", "lastmod": "2023-10-24 23:47:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schram-M", "name": { "family": "Schram", "given": "M." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Greene-J-E", "name": { "family": "Greene", "given": "J. E." } }, { "id": "Brandt-W-N", "name": { "family": "Brandt", "given": "W. N." }, "orcid": "0000-0002-0167-2453" }, { "id": "Luo-Bin", "name": { "family": "Luo", "given": "B." }, "orcid": "0000-0002-9036-0063" }, { "id": "Xue-Y-Q", "name": { "family": "Xue", "given": "Y. Q." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Kakazu-Yuko", "name": { "family": "Kakazu", "given": "Y." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } } ] }, "title": "Unveiling a population of galaxies harboring low-mass black holes with X-rays", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; X-rays: galaxies", "note": "\u00a9 2013 American Astronomical Society. Received 2013 February 22; accepted 2013 May 10; published 2013 August 5. The authors fully appreciate the useful discussions with\nAaron Barth and Masayuki Tanaka that improved the paper.\nThis work was supported by the World Premier International\nResearch Center Initiative (WPI Initiative), MEXT, Japan.\nY.Q.X. acknowledges the financial support of the Thousand\nYoung Talents (QingNianQianRen) program (KJ2030220004),\nthe USTC startup funding (ZC9850290195), and the National\nNatural Science Foundation of China through NSFC-11243008.\nW. N. Brandt and B. Luo acknowledge the NASA ADP grant\nNNX10AC99G and the CXC grant AR3-14015X.\n\nPublished - 0004-637X_773_2_150.pdf
Submitted - 1305.3826v1.pdf
", "abstract": "We report the discovery of three low-mass black hole (BH) candidates residing in the centers of low-mass galaxies at z < 0.3 in the Chandra Deep Field-South Survey. These BHs are initially identified as candidate active galactic nuclei based on their X-ray emission in deep Chandra observations. Multi-wavelength observations are used to strengthen our claim that such emission is powered by an accreting supermassive BH. While the X-ray luminosities are low at L_X ~ 10^(40) erg s^(\u20131) (and variable in one case), we argue that they are unlikely to be attributed to star formation based on H\u03b1 or UV fluxes. Optical spectroscopy from Keck and the VLT allows us to (1) measure accurate redshifts, (2) confirm their low stellar host mass, (3) investigate the source(s) of photo-ionization, and (4) estimate extinction. With stellar masses of M_* < 3 \u00d7 10^9 M_\u2609 determined from Hubble Space Telescope/Advanced Camera for Surveys imaging, the host galaxies are among the lowest mass systems known to host actively accreting BHs. We estimate BH masses M_(BH) ~ 2 \u00d7 10^5 M_\u2609 based on scaling relations between BH mass and host properties for more luminous systems. In one case, a broad component of the H\u03b1 emission-line profile is detected, thus providing a virial mass estimate. BHs in such low-mass galaxies are of considerable interest as the low-redshift analogs to the seeds of the most massive BHs at high redshift which have remained largely elusive to date. Our study highlights the power of deep X-ray surveys to uncover such low-mass systems.", "date": "2013-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "773", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 150", "id_number": "CaltechAUTHORS:20130924-084223399", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130924-084223399", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Thousand Young Talents", "grant_number": "KJ2030220004" }, { "agency": "USTC startup funding", "grant_number": "ZC9850290195" }, { "agency": "National Natural Science Foundation of China", "grant_number": "NSFC-11243008" }, { "agency": "NASA", "grant_number": "NNX10AC99G" }, { "agency": "CXC", "grant_number": "AR3-14015X" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/773/2/150", "primary_object": { "basename": "0004-637X_773_2_150.pdf", "url": "https://authors.library.caltech.edu/records/5fgdh-5w037/files/0004-637X_773_2_150.pdf" }, "related_objects": [ { "basename": "1305.3826v1.pdf", "url": "https://authors.library.caltech.edu/records/5fgdh-5w037/files/1305.3826v1.pdf" } ], "pub_year": "2013", "author_list": "Schram, M.; Silverman, J. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/3w76t-kv562", "eprint_id": 41085, "eprint_status": "archive", "datestamp": "2023-08-22 10:05:21", "lastmod": "2023-10-24 23:26:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wilkes-B-J", "name": { "family": "Wilkes", "given": "Belinda J." }, "orcid": "0000-0003-1809-2364" }, { "id": "Kuraszkiewicz-J", "name": { "family": "Kuraszkiewicz", "given": "Joanna" } }, { "id": "Haas-M", "name": { "family": "Haas", "given": "Martin" } }, { "id": "Barthel-P", "name": { "family": "Barthel", "given": "Peter" } }, { "id": "Leipski-C", "name": { "family": "Leipski", "given": "Christian" } }, { "id": "Willner-S-P", "name": { "family": "Willner", "given": "S. P." }, "orcid": "0000-0002-9895-5758" }, { "id": "Worrall-D-M", "name": { "family": "Worrall", "given": "D. M." } }, { "id": "Birkinshaw-M", "name": { "family": "Birkinshaw", "given": "Mark" } }, { "id": "Antonucci-R", "name": { "family": "Antonucci", "given": "Robert" } }, { "id": "Ashby-M-L-N", "name": { "family": "Ashby", "given": "M. L. N." }, "orcid": "0000-0002-3993-0745" }, { "id": "Chini-R", "name": { "family": "Chini", "given": "Rolf" } }, { "id": "Fazio-G-G", "name": { "family": "Fazio", "given": "G. G." }, "orcid": "0000-0002-0670-0708" }, { "id": "Lawrence-C-R", "name": { "family": "Lawrence", "given": "Charles" } }, { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "Patrick" }, "orcid": "0000-0002-3471-981X" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "Bernhard" } } ] }, "title": "Revealing the Heavily Obscured Active Galactic Nucleus Population of High-redshift 3CRR Sources with Chandra X-Ray Observations", "ispublished": "pub", "full_text_status": "public", "keywords": "quasars: general; X-rays: galaxies", "note": "\u00a9 2013 The American Astronomical Society.\n\nReceived 2013 February 26; accepted 2013 May 30; published 2013 July 19.\n\nSupport for this work was provided by the National Aeronautics\nand Space Administration through Chandra Award Number\nG08-9106X, by the Chandra X-Ray Center, which is operated\nby the Smithsonian Astrophysical Observatory for and on behalf\nof the National Aeronautics Space Administration under contract\nNAS8-03060 (Chandra X-Ray Center) and by the Smithsonian\nInstitution Endowment, Scholarly Studies Program, fund\n40488100HH0017. The scientific results in this article are based\nto a significant degree on observations made by the Chandra\nX-Ray Observatory (CXO). We thank Mark Avara and Margaret\nYellen for their early work on this project.\n\nPublished - 0004-637X_773_1_15.pdf
", "abstract": "Chandra observations of a complete, flux-limited sample of 38 high-redshift (1 < z < 2), low-frequency-selected (and so unbiased in orientation) 3CRR radio sources are reported. The sample includes 21 quasars (=broad-line radio galaxies) and 17 narrow-line radio galaxies (NLRGs) with matched 178 MHz radio luminosity (log L_R(5 GHz) ~44-45). The quasars have high radio core fraction, high X-ray luminosities (log L_X ~45-46), and soft X-ray hardness ratios (HR ~\u20130.5) indicating low obscuration. The NLRGs have lower core fraction, lower apparent X-ray luminosities (log L_X ~43-45), and mostly hard X-ray hardness ratios (HR >0) indicating obscuration (N_H ~10^(22)-10^(24) cm^(\u20132)). These properties and the correlation between obscuration and radio core fraction are consistent with orientation-dependent obscuration as in unification models. About half the NLRGs have soft X-ray hardness ratios and/or a high [O III] emission line to X-ray luminosity ratio suggesting obscuration by Compton thick (CT) material so that scattered nuclear or extended X-ray emission dominates (as in NGC 1068). The ratios of unobscured to Compton-thin (10^(22) cm^(\u20132) < N_H(int) <1.5 \u00d7 10^(24) cm^(\u20132)) to CT (N_H(int) >1.5 \u00d7 10^(24) cm^(\u20132)) is 2.5:1.4:1 in this high-luminosity, radio-selected sample. The obscured fraction is 0.5, higher than is typically reported for active galactic nuclei at comparable luminosities from multi-wavelength surveys (0.1-0.3). Assuming random nuclear orientation, the unobscured half-opening angle of the disk/wind/torus structure is ~60\u00b0 and the obscuring material covers 30\u00b0, ~12\u00b0 of which is CT. The multi-wavelength properties reveal that many NLRGs have intrinsic absorption 10-1000 \u00d7 higher than indicated by their X-ray hardness ratios, and their true L_X values are ~10-100\u00d7 larger than the hardness-ratio absorption corrections would indicate.", "date": "2013-08-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "773", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 15", "id_number": "CaltechAUTHORS:20130904-130436889", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130904-130436889", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "G08-9106X" }, { "agency": "Chandra X-Ray Center" }, { "agency": "NASA", "grant_number": "NAS8-03060" }, { "agency": "Smithsonian Institution", "grant_number": "40488100HH0017" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/773/1/15", "primary_object": { "basename": "0004-637X_773_1_15.pdf", "url": "https://authors.library.caltech.edu/records/3w76t-kv562/files/0004-637X_773_1_15.pdf" }, "pub_year": "2013", "author_list": "Wilkes, Belinda J.; Kuraszkiewicz, Joanna; et el." }, { "id": "https://authors.library.caltech.edu/records/12tv4-45049", "eprint_id": 41060, "eprint_status": "archive", "datestamp": "2023-08-19 21:04:01", "lastmod": "2023-10-24 23:25:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "A." }, "orcid": "0000-0002-9382-9832" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Tacchella-S", "name": { "family": "Tacchella", "given": "S." }, "orcid": "0000-0002-8224-4505" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Keck-I MOSFIRE Spectroscopy of the z ~ 12 Candidate Galaxy UDFj-39546284", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation \u2013 galaxies: high-redshift \u2013 line: identification", "note": "\u00a9 2013 The American Astronomical Society.\n\nReceived 2013 June 10; accepted 2013 July 12; published 2013 July 29.\n\nThe data presented herein were obtained at the W. M. Keck Observatory,\nwhich is operated as a scientific partnership among the California Institute of\nTechnology, the University of California, and the National Aeronautics and\nSpace Administration. The Observatory was made possible by the generous\nfinancial support of the W. M. Keck Foundation.\n\nWe acknowledge the support of the Keck Observatory staff\nwho made these observations possible and the valuable feedback\nfrom Janice Lee and Masami Ouchi while preparing this draft.\nWe also thank Nick Konidaris for providing and supporting the\nMOSFIRE reduction pipeline and Gwen Rude for providing the\nMOSFIRE exposure time calculator. A.F. and S.T. acknowledge\nsupport from the Swiss National Science Foundation; A.F. also\nthanks Caltech for hospitality while this article was prepared.\nThe authors recognize and acknowledge the very significant\ncultural role and reverence that the summit of Mauna Kea has\nalways had within the indigenous Hawaiian community. We are\nmost fortunate to have the opportunity to conduct observations\nfrom this mountain.\nFacility: Keck:I (MOSFIRE)\n\nPublished - 2041-8205_773_1_L14.pdf
Submitted - 1307.4089v1.pdf
", "abstract": "We report the results of deep (4.6 hr) H-band spectroscopy of the well studied z ~ 12 H-band dropout galaxy candidate UDFj-39546284 with MOSFIRE on Keck-I. These data reach a sensitivity of 5-10 \u00d7 10^(\u201319) erg s^(\u20131) cm^(\u20132) per 4.4 \u00c5 resolution element between sky lines. Previous papers have argued that this source could either be a large equivalent width line emitting galaxy at 2 < z < 3.5 or a luminous galaxy at z ~ 12. We find a 2.2\u03c3 peak associated with a line candidate in deep Hubble Space Telescope Wide-Field Camera 3 Infrared grism observations, but at a lower flux than expected. After considering several possibilities, we conclude these data cannot conclusively confirm or reject the previous line detection, and significantly deeper spectroscopic observations are required. We also search for low-redshift emission lines in 10 other 7 < z < 10 z, Y, and J-dropout candidates in our mask and find no significant detections.", "date": "2013-08-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "773", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L14", "id_number": "CaltechAUTHORS:20130903-131308765", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130903-131308765", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/2041-8205/773/1/L14", "primary_object": { "basename": "1307.4089v1.pdf", "url": "https://authors.library.caltech.edu/records/12tv4-45049/files/1307.4089v1.pdf" }, "related_objects": [ { "basename": "2041-8205_773_1_L14.pdf", "url": "https://authors.library.caltech.edu/records/12tv4-45049/files/2041-8205_773_1_L14.pdf" } ], "pub_year": "2013", "author_list": "Capak, P.; Faisst, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/gh30q-t4b36", "eprint_id": 41075, "eprint_status": "archive", "datestamp": "2023-08-22 09:58:41", "lastmod": "2023-10-24 23:26:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brightman-M", "name": { "family": "Brightman", "given": "M." }, "orcid": "0000-0002-8147-2602" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "A statistical relation between the X-ray spectral index and Eddington ratio of active galactic nuclei in deep surveys", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion; accretion discs; galaxies: active; galaxies: nuclei; quasars: emission lines; quasars: general; X-rays: galaxies", "note": "\u00a9 2013 The Authors.\nPublished by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 May 22. Received 2013 May 21; in original form 2013 April.\n\nFirst published online: June 17, 2013.\n\nThe authors would like to thank the anonymous referee for the\ncareful reading and constructive criticism of our manuscript. The\nauthors would also like to thank the builders and operators of XMM\u2013Newton and Chandra and all those involved in the COSMOS and E-CDF-S surveys. MB would like to acknowledge the financial\nsupport at the start of this project from the Japan Society for the\nPromotion of Science (JSPS).\n\nPublished - MNRAS-2013-Brightman-2485-96.pdf
Submitted - 1305.3917v1.pdf
", "abstract": "We present an investigation into how well the properties of the accretion flow on to a supermassive black hole may be coupled to those of the overlying hot corona. To do so, we specifically measure the characteristic spectral index, \u0393, of a power-law energy distribution, over an energy range of 2\u201310\u2009keV, for X-ray selected, broad-lined radio-quiet active galactic nuclei (AGN) up to z \u223c 2 in Cosmic Evolution Survey (COSMOS) and Extended Chandra Deep Field South (E-CDF-S). We test the previously reported dependence between \u0393 and black hole mass, full width at half-maximum (FWHM) and Eddington ratio using a sample of AGN covering a broad range in these parameters based on both the Mg II and H\u03b1 emission lines with the later afforded by recent near-infrared spectroscopic observations using Subaru/Fibre Multi Object Spectrograph. We calculate the Eddington ratios, \u03bb_(Edd), for sources where a bolometric luminosity (L_(Bol)) has been presented in the literature, based on spectral energy distribution fitting, or, for sources where these data do not exist, we calculate L_(Bol) using a bolometric correction to the X-ray luminosity, derived from a relationship between the bolometric correction and L_X/L_(3000). From a sample of 69 X-ray bright sources (>250 counts), where \u0393 can be measured with greatest precision, with an estimate of L_(Bol), we find a statistically significant correlation between \u0393 and \u03bb_(Edd), which is highly significant with a chance probability of 6.59\u00d7 10^(\u22128). A statistically significant correlation between \u0393 and the FWHM of the optical lines is confirmed, but at lower significance than with \u03bb_(Edd) indicating that \u03bb_(Edd) is the key parameter driving conditions in the corona. Linear regression analysis reveals that \u0393 = (0.32 \u00b1 0.05) log_(10)\u03bb_(Edd) + (2.27 \u00b1 0.06) and \u0393 = (\u22120.69 \u00b1 0.11) log_(10)(FWHM/km\u2009s^(\u22121)) + (4.44 \u00b1 0.42). Our results on \u0393\u2013\u03bb_(Edd) are in very good agreement with previous results. While the \u0393\u2013\u03bb_(Edd) relationship means that X-ray spectroscopy may be used to estimate black hole accretion rate, considerable dispersion in the correlation does not make this viable for single sources, however could be valuable for large X-ray spectral samples, such as those to be produced by eROSITA.", "date": "2013-08", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "433", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2485-2496", "id_number": "CaltechAUTHORS:20130904-085052683", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130904-085052683", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stt920", "primary_object": { "basename": "1305.3917v1.pdf", "url": "https://authors.library.caltech.edu/records/gh30q-t4b36/files/1305.3917v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2013-Brightman-2485-96.pdf", "url": "https://authors.library.caltech.edu/records/gh30q-t4b36/files/MNRAS-2013-Brightman-2485-96.pdf" } ], "pub_year": "2013", "author_list": "Brightman, M. and Capak, P." }, { "id": "https://authors.library.caltech.edu/records/xveqb-3ed75", "eprint_id": 41684, "eprint_status": "archive", "datestamp": "2023-08-22 10:01:25", "lastmod": "2023-10-24 23:56:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Mass assembly in quiescent and star-forming galaxies since z \u2243 4 from UltraVISTA", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: distances and redshifts; galaxies: evolution; galaxies: formation; galaxies: star formation; galaxies: stellar content", "note": "\u00a9 2013 ESO. \nArticle published by EDP Sciences.\n\nReceived 14 January 2013. Accepted 30 May 2013. \nPublished online 25 July 2013.\n\nWe are grateful to the referee for a careful reading of the\nmanuscript and useful suggestions. The authors thank M. Kajisawa, L. Pozzetti, P. P\u00e9rez-Gonz\u00e1lez and P. Santini for providing their estimates of the mass function. We also thanks P. Behroozi for his useful suggestions. The authors thank J. Donley for providing her catalogue of IRAC power-laws. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. The HST COSMOS program was supported through\nNASA grant HST-GO-09822. More information on the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. H.J. McCracken acknowledges support from the \"Programme national cosmologie et galaxies\". J.S.D. acknowledges the support of the European Research Council through an\nAdvanced grant, and the support of the Royal Society via a Wolfson Research Merit Award. S. Toft acknowledges support from the Lundbeck foundation. The Dark Cosmology Centre is funded by the Danish National Research Foundation. This paper is based on observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This work is based in part on archival SEDS data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA. This research has\nmade use of the NASA/ IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The Dark Cosmology\nCentre is funded by the Danish National Research Foundation. B.M.J. acknowledges support from the ERC-StG grant EGGS-278202. \n\n\nBased on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme\nID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.\n\nPublished - aa21100-13.pdf
Submitted - 1301.3157v3.pdf
", "abstract": "We estimate the galaxy stellar mass function and stellar mass density for star-forming and quiescent galaxies with 0.2 < z < 4. We construct a large, deep (K_s < 24) sample of 220\u2009000 galaxies selected using the new UltraVISTA DR1 data release. Our analysis is based on precise 30-band photometricredshifts. By comparing these photometric redshifts with 10,800 spectroscopic redshifts from the zCOSMOS bright and faint surveys, we find a precision of \u03c3_(\u0394z/(1 + z)) = 0.008 at i+ < 22.5 and \u03c3_(\u0394z/(1 + z)) = 0.03 at 1.5 < z < 4. We derive the stellar mass function and correct for the Eddington bias. We find a mass-dependent evolution of the global and star-forming populations, with the low-mass end of the mass functions evolving more rapidly than the high-mass end. This mass-dependent evolution is a direct consequence of the star formation being \"quenched\" in galaxies more massive than \u2133 \u2273 1010.7 \u2212 10.9\u2133_\u2299. For the mass function of the quiescent galaxies, we do not find any significant evolution of the high-mass end at z < 1; however we observe a clear flattening of the faint-end slope. From z ~ 3 to z ~ 1, the density of quiescent galaxies increases over the entire mass range. Their comoving stellar mass density increases by 1.6 dex between z ~ 3 and z ~ 1 and by less than 0.2 dex at z < 1. We infer the star formation history from the mass density evolution. This inferred star formation history is in excellent agreement with instantaneous star formation rate measurements at z < 1.5, while we find differences of 0.2 dex at z > 1.5 consistent with the expected uncertainties. We also develop a new method to infer the specific star formation rate from the mass function of star-forming galaxies. We find that the specific star formation rate of 10^(10\u221210.5)\u2133_\u2299 galaxies increases continuously in the redshift range 1 < z < 4. Finally, we compare our results with a semi-analytical model and find that these models overestimate the density of low mass quiescent galaxies by an order of magnitude, while the density of low-mass star-forming galaxies is successfully reproduced.", "date": "2013-08", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "556", "publisher": "EDP Sciences", "pagerange": "Art. No. A55", "id_number": "CaltechAUTHORS:20131004-111419268", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131004-111419268", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "Programme National Cosmologie et Galaxies" }, { "agency": "European Research Council Advanced Grant" }, { "agency": "Royal Society Wolfson Research Merit award" }, { "agency": "Lundbeck Foundation" }, { "agency": "Danish National Research Foundation" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "ERC-StG", "grant_number": "EGGS-278202" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201321100", "primary_object": { "basename": "1301.3157v3.pdf", "url": "https://authors.library.caltech.edu/records/xveqb-3ed75/files/1301.3157v3.pdf" }, "related_objects": [ { "basename": "aa21100-13.pdf", "url": "https://authors.library.caltech.edu/records/xveqb-3ed75/files/aa21100-13.pdf" } ], "pub_year": "2013", "author_list": "Ilbert, O.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/0q8m9-y9w44", "eprint_id": 39946, "eprint_status": "archive", "datestamp": "2023-08-22 09:49:21", "lastmod": "2023-10-24 17:19:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Matsuoka-Kenta", "name": { "family": "Matsuoka", "given": "K." }, "orcid": "0000-0002-2689-4634" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "A Comparative Analysis of Virial Black Hole Mass Estimates of Moderate-luminosity Active Galactic Nuclei Using Subaru/FMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "black hole physics; galaxies: active; quasars: emission lines", "note": "\u00a9 2013 American Astronomical Society.\n\nReceived 2013 January 10; accepted 2013 May 8; published 2013 June 17.\n\nWe thank Kentaro Aoki and Naoyuki Tamura for their\ninvaluable assistance during our Subaru/FMOS observations.\nK.M. acknowledges financial support from the Japan Society for\nthe Promotion of Science (JSPS). T.N. is financially supported\nby JSPS (grant No. 23654068). Data analyses were carried out\nin part on common-use data analysis computer system at the\nAstronomy Data Center, ADC, of the National Astronomical\nObservatory of Japan (NAOJ).\n\nPublished - 0004-637X_771_1_64.pdf
Submitted - 1301.2332v1.pdf
", "abstract": "We present an analysis of broad emission lines observed in moderate-luminosity active galactic nuclei (AGNs), typical of those found in X-ray surveys of deep fields, with the goal of testing the validity of single-epoch virial black hole mass estimates. We have acquired near-infrared spectra of AGNs up to z ~ 1.8 in the COSMOS and Extended Chandra Deep Field-South Survey, with the Fiber Multi-Object Spectrograph mounted on the Subaru telescope. These near-infrared spectra provide a significant detection of the broad H\u03b1 line, shown to be a reliable probe of black hole mass at low redshift. Our sample has existing optical spectroscopy that provides a detection of Mg II, typically used for black hole mass estimation at z gsim 1. We carry out a spectral-line fitting procedure using both H\u03b1 and Mg II to determine the virial velocity of gas in the broad-line region, the continuum luminosity at 3000 \u00c5, and the total H\u03b1 line luminosity. With a sample of 43 AGNs spanning a range of two decades in luminosity, we find a tight correlation between the ultraviolet and emission-line luminosity. There is also a close one-to-one relationship between the full width at half-maximum of H\u03b1 and Mg II. Both of these then lead to there being very good agreement between H\u03b1- and Mg II-based masses over a wide range in black hole mass, i.e., M_BH ~ 10^(7-9) M_\u2609. In general, these results demonstrate that local scaling relations, using Mg II or H\u03b1, are applicable for AGNs at moderate luminosities and up to z ~ 2.", "date": "2013-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "771", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 64", "id_number": "CaltechAUTHORS:20130815-101140877", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130815-101140877", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23654068" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/771/1/64", "primary_object": { "basename": "0004-637X_771_1_64.pdf", "url": "https://authors.library.caltech.edu/records/0q8m9-y9w44/files/0004-637X_771_1_64.pdf" }, "related_objects": [ { "basename": "1301.2332v1.pdf", "url": "https://authors.library.caltech.edu/records/0q8m9-y9w44/files/1301.2332v1.pdf" } ], "pub_year": "2013", "author_list": "Matsuoka, K. and Capak, P." }, { "id": "https://authors.library.caltech.edu/records/6gnfp-xe116", "eprint_id": 39858, "eprint_status": "archive", "datestamp": "2023-08-22 09:39:55", "lastmod": "2023-10-24 17:15:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fern\u00e1ndez-X", "name": { "family": "Fern\u00e1ndez", "given": "Ximena" } }, { "id": "Van-Gorkom-J-H", "name": { "family": "Van Gorkom", "given": "J. H." } }, { "id": "Hess-K-M", "name": { "family": "Hess", "given": "Kelley M." } }, { "id": "Pisano-D-J", "name": { "family": "Pisano", "given": "D. J." } }, { "id": "Kreckel-K", "name": { "family": "Kreckel", "given": "Kathryn" }, "orcid": "0000-0001-6551-3091" }, { "id": "Momjian-E", "name": { "family": "Momjian", "given": "Emmanuel" }, "orcid": "0000-0003-3168-5922" }, { "id": "Popping-A", "name": { "family": "Popping", "given": "Attila" } }, { "id": "Oosterloo-T", "name": { "family": "Oosterloo", "given": "Tom" } }, { "id": "Chomiuk-L", "name": { "family": "Chomiuk", "given": "Laura" }, "orcid": "0000-0002-8400-3705" }, { "id": "Verheijen-M-A-W", "name": { "family": "Verheijen", "given": "M. A. W." } }, { "id": "Henning-P-A", "name": { "family": "Henning", "given": "Patricia A." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Berhady-M-A", "name": { "family": "Bershady", "given": "Matthew A." } }, { "id": "Wilcots-E-M", "name": { "family": "Wilcots", "given": "Eric M." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "A Pilot for a Very Large Array H I Deep Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; radio lines: galaxies", "note": "\u00a9 2013 American Astronomical Society. Received 2013 March 11; accepted 2013 May 5; published 2013 June 3. We thank ASTRON for hosting us for two very successful busy weeks. This work was in part supported by the National Science Foundation under grant No. 1009476 to Columbia University.\nThis work is partly based on observations made with the\nNASA Galaxy Evolution Explorer (GALEX) and SDSS. GALEX\nis operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. The Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The full acknowledgement can be found here: http://www.sdss3.org/.\n\nPublished - 2041-8205_770_2_L29.pdf
Submitted - 1303.2659v2.pdf
", "abstract": "High-resolution 21 cm H I deep fields provide spatially and kinematically resolved images of neutral hydrogen at different redshifts, which are key to understanding galaxy evolution across cosmic time and testing predictions of cosmological simulations. Here we present results from a pilot for an H I deep field done with the Karl G. Jansky Very Large Array (VLA). We take advantage of the newly expanded capabilities of the telescope to probe the redshift interval 0 < z < 0.193 in one observation. We observe the COSMOS field for 50 hr, which contains 413 galaxies with optical spectroscopic redshifts in the imaged field of 34' \u00d7 34' and the observed redshift interval. We have detected neutral hydrogen gas in 33 galaxies in different environments spanning the probed redshift range, including three without a previously known spectroscopic redshift. The detections have a range of H I and stellar masses, indicating the diversity of galaxies we are probing. We discuss the observations, data reduction, results, and highlight interesting detections. We find that the VLA's B-array is the ideal configuration for H I deep fields since its long spacings mitigate radio frequency interference. This pilot shows that the VLA is ready to carry out such a survey, and serves as a test for future H I deep fields planned with other Square Kilometer Array pathfinders.", "date": "2013-06-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "770", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L29", "id_number": "CaltechAUTHORS:20130812-090420703", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130812-090420703", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1009476" }, { "agency": "NASA", "grant_number": "NAS5-98034" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/2041-8205/770/2/L29", "primary_object": { "basename": "1303.2659v2.pdf", "url": "https://authors.library.caltech.edu/records/6gnfp-xe116/files/1303.2659v2.pdf" }, "related_objects": [ { "basename": "2041-8205_770_2_L29.pdf", "url": "https://authors.library.caltech.edu/records/6gnfp-xe116/files/2041-8205_770_2_L29.pdf" } ], "pub_year": "2013", "author_list": "Fern\u00e1ndez, Ximena; Van Gorkom, J. H.; et el." }, { "id": "https://authors.library.caltech.edu/records/kzms5-yq422", "eprint_id": 38923, "eprint_status": "archive", "datestamp": "2023-08-22 09:24:10", "lastmod": "2023-10-24 14:52:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "M." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The Herschel census of infrared SEDs through cosmic time", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimetre: galaxies", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2013 February 19. Received 2013 February 4; in original form 2012 October 21. First published online: April 1, 2013. \n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. \n\nThis paper uses data from Herschel's photometers SPIRE and\nPACS. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain).\n\nPublished - MNRAS-2013-Symeonidis-2317-40.pdf
Accepted Version - 1302.4895.pdf
", "abstract": "Using Herschel data from the deepest SPIRE and PACS surveys (HerMES and PEP) in COSMOS, GOODS-S and GOODS-N, we examine the dust properties of infrared (IR)-luminous (L_IR > 10^10 L_\u2299) galaxies at 0.1 < z < 2 and determine how these evolve with cosmic time. The unique angle of this work is the rigorous analysis of survey selection effects, making this the first study of the star-formation-dominated, IR-luminous population within a framework almost entirely free of selection biases. We find that IR-luminous galaxies have spectral energy distributions (SEDs) with broad far-IR peaks characterized by cool/extended dust emission and average dust temperatures in the 25\u201345 K range. Hot (T > 45\u2009K) SEDs and cold (T < 25\u2009K), cirrus-dominated SEDs are rare, with most sources being within the range occupied by warm starbursts such as M82 and cool spirals such as M51. We observe a luminosity\u2013temperature (L-T) relation, where the average dust temperature of log [L_IR/L_\u2299] \u223c 12.5 galaxies is about 10 K higher than that of their log [L_IR/L_\u2299] \u223c 10.5 counterparts. However, although the increased dust heating in more luminous systems is the driving factor behind the L-T relation, the increase in dust mass and/or starburst size with luminosity plays a dominant role in shaping it. Our results show that the dust conditions in IR-luminous sources evolve with cosmic time: at high redshift, dust temperatures are on average up to 10 K lower than what is measured locally (z \u2272 0.1). This is manifested as a flattening of the L-T relation, suggesting that (ultra)luminous infrared galaxies [(U)LIRGs] in the early Universe are typically characterized by a more extended dust distribution and/or higher dust masses than local equivalent sources. Interestingly, the evolution in dust temperature is luminosity dependent, with the fraction of LIRGs with T < 35 K showing a two-fold increase from z \u223c 0 to z \u223c 2, whereas that of ULIRGs with T < 35 K shows a six-fold increase. Our results suggest a greater diversity in the IR-luminous population at high redshift, particularly for ULIRGs.", "date": "2013-05-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "431", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2317-2340", "id_number": "CaltechAUTHORS:20130612-134204476", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130612-134204476", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stt330", "primary_object": { "basename": "1302.4895.pdf", "url": "https://authors.library.caltech.edu/records/kzms5-yq422/files/1302.4895.pdf" }, "related_objects": [ { "basename": "MNRAS-2013-Symeonidis-2317-40.pdf", "url": "https://authors.library.caltech.edu/records/kzms5-yq422/files/MNRAS-2013-Symeonidis-2317-40.pdf" } ], "pub_year": "2013", "author_list": "Symeonidis, M.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/qh39q-sfk60", "eprint_id": 38753, "eprint_status": "archive", "datestamp": "2023-08-22 09:17:50", "lastmod": "2023-10-23 23:26:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hanish-D-J", "name": { "family": "Hanish", "given": "D. J." } }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H. I." }, "orcid": "0000-0002-7064-5424" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Desai-V", "name": { "family": "Desai", "given": "V." }, "orcid": "0000-0002-1340-0543" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Brinkworth-C", "name": { "family": "Brinkworth", "given": "C." } }, { "id": "Brooke-T-Y", "name": { "family": "Brooke", "given": "T." } }, { "id": "Colbert-J-W", "name": { "family": "Colbert", "given": "J." } }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Huynh-Minh-T", "name": { "family": "Huynh", "given": "M." } }, { "id": "Lacy-M", "name": { "family": "Lacy", "given": "M." }, "orcid": "0000-0002-3032-1783" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E." }, "orcid": "0000-0001-7089-7325" }, { "id": "Noriega-Crespo-A", "name": { "family": "Noriega-Crespo", "given": "A." }, "orcid": "0000-0002-6296-8960" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Shenoy-S-S", "name": { "family": "Shenoy", "given": "S." } } ] }, "title": "Far-infrared Properties of Type 1 Quasars", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; infrared: galaxies; quasars: general; surveys", "note": "\u00a9 2013 American Astronomical Society. Received 2012 October 5; accepted 2013 March 2; published 2013 April 9. Support for this work was provided by NASA through contract\nNASA-ADAP NNX10AD52G. This publication makes use of (1) raw data from the Spitzer Space Telescope, operated by the Jet Propulsion Laboratory/California Institute of Technology under NASA contract, (2) data products from the Two Micron All Sky Survey, a joint project of the University of Massachusetts and the Infrared Processing and Analysis\nCenter/California Institute of Technology, funded by NASA\nand the NSF, and (3) the SDSS, managed by the Astrophysical\nResearch Consortium for the Participating Institutions and\nfunded by the Alfred P. Sloan Foundation, the Participating\nInstitutions, and many others.\n\nPublished - 0004-637X_768_1_13.pdf
", "abstract": "We use the Spitzer Space Telescope Enhanced Imaging Products and the Spitzer Archival Far-InfraRed Extragalactic Survey to study the spectral energy distributions (SEDs) of spectroscopically confirmed type 1 quasars selected from the Sloan Digital Sky Survey (SDSS). By combining the Spitzer and SDSS data with the Two Micron All Sky Survey, we are able to construct a statistically robust rest-frame 0.1-100 \u03bcm type 1 quasar template. We find that the quasar population is well-described by a single power-law SED at wavelengths less than 20 \u03bcm, in good agreement with previous work. However, at longer wavelengths, we find a significant excess in infrared luminosity above an extrapolated power-law, along with significant object-to-object dispersion in the SED. The mean excess reaches a maximum of 0.8 dex at rest-frame wavelengths near 100 \u03bcm.", "date": "2013-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "768", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 13", "id_number": "CaltechAUTHORS:20130603-102636844", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130603-102636844", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX10AD52G" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "SAFIRES Team" ] }, "doi": "10.1088/0004-637X/768/1/13", "primary_object": { "basename": "0004-637X_768_1_13.pdf", "url": "https://authors.library.caltech.edu/records/qh39q-sfk60/files/0004-637X_768_1_13.pdf" }, "pub_year": "2013", "author_list": "Hanish, D. J.; Teplitz, H. I.; et el." }, { "id": "https://authors.library.caltech.edu/records/bb0jf-avy18", "eprint_id": 38954, "eprint_status": "archive", "datestamp": "2023-08-22 09:13:53", "lastmod": "2023-10-24 14:53:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Benson-A-J", "name": { "family": "Benson", "given": "A." }, "orcid": "0000-0001-5501-6008" }, { "id": "Fu-Hai", "name": { "family": "Fu", "given": "Hai" }, "orcid": "0000-0001-9608-6395" }, { "id": "Manohar-S", "name": { "family": "Manohar", "given": "S." } }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P. L." } }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" } ] }, "title": "Evolution of Galaxies and Their Environments at z = 0.1-3 in COSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; large-scale structure of universe", "note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2012 November 5; accepted 2013 March 26; published 2013 April 18. \n\nBased on observations with the NASA/ESA Hubble Space Telescope,\nobtained at the Space Telescope Science Institute, which is operated by AURA Inc., under NASA contract NAS 5-26555, and the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407; also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory under Large Program 175.A-01279, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; and the Canada\u2013France\u2013Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the NRC and CADC of Canada, the CNRS of France, TERAPIX, and the University of Hawaii. \n\nWe thank the referee for helpful suggestions that have very much improved this work and we thank Zara Scoville for proofreading of the manuscript. Support for this work was provided by NASA through Contract Number 12712786 issued by JPL. Additional information on the COSMOS survey is available from the main COSMOS Web site at http://www.astro.caltech.edu/cosmos. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff in providing online archive and server capabilities for the COSMOS data sets. The environmental densities and mpeg versions with all 127 redshift slices of the maps shown in Figures 6\u20138 will be available in FITS format from the NASA IPAC/IRSA archive at http://irsa.ipac.caltech.edu/data/COSMOS/. K.S. acknowledges support from the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. G.Q. acknowledges support from the National basic research program of China (program 973 under grant No. 2009CB24901), the Young Researcher Grant of National Astronomical Observatories, CAS, the NSFC grants program (No. 11143005), and the Partner Group program of the Max Planck Society. \n\nFacilities: HST (ACS), Subaru (SCAM), Spitzer (IRAC).\n\nPublished - 0067-0049_206_1_3.pdf
Submitted - 1303.6689.pdf
", "abstract": "Large-scale structures (LSSs) out to z < 3.0 are measured in the Cosmic Evolution Survey (COSMOS) using extremely accurate photometric redshifts (photoz). The K_s -band-selected sample (from Ultra-Vista) is comprised of 155,954 galaxies. Two techniques\u2014adaptive smoothing and Voronoi tessellation\u2014are used to estimate the environmental densities within 127 redshift slices. Approximately 250 statistically significant overdense structures are identified out to z = 3.0 with shapes varying from elongated filamentary structures to more circularly symmetric concentrations. We also compare the densities derived for COSMOS with those based on semi-analytic predictions for a \u039bCDM simulation and find excellent overall agreement between the mean densities as a function of redshift and the range of densities. The galaxy properties (stellar mass, spectral energy distributions (SEDs), and star formation rates (SFRs)) are strongly correlated with environmental density and redshift, particularly at z < 1.0-1.2. Classifying the spectral type of each galaxy using the rest-frame b \u2013 i color (from the photoz SED fitting), we find a strong correlation of early-type galaxies (E-Sa) with high-density environments, while the degree of environmental segregation varies systematically with redshift out to z ~ 1.3. In the highest density regions, 80% of the galaxies are early types at z = 0.2 compared to only 20% at z = 1.5. The SFRs and the star formation timescales exhibit clear environmental correlations. At z > 0.8, the SFR density is uniformly distributed over all environmental density percentiles, while at lower redshifts the dominant contribution is shifted to galaxies in lower density environments.", "date": "2013-05", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "206", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 3", "id_number": "CaltechAUTHORS:20130617-084030038", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130617-084030038", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL", "grant_number": "12712786" }, { "agency": "National Radio Astronomy Observatory" }, { "agency": "NSF" }, { "agency": "National Key Basic Research Program of China", "grant_number": "2009CB24901" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Chinese Academy of Sciences" }, { "agency": "National Science Foundation of China", "grant_number": "11143005" }, { "agency": "Max Planck Society" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0067-0049/206/1/3", "primary_object": { "basename": "0067-0049_206_1_3.pdf", "url": "https://authors.library.caltech.edu/records/bb0jf-avy18/files/0067-0049_206_1_3.pdf" }, "related_objects": [ { "basename": "1303.6689.pdf", "url": "https://authors.library.caltech.edu/records/bb0jf-avy18/files/1303.6689.pdf" } ], "pub_year": "2013", "author_list": "Scoville, N.; Benson, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/gk8bq-jtb18", "eprint_id": 39619, "eprint_status": "archive", "datestamp": "2023-08-19 19:07:57", "lastmod": "2023-10-24 17:00:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Norris-R-P", "name": { "family": "Norris", "given": "Ray P." }, "orcid": "0000-0002-4597-1906" }, { "id": "Raccanelli-A", "name": { "family": "Raccanelli", "given": "A." } } ] }, "title": "Radio Continuum Surveys with Square Kilometre Array Pathfinders", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2013 Astronomical Society of Australia 2013; published by Cambridge University Press.\n\nReceived June 17, 2012; Accepted October 22, 2012; Online Publication March 27, 2013.\n\nWe are indebted to the Lorentz Center in Leiden for hosting\nand funding the workshop in 2011 February, which gave rise to this paper. Parts of this research were supported by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. JA gratefully acknowledges support from the Science and Technology Foundation (FCT, Portugal) through the research grants PTDC/FIS/100170/2008, PTDC/CTEAST/105287/2008, and PEst-OE/FIS/UI2751/2011. CF and AD acknowledge financial support by the Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. AD acknowledges financial support from the joint PhD program of Observatoire de la C\u00f4te d'Azur and Conseil r\u00e9gional Provence-Alpes-C\u00f4te d'Azur.\n\nSubmitted - 1210.7521v1.pdf
", "abstract": "In the lead-up to the Square Kilometre Array (SKA) project, several next-generation radio telescopes and upgrades are already being built around the world. These include APERTIF (The Netherlands), ASKAP (Australia), e-MERLIN (UK), VLA (USA), e-EVN (based in Europe), LOFAR (The Netherlands), MeerKAT (South Africa), and the Murchison Widefield Array. Each of these new instruments has different strengths, and coordination of surveys between them can help maximise the science from each of them. A radio continuum survey is being planned on each of them with the primary science objective of understanding the formation and evolution of galaxies over cosmic time, and the cosmological parameters and large-scale structures which drive it. In pursuit of this objective, the different teams are developing a variety of new techniques, and refining existing ones. To achieve these exciting scientific goals, many technical challenges must be addressed by the survey instruments. Given the limited resources of the global radio-astronomical community, it is essential that we pool our skills and knowledge. We do not have sufficient resources to enjoy the luxury of re-inventing wheels. We face significant challenges in calibration, imaging, source extraction and measurement, classification and cross-identification, redshift determination, stacking, and data-intensive research. As these instruments extend the observational parameters, we will face further unexpected challenges in calibration, imaging, and interpretation. If we are to realise the full scientific potential of these expensive instruments, it is essential that we devote enough resources and careful study to understanding the instrumental effects and how they will affect the data. We have established an SKA Radio Continuum Survey working group, whose prime role is to maximise science from these instruments by ensuring we share resources and expertise across the projects. Here we describe these projects, their science goals, and the technical challenges which are being addressed to maximise the science return.", "date": "2013-03-27", "date_type": "published", "publication": "Publications of the Astronomical Society of Australia", "volume": "30", "publisher": "Cambridge University Press", "pagerange": "Art. No. e020", "id_number": "CaltechAUTHORS:20130729-100331768", "issn": "1323-3580", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130729-100331768", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council", "grant_number": "CE110001020" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "PTDC/FIS/100170/2008" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "PTDC/CTE-AST/105287/2008" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "PEst-OE/FIS/UI2751/2011" }, { "agency": "Agence Nationale de la Recherche (ANR)", "grant_number": "ANR-09-JCJC-0001-01" }, { "agency": "Observatoire de la C\u00f4te d'Azur" }, { "agency": "Conseil r\u00e9gional Provence-Alpes-C\u00f4te d'Azur" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1017/pas.2012.020", "primary_object": { "basename": "1210.7521v1.pdf", "url": "https://authors.library.caltech.edu/records/gk8bq-jtb18/files/1210.7521v1.pdf" }, "pub_year": "2013", "author_list": "Norris, Ray P. and Raccanelli, A." }, { "id": "https://authors.library.caltech.edu/records/h7xgg-91v51", "eprint_id": 38924, "eprint_status": "archive", "datestamp": "2023-08-22 08:54:20", "lastmod": "2023-10-24 14:52:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hildebrandt-H", "name": { "family": "Hildebrandt", "given": "H." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } } ] }, "title": "Inferring the mass of submillimetre galaxies by exploiting\n their gravitational magnification of background galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: weak; galaxies: high-redshift; submillimetre: galaxies", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2012 December 6. Received 2012 November 26; in original form 2012 November 11.\n\nFirst published online: January 7, 2013.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\nSPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK) and Caltech/JPL, IPAC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA). This research has made use of data from the HerMES project (http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists and a mission scientist. The HerMES data were accessed through the HeDaM data base (http://hedam.oamp.fr) operated by CeSAM and hosted by the Laboratoire d'Astrophysique de Marseille. The optical data are based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada\u2013France\u2013Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre, as part of the Canada\u2013France\u2013Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. HH is supported by the Marie Curie IOF 252760, a CITA National Fellowship and the DFG grant Hi 1495/2-1. LvW is supported by NSERC and CIfAR. DS acknowledges support by NSERC and CSA. TE is supported by the Deutsche Forschungsgemeinschaft through project ER 327/3-1 and the Transregional Collaborative Research Centre TR 33 \u2013 'The Dark Universe'. RFJvdB acknowledges support from the Netherlands Organisation for Scientic Research grant number 639.042.814.\nAuthor Contributions: HH led the analysis and wrote the draft version of the paper. LvW and DS contributed significantly in the development of this project through ideas and discussions on a daily basis. MB provided the redshift distribution of the submillimetre galaxies. TE led the optical data reduction and calibration. RFJvdB\nprovided the luminosity function estimate of the background galaxies. All other co-authors contributed extensively and equally by their varied contributions to the SPIRE instrument, the Herschelmission, analysis of SPIRE and HerMES data, planning of HerMES observations and scientific support of HerMES and by commenting on this manuscript as part of an internal review process.\n\nPublished - MNRAS-2013-Hildebrandt-3230-7.pdf
", "abstract": "Dust emission at submillimetre wavelengths allows us to trace the early phases of star formation in the Universe. In order to understand the physical processes involved in this mode of star formation, it is essential to gain knowledge about the dark matter structures \u2013 most importantly their masses \u2013 that submillimetre galaxies live in. Here we use the magnification effect of gravitational lensing to determine the average mass and dust content of submillimetre galaxies with 250\u2009\u03bcm flux densities of S_250 > 15\u2009mJy selected using data from the Herschel Multi-tiered Extragalactic Survey. The positions of hundreds of submillimetre foreground lenses are cross-correlated with the positions of background Lyman-break galaxies at z \u223c 3\u20135 selected using optical data from the Canada\u2013France\u2013Hawaii Telescope Legacy Survey. We detect a cross-correlation signal at the 7\u03c3 level over a sky area of 1\u2009deg^2, with \u223c80 per cent of this signal being due to magnification, whereas the remaining \u223c20 per cent comes from dust extinction. Adopting some simple assumptions for the dark matter and dust profiles and the redshift distribution enables us to estimate the average mass of the haloes hosting the submillimetre galaxies to be log\u2009_(10)[M_200/M_\u2299] = \n13.17^(+0.05)_(\u22120.08)(stat.) and their average dust mass fraction (at radii of >10\u2009kpc) to be M_dust/M_200 \u2248 6 \u00d7 10^(\u22125). This supports the picture that submillimetre galaxies are dusty, forming stars at a high rate, reside in massive group-sized haloes and are a crucial phase in the assembly and evolution of structure in the Universe.", "date": "2013-03-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "429", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3230-3237", "id_number": "CaltechAUTHORS:20130612-134247579", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130612-134247579", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Marie Curie Fellowship", "grant_number": "252760" }, { "agency": "CITA National Fellowship" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "Hi 1495/2-1" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "ER 327/3-1" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "TR 33" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "639.042.814" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/sts585", "primary_object": { "basename": "MNRAS-2013-Hildebrandt-3230-7.pdf", "url": "https://authors.library.caltech.edu/records/h7xgg-91v51/files/MNRAS-2013-Hildebrandt-3230-7.pdf" }, "pub_year": "2013", "author_list": "Hildebrandt, H.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/r9fen-4fm84", "eprint_id": 38310, "eprint_status": "archive", "datestamp": "2023-08-22 08:48:20", "lastmod": "2023-10-23 20:02:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Berta-S", "name": { "family": "Berta", "given": "S." }, "orcid": "0000-0002-0320-1532" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } } ] }, "title": "Panchromatic spectral energy distributions of Herschel sources", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: galaxies; galaxies: statistics; galaxies: star formation; galaxies: active; galaxies: evolution", "note": "\u00a9 2013 ESO. \nArticle published by EDP Sciences.\nReceived 6 December 2012. Accepted 16 January 2013. Published online 01 March 2013. \nHerschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia and with important\nparticipation from NASA.\n\nThe authors wish to thank Dr. Jacopo Fritz for providing his library of AGN torus emission models, and the anonymous referee for her/his useful comments. This work made use of the code FastEM, distributed by the Auton Lab, and developed by Andrew Moore, Paul Hsiung, Peter Sand, point of contact Saswati Ray. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM(France); MPIA (Germany); INAFIFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada), NAOC (PR China), CEA, LAM (France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK), Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (PR China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA).\n\nPublished - aa20859-12.pdf
", "abstract": "Combining far-infrared Herschel photometry from the PACS Evolutionary Probe (PEP) and Herschel Multi-tiered Extragalactic Survey (HerMES) guaranteed time programs with ancillary datasets in the GOODS-N, GOODS-S, and COSMOS fields, it is possible to sample the 8\u2013500\u2009\u03bcm spectral energy distributions (SEDs) of galaxies with at least 7\u201310 bands. Extending to the UV, optical, and near-infrared, the number of bands increases up to 43. We reproduce the distribution of galaxies in a carefully selected restframe ten colors space, based on this rich data-set, using a superposition of multivariate Gaussian modes. We use this model to classify galaxies and build median SEDs of each class, which are then fitted with a modified version of the magphys code that combines stellar light, emission from dust heated by stars and a possible warm dust contribution heated by an active galactic nucleus (AGN). The color distribution of galaxies in each of the considered fields can be well described with the combination of 6\u20139 classes, spanning a large range of far- to near-infrared luminosity ratios, as well as different strength of the AGN contribution to bolometric luminosities. The defined Gaussian grouping is used to identify rare or odd sources. The zoology of outliers includes Herschel-detected ellipticals, very blue z ~ 1 Ly-break galaxies, quiescent spirals, and torus-dominated AGN with star formation. Out of these groups and outliers, a new template library is assembled, consisting of 32 SEDs describing the intrinsic scatter in the restframe UV-to-submm colors of infrared galaxies. This library is tested against L(IR) estimates with and without Herschel data included, and compared to eightother popular methods often adopted in the literature. When implementing Herschel photometry, these approaches produce L(IR) values consistent with each other within a median absolute deviation of 10\u201320%, the scatter being dominated more by fine tuning of the codes, rather than by the choice of SED templates. Finally, the library is used to classify 24 \u03bcm detected sources in PEP GOODS fields on the basis of AGN content, L(60)/L(100) color and L(160)/L(1.6) luminosity ratio. AGN appear to be distributed in the stellar mass (M_\u2217) vs. star formation rate (SFR) space along with all other galaxies, regardless of the amount of infrared luminosity they are powering, with the tendency to lie on the high SFR side of the \"main sequence\". The incidence of warmer star-forming sources grows for objects with higher specific star formation rates (sSFR), and they tend to populate the \"off-sequence\" region of the M_\u2217 \u2212 SFR \u2212 z space.", "date": "2013-03", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "551", "publisher": "EDP Sciences", "pagerange": "Art. No. A100", "id_number": "CaltechAUTHORS:20130507-082520582", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130507-082520582", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "BMVIT (Austria)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "DLR (Germany)" }, { "agency": "CICYT/MCYT (Spain)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "MCINN (Spain)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201220859", "primary_object": { "basename": "aa20859-12.pdf", "url": "https://authors.library.caltech.edu/records/r9fen-4fm84/files/aa20859-12.pdf" }, "pub_year": "2013", "author_list": "Berta, S. and Viero, M." }, { "id": "https://authors.library.caltech.edu/records/5gfna-hmx87", "eprint_id": 39527, "eprint_status": "archive", "datestamp": "2023-08-22 08:19:11", "lastmod": "2023-10-24 16:54:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sobral-D", "name": { "family": "Sobral", "given": "David" }, "orcid": "0000-0001-8823-4845" }, { "id": "Smail-I", "name": { "family": "Smail", "given": "Ian" }, "orcid": "0000-0003-3037-257X" }, { "id": "Best-P-N", "name": { "family": "Best", "given": "Philip N." } }, { "id": "Geach-J-E", "name": { "family": "Geach", "given": "James E." }, "orcid": "0000-0003-4964-4635" }, { "id": "Matsuda-Yuichi", "name": { "family": "Matsuda", "given": "Yuichi" } }, { "id": "Stott-J-P", "name": { "family": "Stott", "given": "John P." } }, { "id": "Cirasuolo-M", "name": { "family": "Cirasuolo", "given": "Michele" } }, { "id": "Kurk-J", "name": { "family": "Kurk", "given": "Jaron" } } ] }, "title": "A large H\u03b1 survey at z = 2.23, 1.47, 0.84 and 0.40: the 11 Gyr evolution of star-forming galaxies from HiZELS", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: luminosity function, mass function; cosmology: observations", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2012 September 27. Received 2012 September 27; in original form 2012 February 15. First published online: November 7, 2012. \n\nThis work is based on observations obtained using the Wide Field CAMera (WFCAM) on the 3.8-m United Kingdom Infrared Telescope (UKIRT), as part of the High-redshift(Z) Emission Line Survey (HiZELS; U/CMP/3 and U/10B/07). It also relies on observations conducted with HAWK-I on the ESO Very Large Telescope (VLT), programme 086.7878.A, and observations obtained with Suprime-Cam on the Subaru Telescope (S10B-144S). \n\nThe authors would like to thank the reviewer, James Colbert, for many comments and suggestions which improved the paper significantly. DS is supported by a NOVA fellowship. IS acknowledges a Leverhulme Senior Fellowship. PNB acknowledges support from the Leverhulme Trust. YM, JPS and IS thank the UK Science and Technology Facility Council (STFC). JEG is supported by a Banting Fellowship, administered by the Natural Science and Engineering\nResearch Council of Canada. We would like to thank Richard Ellis, Simon Lilly, Peter Capak, Adam Muzzin, Taddy Kodama, Masao Hayashi, Andy Lawrence, Joop Schaye,Marijn Franx, Huub R\u00f6ttgering, Rychard Bouwens and Renske Smit for many interesting and helpful discussions. We would also like to thank Chun Ly for helpful comments. The authors wish to thank all the JAC staff for their help in conducting the observations at the UKIRT telescope and their continuous support, and we are also extremely grateful to all the Subaru staff. We also acknowledge ESO and Subaru for service observations. Finally, the authors fully acknowledge the tremendous work that has been done by both COSMOS and UKIDSS UDS/SXDF teams in assembling such large, state-of-the-art multiwavelength data sets over such wide areas, as those have been crucial for the results presented in this paper.\n\nPublished - MNRAS-2013-Sobral-1128-46.pdf
Supplemental Material - NB_CATALOGUES_S13.zip
", "abstract": "This paper presents new deep and wide narrow-band surveys undertaken with United Kingdom Infrared Telescope (UKIRT), Subaru and the Very Large Telescope (VLT), a unique combined effort to select large, robust samples of H\u03b1 star-forming galaxies at z = 0.40, 0.84, 1.47 and 2.23 (corresponding to look-back times of 4.2, 7.0, 9.2 and 10.6\u2009Gyr) in a uniform manner over \u223c2\u2009deg^2 in the Cosmological Evolution Survey and Ultra Deep Survey fields. The deep multi-epoch H\u03b1 surveys reach a matched 3\u03c3 flux limit of \u22483\u2009M_\u2299\u2009yr^(\u22121) out to z = 2.2 for the first time, while the wide area and the coverage over two independent fields allow us to greatly overcome cosmic variance and assemble by far the largest samples of H\u03b1 emitters. Catalogues are presented for a total of 1742, 637, 515 and 807 H\u03b1 emitters, robustly selected at z = 0.40, 0.84, 1.47 and 2.23, respectively, and used to determine the H\u03b1 luminosity function and its evolution. The faint-end slope of the H\u03b1 luminosity function is found to be \u03b1 = \u22121.60 \u00b1 0.08 over z = 0\u20132.23, showing no significant evolution. The characteristic luminosity of star-forming galaxies, L*_H\u03b1, evolves significantly as log\u2009\u2009L*_H\u03b1(z) = 0.45z + log\u2009\u2009L*_z = 0. This is the first time H\u03b1 has been used to trace star formation activity with a single homogeneous survey at z = 0.4\u20132.23. Overall, the evolution seen with H\u03b1 is in good agreement with the evolution seen using inhomogeneous compilations of other tracers of star formation, such as far-infrared and ultraviolet, jointly pointing towards the bulk of the evolution in the last 11\u2009Gyr being driven by a statistically similar star-forming population across cosmic time, but with a strong luminosity increase from z \u223c 0 to \u223c2.2. Our uniform analysis allows us to derive the H\u03b1 star formation history (SFRH) of the Universe, showing a clear rise up to z \u223c 2.2, for which the simple parametrization log_10\u03c1SFR = \u22122.1(1 + z)^(\u22121) is valid over 80\u2009per cent of the age of the Universe. The results reveal that both the shape and normalization of the H\u03b1 SFRH are consistent with the measurements of the stellar mass density growth, confirming that our H\u03b1 SFRH is tracing the bulk of the formation of stars in the Universe for z < 2.23. The star formation activity over the last \u223c11\u2009Gyr is responsible for producing \u223c95\u2009per cent of the total stellar mass density observed locally, with half of that being assembled in 2\u2009Gyr between z = 1.2 and 2.2, and the other half in 8\u2009Gyr (since z < 1.2). If the star formation rate density continues to decline with time in the same way as seen in the past \u223c11\u2009Gyr, then the stellar mass density of the Universe will reach a maximum which is only 5\u2009per cent higher than the present-day value.", "date": "2013-01-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "428", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1128-1146", "id_number": "CaltechAUTHORS:20130723-114603121", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130723-114603121", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Nederlandse Onderzoekschool Voor Astronomie (NOVA)" }, { "agency": "Leverhulme Trust" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/sts096", "primary_object": { "basename": "MNRAS-2013-Sobral-1128-46.pdf", "url": "https://authors.library.caltech.edu/records/5gfna-hmx87/files/MNRAS-2013-Sobral-1128-46.pdf" }, "related_objects": [ { "basename": "NB_CATALOGUES_S13.zip", "url": "https://authors.library.caltech.edu/records/5gfna-hmx87/files/NB_CATALOGUES_S13.zip" } ], "pub_year": "2013", "author_list": "Sobral, David; Smail, Ian; et el." }, { "id": "https://authors.library.caltech.edu/records/4xnkm-5f241", "eprint_id": 36334, "eprint_status": "archive", "datestamp": "2023-08-22 07:58:09", "lastmod": "2023-10-20 23:01:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Casey-C-M", "name": { "family": "Casey", "given": "C. M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } } ] }, "title": "A Redshift Survey of Herschel Far-infrared Selected Starbursts and Implications for Obscured Star Formation", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimeter: galaxies", "note": "\u00a9 2012 American Astronomical Society. Received 2012 July 26; accepted 2012 October 15; published 2012 December 4. We thank the anonymous reviewer for a very useful, constructive\nreport that improved the manuscript. C.M.C. is generously\nsupported by a Hubble Fellowship from Space Telescope Science Institute, grant HST-HF-51268.01-A. The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge\nthe very significant cultural role and reverence that\nthe summit of Mauna Kea has always had within the indigenous\nHawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This work would not be possible without the hard work and dedication of the Keck Observatory night and day staff; special thanks to Marc Kassis, Luca Rizzi and Greg Wirth for help and advice while observing. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. Thanks to Nick Scoville and Brian Siana for useful discussions which improved the paper. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).\nThis research has made use of data from the HerMES project\n(http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists and a mission scientist. HerMES is described in Oliver et al. (2012). The SPIRE data presented in this paper will be released through the HerMES Database in Marseille, HeDaM (http://hedam.oamp.fr/HerMES).\n\nPublished - 0004-637X_761_2_140.pdf
", "abstract": "We present Keck spectroscopic observations and redshifts for a sample of 767 Herschel-SPIRE selected galaxies (HSGs) at 250, 350, and 500 \u03bcm, taken with the Keck I Low Resolution Imaging Spectrometer and the Keck II DEep Imaging Multi-Object Spectrograph. The redshift distribution of these SPIRE sources from the Herschel Multitiered Extragalactic Survey peaks at z = 0.85, with 731 sources at z < 2 and a tail of sources out to z ~ 5. We measure more significant disagreement between photometric and spectroscopic redshifts (\u3008\u0394z/(1 + z_(spec))\u3009 = 0.29) than is seen in non-infrared selected samples, likely due to enhanced star formation rates and dust obscuration in infrared-selected galaxies. The infrared data are used to directly measure integrated infrared luminosities and dust temperatures independent of radio or 24 \u03bcm flux densities. By probing the dust spectral energy distribution (SED) at its peak, we estimate that the vast majority (72%-83%) of z < 2 Herschel-selected galaxies would drop out of traditional submillimeter surveys at 0.85-1 mm. We find that dust temperature traces infrared luminosity, due in part to the SPIRE wavelength selection biases, and partially from physical effects. As a result, we measure no significant trend in SPIRE color with redshift; if dust temperature were independent of luminosity or redshift, a trend in SPIRE color would be expected. Composite infrared SEDs are constructed as a function of infrared luminosity, showing the increase in dust temperature with luminosity, and subtle change in near-infrared and mid-infrared spectral properties. Moderate evolution in the far-infrared (FIR)/radio correlation is measured for this partially radio-selected sample, with q_(IR) \u221d(1 + z)^(\u20130.30\u00b10.02) at z < 2. We estimate the luminosity function and implied star formation rate density contribution of HSGs at z < 1.6 and find overall agreement with work based on 24 \u03bcm extrapolations of the LIRG, ULIRG, and total infrared contributions. This work significantly increased the number of spectroscopically confirmed infrared-luminous galaxies at z \u00bb 0 and demonstrates the growing importance of dusty starbursts for galaxy evolution studies and the build-up of stellar mass throughout cosmic time.", "date": "2012-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "761", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 140", "id_number": "CaltechAUTHORS:20130111-152856336", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130111-152856336", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51268.01-A" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/761/2/140", "primary_object": { "basename": "0004-637X_761_2_140.pdf", "url": "https://authors.library.caltech.edu/records/4xnkm-5f241/files/0004-637X_761_2_140.pdf" }, "pub_year": "2012", "author_list": "Casey, C. M.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/d4f09-dv665", "eprint_id": 36061, "eprint_status": "archive", "datestamp": "2023-08-22 07:53:15", "lastmod": "2023-10-20 22:11:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mallery-R-P", "name": { "family": "Mallery", "given": "Ryan P." } }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Kakazu-Yuko", "name": { "family": "Kakazu", "given": "Yuko" } }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "Dan" }, "orcid": "0000-0001-5382-6138" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Hemmati-S", "name": { "family": "Hemmati", "given": "Shoubaneh" }, "orcid": "0000-0003-2226-5395" }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "Claudia" }, "orcid": "0000-0002-9136-8876" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "Henry" }, "orcid": "0000-0002-9489-7765" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "Olivier" }, "orcid": "0000-0001-5891-2596" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Ly\u03b1 Emission from High-redshift Sources in COSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: ISM", "note": "\u00a9 2012 American Astronomical Society. Received 2011 August 30; accepted 2012 August 24; published 2012 November 16. Based in part on data obtained at the W. M. Keck Observatory,\nwhich is operated as a scientific partnership among the\nCalifornia Institute of Technology, the University of California, and NASA and was made possible by the generous financial support of the W. M. Keck Foundation.\n\nPublished - 0004-637X_760_2_128.pdf
", "abstract": "We investigate spectroscopically measured Ly\u03b1 equivalent widths (EWs) and escape fractions of 244 sources of which 95 are Lyman break galaxies (LBGs) and 106 Lyman alpha emitters (LAEs) at z ~ 4.2, z ~ 4.8, and z ~ 5.6 selected from intermediate and narrowband observations. The sources were selected from the Cosmic Evolution Survey and observed with the DEIMOS spectrograph. We find that the distribution of EWs shows no evolution with redshift for both the LBG selected sources and the intermediate/narrowband LAEs. We also find that the Ly\u03b1 escape fraction of intermediate/narrowband LAEs is on average higher and has a larger variation than the escape fraction of LBG selected sources. The escape fraction does not show a dependence with redshift. Similar to what has been found for LAEs at low redshifts, the sources with the highest extinctions show the lowest escape fractions. The range of escape fractions increases with decreasing extinction. This is evidence that the dust extinction is the most important factor affecting the escape of Ly\u03b1 photons, but at low extinctions other factors, such as the H I covering fraction and gas kinematics, can be just as effective at inhibiting the escape of Ly\u03b1 photons.", "date": "2012-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "760", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 128", "id_number": "CaltechAUTHORS:20121219-153314783", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121219-153314783", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/760/2/128", "primary_object": { "basename": "0004-637X_760_2_128.pdf", "url": "https://authors.library.caltech.edu/records/d4f09-dv665/files/0004-637X_760_2_128.pdf" }, "pub_year": "2012", "author_list": "Mallery, Ryan P.; Mobasher, Bahram; et el." }, { "id": "https://authors.library.caltech.edu/records/k6k39-8yg42", "eprint_id": 36397, "eprint_status": "archive", "datestamp": "2023-08-19 13:37:59", "lastmod": "2023-10-20 23:06:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" }, { "id": "Navarrete-F", "name": { "family": "Navarrete", "given": "F." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D. A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Feruglio-C", "name": { "family": "Feruglio", "given": "C." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M." }, "orcid": "0000-0003-1033-9684" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Albrecht-M", "name": { "family": "Albrecht", "given": "M." } }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "N." } }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" } ] }, "title": "Millimeter imaging of submillimeter galaxies in the COSMOS field: redshift distribution", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys galaxies: starburst galaxies: fundamental parameters galaxies: high-redshift galaxies: statistics\nsubmillimeter: galaxies", "note": "\u00a9 2012 ESO. Received 8 April 2012. Accepted 24 May 2012. Published online 13 November 2012. \nBased on observations carried out with the IRAM Plateau de Bure\nInterferometer. IRAM is supported by INSU/CNRS (France), MPG\n(Germany) and IGN (Spain).\n\nWe thank the anonymous referee for helpful comments on the manuscript. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. The research leading to these results has received funding from the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement\nNo. 229517 and through the DFG-SFB 956 and the DFG Priority Program 1573. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nPublished - aa19368-12.pdf
", "abstract": "We present new IRAM Plateau de Bure interferometer (PdBI) 1.3\u2009mm continuum observations at ~1.5\" resolution of 28 submillimeter galaxies (SMGs), previously discovered with the 870 \u03bcm bolometer LABOCA at the APEX telescope from the central 0.7\u2009deg^2 of the COSMOS field. Nineteen out of the 28 LABOCA sources were detected with PdBI at a \u22733\u03c3 level of \u22481.4 mJy/beam. A combined analysis of this new sample with existing interferometrically identified SMGs in the COSMOS field yields the following results: i) \u227315%, and possibly up to ~40% of single-dish detected SMGs consist of multiple sources; ii) statistical analysis of multi-wavelength counterparts to single-dish SMGs shows that only ~50% have real radio or IR counterparts; iii) ~18% of interferometric SMGs have either no multi-wavelength counterpart or only a radio-counterpart; and iv) ~50\u201370% of z \u2273 3 SMGs have no radio counterparts (down to an rms of 7\u201312 \u03bcJy at 1.4 GHz). Using the exactinterferometric positions to identify the multi-wavelength counterparts allows us to determine accurate photometric redshifts for these sources. The redshift distributions of the combined and the individual 1.1 mm and 870\u2009\u03bcm selected samples shows a higher mean and a broader width than those derived in previous studies. This study finds that on average brighter and/or mm- selected SMGs are located at higher redshifts, consistent with previous studies. The mean redshift for the 1.1 mm selected sample (z = 3.1 \u00b1 0.4) is tentatively higher than that for the 870 \u03bcm selected sample ( = 2.6 \u00b1 0.4). Based on our nearly complete sample of AzTEC 1.1 mm SMGs in a 0.15 deg^2 area, we infer a higher surface density of z \u2273 4 SMGs than predicted by current cosmological models. In summary, our findings imply that interferometric identifications at (sub-)millimeter wavelengths are crucial to build statistically complete and unbiased samples of SMGs.", "date": "2012-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "548", "publisher": "EDP Sciences", "pagerange": "Art. No. A4", "id_number": "CaltechAUTHORS:20130115-134253660", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130115-134253660", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "229517" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "SFB 956" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "Priority Program 1573" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201219368", "primary_object": { "basename": "aa19368-12.pdf", "url": "https://authors.library.caltech.edu/records/k6k39-8yg42/files/aa19368-12.pdf" }, "pub_year": "2012", "author_list": "Smol\u010di\u0107, V.; Aravena, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/vc4sk-qfw98", "eprint_id": 36401, "eprint_status": "archive", "datestamp": "2023-08-19 13:38:05", "lastmod": "2023-10-20 23:07:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "L\u00f3pez-Sanjuan-C", "name": { "family": "L\u00f3pez-Sanjuan", "given": "C." } }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "C." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" } ] }, "title": "The dominant role of mergers in the size evolution of massive\n early-type galaxies since z \u223c 1", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: elliptical and lenticular, cD galaxies: evolution galaxies: interactions", "note": "\u00a9 2012 ESO. Received 21 February 2012. Accepted 26 August 2012. Published online 12 November 2012. \nBased on observations made at the European Southern Observatory\n(ESO) Very Large Telescope (VLT) under Large Program 175.A-0839.\n\nWe dedicate this paper to the memory of our six IAC colleagues\nand friends who met with a fatal accident in Piedra de los Cochinos, Tenerife, in February 2007, with a special thanks to Maurizio Panniello, whose teachings of python were so important for this paper. We thank the comments and suggestions of the anonymous referee. We also thank Ignacio Trujillo, Fernando Buitrago, Carmen Eliche-Moral, Paolo Cassata, Jairo M\u00e9ndez-Abreu,\nDavid Patton, Sara Ellison, Trevor Mendel, and Jorge Moreno for useful discussions. This work is supported by funding from ANR-07-BLAN-0228 and ERC-2010-AdG-268107-EARLY.\n\nPublished - aa19085-12.pdf
", "abstract": "Aims. The role of galaxy mergers in massive galaxy evolution, and in particular to mass assembly and size growth, remains an open question. In this paper we measure the merger fraction and rate, both minor and major, of massive early-type galaxies (M_\u22c6 \u2265 10^(11) M_\u2299) in the COSMOS field, and study their role in mass and size evolution.\nMethods. We used the 30-band photometric catalogue in COSMOS, complemented with the spectroscopy of the zCOSMOS survey, to define close pairs with a separation on the sky plane 10 h^(-1) kpc \u2264 r_p \u2264 30 h^(-1) kpc and a relative velocity \u0394v \u2264 500 km s^(-1) in redshift space. We measured both major (stellar mass ratio \u03bc \u2261 M_(\u22c6,2)/M_(\u22c6,1) \u2265 1/4) and minor (1/10 \u2264 \u03bc < 1/4) merger fractions of massive galaxies, and studied their dependence on redshift and on morphology (early types vs. late types).\nResults. The merger fraction and rate of massive galaxies evolves as a power-law (1 + z)^n, with major mergers increasing with redshift, n_(MM) = 1.4, and minor mergers showing little evolution, n_(mm) ~ 0. When split by their morphology, the minor merger fraction for early-type galaxies (ETGs) is higher by a factor of three than that for late-type galaxies (LTGs), and both are nearly constant with redshift. The fraction of major mergers for massive LTGs evolves faster (n_(MM)^(LT) ~ 4 ) than for ETGs (n_(MM)^(ET)= 1.8).\nConclusions. Our results show that massive ETGs have undergone 0.89 mergers (0.43 major and 0.46 minor) since z ~ 1, leading to a mass growth of ~30%. We find that \u03bc \u2265 1/10 mergers can explain ~55% of the observed size evolution of these galaxies since z ~ 1. Another ~20% is due to the progenitor bias (younger galaxies are more extended) and we estimate that very minor mergers (\u03bc < 1/10) could contribute with an extra ~20%. The remaining ~5% should come from other processes (e.g., adiabatic expansion or observational effects). This picture also reproduces the mass growth and the velocity dispersion evolution of these galaxies. We conclude from these results, and after exploring all the possible uncertainties in our picture, that merging is the main contributor to the size evolution of massive ETGs at z \u2272 1, accounting for ~50\u221275% of that evolution in the last 8 Gyr. Nearly half of the evolution due to mergers is related to minor (\u03bc < 1/4) events.", "date": "2012-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "548", "publisher": "EDP Sciences", "pagerange": "Art. No. A7", "id_number": "CaltechAUTHORS:20130115-142950078", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130115-142950078", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-07-BLAN-0228" }, { "agency": "European Research Council (ERC)", "grant_number": "2010-AdG-268107-EARLY" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201219085", "primary_object": { "basename": "aa19085-12.pdf", "url": "https://authors.library.caltech.edu/records/vc4sk-qfw98/files/aa19085-12.pdf" }, "pub_year": "2012", "author_list": "L\u00f3pez-Sanjuan, C.; Bridge, C.; et el." }, { "id": "https://authors.library.caltech.edu/records/w06zm-qzp50", "eprint_id": 36004, "eprint_status": "archive", "datestamp": "2023-08-22 07:42:15", "lastmod": "2023-10-20 22:07:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steinhardt-C-L", "name": { "family": "Steinhardt", "given": "Charles L." }, "orcid": "0000-0003-3780-6801" }, { "id": "Schramm-M", "name": { "family": "Schramm", "given": "Malte" } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "John D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Alexandroff-R", "name": { "family": "Alexandroff", "given": "Rachael" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "Francesca" }, "orcid": "0000-0002-2115-1137" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "Dan" }, "orcid": "0000-0001-5382-6138" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Pattarakijwanich-P", "name": { "family": "Pattarakijwanich", "given": "Petchara" } }, { "id": "Strauss-M-A", "name": { "family": "Strauss", "given": "Michael A." }, "orcid": "0000-0002-0106-7755" } ] }, "title": "SDSS 0956+5128: A Broad-line Quasar with Extreme Velocity Offsets", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; black hole physics; galaxies: evolution; galaxies: nuclei; quasars: general", "note": "\u00a9 2012 American Astronomical Society. Received 2012 June 20; accepted 2012 September 4; published 2012 October 12. The authors thank Kevin Bundy, Masahiro Fukugita, Pat Hall, Daniel Proga, Robert Quimby, Allan Sadun, Masayuki Tanaka, and Alexander Tchekhovskoy for valuable comments. This work was supported by the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. M.A.S., P.P., and R.A. acknowledge the support of NSF grant\nAST-0707266. C.L.S. and M.E. thank the Aspen Center for\nPhysics and the NSF Grant No. 1066293 for hospitality during\nthe editing of this paper.\n\nPublished - 0004-637X_759_1_24.pdf
", "abstract": "We report on the discovery of a Type 1 quasar, SDSS 0956+5128, with a surprising combination of extreme velocity offsets. SDSS 0956+5128 is a broad-lined quasar exhibiting emission lines at three substantially different redshifts: a systemic redshift of z ~ 0.714 based on narrow emission lines, a broad Mg II emission line centered 1200 km s^(\u20131) bluer than the systemic velocity, at z ~ 0.707, and broad H\u03b1 and H\u03b2 emission lines centered at z ~ 0.690. The Balmer line peaks are 4100 km s^(\u20131) bluer than the systemic redshift. There are no previously known objects with such an extreme difference between broad Mg II and broad Balmer emission. The two most promising explanations are either an extreme disk emitter or a high-velocity black hole recoil. However, neither explanation appears able to explain all of the observed features of SDSS 0956+5128, so the object may provide a challenge to our general understanding of quasar physics.", "date": "2012-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "759", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 24", "id_number": "CaltechAUTHORS:20121217-092148266", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121217-092148266", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "NSF", "grant_number": "AST-0707266" }, { "agency": "Aspen Center for Physics" }, { "agency": "NSF", "grant_number": "PHY-1066293" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/759/1/24", "primary_object": { "basename": "0004-637X_759_1_24.pdf", "url": "https://authors.library.caltech.edu/records/w06zm-qzp50/files/0004-637X_759_1_24.pdf" }, "pub_year": "2012", "author_list": "Steinhardt, Charles L.; Schramm, Malte; et el." }, { "id": "https://authors.library.caltech.edu/records/pgr6v-vdm96", "eprint_id": 36013, "eprint_status": "archive", "datestamp": "2023-08-22 07:42:29", "lastmod": "2023-10-20 22:08:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Balokovi\u0107-M", "name": { "family": "Balokovi\u0107", "given": "M." }, "orcid": "0000-0003-0476-6647" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Ivezi\u0107-\u017d", "name": { "family": "Ivezi\u0107", "given": "\u017d." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Kelly-B-C", "name": { "family": "Kelly", "given": "B. C." } } ] }, "title": "Disclosing the Radio Loudness Distribution Dichotomy in Quasars: An Unbiased Monte Carlo Approach Applied to the SDSS-FIRST Quasar Sample", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: evolution; galaxies: high-redshift; methods: statistical; quasars: general; radio continuum: galaxies", "note": "\u00a9 2012 American Astronomical Society. Received 2011 January 18; accepted 2012 August 24; published 2012 October 15. The authors wish to thank the anonymous referee for helpful\ncomments and suggestions which improved the paper. M.B.\nacknowledges support from the International Fulbright Science and Technology Award. V.S. acknowledges support from NASA grant HST-GO-09822.31-A. \u017d.I. acknowledges support by NSF grant AST-0807500 to the University of Washington, NSF grant AST-0551161 to LSST for design and development activity, and by the Croatian National Science Foundation grant O-1548-2009. G.Z. acknowledges partial support from the INAF grant PRIN-2010. The research leading to these results has received funding from the European Union's Seventh Framework program under grant agreement 229517. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation\nGroup, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.\n\nPublished - 0004-637X_759_1_30.pdf
", "abstract": "We investigate the dichotomy in the radio loudness distribution of quasars by modeling their radio emission and various selection effects using a Monte Carlo approach. The existence of two physically distinct quasar populations, the radio-loud and radio-quiet quasars, is controversial and over the last decade a bimodal distribution of radio loudness of quasars has been both affirmed and disputed. We model the quasar radio luminosity distribution with simple unimodal and bimodal distribution functions. The resulting simulated samples are compared to a fiducial sample of 8300 quasars drawn from the SDSS DR7 Quasar Catalog and combined with radio observations from the FIRST survey. Our results indicate that the SDSS-FIRST sample is best described by a radio loudness distribution which consists of two components, with (12 \u00b1 1)% of sources in the radio-loud component. On the other hand, the evidence for a local minimum in the loudness distribution (bimodality) is not strong and we find that previous claims for its existence were probably affected by the incompleteness of the FIRST survey close to its faint limit. We also investigate the redshift and luminosity dependence of the radio loudness distribution and find tentative evidence that at high redshift radio-loud quasars were rarer, on average louder, and exhibited a smaller range in radio loudness. In agreement with other recent work, we conclude that the SDSS-FIRST sample strongly suggests that the radio loudness distribution of quasars is not a universal function, and that more complex models than presented here are needed to fully explain available observations", "date": "2012-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "759", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 30", "id_number": "CaltechAUTHORS:20121217-120051560", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121217-120051560", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822.31-A" }, { "agency": "NSF", "grant_number": "AST-0807500" }, { "agency": "NSF", "grant_number": "AST-0551161" }, { "agency": "National Science Foundation (Croatia)", "grant_number": "O-1548-2009" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-2010" }, { "agency": "European Research Council (ERC)", "grant_number": "229517" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Higher Education Funding Council for England" }, { "agency": "Max Planck Society" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/759/1/30", "primary_object": { "basename": "0004-637X_759_1_30.pdf", "url": "https://authors.library.caltech.edu/records/pgr6v-vdm96/files/0004-637X_759_1_30.pdf" }, "pub_year": "2012", "author_list": "Balokovi\u0107, M.; Smol\u010di\u0107, V.; et el." }, { "id": "https://authors.library.caltech.edu/records/bz507-rfy45", "eprint_id": 36001, "eprint_status": "archive", "datestamp": "2023-08-22 07:42:10", "lastmod": "2023-10-20 22:07:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Spectral Energy Distributions of Type 1 Active Galactic Nuclei in the COSMOS Survey. I. The XMM-COSMOS Sample", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; quasars: general; surveys", "note": "\u00a9 2012 American Astronomical Society. Received 2011 December 14; accepted 2012 September 4; published 2012 October 10. M.E. and H.H. thank J. McDowell for useful discussion. This work was supported in part by NASA Chandra grant number GO7-8136A (H.H., F.C., M.E.), NASA contract NAS8-39073 (Chandra X-ray Center), and the Smithsonian Scholarly Studies (F.C.). K.J. acknowledges support from the Emmy Noether Programme of the German Science Foundation (DFG) through grant number JA 1114/3-1. In Italy this work is supported by ASI/INAF contracts I/009/10/0, I/024/05/0, and I/088/06. In Germany this project is supported by the Bundesministerium f\u00fcr Bildung und Forschung/Deutsches Zentrum f\u00fcr Luft und Raumfahrt and the Max Planck Society. M.S. and G.H. acknowledge support bei the Leibniz Prize of the Deutsche Forschungagemeinschaft, DFG (HA 1850/28-1). Y.L. acknowledges partial funding support by the Directional Research Project of the Chinese Academy of Sciences under project No. KJCX2-YW-T03 and by the National Natural Science Foundation of China under grant Nos. 10821061, 10733010, 10725313, and by 973 Program of China under grant 2009CB824800.\n\nPublished - 0004-637X_759_1_6.pdf
", "abstract": "The \"Cosmic Evolution Survey\" (COSMOS) enables the study of the spectral energy distributions (SEDs) of active galactic nuclei (AGNs) because of the deep coverage and rich sampling of frequencies from X-ray to radio. Here we present an SED catalog of 413 X-ray (XMM-Newton)-selected type 1 (emission line FWHM > 2000 km s^(\u20131)) AGNs with Magellan, SDSS, or VLT spectrum. The SEDs are corrected for Galactic extinction, broad emission line contributions, constrained variability, and host galaxy contribution. We present the mean SED and the dispersion SEDs after the above corrections in the rest-frame 1.4 GHz to 40 keV, and show examples of the variety of SEDs encountered. In the near-infrared to optical (rest frame ~8 \u03bcm-4000 \u00c5), the photometry is complete for the whole sample and the mean SED is derived from detections only. Reddening and host galaxy contamination could account for a large fraction of the observed SED variety. The SEDs are all available online.", "date": "2012-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "759", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 6", "id_number": "CaltechAUTHORS:20121217-084324616", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121217-084324616", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Chandra", "grant_number": "GO7-8136A" }, { "agency": "NASA", "grant_number": "NAS8-39073" }, { "agency": "Smithsonian Scholarly Studies" }, { "agency": "German Science Foundation (DFG) Emmy Noether Programme", "grant_number": "JA 1114/3-1" }, { "agency": "ASI/INAF (Italy)", "grant_number": "I/009/10/0" }, { "agency": "ASI/INAF (Italy)", "grant_number": "I/024/05/0" }, { "agency": "ASI/INAF (Italy)", "grant_number": "I/088/06" }, { "agency": "Bundesministerium f\u00fcr Bildung und Forschung/Deutsches Zentrum f\u00fcr Luft und Raumfahrt" }, { "agency": "Max Planck Society" }, { "agency": "Deutsche Forschungsgemeinschaft Leibniz Prize", "grant_number": "HA 1850/28-1" }, { "agency": "China Academy of Sciences Directional Research Project", "grant_number": "KJCX2-YW-T03" }, { "agency": "National Natural Science Foundation of China", "grant_number": "10821061" }, { "agency": "National Natural Science Foundation of China", "grant_number": "10733010" }, { "agency": "National Natural Science Foundation of China", "grant_number": "10725313" }, { "agency": "973 Program of China", "grant_number": "2009CB824800" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/759/1/6", "primary_object": { "basename": "0004-637X_759_1_6.pdf", "url": "https://authors.library.caltech.edu/records/bz507-rfy45/files/0004-637X_759_1_6.pdf" }, "pub_year": "2012", "author_list": "Elvis, M.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/6k479-6mh27", "eprint_id": 35418, "eprint_status": "archive", "datestamp": "2023-08-22 07:08:49", "lastmod": "2023-10-20 16:11:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Lentati-L-T", "name": { "family": "Lentati", "given": "L." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "F." }, "orcid": "0000-0003-4793-7880" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S. C." } }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Magdis-G-E", "name": { "family": "Magdis", "given": "G." }, "orcid": "0000-0002-4872-2294" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S." }, "orcid": "0000-0001-7862-1032" }, { "id": "Riguccini-L", "name": { "family": "Riguccini", "given": "L." } }, { "id": "Berta-S", "name": { "family": "Berta", "given": "S." }, "orcid": "0000-0002-0320-1532" }, { "id": "Magnelli-B", "name": { "family": "Magnelli", "given": "B." }, "orcid": "0000-0002-6777-6490" }, { "id": "Pozzi-F", "name": { "family": "Pozzi", "given": "F." } } ] }, "title": "Deep observations of CO line emission from star-forming galaxies in a cluster candidate at z = 1.5", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general; galaxies: high-redshift; galaxies: ISM", "note": "\u00a9 2012 The Authors. Monthly Notices of the Royal Astronomical Society. \u00a9 2012 RAS.\n\nAccepted 2012 July 10. Received 2012 May 30; in original form 2012 April 8.\n\nWe thank the anonymous referee for the comments and suggestions that helped to improve this manuscript. MA and this work were co-funded under the Marie Curie Actions of the European Commission (FP7-COFUND). CC thanks the Kavli Institute for Cosmology for their hospitality. Based on observations obtained, within the COSMOS Legacy Survey, the National Radio Astronomy Observatory JVLA, CFHT, Subaru, KPNO, Cerro Tololo Inter-American Observatory (CTIO), and ESO Observatories. The National Radio Astronomy Observatory is a facility of the National Science Foundation\n(NSF), operated under cooperative agreement by Associated\nUniversities Inc.\n\nPublished - mnr21697.pdf
", "abstract": "We report results from a deep Jansky Very Large Array (JVLA) search for ^(12)CO J = 1\u20130 line emission from galaxies in a candidate galaxy cluster at z \u223c 1.55 in the COSMOS field. We target four galaxies with optical spectroscopic redshifts in the range z = 1.47\u20131.59, consistent with the likely redshift for the candidate galaxy cluster. Two of these four galaxies, ID 51613 and ID 51813, are nominally detected in CO 1\u20130 line emission at the 3\u20134\u03c3 level. We find CO luminosities of (2.42 \u00b1 0.58) \u00d7 10^(10)\u2009K km s^(\u22121)\u2009pc^2 and (1.26 \u00b1 0.38) \u00d7 10^(10)\u2009K km s^(\u22121)\u2009pc^2, respectively. Taking advantage from the clustering and expanded 2-GHz bandwidth of the JVLA, we perform a search for emission lines in the proximity of optical sources within the field of view of our observations (60 arcsec). We limit our search to galaxies with K_S < 23.5 (AB) and z_phot = 1.2\u20131.8. We find two bright optical galaxies, ID 51207 and ID 51380, to be associated with significant emission line peaks (>4\u03c3) in the data cube, which we identify with the CO 1\u20130 line emission. To test the reliability of the line peaks found, we performed a parallel search for line peaks using a Bayesian inference method. Both CO line emitting candidates are identified with probabilities of 13\u2009per cent and 72\u2009per cent that there are line emitting sources in each case, respectively. Monte Carlo simulations show that such associations are statistically significant, with probabilities of chance association of 3.5\u2009per cent and 10.7\u2009per cent for ID 51207 and ID 51380, respectively. Modelling of their optical/IR spectral energy distributions indicates that the CO detected galaxies and candidates have stellar masses and star formation rates in the range (0.3\u20131.1) \u00d7 10^(11)\u2009M_\u2299 and 60\u2013160\u2009M_\u2299\u2009yr^(\u22121), with star formation efficiencies comparable to that found in other star-forming galaxies at similar redshifts. By comparing the space density of CO emitters derived from our observations with the space density derived from previous CO detections at z \u223c 1.5, and with semi-analytic predictions for the CO luminosity function, we suggest that the latter tend to underestimate the number of CO galaxies detected at high redshift. Finally, we argue about the benefits of future searches for molecular gas line emission in clustered fields with upcoming submillimetre/radio facilities.", "date": "2012-10-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "426", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "258-275", "id_number": "CaltechAUTHORS:20121112-163050209", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121112-163050209", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Marie Curie Fellowship" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2012.21697.x", "primary_object": { "basename": "mnr21697.pdf", "url": "https://authors.library.caltech.edu/records/6k479-6mh27/files/mnr21697.pdf" }, "pub_year": "2012", "author_list": "Aravena, M.; Carilli, C. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/2d86d-nyh73", "eprint_id": 38779, "eprint_status": "archive", "datestamp": "2023-08-22 07:07:28", "lastmod": "2023-10-23 23:28:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Reyes-R", "name": { "family": "Reyes", "given": "R." } }, { "id": "Mandelbaum-R", "name": { "family": "Mandelbaum", "given": "R." }, "orcid": "0000-0003-2271-1527" }, { "id": "Gunn-J-E", "name": { "family": "Gunn", "given": "J. E." } }, { "id": "Nakajima-Reiko", "name": { "family": "Nakajima", "given": "R." } }, { "id": "Seljak-U", "name": { "family": "Seljak", "given": "U." } }, { "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "C. M." }, "orcid": "0000-0002-2951-4932" } ] }, "title": "Optical-to-virial velocity ratios of local disc galaxies from combined kinematics and galaxy\u2013galaxy lensing", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: weak; galaxies: kinematics and dynamics; galaxies: spiral", "note": "\u00a9 2012 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2012 RAS.\n\nAccepted 2012 June 7. Received 2012 June 7; in original form 2011 October 17.\n\nWe thank Michael Strauss, David Weinberg and David Spergel\nfor their comments on this work. CMH is supported by the US\nDepartment of Energy under contract DE-FG03-02-ER40701 and\nthe David & Lucile Packard Foundation. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National\nScience Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, Cambridge University, Case Western Reserve University, University\nof Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle\nAstrophysics and Cosmology, the Korean Scientist Group, the\nChinese Academy of Sciences (LAMOST), Los Alamos National\nLaboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington.\n\nPublished - MNRAS-2012-Reyes-2610-40.pdf
", "abstract": "In this paper, we measure the optical-to-virial velocity ratios V_(opt)/V_(200c) of disc galaxies in the Sloan Digital Sky Survey (SDSS) at a mean redshift of \u3008z\u3009 = 0.07 and with stellar masses 10^9 < M* < 10^(11)\u2009M_\u2299. V_(opt)/V_(200c), the ratio of the circular velocity measured at the optical radius of the disc (\u223c10\u2009kpc) to that at the virial radius of the dark matter halo (\u223c150\u2009kpc), is a powerful observational constraint on disc galaxy formation. It links galaxies to their dark matter haloes dynamically and constrains the total mass profile of disc galaxies over an order of magnitude in length scale. For this measurement, we combine Vopt derived from the Tully\u2013Fisher relation (TFR) from Reyes et al. with V200c derived from halo masses measured with galaxy\u2013galaxy lensing. In anticipation of this combination, we use similarly selected galaxy samples for both the TFR and lensing analysis. For three M* bins with lensing-weighted mean stellar masses of 0.6, 2.7 and 6.5 \u00d7 10^(10)\u2009M_\u2299, we find halo-to-stellar mass ratios M_(200c)/M_* = 41, 23 and 26, with 1\u03c3 statistical uncertainties of around 0.1\u2009dex, and V_(opt)/V_(200c) = 1.27 \u00b1 0.08,\u20091.39 \u00b1 0.06 and 1.27 \u00b1 0.08\u2009(1\u03c3), respectively. Our results suggest that the dark matter and baryonic contributions to the mass within the optical radius are comparable, if the dark matter halo profile has not been significantly modified by baryons. The results obtained in this work will serve as inputs to and constraints on disc galaxy formation models, which will be explored in future work. Finally, we note that this paper presents a new and improved galaxy shape catalogue for weak lensing that covers the full SDSS Data Release 7 footprint.", "date": "2012-10-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "425", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "2610-2640", "id_number": "CaltechAUTHORS:20130604-105159808", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130604-105159808", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG03-02-ER40701" }, { "agency": "David and Lucile Packard Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1111/j.1365-2966.2012.21472.x", "primary_object": { "basename": "MNRAS-2012-Reyes-2610-40.pdf", "url": "https://authors.library.caltech.edu/records/2d86d-nyh73/files/MNRAS-2012-Reyes-2610-40.pdf" }, "pub_year": "2012", "author_list": "Reyes, R.; Mandelbaum, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/1zntf-bfb95", "eprint_id": 35306, "eprint_status": "archive", "datestamp": "2023-08-22 06:55:33", "lastmod": "2023-10-20 15:57:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hathi-N-P", "name": { "family": "Hathi", "given": "Nimish P." }, "orcid": "0000-0001-6145-5090" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Wang-Wei-Hao", "name": { "family": "Wang", "given": "Wei-Hao" }, "orcid": "0000-0003-2588-1265" }, { "id": "Ferguson-H-C", "name": { "family": "Ferguson", "given": "Henry C." }, "orcid": "0000-0001-7113-2738" } ] }, "title": "Near-infrared Survey of the GOODS-North Field: Search for Luminous Galaxy Candidates at z \u2273 6.5", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: evolution; galaxies: formation; galaxies: high-redshift", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2011 November 7; accepted 2012 July 23; published 2012 September 4.\nBased in part on data collected at Subaru Telescope, which is operated by\nthe National Astronomical Observatory of Japan.\nBased on observations obtained with WIRCam, a joint project of CFHT,\nTaiwan, Korea, Canada, France, at the Canada\u2013France\u2013Hawaii Telescope\n(CFHT), which is operated by the National Research Council (NRC) of\nCanada, the Institute National des Sciences de l'Univers of the Centre National\nde la Recherche Scientifique of France, and the University of Hawaii.\nWe thank the referee for helpful comments and suggestions\nthat significantly improved this paper. We acknowledge valuable comments and suggestions from Mark Dickinson. We are grateful to Kyle Penner and Shoubaneh Hemmati for their help in reducing the Keck spectroscopy data. N.P.H. acknowledges support provided by NASA through grants HST-GO-11702.02-A and HST-GO-11359.08-A from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555.\n\nPublished - 0004-637X_757_1_43.pdf
", "abstract": "We present near-infrared (NIR; J and K_s) survey of the Great Observatories Origins Deep Survey-North (GOODS-N) field. The publicly available imaging data were obtained using the MOIRCS instrument on the 8.2 m Subaru and the WIRCam instrument on the 3.6 m Canada-France-Hawaii Telescope (CFHT). These observations fulfill a serious wavelength gap in the GOODS-N data, i.e., lack of deep NIR observations. We combine the Subaru/MOIRCS and CFHT/WIRCam archival data to generate deep J- and K_s-band images, covering the full GOODS-N field (~169 arcmin^2) to an AB magnitude limit of ~25 mag (3\u03c3). We applied z_850-band dropout color selection criteria, using the NIR data generated here. We have identified two possible Lyman break galaxy (LBG) candidates at z \u2273 6.5 with J \u2272 24.5. The first candidate is a likely LBG at z \u2243 6.5 based on a weak spectral feature tentatively identified as Ly\u03b1 line in the deep Keck/DEIMOS spectrum, while the second candidate is a possible LBG at z \u2243 7 based on its photometric redshift. These z 850-dropout objects, if confirmed, are among the brightest such candidates found so far. At z \u2273 6.5, their star formation rate is estimated as 100-200 M_\u2609 yr^(\u20131). If they continue to form stars at this rate, they assemble a stellar mass of ~5 \u00d7 10^(10) M_\u2609 after about 400 million years, becoming the progenitors of massive galaxies observed at z \u2243 5. We study the implication of the z 850-band dropout candidates discovered here, in constraining the bright end of the luminosity function and understanding the nature of high-redshift galaxies.", "date": "2012-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "757", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 43", "id_number": "CaltechAUTHORS:20121106-134127363", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121106-134127363", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-11702.02-A" }, { "agency": "NASA", "grant_number": "HST-GO-11359.08-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/757/1/43", "primary_object": { "basename": "0004-637X_757_1_43.pdf", "url": "https://authors.library.caltech.edu/records/1zntf-bfb95/files/0004-637X_757_1_43.pdf" }, "pub_year": "2012", "author_list": "Hathi, Nimish P.; Mobasher, Bahram; et el." }, { "id": "https://authors.library.caltech.edu/records/h1pk8-sy254", "eprint_id": 35297, "eprint_status": "archive", "datestamp": "2023-08-22 06:51:51", "lastmod": "2023-10-20 15:56:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ikeda-Hideyuki", "name": { "family": "Ikeda", "given": "H." } }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "T." }, "orcid": "0000-0002-7402-5441" }, { "id": "Matsuoka-Kenta", "name": { "family": "Matsuoka", "given": "K." }, "orcid": "0000-0002-2689-4634" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Kajisawa-Masaru", "name": { "family": "Kajisawa", "given": "M." }, "orcid": "0000-0002-1732-6387" }, { "id": "Enoki-Motohiro", "name": { "family": "Enoki", "given": "M." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "D." }, "orcid": "0000-0001-5382-6138" }, { "id": "Morokuma-Tomoki", "name": { "family": "Morokuma", "given": "T." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Constraints on the Faint End of the Quasar Luminosity Function at z ~ 5 in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; quasars: general; surveys", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2011 July 9; accepted 2012 July 6; published 2012 August 24.\n\nWe thank the Subaru staff for their invaluable help and all\nmembers of the COSMOS team. This work was financially\nsupported in part by the Japan Society for the Promotion of\nScience (JSPS; grant Nos. 23244031 and 23654068). This work\nwas also partly supported by the FIRST program \"Subaru\nMeasurements of Images and Redshifts (SuMIRe),\" which was\ninitiated by the Council for Science and Technology Policy\n(CSTP). K.M. is financially supported by the JSPS through the JSPS Research Fellowship.\n\nPublished - 0004-637X_756_2_160.pdf
", "abstract": "We present the result of our low-luminosity quasar survey in the redshift range of 4.5 \u2272 z \u2272 5.5 in the COSMOS field. Using the COSMOS photometric catalog, we selected 15 quasar candidates with 22 < i' < 24 at z ~ 5 that are ~3 mag fainter than the Sloan Digital Sky Survey quasars in the same redshift range. We obtained optical spectra for 14 of the 15 candidates using FOCAS on the Subaru Telescope and did not identify any low-luminosity type-1 quasars at z ~ 5, while a low-luminosity type-2 quasar at z ~ 5.07 was discovered. In order to constrain the faint end of the quasar luminosity function at z ~ 5, we calculated the 1\u03c3 confidence upper limits of the space density of type-1 quasars. As a result, the 1\u03c3 confidence upper limits on the quasar space density are \u03a6 < 1.33 \u00d7 10^(\u20137) Mpc^(\u20133) mag^(\u20131) for \u201324.52 < M_(1450) < \u201323.52 and \u03a6 < 2.88 \u00d7 10^(\u20137) Mpc^(\u20133) mag^(\u20131) for \u201323.52 < M_1450 < \u201322.52. The inferred 1\u03c3 confidence upper limits of the space density are then used to provide constraints on the faint-end slope and the break absolute magnitude of the quasar luminosity function at z ~ 5. We find that the quasar space density decreases gradually as a function of redshift at low luminosity (M_1450 ~ \u201323), being similar to the trend found for quasars with high luminosity (M_1450 < \u201326). This result is consistent with the so-called downsizing evolution of quasars seen at lower redshifts.", "date": "2012-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "756", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 160", "id_number": "CaltechAUTHORS:20121106-101127819", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121106-101127819", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23244031" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23654068" }, { "agency": "Council for Science and Technology Policy (CSTP)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/756/2/160", "primary_object": { "basename": "0004-637X_756_2_160.pdf", "url": "https://authors.library.caltech.edu/records/h1pk8-sy254/files/0004-637X_756_2_160.pdf" }, "pub_year": "2012", "author_list": "Ikeda, H.; Nagao, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/2cwqw-aqb67", "eprint_id": 35151, "eprint_status": "archive", "datestamp": "2023-09-14 19:38:51", "lastmod": "2023-10-23 20:54:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Masters-D-C", "name": { "family": "Masters", "given": "D." }, "orcid": "0000-0001-5382-6138" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Siana-Brian-D", "name": { "family": "Siana", "given": "B." }, "orcid": "0000-0002-4935-9511" }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C. D." } }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "T." }, "orcid": "0000-0002-7402-5441" }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J. R." } }, { "id": "Ikeda-Hideyuki", "name": { "family": "Ikeda", "given": "H." } }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Evolution of the Quasar Luminosity Function over 3 < z < 5 in the COSMOS Survey Field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: luminosity function, mass function; Galaxy: evolution; quasars: general", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2011 November 29; accepted 2012 July 6; published 2012 August 7.\n\nWe gratefully acknowledge the contributions of the entire\nCOSMOS collaboration. More information about the COSMOS\nsurvey is available at http://www.astro.caltech.edu/cosmos. We acknowledge the anonymous referee for suggestions that significantly improved this work. We thank Dr. Eilat Glikman for helpful discussions. M.S. and G.H. acknowledge support by the German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize (FKZ HA 1850/28-1). D.M. gratefully acknowledges the support of the Infrared Processing and Analysis Center (IPAC) Visiting Graduate Fellowship program, as well as the Carnegie Visiting Graduate Fellowship program.\n\nPublished - 0004-637X_755_2_169.pdf
", "abstract": "We investigate the high-redshift quasar luminosity function (QLF) down to an apparent magnitude of I_AB = 25 in the Cosmic Evolution Survey (COSMOS). Careful analysis of the extensive COSMOS photometry and imaging data allows us to identify and remove stellar and low-redshift contaminants, enabling a selection that is nearly complete for type-1 quasars at the redshifts of interest. We find 155 likely quasars at z > 3.1, 39 of which have prior spectroscopic confirmation. We present our sample in detail and use these confirmed and likely quasars to compute the rest-frame UV QLF in the redshift bins 3.1 < z < 3.5 and 3.5 < z < 5. The space density of faint quasars decreases by roughly a factor of four from z ~ 3.2 to z ~ 4, with faint-end slopes of \u03b2 ~ \u20131.7 at both redshifts. The decline in space density of faint optical quasars at z > 3 is similar to what has been found for more luminous optical and X-ray quasars. We compare the rest-frame UV luminosity functions found here with the X-ray luminosity function at z > 3, and find that they evolve similarly between z ~ 3.2 and z ~ 4; however, the different normalizations imply that roughly 75% of X-ray bright active galactic nuclei (AGNs) at z ~ 3-4 are optically obscured. This fraction is higher than found at lower redshift and may imply that the obscured, type-2 fraction continues to increase with redshift at least to z ~ 4. Finally, the implications of the results derived here for the contribution of quasars to cosmic reionization are discussed.", "date": "2012-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "755", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 169", "id_number": "CaltechAUTHORS:20121029-103850313", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121029-103850313", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "FKZ HA 1850/28-1" }, { "agency": "Infrared Processing and Analysis Center (IPAC) Visiting Graduate Fellowship program" }, { "agency": "Carnegie Visiting Graduate Fellowship program" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/755/2/169", "primary_object": { "basename": "0004-637X_755_2_169.pdf", "url": "https://authors.library.caltech.edu/records/2cwqw-aqb67/files/0004-637X_755_2_169.pdf" }, "pub_year": "2012", "author_list": "Masters, D.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/vdjgt-62z57", "eprint_id": 34499, "eprint_status": "archive", "datestamp": "2023-09-14 19:34:10", "lastmod": "2023-10-23 20:53:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N. Y." }, "orcid": "0000-0002-8948-1044" }, { "id": "Marshall-J", "name": { "family": "Marshall", "given": "J." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The Herschel Multi-tiered Extragalactic Survey: HerMES", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys; galaxies: evolution; infrared: galaxies; submillimetre: galaxies", "note": "\u00a9 2012 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2012 RAS.\n\nAccepted 2012 March 12. Received 2012 January 5; in original form 2011 July 20.\nArticle first published online: 6 Jul. 2012.\nWe acknowledge support from the UK Science and Technology\nFacilities Council, grant numbers ST/F002858/1 and ST/I000976/1. HCSS/HSPOT/HIPE are joint developments by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center and the HIFI, PACS and SPIRE consortia. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada), NAOC (China), CEA, LAM (France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK) and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS\n(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC,\nUKSA (UK) and NASA (USA).\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nPublished - mnr20912.pdf
Accepted Version - 1203.2562.pdf
", "abstract": "The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy programme designed to map a set of nested fields totalling \u223c380\u2009deg^2. Fields range in size from 0.01 to \u223c20\u2009deg^2, using the Herschel-Spectral and Photometric Imaging Receiver (SPIRE) (at 250, 350 and 500\u2009\u03bcm) and the Herschel-Photodetector Array Camera and Spectrometer (PACS) (at 100 and 160\u2009\u03bcm), with an additional wider component of 270\u2009deg^2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the reprocessed optical and ultraviolet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multiwavelength understanding of galaxy formation and evolution. \n\nThe survey will detect of the order of 100\u2009000 galaxies at 5\u03c3 in some of the best-studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X-ray wavelengths, it is designed to facilitate redshift determination, rapidly identify unusual objects and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include the total infrared emission of galaxies, the evolution of the luminosity function, the clustering properties of dusty galaxies and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques. \n\nThis paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results.", "date": "2012-08-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "424", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "1614-1635", "id_number": "CaltechAUTHORS:20120927-094554573", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120927-094554573", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "Herschel Science Ground Segment Consortium" }, { "agency": "NASA Herschel Science Center" }, { "agency": "HIFI" }, { "agency": "PACS" }, { "agency": "SPIRE" }, { "agency": "European Space Agency (ESA)" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2012.20912.x", "primary_object": { "basename": "1203.2562.pdf", "url": "https://authors.library.caltech.edu/records/vdjgt-62z57/files/1203.2562.pdf" }, "related_objects": [ { "basename": "mnr20912.pdf", "url": "https://authors.library.caltech.edu/records/vdjgt-62z57/files/mnr20912.pdf" } ], "pub_year": "2012", "author_list": "Oliver, S. J.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/1pppw-kr221", "eprint_id": 33784, "eprint_status": "archive", "datestamp": "2023-08-22 06:23:42", "lastmod": "2023-10-18 20:40:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Onodera-Masato", "name": { "family": "Onodera", "given": "M." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Cappellari-M", "name": { "family": "Cappellari", "given": "M." } }, { "id": "Mancini-C", "name": { "family": "Mancini", "given": "C." }, "orcid": "0000-0002-4297-0561" }, { "id": "Strazzullo-V", "name": { "family": "Strazzullo", "given": "V." } }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "Arimoto-Nobuo", "name": { "family": "Arimoto", "given": "N." } }, { "id": "Gobat-R", "name": { "family": "Gobat", "given": "R." } }, { "id": "Yamada-Y", "name": { "family": "Yamada", "given": "Y." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Kong-X", "name": { "family": "Kong", "given": "X." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Motohara-Kentaro", "name": { "family": "Motohara", "given": "K." } }, { "id": "Ohta-K", "name": { "family": "Ohta", "given": "K." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Tamura-N", "name": { "family": "Tamura", "given": "N." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" } ] }, "title": "Deep Near-infrared Spectroscopy of Passively Evolving Galaxies at z \u2273 1.4", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2012 March 4; accepted 2012 June 7; published 2012 July 23. \n\nBased on data collected at the Subaru telescope, which is operated by the National Astronomical Observatory of Japan. (Proposal IDs: S09A-043 and S10A-058). \n\nWe thank the staff of the Subaru telescope, especially Ichi Tanaka, for supporting the observations. We also thank Mariska Kriek for a permission to use FAST, Stephan Charlot for providing the stellar population synthesis models before publication, Alexis Finoguenov for computing the upper limits from XMM-Newton data for the overdense regions, Masayuki Tanaka for checking the existence of red sequence cluster around redshift spikes, and Masafumi Yagi for fruitful discussion.We are grateful to the anonymous referee for her/his comments. This work has been partly supported by the ASI grant \"COFIS-Analisi Dati\" and by the INAF grant \"PRIN-2008\" and is supported by a Grant-in-Aid for Science Research (No. 23224005) by the Japanese Ministry of Education, Culture, Sports, Science and\nTechnology. \n\nFacility: Subaru (NAOJ)\n\nPublished - Onodera2012p19347Astrophys_J.pdf
", "abstract": "We present the results of new near-IR spectroscopic observations of passive galaxies at z \u2273 1.4 in a concentration of BzK-selected galaxies in the COSMOS field. The observations have been conducted with Subaru/MOIRCS, and have resulted in absorption lines and/or continuum detection for 18 out of 34 objects. This allows us to measure spectroscopic redshifts for a sample that is almost complete to K_AB = 21. COSMOS photometric redshifts are found in fair agreement overall with the spectroscopic redshifts, with a standard deviation of ~0.05; however, ~30% of objects have photometric redshifts systematically underestimated by up to ~25%. We show that these systematic offsets in photometric redshifts can be removed by using these objects as a training set. All galaxies fall in four distinct redshift spikes at z = 1.43, 1.53, 1.67, and 1.82, with this latter one including seven galaxies. SED fits to broadband fluxes indicate stellar masses in the range of ~4-40 \u00d7 10^10 M_\u2609 and that star formation was quenched ~1 Gyr before the cosmic epoch at which they are observed. The spectra of several individual galaxies have allowed us to measure their H\u03b4_F indices and the strengths of the 4000 \u00c5 break, which confirms their identification as passive galaxies, as does a composite spectrum resulting from the co-addition of 17 individual spectra. The effective radii of the galaxies have been measured on the COSMOS HST/ACS i_(F814W)-band image, confirming the coexistence at these redshifts of passive galaxies, which are substantially more compact than their local counterparts with others that follow the local effective radius-stellar mass relation. For the galaxy with the best signal-to-noise spectrum we were able to measure a velocity dispersion of 270 \u00b1 105 km s^(\u20131) (error bar including systematic errors), indicating that this galaxy lies closely on the virial relation given its stellar mass and effective radius.", "date": "2012-08-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "755", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 26", "id_number": "CaltechAUTHORS:20120831-134916301", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120831-134916301", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-2008" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23224005" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/755/1/26", "primary_object": { "basename": "Onodera2012p19347Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/1pppw-kr221/files/Onodera2012p19347Astrophys_J.pdf" }, "pub_year": "2012", "author_list": "Onodera, M.; Renzini, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/zb5ax-xef17", "eprint_id": 33933, "eprint_status": "archive", "datestamp": "2023-08-22 06:24:06", "lastmod": "2023-10-18 21:38:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tinker-J-L", "name": { "family": "Tinker", "given": "Jeremy L." } }, { "id": "George-M-R", "name": { "family": "George", "given": "Matthew R." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "Bundy-K-A", "name": { "family": "Bundy", "given": "Kevin" }, "orcid": "0000-0001-9742-3138" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "Alexis" }, "orcid": "0000-0002-4606-5403" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "Richard" }, "orcid": "0000-0002-6085-3780" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" }, { "id": "Wechsler-R-H", "name": { "family": "Wechsler", "given": "Risa H." }, "orcid": "0000-0003-2229-011X" } ] }, "title": "The Correlated Formation Histories of Massive Galaxies and Their Dark Matter Halos", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: groups: general; galaxies: halos", "note": "\u00a9 2012 American Astronomical Society. Received 2012 March 30; accepted 2012 June 13; published 2012 July 20. We thank Charlie Conroy and Tom Theuns for useful discussions.\nThis work was supported by World Premier International\nResearch Center Initiative (WPI Initiative), MEXT, Japan. The\ninitial HST-COSMOS Treasury program was supported through\nNASA grant HST-GO-09822. We gratefully acknowledge contributions of the entire COSMOS collaboration consisting of more than 140 scientists. More information on COSMOS is\navailable at http://cosmos.astro.caltech.edu/ and the data archive is at IPAC/IRSA. J.R. was supported by JPL, run under contract for NASA by Caltech.\n\nPublished - 2041-8205_755_1_L5.pdf
", "abstract": "Using observations in the COSMOS field, we report an intriguing correlation between the star formation activity of massive (~10^(11.4) M_\u2609) central galaxies, their stellar masses, and the large-scale (~10 Mpc) environments of their group-mass (~10^(13.6) M_\u2609) dark matter halos. Probing the redshift range z = [0.2, 1.0], our measurements come from two independent sources: an X-ray-detected group catalog and constraints on the stellar-to-halo mass relation derived from a combination of clustering and weak lensing statistics. At z = 1, we find that the stellar mass in star-forming (SF) centrals is a factor of two less than in passive centrals at the same halo mass. This implies that the presence or lack of star formation in group-scale centrals cannot be a stochastic process. By z = 0, the offset reverses, probably as a result of the different growth rates of these objects. A similar but weaker trend is observed when dividing the sample by morphology rather than star formation. Remarkably, we find that SF centrals at z ~ 1 live in groups that are significantly more clustered on 10 Mpc scales than similar mass groups hosting passive centrals. We discuss this signal in the context of halo assembly and recent simulations, suggesting that SF centrals prefer halos with higher angular momentum and/or formation histories with more recent growth; such halos are known to evolve in denser large-scale environments. If confirmed, this would be evidence of an early established link between the assembly history of halos on large scales and the future properties of the galaxies that form inside them.", "date": "2012-08-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "755", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L5", "id_number": "CaltechAUTHORS:20120907-113422698", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120907-113422698", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/2041-8205/755/1/L5", "primary_object": { "basename": "2041-8205_755_1_L5.pdf", "url": "https://authors.library.caltech.edu/records/zb5ax-xef17/files/2041-8205_755_1_L5.pdf" }, "pub_year": "2012", "author_list": "Tinker, Jeremy L.; George, Matthew R.; et el." }, { "id": "https://authors.library.caltech.edu/records/10jrs-5pr06", "eprint_id": 33799, "eprint_status": "archive", "datestamp": "2023-08-19 12:00:57", "lastmod": "2023-10-18 20:41:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ford-Jes", "name": { "family": "Ford", "given": "Jes" } }, { "id": "Hildebrandt-H", "name": { "family": "Hildebrandt", "given": "Hendrik" } }, { "id": "Van-Waerbeke-L", "name": { "family": "Van Waerbeke", "given": "Ludovic" } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "Alexis" }, "orcid": "0000-0002-4606-5403" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "Masayuki" }, "orcid": "0000-0002-5011-5178" }, { "id": "George-M-R", "name": { "family": "George", "given": "Matthew R." } }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" } ] }, "title": "Magnification by Galaxy Group Dark Matter Halos", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: photometry", "note": "\u00a9 2012 IOP Publishing.\nReceived 2011 November 15; accepted 2012 June 4; published 2012 July 18.\nThe authors thank Fabian Schmidt and Martha Milkeraitis for\nuseful discussions related to this work. J.F. was supported by JPL grant No. 1394704, and is now supported by NSERC and\nCIfAR. H.H. is supported by the Marie Curie IOF 252760 and\nby a CITA National Fellowship. This work was performed in\npart at JPL, run by Caltech under a contract for NASA. This\nwork was supported by World Premier International Research\nCenter Initiative (WPI Initiative), MEXT, Japan. This work is based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan, and on observations made with the NASA/ESA Hubble Space Telescope. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work is also based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada\u2013France\u2013Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii.\n\nPublished - Ford2012p19344Astrophys_J.pdf
Submitted - 1111.3698v2.pdf
", "abstract": "We report on the detection of gravitational lensing magnification by a population of galaxy groups, at a significance level of 4.9\u03c3. Using X-ray-selected groups in the COSMOS 1.64 deg^2 field, and high-redshift Lyman break galaxies as sources, we measure a lensing-induced angular cross-correlation between the samples. After satisfying consistency checks that demonstrate we have indeed detected a magnification signal, and are not suffering from contamination by physical overlap of samples, we proceed to implement an optimally weighted cross-correlation function to further boost the signal to noise of the measurement. Interpreting this optimally weighted measurement allows us to study properties of the lensing groups. We model the full distribution of group masses using a composite-halo approach, considering both the singular isothermal sphere and Navarro-Frenk-White profiles, and find our best-fit values to be consistent with those recovered using the weak-lensing shear technique. We argue that future weak-lensing studies will need to incorporate magnification along with shear, both to reduce residual systematics and to make full use of all available source information, in an effort to maximize scientific yield of the observations.", "date": "2012-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "754", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 143", "id_number": "CaltechAUTHORS:20120831-143730769", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120831-143730769", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "JPL", "grant_number": "1394704" }, { "agency": "Natural Sciences and Engineering Research Council (NSERC) (Canada)" }, { "agency": "Canada Institute for Advanced Research (CIfAR)" }, { "agency": "Marie Curie International Outgoing Fellowship", "grant_number": "252760" }, { "agency": "CITA National fellowship" }, { "agency": "World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/754/2/143", "primary_object": { "basename": "1111.3698v2.pdf", "url": "https://authors.library.caltech.edu/records/10jrs-5pr06/files/1111.3698v2.pdf" }, "related_objects": [ { "basename": "Ford2012p19344Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/10jrs-5pr06/files/Ford2012p19344Astrophys_J.pdf" } ], "pub_year": "2012", "author_list": "Ford, Jes; Hildebrandt, Hendrik; et el." }, { "id": "https://authors.library.caltech.edu/records/czjb4-mwe20", "eprint_id": 58955, "eprint_status": "archive", "datestamp": "2023-08-19 11:59:11", "lastmod": "2023-10-23 19:54:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Milvang-Jensen-B", "name": { "family": "Milvang-Jensen", "given": "B." }, "orcid": "0000-0002-2281-2785" }, { "id": "Dunlop-J", "name": { "family": "Dunlop", "given": "J." } }, { "id": "Franx-M", "name": { "family": "Franx", "given": "M." }, "orcid": "0000-0002-8871-3026" }, { "id": "Fynbo-J-P-U", "name": { "family": "Fynbo", "given": "J. P. U." }, "orcid": "0000-0002-8149-8298" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Holt-J", "name": { "family": "Holt", "given": "J." } }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K. I." }, "orcid": "0000-0001-8183-1460" }, { "id": "Goranova-Y", "name": { "family": "Goranova", "given": "Y." } }, { "id": "Buitrago-F", "name": { "family": "Buitrago", "given": "F." } }, { "id": "Emerson-J-P", "name": { "family": "Emerson", "given": "J. P." } }, { "id": "Freudling-W", "name": { "family": "Freudling", "given": "W." } }, { "id": "Hudelot-P", "name": { "family": "Hudelot", "given": "P." } }, { "id": "L\u00f3pez-Sanjuan-C", "name": { "family": "L\u00f3pez-Sanjuan", "given": "C." } }, { "id": "Magnard-F", "name": { "family": "Magnard", "given": "F." } }, { "id": "Mellier-Y", "name": { "family": "Mellier", "given": "Y." } }, { "id": "M\u00f8ller-P", "name": { "family": "M\u00f8ller", "given": "P." } }, { "id": "Nilsson-K-K", "name": { "family": "Nilsson", "given": "K. K." } }, { "id": "Sutherland-S", "name": { "family": "Sutherland", "given": "W." } }, { "id": "Tasca-L", "name": { "family": "Tasca", "given": "L." } }, { "id": "Zabl-J", "name": { "family": "Zabl", "given": "J." } } ] }, "title": "UltraVISTA: a new ultra-deep near-infrared survey in COSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys \u2013 galaxies: general \u2013 galaxies: high-redshift \u2013 cosmology: observations \u2013 large-scale structure of Universe", "note": "\u00a9 2012 ESO.\nArticle published by EDP Sciences.\n\nReceived 30 April 2012; Accepted 22 June 2012;\nPublished online 24 August 2012.\n\nH. J. McCracken acknowledges the use of TERAPIX computing\nfacilities. This research has made use of the VizieR catalogue access tool\nprovided by the CDS, Strasbourg, France. This research was supported by ANR\ngrant \"ANR-07-BLAN-0228\". J.P.U.F. and B.M.J. acknowledge support from\nthe ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by\nthe Danish National Research Foundation. OLF, CSJ, LT acknowledge support\nfrom the ERC advanced grant ERC-2010-AdG-268107. J.H. acknowledges support\nfrom NWO. J.S.D. acknowledges the support of the Royal Society via a\nWolfson Research Merit award, and also the support of the European Research\nCouncil via the award of an Advanced Grant. The UltraVISTA team would like\nto thank ESO staff for scheduling and making the UltraVISTA observations, and\nthe Cambridge Astronomy Survey Unit for providing us with pre-preprocessed\nUltraVISTA images. E. Bertin is thanked for useful discussions concerning the\ndata reductions presented here.\n\nBased on data products from observations made with ESO\nTelescopes at the La Silla Paranal Observatory under ESO programme\nID 179.A-2005 and on data products produced by TERAPIX and\nthe Cambridge Astronomy Survey Unit on behalf of the UltraVISTA\nconsortium.\n\nPublished - aa19507-12.pdf
Submitted - 1204.6586v2.pdf
", "abstract": "In this paper we describe the first data release of the UltraVISTA near-infrared imaging survey of the COSMOS field. We summarise the key goals and design of the survey and provide a detailed description of our data reduction techniques. We provide stacked, sky-subtracted images in YJHK_s and narrow-band filters constructed from data collected during the first year of UltraVISTA observations. Our stacked images reach 5\u03c3AB depths in an aperture of 2\u2033 diameter of ~25 in Y and ~24 in JHK_s bands and all have sub-arcsecond seeing. To this 5\u03c3 limit, our K_s catalogue contains 216\u2009268 sources. We carry out a series of quality assessment tests on our images and catalogues, comparing our stacks with existing catalogues. The 1\u03c3 astrometric rms in both directions for stars selected with 17.0 < K_s(AB) < 19.5 is ~0.08\u2033 in comparison to the publicly-available COSMOS ACS catalogues. Our images are resampled to the same pixel scale and tangent point as the publicly available COSMOS data and so may be easily used to generate multi-colour catalogues using this data. All images and catalogues presented in this paper are publicly available through ESO's \"phase 3\" archiving and distribution system and from the UltraVISTA web site.", "date": "2012-08", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "544", "publisher": "EDP Sciences", "pagerange": "Art. No. A156", "id_number": "CaltechAUTHORS:20150721-081450110", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150721-081450110", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-07-BLAN-0228" }, { "agency": "European Research Council (ERC)", "grant_number": "EGGS-278202" }, { "agency": "Danish National Research Foundation" }, { "agency": "European Research Council (ERC)", "grant_number": "ERC-2010-AdG-268107" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "Royal Society" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201219507", "primary_object": { "basename": "aa19507-12.pdf", "url": "https://authors.library.caltech.edu/records/czjb4-mwe20/files/aa19507-12.pdf" }, "related_objects": [ { "basename": "1204.6586v2.pdf", "url": "https://authors.library.caltech.edu/records/czjb4-mwe20/files/1204.6586v2.pdf" } ], "pub_year": "2012", "author_list": "McCracken, H. J.; Milvang-Jensen, B.; et el." }, { "id": "https://authors.library.caltech.edu/records/s9e0s-qdx91", "eprint_id": 35246, "eprint_status": "archive", "datestamp": "2023-08-22 06:20:01", "lastmod": "2023-10-20 15:53:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The Chandra COSMOS Survey. III. Optical and Infrared Identification of X-Ray Point Sources", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; surveys; X-rays: galaxies: clusters", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2011 November 18; accepted 2012 May 21; published 2012 August 2.\n\nThe authors thank the referee for the useful suggestions which helped to improve the paper. F.C. thanks R. D'Abrusco, A. Goulding, M. Mignoli, and M. Povic for inspiring discussions and useful comments. This work was supported in part by NASA Chandra grant number GO7-8136A (M.E., F.C., H.H.), the Blancheflor Boncompagni Ludovisi foundation (F.C.), and the Smithsonian Scholarly Studies (F.C.). In Italy this work is supported by ASI/INAF contracts I/009/10/0 and I/088/06 and by PRIN INAF 2010 \"From the dawn of galaxy formation to the peak of themass assembly.\" M.S. acknowledges support by the German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize (FKZ HA 1850/28-1). InMexico, this work has been supported by CONACyT Grant 83564 and UNAM/DGAPA PAPIIT Grant IN110209. This work is also based on observations made with ESO Telescopes at the La Silla or Paranal Observatories under program ID 175.A-0839.\n\nPublished - 0067-0049_201_2_30.pdf
", "abstract": "The Chandra COSMOS Survey (C-COSMOS) is a large, 1.8 Ms, Chandra program that has imaged the central 0.9 deg^2 of the COSMOS field down to limiting depths of 1.9 \u00d7 10^(\u201316) erg cm^(\u20132) s^(\u20131) in the soft (0.5-2 keV) band, 7.3 \u00d7 10^(\u201316) erg cm^(\u20132) s^(\u20131) in the hard (2-10 keV) band, and 5.7 \u00d7 10^(\u201316) erg cm^(\u20132) s^(\u20131) in the full (0.5-10 keV) band. In this paper we report the i, K, and 3.6 \u03bcm identifications of the 1761 X-ray point sources. We use the likelihood ratio technique to derive the association of optical/infrared counterparts for 97% of the X-ray sources. For most of the remaining 3%, the presence of multiple counterparts or the faintness of the possible counterpart prevented a unique association. For only 10 X-ray sources we were not able to associate a counterpart, mostly due to the presence of a very bright field source close by. Only two sources are truly empty fields. The full catalog, including spectroscopic and photometric redshifts and classification described here in detail, is available online. Making use of the large number of X-ray sources, we update the \"classic locus\" of active galactic nuclei (AGNs) defined 20 years ago in soft X-ray surveys and define a new locus containing 90% of the AGNs in the survey with full-band luminosity >10^(42) erg s^(\u20131). We present the linear fit between the total i-band magnitude and the X-ray flux in the soft and hard bands, drawn over two orders of magnitude in X-ray flux, obtained using the combined C-COSMOS and XMM-COSMOS samples. We focus on the X-ray to optical flux ratio (X/O) and we test its known correlation with redshift and luminosity, and a recently introduced anti-correlation with the concentration index (C). We find a strong anti-correlation (though the dispersion is of the order of 0.5 dex) between X/O computed in the hard band and C and that 90% of the obscured AGNs in the sample with morphological information live in galaxies with regular morphology (bulgy and disky/spiral), suggesting that secular processes govern a significant fraction of the black hole growth at X-ray luminosities of 10^(43)-10^(44.5) erg s^(\u20131). We also investigate the degree of obscuration of the sample using the hardness ratio, and we compare the X-ray color with the near-infrared to optical color.", "date": "2012-08", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "201", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 30", "id_number": "CaltechAUTHORS:20121101-142013998", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121101-142013998", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Chandra Grant", "grant_number": "GO7-8136A" }, { "agency": "Blancheflor Boncompagni Ludovisi Foundation" }, { "agency": "Smithsonian Scholarly Studies" }, { "agency": "ASI/INAF", "grant_number": "I/009/10/0" }, { "agency": "ASI/INAF", "grant_number": "I/088/06" }, { "agency": "PRIN INAF 2010" }, { "agency": "DFG Leibniz Prize", "grant_number": "FKZ HA 1850/28-1" }, { "agency": "CONACyT Grant", "grant_number": "83564" }, { "agency": "UNAM/DGAPA PAPIIT Grant", "grant_number": "IN110209" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0067-0049/201/2/30", "primary_object": { "basename": "0067-0049_201_2_30.pdf", "url": "https://authors.library.caltech.edu/records/s9e0s-qdx91/files/0067-0049_201_2_30.pdf" }, "pub_year": "2012", "author_list": "Civano, F.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/my5dk-p7s22", "eprint_id": 32605, "eprint_status": "archive", "datestamp": "2023-08-22 06:09:21", "lastmod": "2023-10-18 14:35:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mitchell-Wynne-K", "name": { "family": "Mitchell-Wynne", "given": "K." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Gong-Y", "name": { "family": "Gong", "given": "Y." } }, { "id": "B\u00e9thermin-Matthieu", "name": { "family": "B\u00e9thermin", "given": "M." }, "orcid": "0000-0002-3915-2015" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Franceschini-A", "name": { "family": "Franceschini", "given": "A." } }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "J." }, "orcid": "0000-0001-7527-2017" }, { "id": "Griffin-M", "name": { "family": "Griffin", "given": "M." } }, { "id": "Halpern-M", "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "id": "Marchetti-L", "name": { "family": "Marchetti", "given": "L." }, "orcid": "0000-0003-3948-7621" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Page-M-J", "name": { "family": "Page", "given": "M. J." }, "orcid": "0000-0002-6689-6271" }, { "id": "P\u00e9rez-Fournon-I", "name": { "family": "P\u00e9rez-Fournon", "given": "I." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "D." }, "orcid": "0000-0002-6878-9840" }, { "id": "Smidt-J", "name": { "family": "Smidt", "given": "J." } }, { "id": "Smith-A", "name": { "family": "Smith", "given": "A." }, "orcid": "0000-0002-1938-4660" }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" }, { "id": "Vigroux-L", "name": { "family": "Vigroux", "given": "L." } }, { "id": "Wang-Lingyu", "name": { "family": "Wang", "given": "L." } }, { "id": "Wardlow-J-L", "name": { "family": "Wardlow", "given": "J. L." }, "orcid": "0000-0003-2376-8971" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: A Statistical Measurement of the Redshift Distribution of Herschel-SPIRE Sources Using the Cross-correlation Technique", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; submillimeter: galaxies", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2012 February 29; accepted 2012 April 24; published 2012 June 11.\n\nSPIRE has been developed by a consortium of institutes led\nby Cardiff University (UK) and including: the University of\nLethbridge (Canada); NAOC (China); CEA, LAM (France);\nIFSI, the University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL, UKATC, the University of Sussex (UK); and Caltech, JPL, NHSC, the University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). The data presented in this paper will be released through the HeDaM Database in Marseille. This work made use of images and/or data products provided by the NOAO Deep Wide-Field Survey, which is supported by the National Optical Astronomy Observatory (NOAO). NOAO is operated by AURA, Inc., under a cooperative agreement with the National Science Foundation. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSSWeb\nsite is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, the Astrophysical Institute Potsdam, the University of Basel, the University of Cambridge, Case Western Reserve University, the University of Chicago, Drexel University, Fermilab,\nthe Institute for Advanced Study, the Japan Participation\nGroup, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, The Ohio State University, the University of Pittsburgh, the University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. K.M.W., Y.G., A.C., J.S., and J.L.W. are supported by NASA funds for U.S. participants in Herschel through an award from JPL. A.C. and Y.G. also acknowledge support from NSF CAREER AST-0645427 (to A.C.) and K.M.W. acknowledges support from a NSF REU supplement. S.O., A.S., and L.W. acknowledge support from the Science and Technology Facilities Council (grant No. ST/F002858/1) and (grant No. ST/I000976/1). A.F., L.M., and M.V. were supported by the Italian Space Agency (ASI Herschel Science Contract I/005/07/0).\n\nPublished - MitchellWynne2012p18928Astrophys_J.pdf
", "abstract": "The wide-area imaging surveys with the Herschel Space Observatory at submillimeter (sub-mm) wavelengths have now resulted in catalogs of the order of one-hundred-thousand dusty, starburst galaxies. These galaxies capture an important phase of galaxy formation and evolution, but, unfortunately, the redshift distribution of these galaxies, N(z), is still mostly uncertain due to limitations associated with counterpart identification at optical wavelengths and spectroscopic follow-up. We make a statistical estimate of N(z) using a clustering analysis of sub-mm galaxies detected at each of 250, 350 and 500 \u03bcm from the Herschel Multi-tiered Extragalactic Survey centered on the Bo\u00f6tes field. We cross-correlate Herschel galaxies against galaxy samples at optical and near-IR wavelengths from the Sloan Digital Sky Survey, the NOAO Deep Wide Field Survey, and the Spitzer Deep Wide Field Survey. We create optical and near-IR galaxy samples based on their photometric or spectroscopic redshift distributions and test the accuracy of those redshift distributions with similar galaxy samples defined with catalogs from the Cosmological Evolution Survey (COSMOS), which has superior spectroscopic coverage. We model the clustering auto- and cross-correlations of Herschel and optical/IR galaxy samples to estimate N(z) and clustering bias factors. The S_(350) > 20 mJy galaxies have a bias factor varying with redshift as b(z) = 1.0^(+1.0)_(\u20130.5)(1 + z)^1.2^(+0.3)_(\u20130.7). This bias and the redshift dependence is broadly in agreement with galaxies that occupy dark matter halos of mass in the range of 1012 to 10^(13) M_\u2609. We find that galaxy selections in all three Spectral and Photometric Imaging Receiver (SPIRE) bands share a similar average redshift, with = 1.8 \u00b1 0.2 for 250 \u03bcm selected samples, and = 1.9 \u00b1 0.2 for both 350 and 500 \u03bcm samples, while their distributions behave differently. For 250 \u03bcm selected galaxies we find the a larger number of sources with z \u2264 1 when compared with the subsequent two SPIRE bands, with 350 and 500 \u03bcm selected SPIRE samples having peaks in N(z) at progressively higher redshifts. We compare our clustering-based N(z) results to sub-mm galaxy model predictions in the literature, and with an estimate of N(z) using a stacking analysis of COSMOS 24 \u03bcm detections.", "date": "2012-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "753", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 23", "id_number": "CaltechAUTHORS:20120720-094749727", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120720-094749727", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" }, { "agency": "JPL" }, { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/005/07/0" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/753/1/23", "primary_object": { "basename": "MitchellWynne2012p18928Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/my5dk-p7s22/files/MitchellWynne2012p18928Astrophys_J.pdf" }, "pub_year": "2012", "author_list": "Mitchell-Wynne, K.; Cooray, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/d5jg7-ygd03", "eprint_id": 31617, "eprint_status": "archive", "datestamp": "2023-08-22 05:37:42", "lastmod": "2023-10-17 18:43:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jullo-E", "name": { "family": "Jullo", "given": "Eric" }, "orcid": "0000-0002-9253-053X" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" }, { "id": "Kiessling-A", "name": { "family": "Kiessling", "given": "Alina" } }, { "id": "Taylor-J-E", "name": { "family": "Taylor", "given": "James E." } }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "Richard" }, "orcid": "0000-0002-6085-3780" }, { "id": "Berg\u00e9-J", "name": { "family": "Berg\u00e9", "given": "Joel" } }, { "id": "Schimd-C", "name": { "family": "Schimd", "given": "Carlo" } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "Jean-Paul" }, "orcid": "0000-0002-4616-4989" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" } ] }, "title": "COSMOS: Stochastic Bias from Measurements of Weak Lensing and Galaxy Clustering", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; gravitational lensing: weak; large-scale structure of universe", "note": "\u00a9 2012 American Astronomical Society. Received 2011 March 25; accepted 2012 February 22; published 2012 April 13. We thank the referee for his insightful comments that led to\na significant improvement of the paper. It is also a pleasure to\nthank Chris Hirata and Fabian Schmidt for useful discussions\nand helpful suggestions. We also gratefully thank Alexie Leauthaud for her help and advice and for providing the COSMOS\nlensing catalog. This work was done in part at JPL, operated\nby Caltech under a contract for NASA. E.J. acknowledges support\nfrom the Jet Propulsion Laboratory, in contract with the\nCalifornia Institute of Technology, and the NASA Postdoctoral\nProgram. R.M. is supported by an STFC Advanced Fellowship.\nThis work uses observations obtained with the Hubble Space\nTelescope. The HST COSMOS Treasury program was supported\nthrough NASA grant HST-GO-09822. It is also a pleasure to thank Chris Hirata, Fabian Schmidt and Christopher Bonnett for useful discussions and helpful suggestions. Support for Program No. HST-AR-12136.01-A was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.\n\nPublished - Jullo2012p18207Astrophys_J.pdf
", "abstract": "In the theory of structure formation, galaxies are biased tracers of the underlying matter density field. The statistical relation between galaxy and matter density field is commonly referred to as galaxy bias. In this paper, we test the linear bias model with weak-lensing and galaxy clustering measurements in the 2 deg^2 COSMOS field. We estimate the bias of galaxies between redshifts z = 0.2 and z = 1 and over correlation scales between R = 0.2 h^(\u20131) Mpc and R = 15 h^(\u20131) Mpc. We focus on three galaxy samples, selected in flux (simultaneous cuts I_(814W) < 26.5 and K_s < 24) and in stellar mass (10^9 < M_* < 10^(10) h^(\u20132) M_\u2609 and 10^(10) < M_* < 10^(11) h^(\u20132) M_\u2609). At scales R > 2 h^(\u20131) Mpc, our measurements support a model of bias increasing with redshift. The Tinker et al. fitting function provides a good fit to the data. We find the best-fit mass of the galaxy halos to be log (M_(200)/h^(\u20131) M_\u2609) = 11.7^(+0.6)_(\u20131.3) and log (M_(200)/h^(\u20131) M_\u2609) = 12.4^(+0.2)_(\u20132.9), respectively, for the low and high stellar-mass samples. In the halo model framework, bias is scale dependent with a change of slope at the transition scale between the one and the two halo terms. We detect a scale dependence of bias with a turndown at scale R = 2.3 \u00b1 1.5 h^(\u20131) Mpc, in agreement with previous galaxy clustering studies. We find no significant amount of stochasticity, suggesting that a linear bias model is sufficient to describe our data. We use N-body simulations to quantify both the amount of cosmic variance and systematic errors in the measurement.", "date": "2012-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "750", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 37", "id_number": "CaltechAUTHORS:20120523-113027587", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120523-113027587", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/750/1/37", "primary_object": { "basename": "Jullo2012p18207Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/d5jg7-ygd03/files/Jullo2012p18207Astrophys_J.pdf" }, "pub_year": "2012", "author_list": "Jullo, Eric; Rhodes, Jason; et el." }, { "id": "https://authors.library.caltech.edu/records/fz4ec-tnd19", "eprint_id": 31827, "eprint_status": "archive", "datestamp": "2023-08-22 05:34:10", "lastmod": "2023-10-17 21:22:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Navarrete-F", "name": { "family": "Navarrete", "given": "F." } }, { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "M. S." }, "orcid": "0000-0001-7095-7543" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Diener-C", "name": { "family": "Diener", "given": "C." } }, { "id": "Aretxaga-I", "name": { "family": "Aretxaga", "given": "I." }, "orcid": "0000-0002-6590-3994" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D. A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "D." } }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G." }, "orcid": "0000-0002-6572-7089" } ] }, "title": "Quest for COSMOS Submillimeter Galaxy Counterparts using CARMA and VLA: Identifying Three High-redshift Starburst Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: distances and redshifts; galaxies: high-redshift; galaxies: starburst; submillimeter: galaxies", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2011 May 10; accepted 2012 March 21; published 2012 May 4.\n\nThe authors thank the anonymous referee for comments\nthat significantly improved the manuscript. The research leading to these results has received funding from the European Union's Seventh Framework programme under grant agreement 229517. M.S. acknowledges support by the German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize (FKZ HA\n1850/28-1). A.K. acknowledges support by the DFG grant\nSCHI 536/3-3 as part of the Priority Programme 1177 (Witnesses of Cosmic History: Formation and Evolution of Black Holes, Galaxies and their Environment). Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities.\n\nPublished - Smolcic2012p18390Astrophys_J_Suppl_S.pdf
", "abstract": "We report on interferometric observations at 1.3 mm at 2\"-3\" resolution using the Combined Array for Research in Millimeter-wave Astronomy. We identify multi-wavelength counterparts of three submillimeter galaxies (SMGs; F_(1mm) > 5.5 mJy) in the COSMOS field, initially detected with MAMBO and AzTEC bolometers at low, ~10\"-30\", resolution. All three sources\u2014AzTEC/C1, Cosbo-3, and Cosbo-8\u2014are identified to coincide with positions of 20 cm radio sources. Cosbo-3, however, is not associated with the most likely radio counterpart, closest to the MAMBO source position, but with that farther away from it. This illustrates the need for intermediate-resolution (~2\") mm-observations to identify the correct counterparts of single-dish-detected SMGs. All of our three sources become prominent only at NIR wavelengths, and their mm-to-radio flux based redshifts suggest that they lie at redshifts z \u2273 2. As a proof of concept, we show that photometric redshifts can be well determined for SMGs, and we find photometric redshifts of 5.6 \u00b1 1.2, 1.9^(+0.9)_(\u20130.5), and ~4 for AzTEC/C1, Cosbo-3, and Cosbo-8, respectively. Using these we infer that these galaxies have radio-based star formation rates of \u2273 1000 M_\u2609 yr^(\u20131) and IR luminosities of ~10^(13) L_\u2609 consistent with properties of high-redshift SMGs. In summary, our sources reflect a variety of SMG properties in terms of redshift and clustering, consistent with the framework that SMGs are progenitors of z ~ 2 and today's passive galaxies.", "date": "2012-05", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "200", "number": "1", "publisher": "American Astronomical Society", "pagerange": "10", "id_number": "CaltechAUTHORS:20120606-132340653", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120606-132340653", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "229517" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "FKZ HA 1850/28-1" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "SCHI 536/3-3" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0067-0049/200/1/10", "primary_object": { "basename": "Smolcic2012p18390Astrophys_J_Suppl_S.pdf", "url": "https://authors.library.caltech.edu/records/fz4ec-tnd19/files/Smolcic2012p18390Astrophys_J_Suppl_S.pdf" }, "pub_year": "2012", "author_list": "Smol\u010di\u0107, V.; Navarrete, F.; et el." }, { "id": "https://authors.library.caltech.edu/records/n917n-0p936", "eprint_id": 31760, "eprint_status": "archive", "datestamp": "2023-08-22 05:33:35", "lastmod": "2023-10-17 21:07:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Griffith-R-L", "name": { "family": "Griffith", "given": "Roger L." } }, { "id": "Cooper-M-C", "name": { "family": "Cooper", "given": "Michael C." }, "orcid": "0000-0003-1371-6019" }, { "id": "Newman-J-A", "name": { "family": "Newman", "given": "Jeffrey A." }, "orcid": "0000-0001-8684-2222" }, { "id": "Moustakas-L-A", "name": { "family": "Moustakas", "given": "Leonidas A." }, "orcid": "0000-0003-3030-2360" }, { "id": "Stern-D", "name": { "family": "Stern", "given": "Daniel" }, "orcid": "0000-0003-2686-9241" }, { "id": "Comerford-J-M", "name": { "family": "Comerford", "given": "Julia M." }, "orcid": "0000-0001-8627-4907" }, { "id": "Davis-M-E-Astro", "name": { "family": "Davis", "given": "Marc" } }, { "id": "Lotz-J-M", "name": { "family": "Lotz", "given": "Jennifer M." }, "orcid": "0000-0003-3130-5643" }, { "id": "Barden-M", "name": { "family": "Barden", "given": "Marco" } }, { "id": "Conselice-C-J", "name": { "family": "Conselice", "given": "Christopher J." }, "orcid": "0000-0003-1949-7638" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Faber-S-M", "name": { "family": "Faber", "given": "S. M." }, "orcid": "0000-0003-4996-214X" }, { "id": "Kirkpatrick-J-D", "name": { "family": "Kirkpatrick", "given": "J. Davy" }, "orcid": "0000-0003-4269-260X" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Koo-David-C", "name": { "family": "Koo", "given": "David C." }, "orcid": "0000-0003-3385-6799" }, { "id": "Noeske-K-G", "name": { "family": "Noeske", "given": "Kai G." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "Patrick" } }, { "id": "Willmer-C-N-A", "name": { "family": "Willmer", "given": "Christopher N. A." } }, { "id": "Weiner-B-J", "name": { "family": "Weiner", "given": "Benjamin" } } ] }, "title": "The Advanced Camera for Surveys General Catalog: Structural Parameters for Approximately Half a Million Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: evolution; galaxies: photometry; galaxies: structure; surveys", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2012 February 10; accepted 2012 March 7; published 2012 May 4. \n\nWe gratefully acknowledge the principal investigators responsible for the ACS imaging utilized by the ACS-GC. We also acknowledge the GEMS team for creating and sharing the Galapagos code, without which none of this would have been possible. Work on this paper was carried out at the Jet Propulsion Laboratory and Infrared Processing and Analysis Center (IPAC), California Institute of Technology, under contract with NASA and WISE. J.M.C. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1102525. We thank the anonymous referee for his/her useful suggestions, which have improved this manuscript. This work is based on (GO-10134, GO-09822, GO-09425.01, GO-09583.01, GO-9500) program observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Work on this paper is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada\u2013France\u2013Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada\u2013France\u2013Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Funding for the DEEP2 Galaxy Redshift Survey has been provided in part by NSF grant AST00-71048 and NASA LTSA grant NNG04GC89G. This work is also based on zCOSMOS observations carried out using the Very Large Telescope at the ESO Paranal Observatory under Program ID: LP175.A-0839. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration.\n\nPublished - Griffith2012p18389Astrophys_J_Suppl_S.pdf
Submitted - 1203.1651.pdf
", "abstract": "We present the Advanced Camera for Surveys General Catalog (ACS-GC), a photometric and morphological database using publicly available data obtained with the Advanced Camera for Surveys (ACS) instrument on the Hubble Space Telescope. The goal of the ACS-GC database is to provide a large statistical sample of galaxies with reliable structural and distance measurements to probe the evolution of galaxies over a wide range of look-back times. The ACS-GC includes approximately 470,000 astronomical sources (stars + galaxies) derived from the AEGIS, COSMOS, GEMS, and GOODS surveys. GALAPAGOS was used to construct photometric (SEXTRACTOR) and morphological (GALFIT) catalogs. The analysis assumes a single S\u00e9rsic model for each object to derive quantitative structural parameters. We include publicly available redshifts from the DEEP2, COMBO-17, TKRS, PEARS, ACES, CFHTLS, and zCOSMOS surveys to supply redshifts (spectroscopic and photometric) for a considerable fraction (~74%) of the imaging sample. The ACS-GC includes color postage stamps, GALFIT residual images, and photometry, structural parameters, and redshifts combined into a single catalog.", "date": "2012-05", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "200", "number": "1", "publisher": "American Astronomical Society", "pagerange": "9", "id_number": "CaltechAUTHORS:20120531-162211374", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120531-162211374", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Astronomy and Astrophysics Fellowship", "grant_number": "AST-1102525" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0067-0049/200/1/9", "primary_object": { "basename": "1203.1651.pdf", "url": "https://authors.library.caltech.edu/records/n917n-0p936/files/1203.1651.pdf" }, "related_objects": [ { "basename": "Griffith2012p18389Astrophys_J_Suppl_S.pdf", "url": "https://authors.library.caltech.edu/records/n917n-0p936/files/Griffith2012p18389Astrophys_J_Suppl_S.pdf" } ], "pub_year": "2012", "author_list": "Griffith, Roger L.; Cooper, Michael C.; et el." }, { "id": "https://authors.library.caltech.edu/records/36503-wt814", "eprint_id": 31333, "eprint_status": "archive", "datestamp": "2023-08-22 05:24:43", "lastmod": "2023-10-17 16:04:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Donley-J-L", "name": { "family": "Donley", "given": "J. L." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Cardamone-C-N", "name": { "family": "Cardamone", "given": "C. N." } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C. D." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Miyaji-Takamitsu", "name": { "family": "Miyaji", "given": "T." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J. R." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } } ] }, "title": "Identifying Luminous Active Galactic Nuclei in Deep Surveys: Revised IRAC Selection Criteria", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; infrared: galaxies; X-rays: galaxies", "note": "\u00a9 2012 American Astronomical Society. Received 2011 August 4; accepted 2012 January 18; published 2012 March 16. We thank Ranga Chary, Harry Ferguson, Joanna Kuraszkiewicz, Mark Lacy, Daniel Stern, Belinda Wilkes, Steve Willner, and the anonymous referee for helpful discussions and comments that improved this paper. J.L.D. is supported by the Giacconi Fellowship at STScI. This work is partially supported by CONACyT Apoyo 83564, DGAPA UNAM Grant PAPIIT IN110209, and NASA ADP Grant NNX07AT02G.\n\nPublished - Donley2012p18031Astrophys_J.pdf
", "abstract": "Spitzer/IRAC selection is a powerful tool for identifying luminous active galactic nuclei (AGNs). For deep IRAC data, however, the AGN selection wedges currently in use are heavily contaminated by star-forming galaxies, especially at high redshift. Using the large samples of luminous AGNs and high-redshift star-forming galaxies in COSMOS, we redefine the AGN selection criteria for use in deep IRAC surveys. The new IRAC criteria are designed to be both highly complete and reliable, and incorporate the best aspects of the current AGN selection wedges and of infrared power-law selection while excluding high-redshift star-forming galaxies selected via the BzK, distant red galaxy, Lyman-break galaxy, and submillimeter galaxy criteria. At QSO luminosities of log L_(2-10keV)(erg s^(\u20131)) \u226544, the new IRAC criteria recover 75% of the hard X-ray and IRAC-detected XMM-COSMOS sample, yet only 38% of the IRAC AGN candidates have X-ray counterparts, a fraction that rises to 52% in regions with Chandra exposures of 50-160 ks. X-ray stacking of the individually X-ray non-detected AGN candidates leads to a hard X-ray signal indicative of heavily obscured to mildly Compton-thick obscuration (log N H (cm^(\u20132)) = 23.5 \u00b1 0.4). While IRAC selection recovers a substantial fraction of luminous unobscured and obscured AGNs, it is incomplete to low-luminosity and host-dominated AGNs.", "date": "2012-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "748", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 142", "id_number": "CaltechAUTHORS:20120507-113750592", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120507-113750592", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "CONACyT", "grant_number": "Apoyo 83564" }, { "agency": "DGAPA UNAM Grant", "grant_number": "PAPIIT IN110209" }, { "agency": "NASA", "grant_number": "NNX07AT02G" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/748/2/142", "primary_object": { "basename": "Donley2012p18031Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/36503-wt814/files/Donley2012p18031Astrophys_J.pdf" }, "pub_year": "2012", "author_list": "Donley, J. L.; Koekemoer, A. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/5jz6b-fqg93", "eprint_id": 31511, "eprint_status": "archive", "datestamp": "2023-08-22 05:20:12", "lastmod": "2023-10-17 16:38:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Taylor-J-E", "name": { "family": "Taylor", "given": "James E." } }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "Richard J." }, "orcid": "0000-0002-6085-3780" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "George-M-R", "name": { "family": "George", "given": "Matthew R." } }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" }, { "id": "Kitching-T-D", "name": { "family": "Kitching", "given": "Thomas D." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard" }, "orcid": "0000-0001-7782-7071" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "Alexis" }, "orcid": "0000-0002-4606-5403" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Jullo-E", "name": { "family": "Jullo", "given": "Eric" }, "orcid": "0000-0002-9253-053X" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "Jean-Paul" }, "orcid": "0000-0002-4616-4989" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "Masayuki" }, "orcid": "0000-0002-5011-5178" } ] }, "title": "Measuring the Geometry of the Universe from Weak Gravitational Lensing behind Galaxy Groups in the HST COSMOS Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; dark energy; distance scale; galaxies: groups: general; gravitational lensing: weak; large-scale structure of Universe", "note": "\u00a9 2012 The American Astronomical Society. Received 2011 July 29; accepted 2012 February 10; published 2012 March 30.\nBased on observations with the NASA/ESA Hubble Space Telescope obtained at the Space Telescope Science Institute, which is operated by AURA Inc. under the NASA contract NAS 5-26555; the Subaru Telescope, which is\noperated by the National Astronomical Observatory of Japan; the European Southern Observatory under the Large Program 175.A-0839, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the\nNational Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. The authors gratefully acknowledge helpful discussions with Niayesh Afshordi, Hendrik Hildebrandt, Mike Hudson, Fabian\nSchmidt, and Kris Sigurdson. J.E.T. is supported by a NSERC\nCanada Discovery Grant. R.M. is supported by STFC Advanced\nFellowship PP/E006450/1 and ERC grant MIRG-CT-208994.\nA.L. acknowledges support from the Chamberlain Fellowship\nat LBNL and from the Berkeley Center for Cosmological\nPhysics. The work of J.R. was carried out at the Jet Propulsion\nLaboratory, California Institute of Technology, under a contract\nwith NASA. T.K. was supported by a RAS 2010 Fellowship.\nThis work was supported by the World Premier International\nResearch Center Initiative (WPI Initiative), MEXT, Japan.\nThe HST COSMOS Treasury program was supported through\nthe NASA grant HST-GO-09822. We thank Tony Roman,\nDenise Taylor, and David Soderblom for their assistance in\nplanning and scheduling of the extensive COSMOS observations.\nWe gratefully acknowledge the contributions of the entire\nCOSMOS collaboration consisting of more than 70 scientists.\nMore information on the COSMOS survey is available\nat http://cosmos.astro.caltech.edu. It is also a pleasure\nthe acknowledge the excellent services provided by the NASA\nIPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server\ncapabilities for the COSMOS data sets.\n\nPublished - Taylor2012p18124Astrophys_J.pdf
", "abstract": "Gravitational lensing can provide pure geometric tests of the structure of spacetime, for instance by determining empirically the angular diameter distance-redshift relation. This geometric test has been demonstrated several times using massive clusters which produce a large lensing signal. In this case, matter at a single redshift dominates the lensing signal, so the analysis is straightforward. It is less clear how weaker signals from multiple sources at different redshifts can be stacked to demonstrate the geometric dependence. We introduce a simple measure of relative shear which for flat cosmologies separates the effect of lens and source positions into multiplicative terms, allowing signals from many different source-lens pairs to be combined. Applying this technique to a sample of groups and low-mass clusters in the COSMOS survey, we detect a clear variation of shear with distance behind the lens. This represents the first detection of the geometric effect using weak lensing by multiple, low-mass groups. The variation of distance with redshift is measured with sufficient precision to constrain the equation of state of the universe under the assumption of flatness, equivalent to a detection of a dark energy component \u03a9_ X at greater than 99% confidence for an equation-of-state parameter \u20132.5 \u2264 w \u2264 \u20130.1. For the case w = \u20131, we find a value for the cosmological constant density parameter \u03a9_\u039b = 0.85^(+0.044)_( \u20130.19) (68% CL) and detect cosmic acceleration (q_0 < 0) at the 98% CL. We consider the systematic uncertainties associated with this technique and discuss the prospects for applying it in forthcoming weak-lensing surveys.", "date": "2012-04", "date_type": "published", "publication": "Astrophysical Journal", "volume": "749", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 127", "id_number": "CaltechAUTHORS:20120517-073443267", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120517-073443267", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "PP/E006450/1" }, { "agency": "European Research Council (ERC)", "grant_number": "MIRG-CT-208994" }, { "agency": "Lawrence Berkeley National Laboratory" }, { "agency": "Berkeley Center for Cosmological Physics" }, { "agency": "Royal Astronomical Society" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "NASA", "grant_number": "HST-GO-09822" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/749/2/127", "primary_object": { "basename": "Taylor2012p18124Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/5jz6b-fqg93/files/Taylor2012p18124Astrophys_J.pdf" }, "pub_year": "2012", "author_list": "Taylor, James E.; Massey, Richard J.; et el." }, { "id": "https://authors.library.caltech.edu/records/kv4az-93t74", "eprint_id": 31682, "eprint_status": "archive", "datestamp": "2023-08-22 05:21:16", "lastmod": "2023-10-17 18:46:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pierini-D", "name": { "family": "Pierini", "given": "D." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" } ] }, "title": "First simultaneous optical/near-infrared imaging of an X-ray selected, high-redshift cluster of galaxies with GROND:\n The galaxy population of XMMU\u2009J0338.7 + 0030 at z = 1.1", "ispublished": "pub", "full_text_status": "public", "keywords": "X-rays: galaxies: clusters; galaxies: distances and redshifts; galaxies: clusters: general; galaxies: high-redshift", "note": "\u00a9 2012 ESO. Article published by EDP Sciences. \n\nReceived 8 February 2011; Accepted 13 December 2011.\nPublished online 23 March 2012.\nD.P. thanks the anonymous referee for her/his insightful\ncomments, which led to a signficant improvement on the robustness and presentation quality of the results in the final version of the paper. This research was supported by the DFG cluster of excellence \"Origin and Structure of the\nUniverse\" (http://www.universe-cluster.de) through EXC project number 153, the DFG under grants Schw 536/24-1, Schw 536/24-2, BO 702/16-3, and the DLR under grants 50 OR 0405 and 50 QR 0802. R.S. acknowledges support by the DFG in the program SPP 1177. H.Q. thanks the FONDAP Centro\nde Astrof\u00edsica for partial support. F.Z. acknowledges support from and participation in the International Max-Plank Research School on Astrophysics at the\nLudwig-Maximilians University. D.P. acknowledges useful feedback from O. Ilbert. D.P. acknowledges the kind hospitality at the Max-Planck-Institut f\u00fcr extraterrestrische Physik (MPE). This research has made use of observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere (ESO), Chile (079.A\u22120634). This research has made use of observations collected at the Centro Astron\u00f3mico Hispano Alem\u00e1n (CAHA) at Calar Alto, Spain operated jointly by the Max-Planck-Institut f\u00fcr Astronomie and the Istituto de Astrof\u00edsica de Andaluc\u00eda (CSIC). This work has made use\nof the SDSS database. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSSWeb\nSite is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute\nPotsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University,\nthe Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-\nInstitute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States\nNaval Observatory, and the University of Washington. This publication makes use of data products from the TwoMicron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis\nCenter/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the NASA/IPAC Extragalactic Data base (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nPublished - Pierini2012p18293Astron_Astrophys.pdf
", "abstract": "Context. The XMM-Newton Distant Cluster Project is a serendipitous survey for clusters of galaxies at redshifts z \u2265 0.8 based on deep archival XMM-Newton observations. X-ray sources identified as extended are screened against existing optical all-sky surveys for galaxies, in case of candidate high-z clusters followed up with imaging at 4 m-class telescopes and, ultimately, multi-object spectroscopy at 8 m-class telescopes. Low-significance candidate high-z clusters are followed up with the seven-channel imager GROND (Gamma-Ray Burst Optical and Near-Infrared Detector) that is mounted at a 2 m-class telescope. Its unique capability of simultaneous imaging in the g\u2032,r\u2032,i\u2032,z\u2032,J,H,Ks bands enables the use of the photometric redshift technique.\n\nAims. Observing strategy, data reduction and analysis, depth and accuracy of the simultaneous multi-wavelength photometry are discussed with the goal of establishing GROND as a useful instrument to confirm X-ray selected (high-z) clusters.\n\nMethods. The test case is XMMU\u2009J0338.7 + 0030, suggested to be at z ~ 1.45 \u00b1 0.15 (1\u03c3) from the analysis of the z \u2212 H vs. H colour \u2212 magnitude diagram obtained from the follow-up imaging. Later VLT-FORS2 spectroscopy enabled us to identify four members, which set this cluster at z = 1.097 \u00b1 0.002 (1\u03c3). To reach a better knowledge of its galaxy population, we observed XMMU\u2009J0338.7 + 0030 with GROND for about 6 h. The publicly available photo-z code le Phare was used.\n\nResults. The Ks-band number counts of the non-stellar sources out of the 832 detected down to z\u2032 ~ 26 AB mag (1\u03c3) in the 3.9 \u00d7 4.3 arcmin^2 region of XMMU\u2009J0338.7 + 0030 imaged at all GROND bands clearly exceed those computed in deep fields/survey areas at ~20.5\u201322.5 AB mag. The photo-z's of the three imaged spectroscopic members yield z = 1.12 \u00b1 0.09 (1\u03c3). The spatial distribution and the properties of the GROND sources with a photo-z in the range 1.01\u20131.23 confirm the correspondence of the X-ray source with a galaxy over-density at a significance of at least 4.3\u03c3. Candidate members that are spectro-photometrically classified as elliptical galaxies define a red locus in the i\u2032 \u2212 z\u2032 vs. z\u2032 colour \u2212 magnitude diagram that is consistent with the red sequence of the cluster RDCS\u2009J0910 + 5422 at z = 1.106. XMMU\u2009J0338.7 + 0030 hosts also a population of bluer late-type spirals and irregulars. The starbursts among the photometric members populate both loci, consistently with previous results.\n\nConclusions. The analysis of the available data set indicates that XMMU\u2009J0338.7 + 0030 is a low-mass cluster (M_200 ~ 10^(14) M_\u2299) at z = 1.1. With the photometric accuracy yielded by the present unoptimized multi-band observations with GROND, we not only confirm the spectroscopic redshift of this cluster but also show that it hosts a galaxy population that can still undergo significant bursts of star-formation activity.", "date": "2012-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "540", "publisher": "EDP Sciences", "pagerange": "A45", "id_number": "CaltechAUTHORS:20120529-141413485", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120529-141413485", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "DFG Cluster of Excellence EXC Project", "grant_number": "153" }, { "agency": "DFG", "grant_number": "Schw 536/24-1" }, { "agency": "DFG", "grant_number": "Schw 536/24-2" }, { "agency": "DFG", "grant_number": "BO 702/16-3" }, { "agency": "DLR", "grant_number": "50 OR 0405" }, { "agency": "DLR", "grant_number": "50 QR 0802" }, { "agency": "DFG", "grant_number": "SPP 1177" }, { "agency": "FONDAP Centro de Astrof\u00edsica" }, { "agency": "International Max-Plank Research School on Astrophysics" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201116674", "primary_object": { "basename": "Pierini2012p18293Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/kv4az-93t74/files/Pierini2012p18293Astron_Astrophys.pdf" }, "pub_year": "2012", "author_list": "Pierini, D. and Salvato, M." }, { "id": "https://authors.library.caltech.edu/records/cnvkm-vaw08", "eprint_id": 31442, "eprint_status": "archive", "datestamp": "2023-08-22 05:11:47", "lastmod": "2023-10-17 16:35:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Li-I-hui", "name": { "family": "Li", "given": "I. H." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted" } } ] }, "title": "The WiggleZ Dark Energy Survey: Galaxy Evolution at 0.25 \u2264 z \u2264 0.75 Using the Second Red-Sequence Cluster Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: luminosity function, mass function; galaxies: photometry", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2011 April 20; accepted 2012 January 3; published 2012 February 17.\n\nThe RCS2 data in this paper are based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT\nand CEA/DAPNIA, at the Canada\u2013France\u2013Hawaii Telescope\n(CFHT) which is operated by the National Research Council\n(NRC) of Canada, the Institute National des Sciences de\nl'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. I.H.L. thanks the Australian Research Council Linkage International Grant for the early development of this work. I.H.L. and H.K.C.Y. thank the Academia Sinica Institute of Astronomy and Astrophysics, Taiwan, for their hospitality during the early stage of the writing of the paper. The RCS and the research of H.K.C.Y. are supported by grants from the Natural Science and Engineering Research Council of Canada and the Canada Research Chair program. TheWiggleZ team acknowledges financial support from the Australian Research Council through Discovery Project grants. The WiggleZ survey would not have been possible without the dedicated work of the staff of the Anglo-Australian Observatory in the development and support of the AAOmega spectrograph, and the running of the AAT.\n\nPublished - Li2012p18104Astrophys_J.pdf
", "abstract": "We study the evolution of galaxy populations around the spectroscopic WiggleZ sample of star-forming galaxies at 0.25 \u2264 z \u2264 0.75 using the photometric catalog from the Second Red-Sequence Cluster Survey (RCS2). We probe the optical photometric properties of the net excess neighbor galaxies. The key concept is that the marker galaxies and their neighbors are located at the same redshift, providing a sample of galaxies representing a complete census of galaxies in the neighborhood of star-forming galaxies. The results are compared with those using the RCS WiggleZ Spare-Fibre (RCS-WSF) sample as markers, representing galaxies in cluster environments at 0.25 \u2264 z \u2264 0.45. By analyzing the stacked color-color properties of the WiggleZ neighbor galaxies, we find that their optical colors are not a strong function of indicators of star-forming activities such as EW([O II]) or Galaxy Evolution Explorer (GALEX) near-UV luminosity of the markers. The galaxies around the WiggleZ markers exhibit a bimodal distribution on the color-magnitude diagram, with most of them located in the blue cloud. The optical galaxy luminosity functions (GLFs) of the blue neighbor galaxies have a faint-end slope \u03b1 of ~ \u20131.3, similar to that for galaxies in cluster environments drawn from the RCS-WSF sample. The faint-end slope of the GLF for the red neighbors, however, is ~ \u20130.4, significantly shallower than the ~ \u20130.7 found for those in cluster environments. This suggests that the buildup of the faint end of the red sequence in cluster environments is in a significantly more advanced stage than that in the star-forming and lower galaxy density WiggleZ neighborhoods. We find that the red galaxy fraction (f_red) around the star-forming WiggleZ galaxies has similar values from z ~ 0.3 to z ~ 0.6 with f_red ~ 0.28, but drops to f_red ~ 0.20 at z gsim 0.7. This change of f_red with redshift suggests that there is either a higher rate of star-forming galaxies entering the luminosity-limited sample at z \u2273 0.7, or a decrease in the quenching rate of star formation at that redshift. Comparing to that in a dense cluster environment, the f_red of the WiggleZ neighbors is both considerably smaller and has a more moderate change with redshift, pointing to the stronger and more prevalent environmental influences on galaxy evolution in high-density regions.", "date": "2012-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "747", "number": "2", "publisher": "American Astronomical Society", "pagerange": "91", "id_number": "CaltechAUTHORS:20120511-155437070", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120511-155437070", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council Linkage International Grant" }, { "agency": "Academia Sinica Institute of Astronomy and Astrophysics (Taiwan)" }, { "agency": "Natural Science and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canada Research Chair program" }, { "agency": "Australian Research Council Discovery Project grants" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "COSMOS" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/747/2/91", "primary_object": { "basename": "Li2012p18104Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/cnvkm-vaw08/files/Li2012p18104Astrophys_J.pdf" }, "pub_year": "2012", "author_list": "Li, I. H.; Forster, Karl; et el." }, { "id": "https://authors.library.caltech.edu/records/v9mce-9qr27", "eprint_id": 31518, "eprint_status": "archive", "datestamp": "2023-08-22 05:12:16", "lastmod": "2023-10-17 16:38:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. Kevin" }, "orcid": "0000-0002-1588-6700" }, { "id": "Zhao-Yinghe", "name": { "family": "Zhao", "given": "Yinghe" }, "orcid": "0000-0002-9128-818X" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Drory-N", "name": { "family": "Drory", "given": "N." } }, { "id": "Gao-Yu", "name": { "family": "Gao", "given": "Y." }, "orcid": "0000-0003-0007-2197" } ] }, "title": "Major-merger Galaxy Pairs in the COSMOS Field \u2014 Mass-dependent Merger Rate Evolution since z = 1", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: general; galaxies: interactions; galaxies: starburst", "note": "\u00a9 2012 American Astronomical Society. Received 2011 September 7; accepted 2011 November 22; published 2012 February 16. \nThis work is based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555; and the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407; also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory under Large Program 175.A-0839, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; and the Canada\u2013France\u2013Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the NRC and CADC of Canada, the CNRS of France, TERAPIX and the University of Hawaii. C.K.X. acknowledges Kevin Bundy for constructive discussions and Alexie Leauthaud for help in analyzing the COSMOS HST-ACS lensing catalog. Zara Scoville is thanked for proofing the English of the manuscript. Y.Z. and Y.G. are grateful for the financial support from the NSF of China (grant Nos. 10833006 and 10903029). Y.Z. thanks IPAC for the hospitality and the financial support during his visit.\n\nPublished - Xu2012p18097Astrophys_J.pdf
", "abstract": "We present results of a statistical study of the cosmic evolution of the mass-dependent major-merger rate since z = 1. A stellar mass limited sample of close major-merger pairs (the CPAIR sample) was selected from the archive of the COSMOS survey. Pair fractions at different redshifts derived using the CPAIR sample and a local K-band-selected pair sample show no significant variations with stellar mass. The pair fraction exhibits moderately strong cosmic evolution, with the best-fitting function of f_(pair) = 10^(\u20131.88(\u00b1 0.03))(1 + z)^(2.2(\u00b1 0.2)). The best-fitting function for the merger rate is R_(mg) (Gyr^(\u20131)) = 0.053 \u00d7 (M_(star)/10^(10.7) M_\u2609 )^(0.3)(1 + z)^(2.2)/(1 + z/8). This rate implies that galaxies of M_(star) ~ 10^(10)-10^(11.5) M_\u2609 have undergone ~0.5-1.5 major mergers since z = 1. Our results show that, for massive galaxies (M_(star) \u2265 10^(10.5) M_\u2609) at z \u2264 1, major mergers involving star-forming galaxies (i.e., wet and mixed mergers) can account for the formation of both ellipticals and red quiescent galaxies (RQGs). On the other hand, major mergers cannot be responsible for the formation of most low mass ellipticals and RQGs of M_(star) \u227e 10^(10.3) M_\u2609. Our quantitative estimates indicate that major mergers have significant impact on the stellar mass assembly of the most massive galaxies (M_(star) \u2265 10^(11.3) M_\u2609), but for less massive galaxies the stellar mass assembly is dominated by the star formation. Comparison with the mass-dependent (ultra)luminous infrared galaxies ((U)LIRG) rates suggests that the frequency of major-merger events is comparable to or higher than that of (U)LIRGs.", "date": "2012-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "747", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 85", "id_number": "CaltechAUTHORS:20120517-084655672", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120517-084655672", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NASA", "grant_number": "1407" }, { "agency": "ESA Member States" }, { "agency": "European Southern Observatory (ESO)", "grant_number": "175.A-0839" }, { "agency": "Kitt Peak National Observatory" }, { "agency": "Cerro Tololo Inter-American Observatory" }, { "agency": "National Optical Astronomy Observatory (NOAO)" }, { "agency": "NSF" }, { "agency": "National Radio Astronomy Observatory" }, { "agency": "Associated Universities, Inc." }, { "agency": "Canada France Hawaii Telescope" }, { "agency": "CEA/DAPNIA (France)" }, { "agency": "NRC and CADC (Canada)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "TERAPIX" }, { "agency": "University of Hawaii" }, { "agency": "National Natural Science Foundation of China", "grant_number": "10833006" }, { "agency": "National Natural Science Foundation of China", "grant_number": "10903029" }, { "agency": "Infrared Processing and Analysis Center (IPAC)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/747/2/85", "primary_object": { "basename": "Xu2012p18097Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/v9mce-9qr27/files/Xu2012p18097Astrophys_J.pdf" }, "pub_year": "2012", "author_list": "Xu, C. Kevin; Zhao, Yinghe; et el." }, { "id": "https://authors.library.caltech.edu/records/v2wgn-z7a58", "eprint_id": 31449, "eprint_status": "archive", "datestamp": "2023-08-22 05:11:53", "lastmod": "2023-10-17 16:35:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jee-M-James", "name": { "family": "Jee", "given": "M. J." } }, { "id": "Mahdavi-A", "name": { "family": "Mahdavi", "given": "A." }, "orcid": "0000-0002-8111-3343" }, { "id": "Hoekstra-H", "name": { "family": "Hoekstra", "given": "H." } }, { "id": "Babul-A", "name": { "family": "Babul", "given": "A." }, "orcid": "0000-0003-1746-9529" }, { "id": "Dalcanton-J-J", "name": { "family": "Dalcanton", "given": "J. J." } }, { "id": "Carroll-P-B", "name": { "family": "Carroll", "given": "P." }, "orcid": "0000-0002-3191-5401" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "A Study of the Dark Core in A520 with the Hubble Space Telescope: The Mystery Deepens", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; dark matter; galaxies: clusters: individual (A520); galaxies: high-redshift; gravitational lensing: weak; X-rays: galaxies: clusters", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2011 September 16; accepted 2011 December 27; published 2012 February 21. \n\nH. Hoekstra acknowledges support from the Netherlands Organisation for Scientific Research (NWO) through a VIDI grant. H. Hoekstra is also supported by a Marie Curie International Reintegration Grant. A. Babul acknowledges support from an NSERC Discovery grant. J. Dalcanton and A. Mahdavi acknowledge the support by NASA through program GO-11221. \n\nBased on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under program 11221.\n\nPublished - Jee2012p18114Astrophys_J.pdf
", "abstract": "We present a Hubble Space Telescope/Wide Field Planetary Camera 2 weak-lensing study of A520, where a previous analysis of ground-based data suggested the presence of a dark mass concentration. We map the complex mass structure in much greater detail, leveraging more than a factor of three increase in the number density of source galaxies available for lensing analysis. The \"dark core\" that is coincident with the X-ray gas peak, but not with any stellar luminosity peak, is now detected with more than 10\u03c3 significance. The ~1.5 Mpc filamentary structure elongated in the NE-SW direction is also clearly visible. Taken at face value, the comparison among the centroids of dark matter, intracluster medium, and galaxy luminosity is at odds with what has been observed in other merging clusters with a similar geometric configuration. To date, the most remarkable counterexample might be the Bullet Cluster, which shows a distinct bow-shock feature as in A520, but no significant weak-lensing mass concentration around the X-ray gas. With the most up-to-date data, we consider several possible explanations that might lead to the detection of this peculiar feature in A520. However, we conclude that none of these scenarios can be singled out yet as the definite explanation for this puzzle.", "date": "2012-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "747", "number": "2", "publisher": "American Astronomical Society", "pagerange": "96", "id_number": "CaltechAUTHORS:20120514-102651392", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120514-102651392", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "Marie Curie International Reintegration Grant" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "NASA", "grant_number": "GO-11221" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/747/2/96", "primary_object": { "basename": "Jee2012p18114Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/v2wgn-z7a58/files/Jee2012p18114Astrophys_J.pdf" }, "pub_year": "2012", "author_list": "Jee, M. J.; Mahdavi, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/sh1rd-v6289", "eprint_id": 29861, "eprint_status": "archive", "datestamp": "2023-08-22 05:08:03", "lastmod": "2023-10-24 22:30:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ideue-Y", "name": { "family": "Ideue", "given": "Y." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Nagao-T", "name": { "family": "Nagao", "given": "T." } }, { "id": "Shioya-Y", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Kajisawa-M", "name": { "family": "Kajisawa", "given": "M." } }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J. R." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The Role of Galaxy Interaction in Environmental Dependence of the Star Formation Activity at z \u2243 1.2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: interactions; galaxies: star formation", "note": "\u00a9 2012 American Astronomical Society. Received 2010 December 28; accepted 2011 December 9; published 2012 February 13. We thank the anonymous referee for very useful comments\nand suggestions. We also thank all members of the\nCOSMOS team. This work was financially supported in part by\nthe Japan Society for the Promotion of Science (Nos. 17253001,\n19340046, 23244031, and 23654068). Y.I. is financially supported\nby the Japan Society for the Promotion of science (JSPS)\nthrough JSPS Research Fellowship for Young Scientists.\n\nPublished - Ideue2012p17555Astrophys_J.pdf
", "abstract": "In order to understand environmental effects on star formation in high-redshift galaxies, we investigate the physical relationships between the star formation activity, stellar mass, and environment for z \u2243 1.2 galaxies in the 2 deg^2 COSMOS field. We estimate star formation using the [O II]\u03bb3727 emission line and environment from the local galaxy density. Our analysis shows that for massive galaxies (M_* \u2273 10^(10) M_\u2609), the fraction of [O II] emitters in high-density environments (\u03a3_(10th) \u2273 3.9 Mpc^(\u20132)) is 1.7 \u00b1 0.4 times higher than in low-density environments (\u03a3_(10th)\u227e 1.5 Mpc^(\u20132)), while the [O II] emitter fraction does not depend on environment for low-mass M_* \u227e 10^(10) M_\u2609 galaxies. In order to understand what drives these trends, we investigate the role of companion galaxies in our sample. We find that the fraction of [O II] emitters in galaxies with companions is 2.4 \u00b1 0.5 times as high as that in galaxies without companions at M_* \u2273 10^(10) M_\u2609. In addition, massive galaxies are more likely to have companions in high-density environments. However, although the number of star-forming galaxies increases for massive galaxies with close companions and in dense environments, the average star formation rate of star-forming galaxies at a given mass is independent of environment and the presence/absence of a close companion. These results suggest that interactions and/or mergers in a high-density environment could induce star formation in massive galaxies at z ~ 1.2, increasing the fraction of star-forming galaxies with M_* \u2273 10^(10) M_\u2609.", "date": "2012-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "747", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 42", "id_number": "CaltechAUTHORS:20120327-135954776", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120327-135954776", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17253001" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19340046" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23244031" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23654068" }, { "agency": "Japan Society for the Promotion of Science (JSPS) Research Fellowships for Young Scientists" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/747/1/42", "primary_object": { "basename": "Ideue2012p17555Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/sh1rd-v6289/files/Ideue2012p17555Astrophys_J.pdf" }, "pub_year": "2012", "author_list": "Ideue, Y.; Taniguchi, Y.; et el." }, { "id": "https://authors.library.caltech.edu/records/9hgmk-z1661", "eprint_id": 31884, "eprint_status": "archive", "datestamp": "2023-08-22 05:05:44", "lastmod": "2023-10-17 21:40:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Magnelli-B", "name": { "family": "Magnelli", "given": "B." }, "orcid": "0000-0002-6777-6490" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "A Herschel view of the far-infrared properties of submillimetre galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; infrared: galaxies; galaxies: starburst; submillimeter: galaxies", "note": "\u00a9 2012 ESO. Article published by EDP Sciences. Received 21 October 2011; Accepted 30 January 2012. We thank the anonymous referee for suggestions which greatly enhanced this work.We thank C. Hayward for providing us with his simulated SEDs. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding\nagencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada), NAOC (China), CEA, LAM\n(France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK), Caltech, JPL, NHSC, University of Colorado (USA). This development\nhas been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA). The SPIRE data presented in this paper will be released through the Herschel Database in Marseille\nHeDaM (hedam.oamp.fr/HerMES).We acknowledge support from the Science and Technology Facilities Council [grant number ST/F002858/1] and [grant number ST/I000976/1]. This study is based on observations made with ESO telescopes at the Paranal and Atacama Observatories under programme numbers:\n171.A-3045, 168.A-0485, 082.A-0890 and 183.A-0666.\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nPublished - Magnelli2012p18475Astron_Astrophys.pdf
", "abstract": "We study a sample of 61submillimetre galaxies (SMGs) selected from ground-based surveys, with known spectroscopic redshifts and observed with the Herschel Space Observatory as part of the PACS Evolutionary Probe (PEP) and the Herschel Multi-tiered Extragalactic Survey (HerMES) guaranteed time key programmes. Our study makes use of the broad far-infrared and submillimetre wavelength coverage (100\u2212600 \u2009\u03bcm) only made possible by the combination of observations from the PACS and SPIRE instruments aboard the Herschel Space Observatory. Using a power-law temperature distribution model to derive infrared luminosities and dust temperatures, we measure a dust emissivity spectral index for SMGs of \u03b2 = 2.0 \u00b1 0.2. Our results unambiguously unveil the diversity of the SMG population. Some SMGs exhibit extreme infrared luminosities of ~10^(13) L_\u2299 and relatively warm dust components, while others are fainter (a few times 10^(12) L_\u2299) and are biased towards cold dust temperatures. Although at z~2 classical SMGs (>5 mJy at 850 \u2009 \u03bcm) have large infrared luminosities (~10^(13) L_\u2299 ), objects only selected on their submm flux densities (without any redshift informations) probe a large range in dust temperatures and infrared luminosities. The extreme infrared luminosities of some SMGs (L_IR \u2273 10^(12.7) L_\u2299, 26/61 systems) imply star formation rates (SFRs) of >500 M_\u2299 yr^(-1) (assuming a Chabrier IMF and no dominant AGN contribution to the FIR luminosity). Such high SFRs are difficult to reconcile with a secular mode of star formation, and may instead correspond to a merger-driven stage in the evolution of these galaxies. Another observational argument in favour of this scenario is the presence of dust temperatures warmer than that of SMGs of lower luminosities (~40 K as opposed to ~25 K), consistent with observations of local ultra-luminous infrared galaxies triggered by major mergers and with results from hydrodynamic simulations of major mergers combined with radiative transfer calculations. Moreover, we find that luminous SMGs are systematically offset from normal star-forming galaxies in the stellar mass-SFR plane, suggesting that they are undergoing starburst events with short duty cycles, compatible with the major merger scenario. On the other hand, a significant fraction of the low infrared luminosity SMGs have cold dust temperatures, are located close to the main sequence of star formation, and therefore might be evolving through a secular mode of star formation. However, the properties of this latter population, especially their dust temperature, should be treated with caution because at these luminosities SMGs are not a representative sample of the entire star-forming galaxy population.", "date": "2012-03", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "539", "publisher": "EDP Sciences", "pagerange": "Art. No. A155", "id_number": "CaltechAUTHORS:20120612-133308323", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120612-133308323", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "BMVIT (Austria)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "CEA/CNES (France)" }, { "agency": "DLR (Germany)" }, { "agency": "ASI/INAF (Italy)" }, { "agency": "CICYT/MCYT (Spain)" }, { "agency": "CSA (Canada)" }, { "agency": "NAOC (China)" }, { "agency": "MCINN (Spain)" }, { "agency": "SNSB (Sweden)" }, { "agency": "STFC (UK)" }, { "agency": "UKSA (UK)" }, { "agency": "NASA" }, { "agency": "Science and Technology Facilities Council", "grant_number": "ST/F002858/1" }, { "agency": "Science and Technology Facilities Council", "grant_number": "ST/I000976/1" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201118312", "primary_object": { "basename": "Magnelli2012p18475Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/9hgmk-z1661/files/Magnelli2012p18475Astron_Astrophys.pdf" }, "pub_year": "2012", "author_list": "Magnelli, B. and Capak, P." }, { "id": "https://authors.library.caltech.edu/records/c3k44-kf787", "eprint_id": 29495, "eprint_status": "archive", "datestamp": "2023-08-22 04:48:17", "lastmod": "2023-10-24 22:15:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mandelbaum-R", "name": { "family": "Mandelbaum", "given": "Rachel" }, "orcid": "0000-0003-2271-1527" }, { "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "Richard J." }, "orcid": "0000-0002-6085-3780" }, { "id": "Rhodes-J", "name": { "family": "Rhodes", "given": "Jason" } } ] }, "title": "Precision simulation of ground-based lensing data using observations from space", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: weak; methods: data analysis; techniques: image processing; galaxies: structure", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. Accepted 2011 November 3. Received 2011 October 10; in original form 2011 July 23. Article first published online: 13 Dec 2011. \nWe thank the referee for many constructive comments about the organization and content of this paper. The authors would also like to thank Jim Gunn, Robert Lupton, Dustin Lang, David Hogg, Michael Blanton, Barney Rowe, Peter Capak, Chiaki Hikage, Uros Seljak and Gary Bernstein for useful conversations about this project, and Eric Huff both for discussing it and giving the software a name. CMH is supported by the US National Science Foundation (AST-0807337), the US Department of Energy (DE-FG03- 02-ER40701), the Alfred P. Sloan Foundation, and the David and Lucile Packard Foundation. AL acknowledges support from the Chamberlain Fellowship at LBNL and from the Berkeley Center for Cosmological Physics. RJM is supported by STFC Advanced Fellowship #PP/E006450/1 and ERC grant MIRG-CT-208994. This work was done in part at JPL, run under a contract for NASA by Caltech. The HST COSMOS Treasury programme was supported through NASA grant HST-GO-09822. We wish to thank Tony Roman, Denise Taylor and David Soderblom for their assistance in planning and scheduling of the extensive COSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at http://cosmos.astro.caltech.edu/. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Justin Howell, Anastasia Laity, Anastasia Alexov, Bruce Berriman and John Good) in providing online archive and server capabilities for the COSMOS data sets.\n\nPublished - Mandelbaum2012p17285Mon_Not_R_Astron_Soc.pdf
", "abstract": "Current and upcoming wide-field, ground-based, broad-band imaging surveys promise to address a wide range of outstanding problems in galaxy formation and cosmology. Several such uses of ground-based data, especially weak gravitational lensing, require highly precise measurements of galaxy image statistics with careful correction for the effects of the point spread function (PSF). In this paper, we introduce the shera (SHEar Reconvolution Analysis) software to simulate ground-based imaging data with realistic galaxy morphologies and observing conditions, starting from space-based data (from the Cosmological Evolution Survey, COSMOS) and accounting for the effects of the space-based PSF. This code simulates ground-based data, optionally with a weak lensing shear applied, in a model-independent way using a general Fourier space formalism. The utility of this pipeline is that it allows for a precise, realistic assessment of systematic errors due to the method of data processing, for example in extracting weak lensing galaxy shape measurements or galaxy radial profiles, given user-supplied observational conditions and real galaxy morphologies. Moreover, the simulations allow for the empirical test of error estimates and determination of parameter degeneracies, via generation of many noise maps. The public release of this software, along with a large sample of cleaned COSMOS galaxy images (corrected for charge transfer inefficiency), should enable upcoming ground-based imaging surveys to achieve their potential in the areas of precision weak lensing analysis, galaxy profile measurement and other applications involving detailed image analysis.", "date": "2012-02", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "420", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1518-1540", "id_number": "CaltechAUTHORS:20120228-073447796", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120228-073447796", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0807337" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG03-02-ER40701" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Lawrence Berkeley National Laboratory" }, { "agency": "Berkeley Center for Cosmological Physics" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "PP/E006450/1" }, { "agency": "Marie Curie Fellowship", "grant_number": "MIRG-CT-208994" }, { "agency": "NASA/Caltech" }, { "agency": "NASA", "grant_number": "HST-GO-09822" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "COSMOS" } ] }, "doi": "10.1111/j.1365-2966.2011.20138.x", "primary_object": { "basename": "Mandelbaum2012p17285Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/c3k44-kf787/files/Mandelbaum2012p17285Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2012", "author_list": "Mandelbaum, Rachel; Hirata, Christopher M.; et el." }, { "id": "https://authors.library.caltech.edu/records/apat2-eg160", "eprint_id": 29471, "eprint_status": "archive", "datestamp": "2023-08-22 04:48:01", "lastmod": "2023-10-24 22:13:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Vulcani-B", "name": { "family": "Vulcani", "given": "Benedetta" }, "orcid": "0000-0003-0980-1499" }, { "id": "Poggianti-B-M", "name": { "family": "Poggianti", "given": "Bianca M." }, "orcid": "0000-0001-8751-8360" }, { "id": "Fasano-G", "name": { "family": "Fasano", "given": "Giovanni" } }, { "id": "Desai-V", "name": { "family": "Desai", "given": "Vandana" }, "orcid": "0000-0002-1340-0543" }, { "id": "Dressler-A", "name": { "family": "Dressler", "given": "Alan" } }, { "id": "Oemler-A-Jr", "name": { "family": "Oemler", "given": "August, Jr." } }, { "id": "Calvi-R", "name": { "family": "Calvi", "given": "Rosa" } }, { "id": "D'Onofrio-M", "name": { "family": "D'Onofrio", "given": "Mauro" } }, { "id": "Moretti-A", "name": { "family": "Moretti", "given": "Alessia" } } ] }, "title": "The importance of the local density in shaping the galaxy stellar mass functions", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general; galaxies: evolution; galaxies: formation; galaxies: fundamental parameters; galaxies: luminosity function, mass function", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. Accepted 2011 November 3. Received 2011 November 3; in original form 2011 July 26. Article first published online: 30 Dec 2011. \nThis paper includes data gathered with the 6.5-m Magellan Telescopes\nlocated at Las Campanas Observatory, Chile.\nWe thank the referee for useful comments. We would like to thank\nthe whole WINGS team for stimulating discussions. We would\nalso like to thank Alfonso Arag\u03ccn-Salamanca and Gabriella De\nLucia, whose suggestions helped us to improve the paper. BV and\nBMP acknowledge financial support from ASI contract I/016/07/0\nand ASI-INAF I/009/10/0. BV also acknowledges financial support\nfrom the Fondazione Ing. Aldo Gini\n\nPublished - Vulcani2012p17282Mon_Not_R_Astron_Soc.pdf
", "abstract": "Exploiting the capabilities of four different surveys \u2013 the Padova\u2013Millennium Galaxy and Group Catalogue (PM2GC), the WIde-field Nearby Galaxy-cluster Survey (WINGS), the IMACS (Inamori-Magellan Areal Camera and Spectrograph) Cluster Building Survey (ICBS) and the ESO (European Southern Observatory) Distant Cluster Survey (EDisCS) \u2013 we analyse the galaxy stellarmass distribution as a function of local density in mass-limited samples, in the field and in clusters from low (z \u2265 0.04) to high (z \u2264 0.8) redshift. We find that at all redshifts and in all environments, local density plays a role in shaping themass distribution. In the field, it regulates the shape of the mass function at any mass above the mass limits. In clusters, it seems to be important only at low masses (log M_\u2217/M_\u2609 \u2264 10.1 in WINGS and log M_\u2217/M_\u2609 \u2264 10.4 in EDisCS), otherwise it seems not to influence the mass distribution. Putting together our results with those of Calvi et al. and Vulcani et al. for the global environment, we argue that at least at z \u2264 0.8 local density is more important than global environment in determining the\ngalaxy stellar mass distribution, suggesting that galaxy properties are not much dependent on halo mass, but do depend on local scale processes.", "date": "2012-02", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "420", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1481-1494", "id_number": "CaltechAUTHORS:20120224-154439407", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120224-154439407", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/016/07/0" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/009/10/0" }, { "agency": "Fondazione Ing. Aldo Gini" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2011.20135.x", "primary_object": { "basename": "Vulcani2012p17282Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/apat2-eg160/files/Vulcani2012p17282Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2012", "author_list": "Vulcani, Benedetta; Poggianti, Bianca M.; et el." }, { "id": "https://authors.library.caltech.edu/records/w8sbd-9k124", "eprint_id": 29472, "eprint_status": "archive", "datestamp": "2023-08-19 09:45:04", "lastmod": "2023-10-24 22:13:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "Min S." }, "orcid": "0000-0001-7095-7543" }, { "id": "Scott-K-S", "name": { "family": "Scott", "given": "K. S." } }, { "id": "Guo-Yicheng", "name": { "family": "Guo", "given": "Yicheng" }, "orcid": "0000-0003-2775-2002" }, { "id": "Aretxaga-I", "name": { "family": "Aretxaga", "given": "I." }, "orcid": "0000-0002-6590-3994" }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Austermann-J-E", "name": { "family": "Austermann", "given": "J. E." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Chen-Yuxin", "name": { "family": "Chen", "given": "Yuxin" } }, { "id": "Ezawa-Hajime", "name": { "family": "Ezawa", "given": "H." } }, { "id": "Hatsukade-Bunyo", "name": { "family": "Hatsukade", "given": "B." } }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "D. H." } }, { "id": "Iono-Daisuke", "name": { "family": "Iono", "given": "D." }, "orcid": "0000-0002-2364-0823" }, { "id": "Johnson-S", "name": { "family": "Johnson", "given": "S." }, "orcid": "0000-0001-9487-8583" }, { "id": "Kawabe-Ryohei", "name": { "family": "Kawabe", "given": "R." }, "orcid": "0000-0002-8049-7525" }, { "id": "Kohno-Kotaro", "name": { "family": "Kohno", "given": "K." }, "orcid": "0000-0002-4052-2394" }, { "id": "Lowenthal-J-D", "name": { "family": "Lowenthal", "given": "J." } }, { "id": "Miller-N", "name": { "family": "Miller", "given": "N." } }, { "id": "Morrison-G-E", "name": { "family": "Morrison", "given": "G." } }, { "id": "Oshima-Takeharu", "name": { "family": "Oshima", "given": "T." } }, { "id": "Perera-T-A", "name": { "family": "Perera", "given": "T. A." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Tamura-Yoichi", "name": { "family": "Tamura", "given": "Y." } }, { "id": "Williams-C-C", "name": { "family": "Williams", "given": "C. C." }, "orcid": "0000-0003-2919-7495" }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G. W." } } ] }, "title": "Deep 1.1 mm-wavelength imaging of the GOODS-S field by AzTEC/ASTE \u2013 II. Redshift distribution and nature of the submillimetre galaxy population", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxy: evolution galaxies: high-redshift galaxies: starburst infrared: galaxies", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. \n\nAccepted 2011 September 27. Received 2011 September 11; in original form 2011 June 6. Article first published online: 30 Dec 2011. \n\nThe authors would like to thank M. Dickinson and R.-R. Chary for use of the Spitzer GOODS-S IRAC/MIPS catalogues. This work has also benefited from valuable discussions with C. Carilli, E. Chapin, R. Ivison, A. Pope, D. Sanders, N. Scoville and many others. We would also like to thank everyone who helped staff and support the AzTEC/ASTE 2007 operations, including K. Tanaka, M. Tashiro, K. Nakanishi, T. Tsukagoshi, M. Uehara, S. Doyle, P. Horner, J. Cortes, J. Karakla and G. Wallace. Support for this work was provided in part by the National Science Foundation grants AST-0838222 and AST-0907952.\n\nPublished - Yun2012p17271Mon_Not_R_Astron_Soc.pdf
", "abstract": "We report the results of the counterpart identification and a detailed analysis of the physical properties of the 48 sources discovered in our deep 1.1-mm wavelength imaging survey of the Great Observatories Origins Deep Survey-South (GOODS-S) field using the AzTEC instrument on the Atacama Submillimeter Telescope Experiment. One or more robust or tentative counterpart candidate is found for 27 and 14 AzTEC sources, respectively, by employing deep radio continuum, Spitzer/Multiband Imaging Photometer for Spitzer and Infrared Array Camera, and Large APEX Bolometer Camera 870 \u03bcm data. Five of the sources (10 per cent) have two robust counterparts each, supporting the idea that these galaxies are strongly clustered and/or heavily confused. Photometric redshifts and star formation rates (SFRs) are derived by analysing ultraviolet(UV)-to-optical and infrared(IR)-to-radio spectral energy distributions (SEDs). The median redshift of z_(med)\u223c 2.6 is similar to other earlier estimates, but we show that 80 per cent of the AzTEC\u2013GOODS sources are at z\u2265 2, with a significant high-redshift tail (20 per cent at z\u2265 3.3). Rest-frame UV and optical properties of AzTEC sources are extremely diverse, spanning 10 mag in the i- and K-band photometry (a factor of 10^4 in flux density) with median values of i= 25.3 and K= 22.6 and a broad range of red colour (i\u2212K= 0\u20136) with an average value of i\u2212K \u2248 3. These AzTEC sources are some of the most luminous galaxies in the rest-frame optical bands at z\u2265 2, with inferred stellar masses M_*= (1\u201330) \u00d7 10^(10) M_\u2299 and UV-derived SFRs of SFRUV\u2273 10^(1-3) M_\u2299 yr^(\u22121). The IR-derived SFR, 200\u20132000 M_\u2299 yr^(\u22121), is independent of z or M_*. The resulting specific star formation rates, SSFR \u2248 1\u2013100 Gyr^(\u22121), are 10\u2013100 times higher than similar mass galaxies at z= 0, and they extend the previously observed rapid rise in the SSFR with redshift to z = 2\u20135. These galaxies have a SFR high enough to have built up their entire stellar mass within their Hubble time. We find only marginal evidence for an active galactic nucleus (AGN) contribution to the near-IR and mid-IR SEDs, even among the X-ray detected sources, and the derived M_* and SFR show little dependence on the presence of an X-ray bright AGN.", "date": "2012-02", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "420", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "957-985", "id_number": "CaltechAUTHORS:20120224-154618903", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120224-154618903", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0838222" }, { "agency": "NSF", "grant_number": "AST-0907952" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2011.19898.x", "primary_object": { "basename": "Yun2012p17271Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/w8sbd-9k124/files/Yun2012p17271Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2012", "author_list": "Yun, Min S.; Scott, K. S.; et el." }, { "id": "https://authors.library.caltech.edu/records/0fzbk-hw490", "eprint_id": 29942, "eprint_status": "archive", "datestamp": "2023-08-19 09:48:14", "lastmod": "2023-10-24 22:36:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Giodini-S", "name": { "family": "Giodini", "given": "S." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Pierini-D", "name": { "family": "Pierini", "given": "D." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" } ] }, "title": "The galaxy stellar mass function of X-ray detected groups.\n Environmental dependence of galaxy evolution in the COSMOS survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: groups: general", "note": "\u00a9 2012 ESO. Received 14 July 2011. Accepted 24 November 2011. Published online 13 February 2012.\nS.G. acknowledges support from The Netherlands\nOrganization for Scientific Research (NWO) through a VIDI grant. We acknowledge the contributions of the entire COSMOS collaboration; more informations on the COSMOS survey are available at http://www.astr.caltech.edu/~cosmos. S.G. acknowledge H. Boehringer for having contributed\nto the start of this project and H. Hoekstra, G. Guzzo, J. Brinchmann, S. Weinmann, D. Capozzi, T. Ponman, B. Vulcani and A. Leauthaud for helpful discussion. D.P. acknowledges the kind hospitality of the MPE.\n\nPublished - Giodini2012p17623Astron_Astrophys.pdf
", "abstract": "We study the stellar mass distribution for galaxies in 160 X-ray detected groups of 10^(13) < Log(M_(200)/M_\u2299) < 2 \u00d7 10^(14) and compare it with that of galaxies in the field to investigate the action of environment on the build-up of the stellar mass. We highlight differences in the build-up of the passive population in the field, which imprint features in the distribution of stellar mass of passive galaxies at Log(M/M_\u2299) < 10.5. The gradual diminishing of the effect when moving to groups of increasing total masses indicates that the growing influence of the environment in bound structures is responsible for the build-up of a quenched component at Log(M/M_\u2299) < 10.5. Differently, the stellar mass distribution of star-forming galaxies is similar in shape in all environments, and can be described by a single Schechter function both in groups and in the field. Little evolution is seen up to redshift 1. Nevertheless at z = 0.2\u20130.4 groups with M_(200) < 6 \u00d7 10^(13) M_\u2299 (low-mass groups) tend to have a characteristic mass for star-forming galaxies that is 50% higher than in higher mass groups; we interpret it as a reduced action of environmental processes in these systems. Furthermore, we analyse the distribution of sSFR\u2013Log(M) in groups and in the field, and find that groups show on average a lower sSFR (by ~0.2 dex) at z < 0.8. Accordingly, we find that the fraction of star-forming galaxies is increasing with redshift in all environments, but at a faster pace in the denser ones. Finally, our analysis highlights that low-mass groups have a higher fraction (by 50%) of the stellar mass locked in star-forming galaxies than higher mass systems (i.e. 2/3 of their stellar mass).", "date": "2012-02", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "538", "publisher": "EDP Sciences", "pagerange": "Art. No. A104", "id_number": "CaltechAUTHORS:20120403-073218005", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120403-073218005", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201117696", "primary_object": { "basename": "Giodini2012p17623Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/0fzbk-hw490/files/Giodini2012p17623Astron_Astrophys.pdf" }, "pub_year": "2012", "author_list": "Giodini, S.; Finoguenov, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/va3bg-mmq13", "eprint_id": 29003, "eprint_status": "archive", "datestamp": "2023-08-22 04:34:47", "lastmod": "2023-10-24 18:18:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lake-S-E", "name": { "family": "Lake", "given": "S. E." } }, { "id": "Wright-E-L", "name": { "family": "Wright", "given": "E. L." }, "orcid": "0000-0001-5058-1593" }, { "id": "Petty-S", "name": { "family": "Petty", "given": "S." } }, { "id": "Assef-R-J", "name": { "family": "Assef", "given": "R. J." }, "orcid": "0000-0002-9508-3667" }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Stanford-S-A", "name": { "family": "Stanford", "given": "S. A." } }, { "id": "Stern-D", "name": { "family": "Stern", "given": "D." }, "orcid": "0000-0003-2686-9241" }, { "id": "Tsai-Chao-Wei", "name": { "family": "Tsai", "given": "C.-W." }, "orcid": "0000-0002-9390-9672" } ] }, "title": "Optical Spectroscopic Survey of High-latitude WISE-selected Sources", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: general; Galaxy: stellar content; surveys", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2011 July 28; accepted 2011 October 28; published 2011 December 1.\n\nThis publication makes use of data products from WISE, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The WISE Web site is http://wise.ssl.berkeley.edu/. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from the NSF grant AST-0071048. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy. The SDSS-III Web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, University of Florida, the French Participation Group, the German Participation Group, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, New Mexico State University, New York University, The Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. R.J.A. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA.\n\nPublished - Lake2012p16883Astron_J.pdf
", "abstract": "We report on the results of an optical spectroscopic survey at high Galactic latitude (|b| \u2265 30\u00b0) of a sample of WISE-selected targets, grouped by WISE W1 (\u03bb_eff = 3.4 \u03bcm) flux, which we use to characterize the sources WISE detected. We observed 762 targets in 10 disjoint fields centered on ultraluminous infrared galaxy candidates using DEIMOS on Keck II. We find 0.30 \u00b1 0.02 galaxies arcmin\u20132 with a median redshift of z = 0.33 \u00b1 0.01 for the sample with W1 \u2265 120 \u03bcJy. The foreground stellar densities in our survey range from 0.23 \u00b1 0.07 arcmin\u20132 to 1.1 \u00b1 0.1 arcmin\u20132 for the same sample. We obtained spectra that produced science grade redshifts for \u226590% of our targets for sources with W1 flux \u2265120 \u03bcJy that also had an i-band flux gsim 18 \u03bcJy. We used this for targeting very preliminary data reductions available to the team in 2010 August. Our results therefore present a conservative estimate of what is possible to achieve using WISE's Preliminary Data Release for the study of field galaxies.", "date": "2012-01", "date_type": "published", "publication": "Astronomical Journal", "volume": "143", "number": "1", "publisher": "American Astronomical Society", "pagerange": "7", "id_number": "CaltechAUTHORS:20120127-114550424", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120127-114550424", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Postdoctoral Program" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-6256/143/1/7", "primary_object": { "basename": "Lake2012p16883Astron_J.pdf", "url": "https://authors.library.caltech.edu/records/va3bg-mmq13/files/Lake2012p16883Astron_J.pdf" }, "pub_year": "2012", "author_list": "Lake, S. E.; Wright, E. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/gbh7t-61h89", "eprint_id": 30126, "eprint_status": "archive", "datestamp": "2023-08-22 04:38:38", "lastmod": "2023-10-17 15:23:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Popesso-P", "name": { "family": "Popesso", "given": "P." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" } ] }, "title": "The evolution of the star formation activity per halo mass up to redshift ~1.6 as seen by Herschel", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general; galaxies: evolution; galaxies: high-redshift", "note": "\u00a9 2012 ESO. Article published by EDP Sciences.\n\nReceived: 30 August 2011; Accepted: 13 October 2011.\nPublished online 09 January 2012.\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\nPACS has been developed by a consortium of institutes\nled by MPE (Germany) and including UVIE (Austria); KUL, CSL,\nIMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy), and CICYT/MCYT (Spain). We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information about the\nCOSMOS survey is available at http://www.astro.caltech.edu/~cosmos. This research has made use of NASA's Astrophysics Data System, of NED, which is operated by JPL/Caltech, under contract with NASA, and of SDSS, which has been funded by the Sloan Foundation, NSF, the US Department of\nEnergy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council of England. The SDSS is managed by the participating institutions (www.sdss.org/collaboration/credits.html).\n\nPublished - Popesso2012p17740Astron_Astrophys.pdf
", "abstract": "Aims. Star formation in massive galaxies is quenched at some point during hierarchical mass assembly. To understand where and when the quenching processes takes place, we study the evolution of the total star formation rate per unit total halo mass (\u03a3(SFR)/M) in three different mass scales: low mass halos (field galaxies), groups, and clusters, up to a redshift z \u2248 1.6.\n\nMethods. We use deep far-infrared PACS data at 100 and 160 \u03bcm\u2009to accurately estimate the total star formation rate of the luminous infrared galaxy population of 9 clusters with mass ~10^(15) M_\u2299, and 9 groups/poor clusters with mass ~5 \u00d7 10^(13) M_\u2299. Estimates of the field \u03a3(SFR)/M\u2009are derived from the literature, by dividing the star formation rate density by the mean comoving matter density of the universe.\n\nResults. The field \u03a3(SFR)/M\u2009increases with redshift up to z ~ 1 and it is constant thereafter. The evolution of the \u03a3(SFR)/M\u2009\u2013\u2009z relation in galaxy systems is much faster than in the field. Up to redshift z ~ 0.2, the field has a higher \u03a3(SFR)/M\u2009than galaxy groups and galaxy clusters. At higher redshifts, galaxy groups and the field have similar \u03a3(SFR)/M, while massive clusters have significantly lower \u03a3(SFR)/M\u2009than both groups and the field. There is a hint of a reversal of the SFR activity vs. environment at z ~ 1.6, where the group \u03a3(SFR)/M\u2009lies above the field \u03a3(SFR)/M \u2212 z relation. We discuss possible interpretations of our results in terms of the processes of downsizing, and star-formation quenching.", "date": "2012-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "537", "publisher": "EDP Sciences", "pagerange": "A58", "id_number": "CaltechAUTHORS:20120417-095333719", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120417-095333719", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "BMVIT (Austria)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "CEA/CNES (France)" }, { "agency": "DLR (Germany)" }, { "agency": "ASI (Italy)" }, { "agency": "CICYT/MCYT (Spain)" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201117973", "primary_object": { "basename": "Popesso2012p17740Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/gbh7t-61h89/files/Popesso2012p17740Astron_Astrophys.pdf" }, "pub_year": "2012", "author_list": "Popesso, P.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/36vqj-c9231", "eprint_id": 29078, "eprint_status": "archive", "datestamp": "2023-08-22 04:22:02", "lastmod": "2023-10-24 18:21:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Fu-Hai", "name": { "family": "Fu", "given": "H." }, "orcid": "0000-0001-9608-6395" } ] }, "title": "The Impact of Galaxy Interactions on Active Galactic Nucleus Activity in zCosmos", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: interactions; quasars: general; X-rays: galaxies", "note": "\u00a9 2011 The American Astronomical Society. Received 2011 July 15; accepted 2011 August 29; published 2011 November 17. The authors appreciate the useful discussions with Charles Steinhardt, Yen-Ting Lin, and Ed Turner. This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. K.J. is supported by the Emmy Noether Programme by the German Science Foundation (DFG). R.A. is funded by the Klaus Tschira Foundation via the Heidelberg Graduate School of Fundamental Physics (HGSFP).\nFacilities: CXO(ACIS), VLT:Melipal (VIMOS).\n\nPublished - Silverman2011p16917Astrophys_J.pdf
", "abstract": "Close encounters between galaxies are expected to be a viable mechanism, as predicted by numerical simulations, by which accretion onto supermassive black holes can be initiated. To test this scenario, we construct a sample of 562 galaxies (M_* > 2.5 \u00d7 10^(10) M_\u2609) in kinematic pairs over the redshift range 0.25 < z < 1.05 that are more likely to be interacting than a well-matched control sample of 2726 galaxies not identified as being in a pair, both from the zCOSMOS 20k spectroscopic catalog. Galaxies that harbor an active galactic nucleus (AGN) are identified on the basis of their X-ray emission (L_(0.5-10keV) > 2 \u00d7 10^(42) erg s^(\u20131)) detected by Chandra. We find a higher fraction of an AGN in galaxies in pairs relative to isolated galaxies of similar stellar mass. Our result is primarily due to an enhancement of AGN activity, by a factor of 1.9 (observed) and 2.6 (intrinsic), for galaxies in pairs of projected separation less than 75 kpc and line-of-sight velocity offset less than 500 km s^(\u20131). This study demonstrates that close kinematic pairs are conducive environments for black hole growth, either indicating a causal physical connection or an inherent relation, such as, to enhanced star formation. In the Appendix, we describe a method for estimating the intrinsic fractions of galaxies (either in pairs or the field) hosting an AGN with confidence intervals, and an excess fraction in pairs. We estimate that 17.8^(+8.4)_(\u20137.4)% of all moderate-luminosity AGN activity takes place within galaxies undergoing early stages of interaction that leaves open the question as to what physical processes are responsible for fueling the remaining ~80% that may include late-stage mergers.", "date": "2011-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "743", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 2", "id_number": "CaltechAUTHORS:20120201-153641202", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120201-153641202", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan" }, { "agency": "German Science Foundation Emmy Noether Programme" }, { "agency": "Heidelberg Graduate School of Fundamental Physics (HGSFP) Klaus Tschira Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/743/1/2", "primary_object": { "basename": "Silverman2011p16917Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/36vqj-c9231/files/Silverman2011p16917Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Silverman, J. D. and Fu, H." }, { "id": "https://authors.library.caltech.edu/records/6v01d-8h326", "eprint_id": 28595, "eprint_status": "archive", "datestamp": "2023-08-22 04:19:39", "lastmod": "2023-10-24 18:00:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "George-M-R", "name": { "family": "George", "given": "Matthew R." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "Bundy-K-A", "name": { "family": "Bundy", "given": "Kevin" }, "orcid": "0000-0001-9742-3138" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "Alexis" }, "orcid": "0000-0002-4606-5403" }, { "id": "Tinker-J-L", "name": { "family": "Tinker", "given": "Jeremy" } }, { "id": "Lin-Yen-Ting", "name": { "family": "Lin", "given": "Yen-Ting" } }, { "id": "Mei-Simona", "name": { "family": "Mei", "given": "Simona" }, "orcid": "0000-0002-2849-559X" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "Jean-Paul" }, "orcid": "0000-0002-4616-4989" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "Herve" }, "orcid": "0000-0002-1371-5705" }, { "id": "Behroozi-P-S", "name": { "family": "Behroozi", "given": "Peter S." } }, { "id": "Busha-M-T", "name": { "family": "Busha", "given": "Michael T." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Coccato-L", "name": { "family": "Coccato", "given": "Lodovico" } }, { "id": "Covone-G", "name": { "family": "Covone", "given": "Giovanni" } }, { "id": "Faure-C", "name": { "family": "Faure", "given": "Cecile" } }, { "id": "Fiorenza-S-L", "name": { "family": "Fiorenza", "given": "Stephanie L." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "Emeric" } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "Masayuki" }, "orcid": "0000-0002-5011-5178" }, { "id": "Wechsler-R-H", "name": { "family": "Wechsler", "given": "Risa H." }, "orcid": "0000-0003-2229-011X" }, { "id": "Wolk-M", "name": { "family": "Wolk", "given": "Melody" } } ] }, "title": "Galaxies in X-Ray Groups. I. Robust Membership Assignment and the Impact of Group Environments on Quenching", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: groups: general; galaxies: star formation", "note": "\u00a9 2011 The American Astronomical Society. Received 2011 June 6; accepted 2011 September 23; published 2011 November 15. We thank Joanne Cohn, Eliot Quataert, Eli Rykoff,\nDavid Schlegel, Uros Seljak, Erik Shirokoff, Andrew Wetzel,\nand Martin White for helpful conversations. We also thank\nMichael Cooper and Marc Davis for providing software and\ntemplate spectra used in our spectroscopic analysis, as well as comments on the paper. M.R.G. is supported by a Graduate\nResearch Fellowship from the National Science Foundation.\nThis work is partly based on observations made with ESO\nTelescopes at Paranal Observatory under program ID 084.B-\n0523.We gratefully acknowledge the contributions of the entire\nCOSMOS collaboration consisting of more than 70 scientists.\nMore information on the COSMOS survey is available at\nhttp://www.astro.caltech.edu/cosmos. This work is based on\nobservations with the NASA/ESA Hubble Space Telescope,\nobtained at the Space Telescope Science Institute, which is\noperated by AURA Inc., under NASA contract NAS 5-26555;\nalso based on data collected at: the Subaru Telescope, which is\noperated by the National Astronomical Observatory of Japan;\nthe XMM-Newton, an ESA science mission with instruments\nand contributions directly funded by ESA Member States\nand NASA; the European Southern Observatory under Large\nProgram 175.A-0839, Chile; Kitt Peak National Observatory,\nCerro Tololo Inter-American Observatory, and the National\nOptical Astronomy Observatory, which are operated by the\nAssociation of Universities for Research in Astronomy, Inc.\n(AURA) under cooperative agreement with the National Science\nFoundation; and the Canada\u2013France\u2013Hawaii Telescope with\nMegaPrime/MegaCam operated as a joint project by the CFHT\nCorporation, CEA/DAPNIA, the National Research Council\nof Canada, the Canadian Astronomy Data Centre, the Centre\nNational de la Recherche Scientifique de France, TERAPIX,\nand the University of Hawaii.\n\nPublished - George2011p16569Astrophys_J.pdf
", "abstract": "Understanding the mechanisms that lead dense environments to host galaxies with redder colors, more spheroidal morphologies, and lower star formation rates than field populations remains an important problem. As most candidate processes ultimately depend on host halo mass, accurate characterizations of the local environment, ideally tied to halo mass estimates and spanning a range in halo mass and redshift, are needed. In this work, we present and test a rigorous, probabilistic method for assigning galaxies to groups based on precise photometric redshifts and X-ray-selected groups drawn from the COSMOS field. The groups have masses in the range 10^(13) \u227e M_(200c)/M_\u2609 \u227e 10^(14) and span redshifts 0 < z < 1. We characterize our selection algorithm via tests on spectroscopic subsamples, including new data obtained at the Very Large Telescope, and by applying our method to detailed mock catalogs. We find that our group member galaxy sample has a purity of 84% and completeness of 92% within 0.5R_(200c). We measure the impact of uncertainties in redshifts and group centering on the quality of the member selection with simulations based on current data as well as future imaging and spectroscopic surveys. As a first application of our new group member catalog which will be made publicly available, we show that member galaxies exhibit a higher quenched fraction compared to the field at fixed stellar mass out to z ~ 1, indicating a significant relationship between star formation and environment at group scales. We also address the suggestion that dusty star-forming galaxies in such groups may impact the high-\u2113 power spectrum of the cosmic microwave background and find that such a population cannot explain the low power seen in recent Sunyaev-Zel'dovich measurements.", "date": "2011-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "742", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 125", "id_number": "CaltechAUTHORS:20111223-114152671", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111223-114152671", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship" }, { "agency": "Paranal Observatory", "grant_number": "ID 084.B-0523" }, { "agency": "NASA", "grant_number": "NAS-5-26555" }, { "agency": "ESA Member States" }, { "agency": "European Southern Observatory (ESO)", "grant_number": "175.A-0839" }, { "agency": "Kitt Peak National Observatory" }, { "agency": "Cerro Tololo Inter-American Observatory" }, { "agency": "National Optical Astronomy Observatory (NOAO)" }, { "agency": "NSF" }, { "agency": "Canada-France-Hawaii Telescope (CFHT)" }, { "agency": "CEA/DAPNIA (France)" }, { "agency": "National Research Council of Canada" }, { "agency": "Canadian Astronomy Data Centre" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "TERAPIX" }, { "agency": "University of Hawaii" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/742/2/125", "primary_object": { "basename": "George2011p16569Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/6v01d-8h326/files/George2011p16569Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "George, Matthew R.; Leauthaud, Alexie; et el." }, { "id": "https://authors.library.caltech.edu/records/f3xqw-hyw21", "eprint_id": 28689, "eprint_status": "archive", "datestamp": "2023-08-22 04:19:44", "lastmod": "2023-10-24 18:05:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Kakazu-Yuko", "name": { "family": "Kakazu", "given": "Y." } }, { "id": "Manohar-S", "name": { "family": "Manohar", "given": "S." } }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "D." }, "orcid": "0000-0001-5382-6138" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P." } } ] }, "title": "Dissecting Photometric Redshift for Active Galactic Nucleus Using XMM- and Chandra-COSMOS Samples", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: distances and redshifts; methods: data analysis; surveys; techniques: photometric; X-rays: galaxies", "note": "\u00a9 2011 American Astronomical Society. Received 2011 June 19; accepted 2011 July 15; published 2011 November 4.\nBased on observations by the Chandra X-ray Observatory Center, which is\noperated by the Smithsonian Astrophysical Observatory for and on behalf of\nthe National Aeronautics Space Administration under contract NAS8-03060.\nAlso based on observations with the NASA/ESA Hubble Space Telescope,\nobtained at the Space Telescope Science Institute, which is operated by AURA\nInc., under NASA contract NAS 5-26555. Also based on observations made\nwith the Spitzer Space Telescope, which is operated by the Jet Propulsion\nLaboratory, California Institute of Technology, under NASA contract 1407.\nAlso based on data collected at the Subaru Telescope, which is operated by the\nNational Astronomical Observatory of Japan; the XMM-Newton, an ESA\nscience mission with instruments and contributions directly funded by ESA\nMember States and NASA; the European Southern Observatory under Large\nProgram 175.A-0839, Chile; the Kitt Peak National Observatory, Cerro Tololo\nInter-American Observatory and the National Optical Astronomy Observatory,\nwhich are operated by the Association of Universities for Research in\nAstronomy, Inc. (AURA), under cooperative agreement with the National\nScience Foundation; the Canada\u2013France\u2013Hawaii Telescope with\nMegaPrime/MegaCam operated as a joint project by the CFHT Corporation,\nCEA/DAPNIA, the NRC and CADC of Canada, the CNRS of France,\nTERAPIX, and the University of Hawaii.\nWe gratefully acknowledge the contributions of the entire\nCOSMOS collaboration consisting of more than 100 scientists.\nMore information about the COSMOS survey is available at\nhttp://www.astro.caltech.edu/\u223ccosmos. We also acknowledge\nthe use of STILTS and TOPCAT tools (Taylor 2005). We acknowledge\nthe anonymous referee for helpful comments that\nimproved the paper. M.S. and G.H. acknowledge support by\nthe German Deutsche Forschungsgemeinschaft, DFG Leibniz\nPrize (FKZ HA 1850/28-1). F.C. was supported in part\nby NASA Chandra grant No. GO7-8136A, the Blancheflor\nBoncompagni Ludovisi foundation, and the Smithsonian Scholarly\nStudies. A.C., C.V., N.C., and F.F. acknowledge financial\ncontribution from agreement ASI-INAF I/009/10/0.\nFacilities: Keck:II, HST, VLT:Melipan, CXO, Sloan, XMM,\nSubaru\n\nPublished - Salvato2011p16568Astrophys_J.pdf
", "abstract": "In this paper, we release accurate photometric redshifts for 1692 counterparts to Chandra sources in the central square degree of the Cosmic Evolution Survey (COSMOS) field. The availability of a large training set of spectroscopic redshifts that extends to faint magnitudes enabled photometric redshifts comparable to the highest quality results presently available for normal galaxies. We demonstrate that morphologically extended, faint X-ray sources without optical variability are more accurately described by a library of normal galaxies (corrected for emission lines) than by active galactic nucleus (AGN) dominated templates, even if these sources have AGN-like X-ray luminosities. Preselecting the library on the bases of the source properties allowed us to reach an accuracy \u03c3_(\u0394z/(1+z(spec))~0.015 with a fraction of outliers of 5.8% for the entire Chandra-COSMOS sample. In addition, we release revised photometric redshifts for the 1735 optical counterparts of the XMM-detected sources over the entire 2 deg^2 of COSMOS. For 248 sources, our updated photometric redshift differs from the previous release by \u0394z > 0.2. These changes are predominantly due to the inclusion of newly available deep H-band photometry (H_(AB) = 24 mag). We illustrate once again the importance of a spectroscopic training sample and how an assumption about the nature of a source together, with the number and the depth of the available bands, influences the accuracy of the photometric redshifts determined for AGN. These considerations should be kept in mind when defining the observational strategies of upcoming large surveys targeting AGNs, such as eROSITA at X-ray energies and the Australian Square Kilometre Array Pathfinder Evolutionary Map of the Universe in the radio band.", "date": "2011-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "742", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 61", "id_number": "CaltechAUTHORS:20120106-082414162", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120106-082414162", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "HA 1850/28-1" }, { "agency": "NASA", "grant_number": "GO7-8136A" }, { "agency": "Blancheflor Boncompagni Ludovisi foundation" }, { "agency": "Smithsonian Institution" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/INAF I/009/10/0" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/742/2/61", "primary_object": { "basename": "Salvato2011p16568Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/f3xqw-hyw21/files/Salvato2011p16568Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Salvato, M.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/b0cqk-a0592", "eprint_id": 28973, "eprint_status": "archive", "datestamp": "2023-08-22 04:15:37", "lastmod": "2023-10-24 18:16:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kirkpatrick-J-D", "name": { "family": "Kirkpatrick", "given": "J. Davy" }, "orcid": "0000-0003-4269-260X" }, { "id": "Gelino-C-R", "name": { "family": "Gelino", "given": "Christopher R." } }, { "id": "Griffith-R-L", "name": { "family": "Griffith", "given": "Roger L." } }, { "id": "Marsh-K-A", "name": { "family": "Marsh", "given": "Kenneth A." }, "orcid": "0000-0003-0107-7803" }, { "id": "Tsai-Chao-Wei", "name": { "family": "Tsai", "given": "Chao-Wei" }, "orcid": "0000-0002-9390-9672" }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "Charles A." }, "orcid": "0000-0002-5627-5471" }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "Carrie R." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Morales-Calder\u00f3n-M", "name": { "family": "Morales-Calder\u00f3n", "given": "Mar\u00eda" } }, { "id": "Manohar-S", "name": { "family": "Manohar", "given": "Swarnima" } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Schurr-S-D", "name": { "family": "Schurr", "given": "Steven D." } } ] }, "title": "The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE)", "ispublished": "pub", "full_text_status": "public", "keywords": "brown dwarfs; infrared: stars; parallaxes; proper motions; solar neighborhood; stars: luminosity function, mass function", "note": "\u00a9 2011 The American Astronomical Society. \n\nReceived 2011 May 31; accepted 2011 August 22; published 2011 November 22. \n\nThis paper represents the culmination of a year's worth of effort following up the first batch of brown dwarf candidates identified by WISE. There are many hundreds more candidates still being scrutinized, and there are still areas of sky not yet searched. It is therefore clear that these first hundred brown dwarf discoveries are harbingers of a much larger trove of brown dwarfs yet to be uncovered by WISE. Not only is the WISE data archive uniquely suited to finding even colder objects than the current batch of early-Y dwarfs, the all-sky and multiepoch nature of the mission will enable many other brown dwarf studies\u2014the search for the lowest mass objects in nearby moving groups, hunting for low-metallicity objects via their high proper motions, etc.\u2014that are well beyond the scope of the photometric search presented here. This publication makes use of data products from the Widefield Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. We acknowledge fruitful discussions with Tim Conrow, Roc Cutri, and Frank Masci, and acknowledge assistance with Magellan/FIRE observations by Emily Bowsher. This publication also makes use of data products from 2MASS, SDSS, and UKIDSS. 2MASS is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration\nand the National Science Foundation. SDSS is funded by the Alfred P. Sloan Foundation, the Participating Institutions,\nthe National Science Foundation, the U.S. Department\nof Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. UKIDSS uses the Wide Field Camera at the United Kingdom Infrared Telescope atop Mauna Kea, Hawai'i. We are grateful for the efforts of the instrument, calibration, and pipeline teams that have made the UKIDSS data possible. We acknowledge use of the DSS, which were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. This research has made use of the NASA/IPAC Infrared Science Archive (IRSA), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Our research has benefited from the M, L,\nand T dwarf compendium housed at DwarfArchives.org, whose\nserver was funded by a NASA Small Research Grant, administered by the American Astronomical Society. We are also indebted to the SIMBAD database, operated at CDS, Strasbourg, France. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued to program 70062 by JPL/Caltech. This work is also based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program 12330. Support for program 12330 was provided by NASA through a grant from the Space Telescope Science Institute. Some of the spectroscopic data presented\nherein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. In acknowledgement of our observing time at Keck and the IRTF, we further wish to recognize the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawai'ian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We acknowledge use of PAIRITEL, which is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, the camera loaned from the University of Virginia, and the continued support of the SAO and UC Berkeley. The PAIRITEL project is supported by NASA Grant NNX10AI28G. We thank Dan Starr, Cullen Blake, Adam Morgan, Adam Miller, and Chris Klein for their assistance. This paper also includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Portions of our Magellan telescope time were granted by the National Optical Astronomy Observatory (NOAO; Proposal ID 2010B-0184), through the Telescope System Instrumentation Program (TSIP). TSIP is funded by NOAO, which is operated by the Association of Universities for Research in Astronomy under cooperative agreement with the National Science Foundation. We thank Alan Tokunaga for granting director's discretionary time with IRTF/SpeX for some of the observations presented herein.\n\nPublished - Kirkpatrick2011p16850Astrophys_J_Suppl_S.pdf
Accepted Version - 1108.4677.pdf
", "abstract": "We present ground-based spectroscopic verification of 6 Y dwarfs (see also Cushing et al.), 89 T dwarfs, 8 L dwarfs, and 1 M dwarf identified by the Wide-field Infrared Survey Explorer (WISE). Eighty of these are cold brown dwarfs with spectral types \u2265T6, six of which have been announced earlier by Mainzer et al. and Burgasser et al. We present color-color and color-type diagrams showing the locus of M, L, T, and Y dwarfs in WISE color space. Near-infrared and, in a few cases, optical spectra are presented for these discoveries. Near-infrared classifications as late as early Y are presented and objects with peculiar spectra are discussed. Using these new discoveries, we are also able to extend the optical T dwarf classification scheme from T8 to T9. After deriving an absolute WISE 4.6 \u03bcm (W2) magnitude versus spectral type relation, we estimate spectrophotometric distances to our discoveries. We also use available astrometric measurements to provide preliminary trigonometric parallaxes to four of our discoveries, which have types of L9 pec (red), T8, T9, and Y0; all of these lie within 10 pc of the Sun. The Y0 dwarf, WISE 1541\u20132250, is the closest at 2.8^(+1.3)_(\u20130.6) pc; if this 2.8 pc value persists after continued monitoring, WISE 1541\u20132250 will become the seventh closest stellar system to the Sun. Another 10 objects, with types between T6 and >Y0, have spectrophotometric distance estimates also placing them within 10 pc. The closest of these, the T6 dwarf WISE 1506+7027, is believed to fall at a distance of ~4.9 pc. WISE multi-epoch positions supplemented with positional info primarily from the Spitzer/Infrared Array Camera allow us to calculate proper motions and tangential velocities for roughly one-half of the new discoveries. This work represents the first step by WISE to complete a full-sky, volume-limited census of late-T and Y dwarfs. Using early results from this census, we present preliminary, lower limits to the space density of these objects and discuss constraints on both the functional form of the mass function and the low-mass limit of star formation.", "date": "2011-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "197", "number": "2", "publisher": "American Astronomical Society", "pagerange": "19", "id_number": "CaltechAUTHORS:20120125-151623435", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120125-151623435", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NASA/JPL/Caltech", "grant_number": "70062" }, { "agency": "Space Telescope Science Institute", "grant_number": "NAG W-2166" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Harvard University Milton Fund" }, { "agency": "Smithsonian Astrophysical Observatory (SAO)" }, { "agency": "University of California, Berkeley" }, { "agency": "NASA", "grant_number": "NNX10AI28G" }, { "agency": "NSF" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Funding Council for England" }, { "agency": "NASA/Space Telescope Science Institute", "grant_number": "12330" }, { "agency": "University of Virginia" }, { "agency": "National Optical Astronomy Observatory (NOAO)", "grant_number": "2010B-0184" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0067-0049/197/2/19", "primary_object": { "basename": "1108.4677.pdf", "url": "https://authors.library.caltech.edu/records/b0cqk-a0592/files/1108.4677.pdf" }, "related_objects": [ { "basename": "Kirkpatrick2011p16850Astrophys_J_Suppl_S.pdf", "url": "https://authors.library.caltech.edu/records/b0cqk-a0592/files/Kirkpatrick2011p16850Astrophys_J_Suppl_S.pdf" } ], "pub_year": "2011", "author_list": "Kirkpatrick, J. Davy; Gelino, Christopher R.; et el." }, { "id": "https://authors.library.caltech.edu/records/yntxw-97159", "eprint_id": 28918, "eprint_status": "archive", "datestamp": "2023-08-22 04:09:11", "lastmod": "2023-10-24 18:14:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Fiore-F", "name": { "family": "Fiore", "given": "F." } }, { "id": "Gilli-R", "name": { "family": "Gilli", "given": "R." } }, { "id": "Hao-Heng", "name": { "family": "Hao", "given": "H." } }, { "id": "Ikeda-Hideyuki", "name": { "family": "Ikeda", "given": "H." } }, { "id": "Kakazu-Yuko", "name": { "family": "Kakazu", "given": "Y." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "D." }, "orcid": "0000-0001-5382-6138" }, { "id": "Miyaji-Takamitsu", "name": { "family": "Miyaji", "given": "T." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Puccetti-S", "name": { "family": "Puccetti", "given": "S." }, "orcid": "0000-0002-2734-7835" }, { "id": "Shankar-F", "name": { "family": "Shankar", "given": "F." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "C." }, "orcid": "0000-0002-8853-9611" }, { "id": "Zezas-A", "name": { "family": "Zezas", "given": "A." }, "orcid": "0000-0001-8952-676X" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" } ] }, "title": "The Population of High-Redshift Active Galactic Nuclei in the CHANDRA-Cosmos Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "evolution; galaxies: active; surveys; X-rays: galaxies", "note": "\u00a9 2011 The American Astronomical Society. Received 2010 December 23; accepted 2011 August 8; published 2011 October 21. The authors thank the referee for suggestions which improved this paper's content. The authors thank J. Aird and E. Glikman for sharing their luminosity functions, and G. Risaliti, R. D'Abrusco, and A. Goulding for useful discussions. This work was supported in part by NASA Chandra grant No. GO7-8136A (M.E., F.C., H.H.), the Blancheflor Boncompagni Ludovisi foundation (F.C.) and the Smithsonian Scholarly Studies (F.C.). F.S. acknowledges the Alexander von Humboldt Foundation for support. In Italy this work is supported by ASI/INAF contracts I/009/10/0 and I/088/06.\nFacilities: CXO (ACIS), HST (ACS), XMM\n\nPublished - Civano2011p16864Astrophys_J.pdf
", "abstract": "We present the high-redshift (3 3. Eighty-one sources are selected in the 0.5-2 keV band, fourteen are selected in the 2-10 keV and six in the 0.5-10 keV bands. We sample the high-luminosity (log L_((2-10keV)) > 44.15 erg s^(\u20131)) space density up to z ~ 5 and a fainter luminosity range (43.5 erg s^(\u20131) < log L_((2-10keV)) < 44.15 erg s^(\u20131)) than previous studies, up to z = 3.5. We weighted the contribution to the number counts and the space density of the sources with photometric redshift by using their probability of being at z > 3. We find that the space density of high-luminosity AGNs declines exponentially at all the redshifts, confirming the trend observed for optically selected quasars. At lower luminosity, the measured space density is not conclusive, and a larger sample of faint sources is needed. Comparisons with optical luminosity functions and black hole formation models are presented together with prospects for future surveys.", "date": "2011-11-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "741", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 91", "id_number": "CaltechAUTHORS:20120123-115613901", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120123-115613901", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO7-8136A" }, { "agency": "Blancheflor Boncompagni Ludovisi foundation" }, { "agency": "Smithsonian Institution" }, { "agency": "Alexander von Humboldt Foundation" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/009/10/0" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/088/06/0" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/741/2/91", "primary_object": { "basename": "Civano2011p16864Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/yntxw-97159/files/Civano2011p16864Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Civano, F.; Brusa, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/1hjw7-zsb93", "eprint_id": 29288, "eprint_status": "archive", "datestamp": "2023-08-22 04:05:37", "lastmod": "2023-10-24 22:04:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Black hole accretion and host galaxies of obscured\n quasars in XMM-COSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "quasars: general; galaxies: active; galaxies: nuclei; X-rays: general; galaxies: star formation", "note": "\u00a9 2011 ESO. Received 14 May 2011. Accepted 14 September 2011.\nPublished online: 11 November 2011. \n\n\nWe are grateful to Hagai Netzer for inspiring discussions\nand to Giulia Rodighiero for providing the Herschel curves in Fig. 9 in electronic\nformat. We thank the referee, Montse Villar-Martin, for a careful reading of the\nmanuscript and useful comments. This work is based on observations made\nwith ESO Telescopes at the La Silla/Paranal Observatories under the zCOSMOS\nLarge Programme 175.A-0839; the XMM-Newton satellite, an ESA science\nmission with instruments and contributions directly funded by ESA Member\nStates and the US (NASA); the Magellan Telescope, operated by the Carnegie\nObservatorie and the MMT Observatory, a joint facility of the University of\nArizona and the Smithsonian Institution; the Subaru Telescope, operated by the\nNational Astronomical Observatory of Japan; and the NASA/ESA Hubble Space\nTelescope, operated at the Space Telescope Science Institute, which is operated\nby AURA Inc, under NASA contract NAS 5-26555. Support from the Italian\nSpace Agency (ASI) under the contracts ASI-INAF I/088/06/0 and I/009/10/0\nis acknowledged. G.H. and M.S. acknowledge support by the German Deutsche\nForschungsgemeinschaft, DFG Leibniz Prize (FKZ HA 1850/28-1).\n\nPublished - Mainieri2011p17096Astron_Astrophys.pdf
", "abstract": "Aims. We explore the connection between black hole growth at the center of obscured quasars selected from the XMM-COSMOS survey and the physical properties of their host galaxies. We study a bolometric regime ( \u27e8 L_(bol) \u27e9 = 8 \u00d7 10^(45) erg s^(-1)) where several theoretical models invoke major galaxy mergers as the main fueling channel for black hole accretion.\nMethods. To derive robust estimates of the host galaxy properties, we use an SED fitting technique to distinguish the AGN and host galaxy emission. We evaluate the effect on galaxy properties estimates of being unable to remove the nuclear emission from the SED. The superb multi-wavelength coverage of the COSMOS field allows us to obtain reliable estimates of the total stellar masses and star formation rates (SFRs) of the hosts. We supplement this information with a morphological analysis of the ACS/HST images, optical spectroscopy, and an X-ray spectral analysis.\nResults. We confirm that obscured quasars mainly reside in massive galaxies (M_\u22c6 > 10^(10)M_\u2299) and that the fraction of galaxies hosting such powerful quasars monotonically increases with the stellar mass. We stress the limitation of the use of rest-frame color \u2212 magnitude diagrams as a diagnostic tool for studying galaxy evolution and inferring the influence that AGN activity can have on such a process. We instead use the correlation between SFR and stellar mass found for star-forming galaxies to discuss the physical properties of the hosts. We find that at z ~ 1, \u224862% of Type-2 QSOs hosts are actively forming stars and that their rates are comparable to those measured for normal star-forming galaxies. The fraction of star-forming hosts increases with redshift: \u2248 71% at z ~ 2, and 100% at z ~ 3. We also find that the evolution from z ~ 1 to z ~ 3 of the specific SFR of the Type-2 QSO hosts is in excellent agreement with that measured for star-forming galaxies. From the morphological analysis, we conclude that most of the objects are bulge-dominated galaxies, and that only a few of them exhibit signs of recent mergers or disks. Finally, bulge-dominated galaxies tend to host Type-2 QSOs with low Eddington ratios (\u03bb < 0.1), while disk-dominated or merging galaxies have at their centers BHs accreting at high Eddington ratios (\u03bb > 0.1).", "date": "2011-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "535", "publisher": "EDP Sciences", "pagerange": "Art. No. A80", "id_number": "CaltechAUTHORS:20120214-151514942", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120214-151514942", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "zCOSMOS", "grant_number": "175.A-0839" }, { "agency": "ESA Member States" }, { "agency": "NASA" }, { "agency": "Carnegie Observatory Magellan Telescope" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "University of Arizona" }, { "agency": "Smithsonian Institution" }, { "agency": "ASI-INAF", "grant_number": "I/088/06/0" }, { "agency": "ASI-INAF", "grant_number": "I/009/10/0" }, { "agency": "German Deutsche Forschungsgemeinschaft (DFG) Leibniz Prize", "grant_number": "HA 1850/28-1" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201117259", "primary_object": { "basename": "Mainieri2011p17096Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/1hjw7-zsb93/files/Mainieri2011p17096Astron_Astrophys.pdf" }, "pub_year": "2011", "author_list": "Mainieri, V.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/fw1wm-gpp35", "eprint_id": 29278, "eprint_status": "archive", "datestamp": "2023-08-22 04:05:25", "lastmod": "2023-10-24 22:03:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The bimodality of the 10k zCOSMOS-bright galaxies up to z\u2009 ~ 1: a new statistical and portable classification based on optical galaxy properties", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: general; galaxies: evolution; galaxies: fundamental parameters", "note": "\u00a9 2011 ESO. Article published by EDP Sciences. \nReceived 11 November 2010; Accepted 3 August 2011.\nPublished online 25 October 2011.\nBased on observations undertaken at the European Southern\nObservatory (ESO) Very Large Telescope (VLT) under Large Program\n175.A-0839. Also based on observations with the NASA/ESA Hubble\nSpace Telescope, obtained at the Space Telescope Science Institute, operated\nby AURA Inc., under NASA contract NAS 5-26555, with the\nSubaru Telescope, operated by the National Astronomical Observatory\nof Japan, with the telescopes of the National Optical Astronomy\nObservatory, operated by the Association of Universities for Research\nin Astronomy, Inc. (AURA) under cooperative agreement with the\nNational Science Foundation, and with the Canada-France-Hawaii\nTelescope, operated by the National Research Council of Canada,\nthe Centre National de la Recherche Scientifique de France, and the\nUniversity of Hawaii.\nThis work was partially supported by INAF under PRIN-2006/1.06.10.08 and by ASI under grant ASI/COFIS I/016/07/0.\n\nPublished - Coppa2011p17084Astron_Astrophys.pdf
", "abstract": "Aims. Our goal is to develop a new and reliable statistical method to classify galaxies from large surveys. We probe the reliability of the method by comparing it with a three-dimensional classification cube, using the same set of spectral, photometric and morphological parameters.\n\nMethods. We applied two different methods of classification to a sample of galaxies extracted from the zCOSMOS redshift survey, in the redshift range 0.5 \u2272 z \u2272 1.3. The first method is a combination of three independent classification schemes \u2013 a spectroscopic one based on the strength of the continuum break at 4000 \u00c5 and the rest-frame equivalent width of the [O\u2009ii] emission line, a photometric one based on the observed B \u2212 z colours, and a morphological one. The second method exploits an entirely new approach based on statistical analyses like principal component analysis (PCA) and unsupervised fuzzy partition (UFP) clustering method. The PCA+UFP method has also been applied to a lower redshift sample (z \u2272 0.5), exploiting the same set of data but replacing the spectroscopic indicators with the equivalent width of H\u03b1.\n\nResults. The comparison between the two methods shows fairly good agreement on the definition on the two main populations, the early-type and the late-type galaxies. Our PCA+UFP method of classification is robust, flexible and capable of identifying the two main populations of galaxies as well as an intermediate population. The intermediate galaxy population shows many of the properties of \"green valley\" galaxies, and constitutes a more coherent and homogeneous population. The large redshift range of the studied sample allows us to characterize downsizing: galaxies with masses of the order of 3 \u00d7 10^(10) M_\u2299 are predominantly found in the transition from the late-type to the early-type group at z > 0.5, while galaxies with lower masses, of the order of 10^(10) M_\u2299, are in transition at later epochs. Galaxies with M < 10^(10) M_\u2299 have not yet begun to transition, while galaxies with very large masses (M > 5 \u00d7 10^(10 M_\u2299) have mostly completed their transition to the early-type regime before z ~ 1.", "date": "2011-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "535", "publisher": "EDP Sciences", "pagerange": "A10", "id_number": "CaltechAUTHORS:20120214-111508456", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120214-111508456", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "INAF", "grant_number": "PRIN-2006/1.06.10.08" }, { "agency": "ASI", "grant_number": "ASI/COFIS I/016/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201016130", "primary_object": { "basename": "Coppa2011p17084Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/fw1wm-gpp35/files/Coppa2011p17084Astron_Astrophys.pdf" }, "pub_year": "2011", "author_list": "Coppa, G.; Scarlata, C.; et el." }, { "id": "https://authors.library.caltech.edu/records/7gzv5-4qa97", "eprint_id": 28671, "eprint_status": "archive", "datestamp": "2023-08-22 04:04:58", "lastmod": "2023-10-24 18:04:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pierini-D", "name": { "family": "Pierini", "given": "D." } }, { "id": "Giodini-S", "name": { "family": "Giodini", "given": "S." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "B\u00f6hringer-H", "name": { "family": "B\u00f6hringer", "given": "H." } }, { "id": "D'Onghia-E", "name": { "family": "D'Onghia", "given": "E." } }, { "id": "Pratt-G-W", "name": { "family": "Pratt", "given": "G. W." } }, { "id": "D\u00e9mocl\u00e8s-J", "name": { "family": "D\u00e9mocl\u00e8s", "given": "J." } }, { "id": "Pannella-M", "name": { "family": "Pannella", "given": "M." } }, { "id": "Zibetti-S", "name": { "family": "Zibetti", "given": "S." } }, { "id": "Braglia-F-G", "name": { "family": "Braglia", "given": "F. G." } }, { "id": "Verdugo-M", "name": { "family": "Verdugo", "given": "M." } }, { "id": "Ziparo-F", "name": { "family": "Ziparo", "given": "F." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" } ] }, "title": "Two fossil groups of galaxies at z \u2248 0.4 in the Cosmic Evolution Survey: accelerated stellar-mass build-up, different progenitors", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: groups: general; galaxies: luminosity function, mass function; X-rays: galaxies: clusters", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. Accepted 2011 July 14. Received 2011 July 14; in original form 2011 January 21. Article first published online: 8 Sep 2011. We thank the referee, Paul Eigenthaler, for a careful reading of the\noriginal version of the paper and the useful comments that improved the presentation of the paper. DP acknowledges the kind and fruitful hospitality at the Max-Planck-Institut f\u00fcr extraterrestrische Physik (MPE).\n\nPublished - Pierini2011p16549Mon_Not_R_Astron_Soc.pdf
", "abstract": "We report on two fossil groups of galaxies at redshifts z= 0.425 and 0.372 discovered in the Cosmic Evolution Survey (COSMOS) area. Selected as X-ray extended sources, they have total masses (M_(200)) equal to 1.9(\u00b10.41) \u00d7 10^(13) and 9.5(\u00b10.42) \u00d7 10^(13) M_\u2299, respectively, as obtained from a recent X-ray luminosity\u2013mass scaling relation. The lower mass system appears isolated, whereas the other sits in a well-known large-scale structure (LSS) populated by 27 other X-ray emitting groups. The identification as fossil is based on the i-band photometry of all the galaxies with a photometric redshift consistent with that of the group at the 2\u03c3 confidence level and within a projected groupcentric distance equal to 0.5R_(200), and i_(AB)\u2264 22.5 mag limited spectroscopy. Both fossil groups exhibit high stellar-to-total mass ratios compared to all the X-ray selected groups of similar mass at 0.3 \u2264z\u2264 0.5 in the COSMOS. At variance with the composite galaxy stellar mass functions (GSMFs) of similarly massive systems, both fossil group GSMFs are dominated by passively evolving galaxies down to M^(stars)\u223c 10^(10) M_\u2299 (according to the galaxy broad-band spectral energy distributions). The relative lack of star-forming galaxies with 10^(10) \u2264 M^(stars) \u2264 10^(11) M_\u2299 is confirmed by the galaxy distribution in the b\u2212r versus i colour\u2013magnitude diagram. Hence, the two fossil groups appear as more mature than the coeval, similarly massive groups. Their overall star formation activity ended rapidly after an accelerated build up of the total stellar mass; no significant infall of galaxies with M^(stars) \u2265 10^(10) M_\u2299 took place in the last 3 to 6 Gyr. This similarity holds although the two fossil groups are embedded in two very different density environments of the LSS, which suggests that their galaxy populations were shaped by processes that do not depend on the LSS. However, their progenitors may do so. We discuss why the late merging of a compact group is favoured over the early assembly as a formation scenario for the isolated, low-mass fossil group.", "date": "2011-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "417", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "2927-2937", "id_number": "CaltechAUTHORS:20120105-111108015", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120105-111108015", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "COSMOS Collaboration" ] }, "doi": "10.1111/j.1365-2966.2011.19454.x", "primary_object": { "basename": "Pierini2011p16549Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/7gzv5-4qa97/files/Pierini2011p16549Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2011", "author_list": "Pierini, D.; Giodini, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/jye6s-vg219", "eprint_id": 28652, "eprint_status": "archive", "datestamp": "2023-08-22 03:51:27", "lastmod": "2023-10-24 18:03:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dom\u00ednguez-S\u00e1nchez-H", "name": { "family": "Dom\u00ednguez-S\u00e1nchez", "given": "H." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "The evolution of quiescent galaxies at high redshifts (z \u2265 1.4)", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: star formation", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. Accepted 2011 June 15. Received 2011 June 15; in original form 2011 March 30. Article first published online: 15 Sep 2011. This work was supported by an International grant from Instituto\nde Astrof\u00edsica de Canarias (IAC) with funding from the Research Structures Departments of Instituto Nazionale di Astrof\u00edsica (INAF). We thank the anonymous referee for the useful comments which helped to improve the original manuscript.\n\nPublished - DominguezSanchez2011p16660Mon_Not_R_Astron_Soc.pdf
", "abstract": "The goal of this work is to study the evolution of high-redshift (z \u2265 1.4) quiescent galaxies over an effective area of ~ 1.7 deg^2 in the COSMOS field. Galaxies have been divided according to their star formation activity and the evolution of the different populations, in particular of the quiescent galaxies, has been investigated in detail. We have studied an IRAC (ma_( 3.6 \u03bcm) < 22.0) selected sample of ~ 18 000 galaxies at z \u2265 1.4 in the COSMOS field with multiwavelength coverage extending from the U band to the Spitzer 24 \u03bcm one. We have derived accurate photometric redshifts (\u03c3_(\u0394z/(1+zs)) = 0.06) through a SED-fitting procedure. Other important physical parameters [masses, ages and star formation rates (SFR)] of the galaxies have been obtained using Maraston models. We have divided our sample into actively star-forming, intermediate and quiescent galaxies depending on their specific star formation rate (SSFR = SFR/M). We have computed the galaxy stellar mass function (GSMF) of the total sample and the different populations at z = 1.4\u20133.0. We have studied the properties of high-redshift quiescent galaxies finding that they are old (1\u20134 Gyr), massive (\u3008M\u3009~ 10^(10.65) M_\u2299), weakly star-forming stellar populations with low dust extinction [E(B\u2212V) \u2264 0.15] and small e-folding time-scales (\u03c4~ 0.1\u20130.3 Gyr). We observe a significant evolution of the quiescent stellar mass function from 2.5 < z < 3.0 to 1.4 < z < 1.6, increasing by ~1 dex in this redshift interval. We find that z ~ 1.5 is an epoch of transition of the GSMF: while the GSMF at z \u2273 1.5 is dominated by the star-forming galaxies at all stellar masses, at z \u2272 1.5 the contribution to the total GSMF of the quiescent galaxies is significant and becomes higher than that of the star-forming population for M \u2265 10^(10.75) M_\u2299. The fraction of star-forming galaxies decreases from 60\u201320 per cent from z ~ 2.5\u20133.0 to 1.4\u20131.6 for M~10^(11.0) M_\u2299, while the quiescent population increases from 10\u201350 per cent at the same redshift and mass intervals. We compare the fraction of quiescent galaxies derived with that predicted by theoretical models and find that the Kitzbichler & White model, implemented on the Millennium Simulation, is the one that better reproduces the shape of the data. Finally, we calculate the stellar mass density of the star-forming and quiescent populations as a function of redshift and find that there is already a significant number of quiescent galaxies at z > 2.5 (log_\u03c1[M_\u2299 Mpc^(\u22123)]~ 6), meaning that efficient star formation had to take place before that time.", "date": "2011-10", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "417", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "900-915", "id_number": "CaltechAUTHORS:20120104-131920085", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120104-131920085", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Instituto de Astrofisica de Canarias (IAC)" }, { "agency": "Instituto Nazionale di Astrofisica (INAF) Research Structures Departments" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1111/j.1365-2966.2011.19263.x", "primary_object": { "basename": "DominguezSanchez2011p16660Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/jye6s-vg219/files/DominguezSanchez2011p16660Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2011", "author_list": "Dom\u00ednguez-S\u00e1nchez, H. and Capak, P." }, { "id": "https://authors.library.caltech.edu/records/tn5f1-hnn66", "eprint_id": 27990, "eprint_status": "archive", "datestamp": "2023-08-22 03:50:52", "lastmod": "2023-10-24 17:33:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Riguccini-L", "name": { "family": "Riguccini", "given": "L." } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Dust-obscured star formation and the contribution of galaxies escaping UV/optical color selections at z ~ 2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; infrared: galaxies; cosmology: observations", "note": "\u00a9 2011 ESO. Article published by EDP Sciences.\n\nReceived 24 March 2011; Accepted 31 May 2011.\nPublished online 06 October 2011.\nIt is a pleasure to acknowledge the contribution from all our colleagues in the COSMOS collaboration. More information on the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. This work is based on observations made with the Spitzer Space Telescope, a facility operated by NASA/JPL. Financial supports were provided by NASA through contracts Nos. 1289085, 1310136, 1282612, and 1298231 issued by the Jet Propulsion Laboratory. We also want to warmly thank our referee for his/her critical review of the manuscript, as well as Tanio D\u00edaz-Santos for useful discussions related to our work. We are finally grateful to Marc Sauvage for his help and for his useful and numerous comments.\n\nPublished - Riguccini2011p16336Astron_Astrophys.pdf
", "abstract": "Context. A substantial amount of the stellar mass growth across cosmic time occurred within dust-enshrouded environments. So far, identification of complete samples of distant star-forming galaxies from the short wavelength range has been strongly biased by the effect of dust extinction. Nevertheless, the exact amount of star-forming activity that took place in high-redshift dusty galaxies but that has currently been missed by optical surveys has barely been explored.\n\nAims. Our goal is to determine the number of luminous star-forming galaxies at 1.5 \u2272 z \u2272 3 that are potentially missed by the traditional color selection techniques because of dust extinction. We also aim at quantifying the contribution of these sources to the IR luminosity and cosmic star formation density at high redshift.\n\nMethods. We based our work on a sample of 24 \u03bcm sources brighter than 80 \u03bcJy and taken from the Spitzer survey of the COSMOS field. Almost all of these sources have accurate photometric redshifts. We applied to this mid-IR selected sample the BzK and BM/BX criteria, as well as the selections of the IRAC peakers and the Optically-Faint IR-bright (OFIR) galaxies. We analyzed the fraction of sources identified with these techniques. We also computed 8 \u03bcm rest-frame luminosity from the 24 \u03bcm fluxes of our sources, and considering the relationships between L_(8\u03bcm) and L_(Pa_\u03b1) and between L_(8\u03bcm) and L_IR, we derived \u03c1IR and then \u03c1_SFR for our MIPS sources.\n\nResults. The BzK criterion offers an almost complete (~90%) identification of the 24 \u03bcm sources at 1.4 < z < 2.5. In contrast, the BM/BX criterion misses 50% of the MIPS sources. We attribute this bias to the effect of extinction, which reddens the typical colors of galaxies. The contribution of these two selections to the IR luminosity density produced by all the sources brighter than 80 \u03bcJy are on the same order. Moreover the criterion based on the presence of a stellar bump in their spectra (IRAC peakers) misses up to 40% of the IR luminosity density, while only 25% of the IR luminosity density at z ~ 2 is produced by OFIR galaxies characterized by extreme mid-IR to optical flux ratios.\n\nConclusions. Color selections of distant star-forming galaxies must be used with care given the substantial bias they can suffer. In particular, the effect of dust extinction strongly affects the completeness of identifications at the bright end of the bolometric luminosity function, which implies large and uncertain extrapolations to account for the contribution of dusty galaxies missed by these selections. In the context of forthcoming facilities that will operate at long wavelengths (e.g., JWST, ALMA, SAFARI, EVLA, SKA), this emphasizes the importance of minimizing the extinction biases when probing the activity of star formation in the early Universe.", "date": "2011-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "534", "publisher": "EDP Sciences", "pagerange": "A81", "id_number": "CaltechAUTHORS:20111129-101708704", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111129-101708704", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1289085" }, { "agency": "NASA", "grant_number": "1310136" }, { "agency": "NASA", "grant_number": "1282612" }, { "agency": "NASA", "grant_number": "1298231" }, { "agency": "JPL" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "COSMOS Collaboration" ] }, "doi": "10.1051/0004-6361/201116950", "primary_object": { "basename": "Riguccini2011p16336Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/tn5f1-hnn66/files/Riguccini2011p16336Astron_Astrophys.pdf" }, "pub_year": "2011", "author_list": "Riguccini, L.; Le Floc'h, E.; et el." }, { "id": "https://authors.library.caltech.edu/records/gqy2e-kc451", "eprint_id": 25256, "eprint_status": "archive", "datestamp": "2023-08-22 03:36:57", "lastmod": "2023-10-24 15:44:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dwek-E", "name": { "family": "Dwek", "given": "Eli" }, "orcid": "0000-0001-8033-1181" }, { "id": "Staguhn-J-G", "name": { "family": "Staguhn", "given": "Johannes G." }, "orcid": "0000-0002-8437-0433" }, { "id": "Arendt-R-G", "name": { "family": "Arendt", "given": "Richard G." }, "orcid": "0000-0001-8403-8548" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Kovacs-A", "name": { "family": "Kovacs", "given": "Attila" } }, { "id": "Benford-D-J", "name": { "family": "Benford", "given": "Dominic J." }, "orcid": "0000-0002-9884-4206" }, { "id": "Fixsen-D-J", "name": { "family": "Fixsen", "given": "Dale" } }, { "id": "Karim-A", "name": { "family": "Karim", "given": "Alexander" }, "orcid": "0000-0002-8414-9579" }, { "id": "Leclercq-S", "name": { "family": "Leclercq", "given": "Samuel" } }, { "id": "Maher-S-F", "name": { "family": "Maher", "given": "Stephen F." } }, { "id": "Moseley-S-H", "name": { "family": "Moseley", "given": "Samuel H." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Sharp-E-H", "name": { "family": "Sharp", "given": "Elmer H." } } ] }, "title": "Star and Dust Formation Activities in AzTEC-3, a Starburst Galaxy at z = 5.3", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: starburst; infrared: galaxies", "note": "\u00a9 2011 The American Astronomical Society. \n\nReceived 2011 May 16; accepted 2011 June 8; published 2011 August 10. \n\nE.D. acknowledges helpful discussions with Dominik Riechers. GISMO millimeter observations used in the analysis were supported through NSF grants AST-0705185 and AST-1020981.\n\nPublished - Dwek2011p15678Astrophys_J.pdf
Accepted Version - 1106.2092.pdf
", "abstract": "Analyses of high-redshift ultraluminous infrared (IR) galaxies traditionally use the observed optical to submillimeter spectral energy distribution (SED) and estimates of the dynamical mass as observational constraints to derive the star formation rate (SFR), the stellar mass, and age of these objects. An important observational constraint neglected in the analysis is the mass of dust giving rise to the IR emission. In this paper we add this constraint to the analysis of AzTEC-3. Adopting an upper limit to the mass of stars and a bolometric luminosity for this object, we construct different stellar and chemical evolutionary scenarios, constrained to produce the inferred dust mass and observed luminosity before the associated stellar mass exceeds the observational limit. We use the P\u00c9GASE population synthesis code and a chemical evolution model to follow the evolution of the galaxy's SED and its stellar and dust masses as a function of galactic age for seven different stellar initial mass functions (IMFs). We find that the model with a Top Heavy IMF provided the most plausible scenario consistent with the observational constraints. In this scenario the dust formed over a period of ~200 Myr, with an SFR of ~500 M_\u2609 yr^(\u20131). These values for the age and SFR in AzTEC-3 are significantly higher and lower, respectively, from those derived without the dust mass constraint. However, this scenario is not unique, and others cannot be completely ruled out because of the prevailing uncertainties in the age of the galaxy, its bolometric luminosity, and its stellar and dust masses. A robust result of our models is that all scenarios require most of the radiating dust mass to have been accreted in molecular clouds. Our new procedure highlights the importance of a multiwavelength approach, and of the use of dust evolution models in constraining the age and the star formation activity and history in galaxies.", "date": "2011-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "738", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 36", "id_number": "CaltechAUTHORS:20110908-113958497", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110908-113958497", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0705185" }, { "agency": "NSF", "grant_number": "AST-1020981" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/738/1/36", "primary_object": { "basename": "1106.2092.pdf", "url": "https://authors.library.caltech.edu/records/gqy2e-kc451/files/1106.2092.pdf" }, "related_objects": [ { "basename": "Dwek2011p15678Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/gqy2e-kc451/files/Dwek2011p15678Astrophys_J.pdf" } ], "pub_year": "2011", "author_list": "Dwek, Eli; Staguhn, Johannes G.; et el." }, { "id": "https://authors.library.caltech.edu/records/ky8cw-wyd83", "eprint_id": 25441, "eprint_status": "archive", "datestamp": "2023-08-22 03:20:49", "lastmod": "2023-10-24 15:52:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aretxaga-I", "name": { "family": "Aretxaga", "given": "I." }, "orcid": "0000-0002-6590-3994" }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G. W." } }, { "id": "Aguilar-E", "name": { "family": "Aguilar", "given": "E." } }, { "id": "Alberts-S", "name": { "family": "Alberts", "given": "S." } }, { "id": "Scott-K-S", "name": { "family": "Scott", "given": "K. S." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "M. S." }, "orcid": "0000-0001-7095-7543" }, { "id": "Austermann-J", "name": { "family": "Austermann", "given": "J." } }, { "id": "Downes-T-P", "name": { "family": "Downes", "given": "T. P." } }, { "id": "Ezawa-Hajime", "name": { "family": "Ezawa", "given": "H." } }, { "id": "Hatsukade-Bunyo", "name": { "family": "Hatsukade", "given": "B." } }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "D. H." } }, { "id": "Kawabe-Ryohei", "name": { "family": "Kawabe", "given": "R." }, "orcid": "0000-0002-8049-7525" }, { "id": "Kohno-Kotaro", "name": { "family": "Kohno", "given": "K." }, "orcid": "0000-0002-4052-2394" }, { "id": "Oshima-Takeharu", "name": { "family": "Oshima", "given": "T." } }, { "id": "Perera-T-A", "name": { "family": "Perera", "given": "T. A." } }, { "id": "Tamura-Yoichi", "name": { "family": "Tamura", "given": "Y." } }, { "id": "Zeballos-M", "name": { "family": "Zeballos", "given": "M." } } ] }, "title": "AzTEC millimetre survey of the COSMOS field \u2013 III. Source catalogue over 0.72 deg^2 and plausible boosting by large-scale structure", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys; galaxies: evolution; cosmology: miscellaneous; submillimetre: galaxies", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. \n\nAccepted 2011 April 28. Received 2011 April 26; in original form 2011 February 4. Article first published online: 19 Jul 2011. \n\nThis work has been supported in part by Conacyt (Mexico) grants 39953-F and 39548-F, NSF (USA) grants AST-0907952 and AST-0838222, and by the MEXT Grant-in-Aid for Specially Promoted Research (No. 20001003). Observations with ASTE carried out remotely from Japan used NNT's GEMnet2 and its partner R&E networks, which are based on the AccessNova collaboration of the University of Chile, NTT Laboratories and the NOAJ. We would like to thank everyone who supported the AzTEC/ASTE observations of the COSMOS field, including E. Akiyama, R. Cybulski, K. Fukue, S. Harasawa, S. Ikarashi, H. Inoue, M. Kawamura, A. Kuboi, J. Rand, M. Tashiro, T. Tosaki, T. Tsukagoshi, Y. Shimajiri and C. Williams. The ASTE project is driven by the Nobeyama Radio Observatory (NRO), a branch of the National Astronomical Observatory of Japan (NAOJ), in collaboration with the University of Chile and Japanese institutions including the University of Tokyo, Nagoya University, Osaka Prefecture University, Ibaraki University and Hokkaido University.\n\nPublished - Aretxaga2011p15879Mon_Not_R_Astron_Soc.pdf
", "abstract": "We present a 0.72 deg^2 contiguous 1.1-mm survey in the central area of the Cosmological Evolution Survey field carried out to a 1\u03c3 \u2248 1.26 mJy beam^(\u22121) depth with the AzTEC camera mounted on the 10-m Atacama Submillimeter Telescope Experiment. We have uncovered 189 candidate sources at a signal-to-noise ratio (S/N) \u2265 3.5, out of which 129, with S/N \u2265 4, can be considered to have little chance of being spurious (\u2272 2 per cent). We present the number counts derived with this survey, which show a significant excess of sources when compared to the number counts derived from the ~0.5 deg^2 area sampled at similar depths in the Submillimetre Common-User Bolometer Array (SCUBA) HAlf Degree Extragalactic Survey (SHADES). They are, however, consistent with those derived from fields that were considered too small to characterize the overall blank-field population. We identify differences to be more significant in the S_(1.1mm) \u2273 5 mJy regime, and demonstrate that these excesses in number counts are related to the areas where galaxies at redshifts z \u2272 1.1 are more densely clustered. The positions of optical\u2013infrared galaxies in the redshift interval 0.6 \u2272 z \u2272 0.75 are the ones that show the strongest correlation with the positions of the 1.1-mm bright population (S_(1.1mm) \u2273 5 mJy), a result which does not depend exclusively on the presence of rich clusters within the survey sampled area. The most likely explanation for the observed excess in number counts at 1.1-mm is galaxy\u2013galaxy and galaxy\u2013group lensing at moderate amplification levels, which increases in amplitude as one samples larger and larger flux densities. This effect should also be detectable in other high-redshift populations.", "date": "2011-08", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "415", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3831-3850", "id_number": "CaltechAUTHORS:20110927-072547840", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110927-072547840", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "39953-F" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "39548-F" }, { "agency": "NSF", "grant_number": "AST-0907952" }, { "agency": "NSF", "grant_number": "AST-0838222" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "20001003" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2011.18989.x", "primary_object": { "basename": "Aretxaga2011p15879Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/ky8cw-wyd83/files/Aretxaga2011p15879Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2011", "author_list": "Aretxaga, I.; Wilson, G. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/c9vdx-06812", "eprint_id": 24618, "eprint_status": "archive", "datestamp": "2023-08-22 03:13:51", "lastmod": "2023-10-23 23:30:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Norris-R-P", "name": { "family": "Norris", "given": "Ray P." }, "orcid": "0000-0002-4597-1906" }, { "id": "Afonso-J", "name": { "family": "Afonso", "given": "Jos\u00e9" }, "orcid": "0000-0002-9149-2973" }, { "id": "Cava-A", "name": { "family": "Cava", "given": "Antonio" } }, { "id": "Farrah-D", "name": { "family": "Farrah", "given": "Duncan" }, "orcid": "0000-0003-1748-2010" }, { "id": "Huynh-Minh-T", "name": { "family": "Huynh", "given": "Minh T." } }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Jarvis-M-J", "name": { "family": "Jarvis", "given": "Matt" }, "orcid": "0000-0001-7039-9078" }, { "id": "Lacy-M", "name": { "family": "Lacy", "given": "Mark" }, "orcid": "0000-0002-3032-1783" }, { "id": "Mao-Minnie-Y", "name": { "family": "Mao", "given": "Minnie" } }, { "id": "Maraston-C", "name": { "family": "Maraston", "given": "Claudia" }, "orcid": "0000-0001-7711-3677" }, { "id": "Mauduit-J-C", "name": { "family": "Mauduit", "given": "Jean-Christophe" } }, { "id": "Middelberg-E", "name": { "family": "Middelberg", "given": "Enno" } }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "Seb" }, "orcid": "0000-0001-7862-1032" }, { "id": "Seymour-N", "name": { "family": "Seymour", "given": "Nick" }, "orcid": "0000-0003-3506-5536" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "Deep Spitzer Observations of Infrared-faint Radio Sources: High-redshift Radio-loud Active Galactic Nuclei?", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: starburst", "note": "\u00a9 2011 American Astronomical Society.\n\nReceived 2010 April 6; accepted 2011 May 4; published 2011 July 6.\n\nThis work is based in part on observations made with\nSpitzer, which is operated by the Jet Propulsion Laboratory,\nCalifornia Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an\naward issued by JPL/Caltech. This research has made use\nof the NASA/IPAC Extragalactic Database (NED) which is\noperated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. J.A. gratefully acknowledges the support from the Science and Technology Foundation (FCT, Portugal) through the research grant PTDC/FIS/100170/2008. M.Y.M. acknowledges the support of an Australian Postgraduate Award as well as Postgraduate Scholarships from AAO and ATNF. We thank P. Barmby for providing unpublished details of her source density calculations, Barnaby Norris for generating the stacked median image, and George Hobbs for helpful comments\non the pulsar density at high galactic latitude.\n\nPublished - Norris2011p15387Astrophys_J.pdf
", "abstract": "Infrared-faint radio sources (IFRSs) are a rare class of objects which are relatively bright at radio wavelengths but very faint at infrared and optical wavelengths. Here we present sensitive near-infrared observations of a sample of these sources taken as part of the Spitzer Extragalactic Representative Volume Survey. Nearly all the IFRSs are undetected at a level of ~1 \u03bcJy in these new deep observations, and even the detections are consistent with confusion with unrelated galaxies. A stacked image implies that the median flux density is S_(3.6 \u03bcm) ~ 0.2 \u03bcJy or less, giving extreme values of the radio-infrared flux density ratio. Comparison of these objects with known classes of object suggests that the majority are probably high-redshift radio-loud galaxies, possibly suffering from significant dust extinction.", "date": "2011-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "736", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 55", "id_number": "CaltechAUTHORS:20110801-133216892", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110801-133216892", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "PTDC/FIS/100170/2008" }, { "agency": "Australian Postgraduate Award" }, { "agency": "AAO Postgraduate Scholarship" }, { "agency": "ATNF Postgraduate Scholarship" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/736/1/55", "primary_object": { "basename": "Norris2011p15387Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/c9vdx-06812/files/Norris2011p15387Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Norris, Ray P.; Afonso, Jos\u00e9; et el." }, { "id": "https://authors.library.caltech.edu/records/6st5z-w8f32", "eprint_id": 23644, "eprint_status": "archive", "datestamp": "2023-08-22 02:37:03", "lastmod": "2023-10-23 19:49:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Conselice-C-J", "name": { "family": "Conselice", "given": "C. J." }, "orcid": "0000-0003-1949-7638" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Siana-Brian-D", "name": { "family": "Siana", "given": "B." }, "orcid": "0000-0002-4935-9511" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H." }, "orcid": "0000-0002-7064-5424" } ] }, "title": "The Hubble Space Telescope GOODS NICMOS Survey: overview\n and the evolution of massive galaxies at 1.5 < z < 3", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: structure", "note": "\u00a9 2011 The Authors. \n\nMonthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. \nAccepted 2010 November 26. Received 2010 November 17; in original form 2010 August 28. Article first published online: 23 Feb 2011. The data and catalogues as used in the GNS survey are online at http://www.nottingham.ac.uk/astronomy/gns/. We thank Will Hartley for providing diagnostic lines of stellar populations and Omar\nAlmaini for discussions on various aspects of this analysis. We thank STFC for support through studentships and PDRA funding. Support was also provided by NASA/STScI grant HST-GO11082. SJ and TW acknowledge support from the National Aeronautics and Space Administration (NASA) LTSA grant NAG5-13063, NSF grant AST-0607748 and HST grant GO-11082 from STScI, which is operated by AURA, Inc., for NASA, under NAS5-26555.\n\nPublished - Conselice2011p13723Mon_Not_R_Astron_Soc.pdf
", "abstract": "We present the details and early results from a deep near-infrared survey utilizing the NICMOS instrument on the Hubble Space Telescope centred around massive M_* > 10^(11) M_\u2299 galaxies at 1.7 < z < 2.9 found within the Great Observatories Origins Deep Survey (GOODS) fields North and South. The GOODS NICMOS Survey (GNS) was designed to obtain deep F160W (H-band) imaging of 80 of these massive galaxies and other colour-selected objects such as Lyman-break dropouts, BzK objects, distant red galaxies (DRGs), extremely red objects (EROs), Spitzer-selected EROs, BX/BM galaxies, as well as flux-selected submillimetre galaxies. We present in this paper details of the observations, our sample selection, as well as a description of the properties of the massive galaxies found within our survey fields. This includes photometric redshifts, rest-frame colours and stellar masses. We furthermore provide an analysis of the selection methods for finding massive galaxies at high redshifts, including colour-selection methods and how galaxy populations selected through these colour methods overlap. We find that a single colour selection method cannot locate all of the massive galaxies, with no one method finding more than 70 per cent. We however find that the combination of these colour methods finds nearly all of the massive galaxies that would have been identified in a photometric redshift sample, with the exception of apparently rare blue massive galaxies. By investigating the rest-frame (U\u2212B) versus MB diagram for these galaxies, we furthermore show that there exists a bimodality in colour\u2013magnitude space at z < 2, driven by stellar mass, such that the most massive galaxies are systematically red up to z\u223c 2.5, while lower mass galaxies tend to be blue. We also discuss the number densities for galaxies with stellar masses M_* > 10^(11) M_\u2299, whereby we find an increase of a factor of 8 between z= 3 and 1.5, demonstrating that this is an epoch when massive galaxies establish most of their stellar mass. We also provide an overview of the evolutionary properties of these galaxies, such as their merger histories, and size evolution.", "date": "2011-05", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "413", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "80-100", "id_number": "CaltechAUTHORS:20110511-113157983", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110511-113157983", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "PDRA" }, { "agency": "NASA", "grant_number": "NAG5-13063" }, { "agency": "NSF", "grant_number": "AST-0607748" }, { "agency": "NASA", "grant_number": "HST-GO-11082" }, { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2010.18113.x", "primary_object": { "basename": "Conselice2011p13723Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/6st5z-w8f32/files/Conselice2011p13723Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2011", "author_list": "Conselice, C. J.; Chary, R.-R.; et el." }, { "id": "https://authors.library.caltech.edu/records/ejs41-qhd12", "eprint_id": 23546, "eprint_status": "archive", "datestamp": "2023-08-19 06:19:02", "lastmod": "2023-10-23 19:44:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Faure-C", "name": { "family": "Faure", "given": "C." } }, { "id": "Anguita-T", "name": { "family": "Anguita", "given": "T." } }, { "id": "Alloin-D", "name": { "family": "Alloin", "given": "D." } }, { "id": "Bundy-K-A", "name": { "family": "Bundy", "given": "K." }, "orcid": "0000-0001-9742-3138" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Jullo-E", "name": { "family": "Jullo", "given": "E." }, "orcid": "0000-0002-9253-053X" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L. A. M." } } ] }, "title": "On the evolution of environmental and mass properties of strong lens galaxies in COSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: strong", "note": "\u00a9 2011 ESO. Received 19 October 2009, Accepted 12 February 2011, Published online 05 April 2011. Based on observations made with ESO telescopes at Paranal observatory\nunder program ID 077.A-0473(A) and under large program\nID 175.A-083911. We acknowledge the anonymous referee for providing a detailed\nand very useful report. We are gratefully indebted to M. Limousin and R.\nGavazzi for enlightening discussions. D.A. thanks CNRS and CEA for support and visits to the Geneva observatory, where this work was finalized. J.P.K. thanks\nfor support from CNRS and SL2S ANR-06-BLAN-0067 and DESIR ANR-07-\nBLAN-0228. E.J. acknowledges the support of the NPP, administered by Oak\nRidge Associated Universities through a contract with NASA.\n\nPublished - Faure2011p13694Astron_Astrophys.pdf
", "abstract": "Context. Nearly 100 new strong-lens candidates have been discovered in the COSMOS field. Among these, 20 lens candidates with 0.34 \u2272 z_(lens) \u2272 1.13 feature multiple images of background sources.\nAims. Using the multi-wavelength coverage of the field and its spectroscopic follow-up, we characterize the evolution with redshift of the environment and of the dark-matter (DM) fraction of the lens galaxies.\nMethods. We present spectroscopic and new photometric redshifts of the strong-lens candidates. The lens environment is characterized in the following way: we account for the projected 10 closest galaxies around each lens and for galaxies with a projected distance less than 1 Mpc at the lens galaxy redshift. In both cases, we perform similar measurements on a control sample of \"twin\" non-lens early-type galaxies (ETGs). In addition, we identify group members and field galaxies in the X-ray and optical catalogs of galaxy groups and clusters. From those catalogs, we measure the external shear contribution of the groups/clusters surrounding the lens galaxies. The systems are then modeled using a singular isothermal ellipsoid for the lens galaxies plus the external shear produced by the groups/clusters. \nResults. We observe that the average stellar mass of lens galaxies increases with redshift. In addition, we measure that the environment of lens galaxies is compatible with that of the twins over the whole redshift range tested here. During the lens modeling, we notice that when let free, the external shear points in a direction which is the mean direction of the external shear produced by the groups/clusters and of the closest galaxy to the lens. We also notice that the DM fraction of the lens galaxies measured within the Einstein radius significantly decreases as the redshift increases.\nConclusions. Given these observations, we conclude that while the environment of lens galaxies is compatible with that of non-lens ETGS over a wide range of redshifts, their mass properties evolves significantly with redshift: it is still not clear whether this advocates in favor of a stronger lensing bias toward massive objects at high redshift or if it is simply representative of the high proportion of massive and high stellar density galaxies at high redshift.", "date": "2011-05", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "529", "publisher": "EDP Sciences", "pagerange": "Art. No. A72", "id_number": "CaltechAUTHORS:20110504-104744333", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110504-104744333", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-06-BLAN-0067" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-07-BLAN-0228" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/200913498", "primary_object": { "basename": "Faure2011p13694Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/ejs41-qhd12/files/Faure2011p13694Astron_Astrophys.pdf" }, "pub_year": "2011", "author_list": "Faure, C.; Anguita, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/vg4sg-3ap77", "eprint_id": 58881, "eprint_status": "archive", "datestamp": "2023-08-19 06:25:12", "lastmod": "2023-10-23 19:50:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Masters-D-C", "name": { "family": "Masters", "given": "D." }, "orcid": "0000-0001-5382-6138" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "SpecPro: An Interactive IDL Program for Viewing and Analyzing Astronomical Spectra", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2011 The Astronomical Society of the Pacific.\n\nReceived 2011 February 8; accepted 2011 March 7; published 2011 April 13.\n\nThe authors would like to thank Yuko Kakazu, Hai Fu, Lin\nYan, and Nick Scoville from the California Institute of Astronomy\nfor their helpful comments and suggestions during the\ndevelopment of the software. In addition, we would like to acknowledge\nand thank Mara Salvato of the Max Planck Institute\nfor Plasma Physics and Francesca Civano of the Harvard-Smithsonian\nCenter for Astronomy for providing useful feedback on\nearly versions of the code. We also thank Bahram Mobasher of\nthe University of California, Riverside, for carefully reading a\ndraft of this article and making suggestions that significantly\nimproved its content. SpecPro makes use of IDL code written\nand maintained by others. We thank Wayne Landsman at NASA\nGoddard Space Flight Center for his work maintaining the IDL\nAstronomy User's Library. We also thank the authors of code\nwe have used for our implementation of automated cross-correlation,\nincluding David Schlegel, Doug Finkbeiner,\nMichael Cooper, and John Johnson. We thank Craig Markwardt,\nwhose MPFIT least-squares fitting package is integral\nto the cross-correlation functionality. Finally, we thank an anonymous\nreferee for carefully reading this article and providing\nvery constructive feedback, both in terms of content and with\nregard to the online distribution of the software. This work was\nsupported in part by a visiting Graduate Student Fellowship at\nthe Caltech Infrared Processing and Analysis Center (IPAC).\n\nPublished - 660023.pdf
", "abstract": "We present an interactive IDL program for viewing and analyzing astronomical spectra in the context of modern imaging surveys. SpecPro's interactive design lets the user simultaneously view spectroscopic, photometric, and imaging data, allowing for rapid object classification and redshift determination. The spectroscopic redshift can be determined with automated cross-correlation against a variety of spectral templates or by manually overlaying common emission and absorption features on the 1-D and 2-D spectra. Stamp images and the spectral energy distribution (SED) of a source can be displayed with the interface, with the positions of prominent photometric features indicated on the SED plot. Results can easily be saved to file from within the interface. In this article we briefly discuss key interface features and provide an overview of the data formats required by the program.", "date": "2011-05", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "123", "number": "903", "publisher": "Astronomical Society of the Pacific", "pagerange": "638-644", "id_number": "CaltechAUTHORS:20150714-113743924", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150714-113743924", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Infrared Processing and Analysis Center (IPAC)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/660023", "primary_object": { "basename": "660023.pdf", "url": "https://authors.library.caltech.edu/records/vg4sg-3ap77/files/660023.pdf" }, "pub_year": "2011", "author_list": "Masters, D. and Capak, P." }, { "id": "https://authors.library.caltech.edu/records/k69r2-e5j66", "eprint_id": 24831, "eprint_status": "archive", "datestamp": "2023-08-22 02:33:46", "lastmod": "2023-10-24 14:57:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Mori\u0107-I", "name": { "family": "Mori\u0107", "given": "I." } }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D. A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E." }, "orcid": "0000-0001-7089-7325" }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "D." }, "orcid": "0000-0001-5382-6138" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The Redshift and Nature of AzTEC/COSMOS 1: A Starburst Galaxy at z = 4.6", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: distances and redshifts; galaxies: high-redshift; galaxies: starburst", "note": "\u00a9 2011 American Astronomical Society.\n\nReceived 2010 December 13; accepted 2011 February 15; published 2011 March 25.\nBased on observations with the W. M. Keck Observatory, the\nCanada\u2013France\u2013Hawaii Telescope, the United Kingdom Infrared Telescope,\nthe Subaru Telescope, the NASA/ESA Hubble Space Telescope, the NASA\nSpitzer Telescope, the Caltech Sub-mm Observatory, the Smithsonian\nMillimeter Array, and the National Radio Astronomy Observatory. Herschel is\nan ESA space observatory with science instruments provided by European-led\nPrincipal Investigator consortia and with important participation from NASA.\nThe authors acknowledge the significant cultural role that\nthe summit of Mauna Kea has within the indigenous Hawaiian\ncommunity; NASA grants HST-GO-09822 (contracts 1407,\n1278386; SSC); HST-HF-51235.01 (contract NAS 5-26555;\nSTScI); GO7-8136A; Blancheflor Boncompagni Ludovisi foundation (F.C.); French Agence National de la Recheche fund ANR-07-BLAN-0228; CNES; Programme National Cosmologie et Galaxies; UKF; DFG; DFG Leibniz Prize (FKZ HA 1850/28-1); European Union's Seventh Framework programme (grant\nagreement 229517); making use of the NASA/IPAC IRSA, by\nJPL/Caltech, under contract with the National Aeronautics and Space Administration; IRAM PdBI supported by INSU/CNRS\n(France), MPG (Germany), and IGN (Spain); CARMA supported\nby the states of California, Illinois, and Maryland, the\nGordon and Betty Moore Foundation, the Eileen and Kenneth\nNorris Foundation, the Caltech Associates, and NSF.\n\nPublished - Smolcic2011p15492Astrophys_J_Lett.pdf
", "abstract": "Based on broadband/narrowband photometry and Keck DEIMOS spectroscopy, we report a redshift of z = 4.64^(+0.06)_(\u20130.08) for AzTEC/COSMOS 1, the brightest submillimeter galaxy (SMG) in the AzTEC/COSMOS field. In addition to the COSMOS-survey X-ray to radio data, we report observations of the source with Herschel/PACS (100, 160 \u03bcm), CSO/SHARC II (350 \u03bcm), and CARMA and PdBI (3 mm). We do not detect CO(5 \u2192 4) line emission in the covered redshift ranges, 4.56-4.76 (PdBI/CARMA) and 4.94-5.02 (CARMA). If the line is within this bandwidth, this sets 3\u03c3 upper limits on the gas mass to \u22728 \u00d7 10^9 M_\u2609 and \u22725 \u00d7 10^(10) M_\u2609, respectively (assuming similar conditions as observed in z ~ 2 SMGs). This could be explained by a low CO-excitation in the source. Our analysis of the UV-IR spectral energy distribution of AzTEC 1 shows that it is an extremely young (\u227250 Myr), massive (M * ~ 10^(11) M_\u2609), but compact (\u22722 kpc) galaxy, forming stars at a rate of ~1300 M_\u2609 yr^(\u20131). Our results imply that AzTEC 1 is forming stars in a \"gravitationally bound\" regime in which gravity prohibits the formation of a superwind, leading to matter accumulation within the galaxy and further generations of star formation.", "date": "2011-04-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "731", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L27", "id_number": "CaltechAUTHORS:20110812-111634392", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110812-111634392", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51235.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Blancheflor Boncompagni Ludovisi foundation" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-07-BLAN-0228" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "European Research Council (ERC)", "grant_number": "229517" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Eileen and Kenneth Norris Foundation" }, { "agency": "Caltech Associates" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/2041-8205/731/2/L27", "primary_object": { "basename": "Smolcic2011p15492Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/k69r2-e5j66/files/Smolcic2011p15492Astrophys_J_Lett.pdf" }, "pub_year": "2011", "author_list": "Smol\u010di\u0107, V.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/d30gw-myy94", "eprint_id": 23299, "eprint_status": "archive", "datestamp": "2023-08-22 02:27:02", "lastmod": "2023-10-23 18:59:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Men\u00e9ndez-Delmestre-K", "name": { "family": "Men\u00e9ndez-Delmestre", "given": "K." }, "orcid": "0000-0003-3153-5123" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C." }, "orcid": "0000-0001-6647-3861" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Jullo-E", "name": { "family": "Jullo", "given": "E." }, "orcid": "0000-0002-9253-053X" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Tanaguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } }, { "id": "Willott-C-J", "name": { "family": "Willott", "given": "C. J." }, "orcid": "0000-0002-4201-7367" } ] }, "title": "Spectroscopy of Luminous z > 7 Galaxy Candidates and Sources of Contamination in z > 7 Galaxy Searches", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift", "note": "\u00a9 2011 American Astronomical Society. Received 2009 October 1; accepted 2010 December 26; published 2011 March 7. \n\nBased on observations with the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration and made possible by the generous financial support of the W. M. Keck Foundation; the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA; the Canada\u2013France\u2013Hawaii Telescope with WIRCam, a joint project of CFHT, Taiwan, Korea, Canada, France, at the Canada\u2013France\u2013Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii; the United Kingdom Infrared Telescope operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the U.K; the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the Canada\u2013France\u2013Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the National Research Council of Canada, the Canadian Astronomy Data Centre, the Centre National de la Recherche Scientifique de France, TERAPIX and the University of Hawaii; the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc., under NASA contract NAS5-26555; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the Chandra X-ray Observatory, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060; the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; the 30 m telescope of the Institute for Radioastronomy at Millimeter Wavelengths (IRAM), which is funded by the German Max-Planck-Society, the French CNRS, and the Spanish National Geographical Institute.\n\nThe authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Support for this work was provided by the Spitzer Science Center which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology under NASA contract 1407, NASA through contract 1278386 issued by the JPL and NASA grant HST-GO-\n09822. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This research has made use of the NASA/ IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. H.J.M. and J.P.K. acknowledge support from the French Agene National de la Recheche fund ANR-07-BLAN-0228 as well as from CNES and the Programme National Cosmologie et Galaxies. P.C. acknowledges the Keck remote observing staff who allowed him to simultaneously attend the NIRSPEC observations and the birth of his daughter.\n\nPublished - Capak2011p13393Astrophys_J.pdf
", "abstract": "We present three bright z ^+-dropout candidates selected from deep near-infrared (NIR) imaging of the COSMOS 2 deg^2 field. All three objects match the 0.8-8 \u03bcm colors of other published z > 7 candidates but are 3 mag brighter, facilitating further study. Deep spectroscopy of two of the candidates covering 0.64-1.02 \u03bcm with Keck-DEIMOS and all three covering 0.94-1.10 \u03bcm and 1.52-1.80 \u03bcm with Keck-NIRSPEC detects weak spectral features tentatively identified as Ly\u03b1 at z = 6.95 and z = 7.69 in two of the objects. The third object is placed at z ~ 1.6 based on a 24 \u03bcm and weak optical detection. A comparison with the spectral energy distributions of known z < 7 galaxies, including objects with strong spectral lines, large extinction, and large systematic uncertainties in the photometry, yields no objects with similar colors. However, the \u03bb > 1 \u03bcm properties of all three objects can be matched to optically detected sources with photometric redshifts at z ~ 1.8, so the non-detection in the i ^+ and z ^+ bands is the primary factor which favors a z > 7 solution. If any of these objects are at z ~ 7, the bright end of the luminosity function is significantly higher at z > 7 than suggested by previous studies, but consistent within the statistical uncertainty and the dark matter halo distribution. If these objects are at low redshift, the Lyman break selection must be contaminated by a previously unknown population of low-redshift objects with very strong breaks in their broadband spectral energy distributions and blue NIR colors. The implications of this result on luminosity function evolution at high redshift are discussed. We show that the primary limitation of z > 7 galaxy searches with broad filters is the depth of the available optical data.", "date": "2011-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "730", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 68", "id_number": "CaltechAUTHORS:20110413-081502578", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110413-081502578", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Spitzer Science Center" }, { "agency": "NASA", "grant_number": "1407" }, { "agency": "NASA", "grant_number": "1278386" }, { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NASA" }, { "agency": "JPL/Caltech" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-07-BLAN-0228" }, { "agency": "Programme National Cosmologie et Galaxies (PNCG)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/730/2/68", "primary_object": { "basename": "Capak2011p13393Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/d30gw-myy94/files/Capak2011p13393Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Capak, P.; Mobasher, B.; et el." }, { "id": "https://authors.library.caltech.edu/records/s9wrb-4hg71", "eprint_id": 23140, "eprint_status": "archive", "datestamp": "2023-08-19 05:59:25", "lastmod": "2023-10-23 17:58:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jacobs-B-A", "name": { "family": "Jacobs", "given": "B. A." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Rupke-D-S-N", "name": { "family": "Rupke", "given": "D. S. N." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Kawara-K", "name": { "family": "Kawara", "given": "K." } }, { "id": "Kim-D-C", "name": { "family": "Kim", "given": "D.-C." } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J. A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Veilleux-S", "name": { "family": "Veilleux", "given": "S." }, "orcid": "0000-0002-3158-6820" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "M. S." }, "orcid": "0000-0001-7095-7543" } ] }, "title": "Identification of a Complete 160 \u03bcm Flux-limited Sample of Infrared Galaxies in the ISO Lockman Hole 1 deg^2 Deep Fields: Source Properties and Evidence for Strong Evolution in the FIR Luminosity Function for ULIRGs", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 infrared: galaxies", "note": "\u00a9 2011 American Astronomical Society. Received 2010 September 10; accepted 2010 November 17; published 2011 February 24. \n\n\nWe benefited from the published data and preliminary analyses\nof S. Oyabu. V.S. acknowledges support from the Owens Valley Radio Observatory, which is supported by the National\nScience Foundation through grant AST-0838260, and also received\nfunding from the European Union's Seventh Framework\nprogramme under grant agreement 229517. Y.T. was financially\nsupported in part by the Ministry of Education, Culture, Sports,\nScience and Technology (Nos. 10044052 and 10304013), and by\nthe JSPS (Nos. 15340059, 17253001, and 19340046). This research\nhas made use of the NASA/IPAC Extragalactic Database\n(NED) which is operated by the Jet Propulsion Laboratory, California\nInstitute of Technology, under contract with the National\nAeronautics and Space Administration. This publication makes\nuse of data products from the Two Micron All Sky Survey,\nwhich is a joint project of the University of Massachusetts and\nthe Infrared Processing and Analysis Center/California Institute\nof Technology, funded by the National Aeronautics and\nSpace Administration and the National Science Foundation.\nFunding for the SDSS and SDSS-II has been provided by the\nAlfred P. Sloan Foundation, the Participating Institutions, the\nNational Science Foundation, the U. S. Department of Energy,\nthe National Aeronautics and Space Administration, the\nJapanese Monbukagakusho, the Max Planck Society, and the\nHigher Education Funding Council for England. The SDSS Web\nsite is http://www.sdss.org/.\n\nThe SDSS is managed by the Astrophysical Research Consortium\nfor the Participating Institutions. The participating institutions\nare the American Museum of Natural History, Astrophysical\nInstitute Potsdam, University of Basel, University\nof Cambridge, Case Western Reserve University, University\nof Chicago, Drexel University, Fermilab, the Institute for Advanced\nStudy, the Japan Participation Group, Johns Hopkins\nUniversity, the Joint Institute for Nuclear Astrophysics, the\nKavli Institute for Particle Astrophysics and Cosmology, the\nKorean Scientist Group, the Chinese Academy of Sciences\n(LAMOST), Los Alamos National Laboratory, the Max-Planck-\nInstitute for Astronomy (MPIA), the Max-Planck-Institute for\nAstrophysics (MPA), New Mexico State University, Ohio State\nUniversity, University of Pittsburgh, University of Portsmouth,\nPrinceton University, the United States Naval Observatory, and\nthe University of Washington.\n\nPublished - Jacobs2011p13237Astron_J.pdf
", "abstract": "We have identified a complete, flux-limited (S_(160) > 120 mJy) sample of 160 \u03bcm selected sources from Spitzer observations of the 1 deg^2 Infrared Space Observatory (ISO) Deep Field region in the Lockman Hole (LH). Ground-based UV, optical, and near-infrared (NIR) photometry and optical spectroscopy have been used to determine colors, redshifts, and masses for the complete sample of 40 galaxies. Spitzer-IRAC+MIPS photometry, supplemented by ISOPHOT data at 90 \u03bcm and 170 \u03bcm, has been used to calculate accurate total infrared luminosities, L_(IR)(8-1000 \u03bcm), and to determine the IR luminosity function (LF) of luminous infrared galaxies (LIRGs). The maximum observed redshift is z ~ 0.80 and the maximum total infrared luminosity is log (L_(IR)/L_\u2299) = 12.74. Over the luminosity range log (L_(IR)/L_\u2299)) = 10-12, the LF for LIRGs in the LH Deep Field is similar to that found previously for local sources at similar infrared luminosities. The mean host galaxy mass, log (M/M_\u2299 ) = 10.7, and dominance of H_(II)-region spectral types, is also similar to what has been found for local LIRGs, suggesting that intense starbursts likely power the bulk of the infrared luminosity for sources in this range of L_(IR). However for the most luminous sources, log (L_(IR)/L_\u2299 ) > 12.0, we find evidence for strong evolution in the LF \u221d (1 + z)^(6\u00b11), assuming pure number density evolution. These ultraluminous infrared galaxies (ULIRGs) have a larger mean host mass, log (M/M_\u2299) = 11.0, and exhibit disturbed morphologies consistent with strong interactions/mergers, and they are also more likely to be characterized by starburst-active galactic nucleus (AGN) composite or AGN spectral types.", "date": "2011-04", "date_type": "published", "publication": "Astronomical Journal", "volume": "141", "number": "4", "publisher": "American Astronomical Society", "pagerange": "Art. No. 110", "id_number": "CaltechAUTHORS:20110328-142023974", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110328-142023974", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Owens Valley Radio Observatory" }, { "agency": "NSF", "grant_number": "AST-0838260" }, { "agency": "European Research Council (ERC)", "grant_number": "229517" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "10044052" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "10304013" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15340059" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17253001" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19340046" }, { "agency": "NASA" }, { "agency": "NSF" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Funding Council for England" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-6256/141/4/110", "primary_object": { "basename": "Jacobs2011p13237Astron_J.pdf", "url": "https://authors.library.caltech.edu/records/s9wrb-4hg71/files/Jacobs2011p13237Astron_J.pdf" }, "pub_year": "2011", "author_list": "Jacobs, B. A.; Sanders, D. B.; et el." }, { "id": "https://authors.library.caltech.edu/records/rtnf2-3sq78", "eprint_id": 22913, "eprint_status": "archive", "datestamp": "2023-08-19 05:40:49", "lastmod": "2023-10-23 17:20:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chou-Richard-C-Y", "name": { "family": "Chou", "given": "Richard C. Y." } }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "Carrie R." } }, { "id": "Abraham-R-G", "name": { "family": "Abraham", "given": "Roberto G." }, "orcid": "0000-0002-4542-921X" } ] }, "title": "The Space Density Evolution of Wet and Dry Mergers in the Canada-France-Hawaii Telescope Legacy Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: formation \u2013 galaxies: interactions", "note": "\u00a9 2011 American Astronomical Society. Received 2010 April 13; accepted 2010 December 4; published 2011 February 7. The authors thank NSERC and the Government of Ontario\nfor funding this research. We also thank Damien Le Borgne and\nKarl Glazebrook for useful discussions.\n\nPublished - Chou2011p13020Astron_J.pdf
", "abstract": "We analyze 1298 merging galaxies with redshifts up to z = 0.7 from the Canada-France-Hawaii Telescope Legacy Survey, taken from the catalog presented in the work of Bridge et al. By analyzing the internal colors of these systems, we show that the so-called wet and dry mergers evolve in different senses, and quantify the space densities of these systems. The local space density of wet mergers is essentially identical to the local space density of dry mergers. The evolution in the total merger rate is modest out to z ~ 0.7, although the wet and dry populations have different evolutionary trends. At higher redshifts, dry mergers make a smaller contribution to the total merging galaxy population, but this is offset by a roughly equivalent increase in the contribution from wet mergers. By comparing the mass density function of early-type galaxies to the corresponding mass density function for merging systems, we show that not all the major mergers with the highest masses (M_(stellar) > 10^(11) M_\u2299) will end up with the most massive early-type galaxies, unless the merging timescale is dramatically longer than that usually assumed. On the other hand, the usually assumed merging timescale of ~0.5-1 Gyr is quite consistent with the data if we suppose that only less massive early-type galaxies form via mergers. Since low-intermediate-mass ellipticals are 10-100 times more common than their most massive counterparts, the hierarchical explanation for the origin of early-type galaxies may be correct for the vast majority of early types, even if incorrect for the most massive ones.", "date": "2011-03", "date_type": "published", "publication": "Astronomical Journal", "volume": "141", "number": "3", "publisher": "American Astronomical Society", "pagerange": "Art. No. 87", "id_number": "CaltechAUTHORS:20110315-152141116", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110315-152141116", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Government of Ontario" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-6256/141/3/87", "primary_object": { "basename": "Chou2011p13020Astron_J.pdf", "url": "https://authors.library.caltech.edu/records/rtnf2-3sq78/files/Chou2011p13020Astron_J.pdf" }, "pub_year": "2011", "author_list": "Chou, Richard C. Y.; Bridge, Carrie R.; et el." }, { "id": "https://authors.library.caltech.edu/records/pc9mk-nx863", "eprint_id": 23058, "eprint_status": "archive", "datestamp": "2023-08-22 02:09:41", "lastmod": "2023-10-23 17:51:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kaviraj-S", "name": { "family": "Kaviraj", "given": "Sugata" } }, { "id": "Tan-K-M", "name": { "family": "Tan", "given": "Kok-Meng" } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Silk-J", "name": { "family": "Silk", "given": "Joseph" } } ] }, "title": "A coincidence of disturbed morphology and blue UV colour: minor-merger-driven star formation in early-type galaxies at z ~ 0.6", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation; galaxies: interactions; ultraviolet: galaxies", "note": "\u00a9 2011 The Authors. \nMonthly Notices of the Royal Astronomical Society \u00a9 2011 RAS.\n\nAccepted 2010 September 22. Received 2010 August 17; in original form 2009 December 25. Article first published online: 31 Jan 2011. The anonymous referee is gratefully acknowledged for a thorough report which significantly improved the original manuscript. SK acknowledges an Imperial College Junior Research Fellowship, a Research Fellowship from the Royal Commission for the Exhibition of 1851, a Senior Research Fellowship from Worcester College, Oxford, and support from the BIPAC institute at Oxford. Some of this work was supported by a Leverhulme Early-Career Fellowship\n(SK). RSE acknowledges support from the Royal Society. Roger\nDavies, Kevin Bundy, Martin Bureau, Chris Conselice, Jerry Sellwood and Sukyoung Yi are thanked for interesting discussions and useful comments. Some of this research utilized the undergraduate computing facilities in the Department of Physics at the University of Oxford.\n\nPublished - Kaviraj2011p13086Mon_Not_R_Astron_Soc.pdf
", "abstract": "We exploit multiwavelength photometry of early-type galaxies (ETGs) in the Cosmological Evolution Survey (COSMOS) to demonstrate that the low-level star formation activity in the ETG population at intermediate redshift is likely to be driven by minor mergers. Splitting the ETGs into galaxies that show disturbed morphologies indicative of recent merging and those that appear relaxed, we find that ~32 per cent of the ETG population appears to be\nmorphologically disturbed. While the relaxed objects are almost entirely contained within the UV red sequence, their morphologically disturbed counterparts dominate the scatter to blue UV colours, regardless of luminosity. Empirically and theoretically determined major-merger rates in the redshift range z < 1 are several times too lowto account for the fraction of disturbed ETGs in our sample, suggesting that minor mergers represent the principal mechanism driving\nthe observed star formation activity in our sample. The young stellar components forming in these events have ages between 0.03 and 0.3 Myr and typically contribute \u2264 10 per cent of the stellar mass of the remnant. Together with recent work which demonstrates that the structural\nevolution of nearby ETGs is consistent with one or more minor mergers, our results indicate that the overall evolution of massive ETGs may be heavily influenced by minor merging at late epochs and highlights the need to systematically study this process in future observational\nsurveys.", "date": "2011-03", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "411", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "2148-2160", "id_number": "CaltechAUTHORS:20110323-080916064", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110323-080916064", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Leverhulme Early-Career Fellowship" }, { "agency": "Royal Society" }, { "agency": "Imperial College Junior Research Fellowship" }, { "agency": "Royal Commission Research Fellowship" }, { "agency": "Worcester College Senior Research Fellowship" }, { "agency": "Oxford BIPAC Institute" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1111/j.1365-2966.2010.17754.x", "primary_object": { "basename": "Kaviraj2011p13086Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/pc9mk-nx863/files/Kaviraj2011p13086Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2011", "author_list": "Kaviraj, Sugata; Tan, Kok-Meng; et el." }, { "id": "https://authors.library.caltech.edu/records/07h3j-v5n67", "eprint_id": 22962, "eprint_status": "archive", "datestamp": "2023-08-22 02:05:59", "lastmod": "2023-10-23 17:46:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ikeda-Hideyuki", "name": { "family": "Ikeda", "given": "H." } }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "T." }, "orcid": "0000-0002-7402-5441" }, { "id": "Matsuoka-Kenta", "name": { "family": "Matsuoka", "given": "K." }, "orcid": "0000-0002-2689-4634" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J. R." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Enoki-Motohiro", "name": { "family": "Enoki", "given": "M." } }, { "id": "Ideue-Y", "name": { "family": "Ideue", "given": "Y." } }, { "id": "Kakazu-Yuko", "name": { "family": "Kakazu", "given": "Y." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Morokuma-Tomoki", "name": { "family": "Morokuma", "given": "T." } }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Saito-T", "name": { "family": "Saito", "given": "T." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" } ] }, "title": "Probing the Faint End of the Quasar Luminosity Function at z~4 in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; quasars: general; surveys", "note": "\u00a9 2011 American Astronomical Society. Received 2010 November 9; accepted 2010 December 20; published 2011 January 25. We thank the Subaru staff for their invaluable help and all\nmembers of the COSMOS team. T.M., K.M., and Y.I. are\nfinancially supported by the Japan Society for the Promotion\nof Science (JSPS) through the JSPS Research Fellowship.\n\nPublished - Ikeda2011p13025Astrophys_J_Lett.pdf
", "abstract": "We searched for quasars that are ~3 mag fainter than the SDSS quasars in the redshift range 3.7 \u227e z \u227e 4.7 in the COSMOS field to constrain the faint end of the quasar luminosity function (QLF). Using optical photometric data, we selected 31 quasar candidates with 22 < i < 24 at z ~ 4. We obtained optical spectra for most of these candidates using FOCAS on the Subaru telescope and identified eight low-luminosity quasars at z ~ 4. In order to derive the QLF based on our spectroscopic follow-up campaign, we estimated the photometric completeness of our quasar survey through detailed Monte Carlo simulations. Our QLF at z ~ 4 has a much shallower faint-end slope (\u03b2 = \u22121.67^(+0.11)_(\u22120.17)) than that obtained by other recent surveys in the same redshift. Our result is consistent with the scenario of downsizing evolution of active galactic nuclei inferred by recent optical and X-ray quasar surveys at lower redshifts.", "date": "2011-02-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "728", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L25", "id_number": "CaltechAUTHORS:20110317-130412253", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110317-130412253", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/2041-8205/728/2/L25", "primary_object": { "basename": "Ikeda2011p13025Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/07h3j-v5n67/files/Ikeda2011p13025Astrophys_J_Lett.pdf" }, "pub_year": "2011", "author_list": "Ikeda, H.; Nagao, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/ngd7v-0ng08", "eprint_id": 22548, "eprint_status": "archive", "datestamp": "2023-08-19 05:31:24", "lastmod": "2023-10-23 16:59:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "Dominik" }, "orcid": "0000-0001-9585-1462" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "Chris" }, "orcid": "0000-0001-6647-3861" }, { "id": "Cox-Pierre", "name": { "family": "Cox", "given": "Pierre" }, "orcid": "0000-0003-2027-8221" }, { "id": "Neri-Roberto", "name": { "family": "Neri", "given": "Roberto" }, "orcid": "0000-0002-7176-4046" }, { "id": "Robertson-B-E", "name": { "family": "Robertson", "given": "Brant" }, "orcid": "0000-0002-4271-0364" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "Grant W." }, "orcid": "0000-0003-2705-9152" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "Min" }, "orcid": "0000-0001-7095-7543" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "Francesca" }, "orcid": "0000-0002-2115-1137" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "id": "Karim-A", "name": { "family": "Karim", "given": "Alexander" }, "orcid": "0000-0002-8414-9579" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Staguhn-J-G", "name": { "family": "Staguhn", "given": "Johannes G." }, "orcid": "0000-0002-8437-0433" } ] }, "title": "A massive protocluster of galaxies at a redshift of z\u2009\u2248\u20095.3", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2011 Macmillan Publishers Limited. \n\nReceived 18 May; accepted 16 November 2010. Published online 12 January 2011. \n\nThese results are based on observations with: the W. M. Keck Observatory, the IRAM Plateau de Bure Interferometer, the IRAM 30-m telescope with the GISMO 2-mm camera, the Chandra X-ray Observatory, the Subaru Telescope, the Hubble Space Telescope, the Canada-France-Hawaii Telescope with WIRCam and MegaPrime, the United Kingdom Infrared Telescope, the Spitzer Space Telescope, the Smithsonian Submillimeter Array Telescope, the James Clerk Maxwell Telescope with the AzTEC 1.1mm camera, and the National Radio Astronomy Observatory's Very Large Array. D.R. and B.R. acknowledge support from NASA through Hubble Fellowship grants awarded by the Space Telescope Science Institute. P.L.C. and N.Z.S. acknowledge grant support from NASA. G.W.W., M.Y. and J.G.S. acknowledge grant support from the NSF. \n\nAuthor Contributions: P.L.C. led the spectroscopic effort, reduced the spectroscopic and photometric data, and led the scientific analysis including the optical and radio/millimetre fitting analysis and cluster properties. N.Z.S. led the spectroscopic and photometric follow-up efforts. D.R., C.C., P.C. and R.N. assisted with the physical interpretation of the radio data. B.R. provided cosmological simulations to check the significance of the protocluster and the likelihood of finding it. M.S., L.Y., M.E., F.C. and B.M. carried out the Keck observations and assisted with the data reduction. E.S. reduced and analysed the radio data. G.W.W. and M.Y. assisted with the submillimetre data analysis. F.C. and M.E. assisted with the X-ray data analysis. A.K. coordinated the 2-mm observations. J.G.S. conducted and reduced the 2-mm observations.\n\nAccepted Version - 1101.3586.pdf
Submitted - A_massive_protocluster_of_galaxies_at_a_redshift_of_z---5.3.pdf
Supplemental Material - nature09681-s1.pdf
", "abstract": "Massive clusters of galaxies have been found that date from as early as 3.9 billion years (3.9\u2009Gyr; z = 1.62) after the Big Bang, containing stars that formed at even earlier epochs. Cosmological simulations using the current cold dark matter model predict that these systems should descend from 'protoclusters'\u2014early overdensities of massive galaxies that merge hierarchically to form a cluster. These protocluster regions themselves are built up hierarchically and so are expected to contain extremely massive galaxies that can be observed as luminous quasars and starbursts. Observational evidence for this picture, however, is sparse because high-redshift protoclusters are rare and difficult to observe. Here we report a protocluster region that dates from 1\u2009Gyr (z = 5.3) after the Big Bang. This cluster of massive galaxies extends over more than 13 megaparsecs and contains a luminous quasar as well as a system rich in molecular gas. These massive galaxies place a lower limit of more than 4\u2009\u00d7\u200910^(11) solar masses of dark and luminous matter in this region, consistent with that expected from cosmological simulations for the earliest galaxy clusters.", "date": "2011-02-10", "date_type": "published", "publication": "Nature", "volume": "470", "number": "7333", "publisher": "Nature Publishing Group", "pagerange": "233-235", "id_number": "CaltechAUTHORS:20110228-112031430", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110228-112031430", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "NSF" }, { "agency": "Space Telescope Science Institute" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1038/nature09681", "primary_object": { "basename": "1101.3586.pdf", "url": "https://authors.library.caltech.edu/records/ngd7v-0ng08/files/1101.3586.pdf" }, "related_objects": [ { "basename": "A_massive_protocluster_of_galaxies_at_a_redshift_of_z---5.3.pdf", "url": "https://authors.library.caltech.edu/records/ngd7v-0ng08/files/A_massive_protocluster_of_galaxies_at_a_redshift_of_z---5.3.pdf" }, { "basename": "nature09681-s1.pdf", "url": "https://authors.library.caltech.edu/records/ngd7v-0ng08/files/nature09681-s1.pdf" } ], "pub_year": "2011", "author_list": "Capak, Peter L.; Riechers, Dominik; et el." }, { "id": "https://authors.library.caltech.edu/records/zkdt4-kgw91", "eprint_id": 22878, "eprint_status": "archive", "datestamp": "2023-08-19 05:32:20", "lastmod": "2023-10-23 17:17:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brooks-A-M", "name": { "family": "Brooks", "given": "A. M." } }, { "id": "Solomon-A-R", "name": { "family": "Solomon", "given": "A. R." } }, { "id": "Governato-F", "name": { "family": "Governato", "given": "F." } }, { "id": "McCleary-J", "name": { "family": "McCleary", "given": "J." } }, { "id": "MacArthur-L-A", "name": { "family": "MacArthur", "given": "L. A." } }, { "id": "Brook-C-B-A", "name": { "family": "Brook", "given": "C. B. A." } }, { "id": "Jonsson-P", "name": { "family": "Jonsson", "given": "P." } }, { "id": "Quinn-T-R", "name": { "family": "Quinn", "given": "T. R." } }, { "id": "Wadsley-J", "name": { "family": "Wadsley", "given": "J." } } ] }, "title": "Interpreting the Evolution of the Size-Luminosity Relation for Disk Galaxies from Redshift 1 to the Present", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: fundamental parameters \u2013 methods: numerical", "note": "\u00a9 2011 American Astronomical Society. Received 2010 August 9; accepted 2010 December 1; published 2011 January 19. We thank S. Miller and R. Ellis for the use of their z = 1 disk scale length data. A.M.B. acknowledges support from\nthe Sherman Fairchild Foundation. A.R.S. was supported by\nthe Gordon & Betty Moore Foundation. F.G. and T.R.Q. were\nfunded by NSF AST-0908499. F.G. acknowledges support from\na Theodore Dunham grant, HST GO-1125, NSF grant AST-\n0607819, and NASA ATP NNX08AG84G. P.J. acknowledges\nsupport from the W. M. Keck Foundation. Simulations were\nrun at TACC, ARSC, and NAS. C.B.A.B. acknowledges the\nsupport of the UK's Science & Technology Facilities Council\n(STFC Grant ST/F002432/1).\n\nPublished - Brooks2011p13000Astrophys_J.pdf
", "abstract": "A sample of very high resolution cosmological disk galaxy simulations is used to investigate the evolution of galaxy disk sizes back to redshift 1 within the \u039bCDM cosmology. Artificial images in the rest-frame B band are generated, allowing for a measurement of disk scale lengths using surface brightness profiles as observations would, and avoiding any assumption that light must follow mass as previous models have assumed. We demonstrate that these simulated disks are an excellent match to the observed magnitude-size relation for both local disks and for disks at z = 1 in the magnitude/mass range of overlap. We disentangle the evolution seen in the population as a whole from the evolution of individual disk galaxies. In agreement with observations, our simulated disks undergo roughly 1.5 mag arcsec^(\u20132) of surface brightness dimming since z = 1. We find evidence that evolution in the magnitude-size plane varies by mass, such that galaxies with M_* \u2265 10^9 M_\u2299 undergo more evolution in size than luminosity, while dwarf galaxies tend to evolve potentially more in luminosity. The disks grow in such a way as to stay on roughly the same stellar-mass-size relation with time. Finally, due to an evolving stellar-mass-star-formation-rate (SFR) relation, a galaxy at a given stellar mass (or size) at z = 1 will reside in a more massive halo and have a higher SFR, and thus a higher luminosity, than a counterpart of the same stellar mass at z = 0.", "date": "2011-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "728", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 51", "id_number": "CaltechAUTHORS:20110315-084038410", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110315-084038410", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "Gordon & Betty Moore Foundation" }, { "agency": "NSF", "grant_number": "AST-0908499" }, { "agency": "NSF", "grant_number": "AST-0607819" }, { "agency": "NASA ATP", "grant_number": "NNX08AG84G" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Science and Technology Facilities Council (STFC) (UK)", "grant_number": "ST/F002432/1" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/728/1/51", "primary_object": { "basename": "Brooks2011p13000Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/zkdt4-kgw91/files/Brooks2011p13000Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Brooks, A. M.; Solomon, A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/x3vxz-ksp20", "eprint_id": 21942, "eprint_status": "archive", "datestamp": "2023-08-19 05:14:45", "lastmod": "2023-10-23 15:31:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cisternas-M", "name": { "family": "Cisternas", "given": "Mauricio" } }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "Knud" }, "orcid": "0000-0003-3804-2137" }, { "id": "Inskip-K-J", "name": { "family": "Inskip", "given": "Katherine J." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "Jeyhan" }, "orcid": "0000-0001-9187-3605" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Lisker-T", "name": { "family": "Lisker", "given": "Thorsten" } }, { "id": "Robaina-A-R", "name": { "family": "Robaina", "given": "Aday R." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "Marco" } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "Jonathan R." } }, { "id": "Andrae-R", "name": { "family": "Andrae", "given": "Ren\u00e9" } }, { "id": "Miyaji-Takamitsu", "name": { "family": "Miyaji", "given": "Takamitsu" } }, { "id": "Lusso-E", "name": { "family": "Lusso", "given": "Elisabeta" }, "orcid": "0000-0003-0083-1157" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "Marcella" }, "orcid": "0000-0002-5059-6848" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "Nico" } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "Francesca" }, "orcid": "0000-0002-2115-1137" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "Chris D." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "Simon J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The bulk of the black hole growth since z ~ 1 occurs in a secular universe: no major merger-AGN connection", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active \u2013 galaxies: evolution \u2013 galaxies: interactions \u2013 quasars: general", "note": "\u00a9 2011 The American Astronomical Society. Received 2010 September 17; accepted 2010 October 21; published 2010 December 15. Based on observations with the NASA/ESA Hubble Space Telescope,\nobtained at the Space Telescope Science Institute, which is operated by AURA\nInc., under NASA contract NAS 5-26555; the XMM-Newton, an ESA science\nmission with instruments and contributions directly funded by ESA Member\nStates and NASA; European Southern Observatory under Large Program\n175.A-0839; and the Subaru Telescope, which is operated by the National\nAstronomical Observatory of Japan. M.C. thanks G. De Rosa for productive discussions, C. M.\nUrry for useful comments, and the anonymous referee for practical\nsuggestions. M.C., K.J., and K.I. are supported through\nthe Emmy Noether Programme of the German Science Foundation\n(DFG). T.M. acknowledges support by CONACyT Apoyo\n83564 and UNAM-DGAPA PAPIIT IN110209.\nFacilities: CXO, VLT:Melipal (VIMOS), HST (ACS),\nMagellan: Baade (IMACS), XMM, Subaru (SuprimeCam)\n\nPublished - Cisternas2011p12488Astrophys_J.pdf
", "abstract": "What is the relevance of major mergers and interactions as triggering mechanisms for active galactic nuclei (AGNs)\nactivity? To answer this long-standing question, we analyze 140 XMM-Newton-selected AGN host galaxies and\na matched control sample of 1264 inactive galaxies over z ~ 0.3\u20131.0 and M_\u2217 < 10^(11.7) M_\u2299 with high-resolution\nHubble Space Telescope/Advanced Camera for Surveys imaging from the COSMOS field. The visual analysis of\ntheir morphologies by 10 independent human classifiers yields a measure of the fraction of distorted morphologies\nin the AGN and control samples, i.e., quantifying the signature of recent mergers which might potentially be\nresponsible for fueling/triggering the AGN. We find that (1) the vast majority (>85%) of the AGN host galaxies\ndo not show strong distortions and (2) there is no significant difference in the distortion fractions between active\nand inactive galaxies. Our findings provide the best direct evidence that, since z ~ 1, the bulk of black hole (BH)\naccretion has not been triggered by major galaxy mergers, therefore arguing that the alternative mechanisms, i.e.,\ninternal secular processes and minor interactions, are the leading triggers for the episodes of major BH growth.We\nalso exclude an alternative interpretation of our results: a substantial time lag between merging and the observability\nof the AGN phase could wash out the most significant merging signatures, explaining the lack of enhancement\nof strong distortions on the AGN hosts. We show that this alternative scenario is unlikely due to (1) recent major\nmergers being ruled out for the majority of sources due to the high fraction of disk-hosted AGNs, (2) the lack of\na significant X-ray signal in merging inactive galaxies as a signature of a potential buried AGN, and (3) the low\nlevels of soft X-ray obscuration for AGNs hosted by interacting galaxies, in contrast to model predictions.", "date": "2011-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "726", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 57", "id_number": "CaltechAUTHORS:20110201-083149718", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110201-083149718", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "83564" }, { "agency": "Universidad Nacional Aut\u00f3noma de M\u00e9xico (UNAM) - Programa de Apoyo a Proyectos de Investigaci\u00f3n e Innovaci\u00f3n Tecnol\u00f3gica (PAPIIT)", "grant_number": "IN110209" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/726/2/57", "primary_object": { "basename": "Cisternas2011p12488Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/x3vxz-ksp20/files/Cisternas2011p12488Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Cisternas, Mauricio; Jahnke, Knud; et el." }, { "id": "https://authors.library.caltech.edu/records/kmrss-7yz47", "eprint_id": 21738, "eprint_status": "archive", "datestamp": "2023-08-19 04:43:19", "lastmod": "2023-10-21 00:17:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hu-Esther-M", "name": { "family": "Hu", "given": "E. M." } }, { "id": "Cowie-L-L", "name": { "family": "Cowie", "given": "L. L." }, "orcid": "0000-0002-6319-1575" }, { "id": "Barger-A-J", "name": { "family": "Barger", "given": "A. J." }, "orcid": "0000-0002-3306-1606" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Kakazu-Yuko", "name": { "family": "Kakazu", "given": "Y." } }, { "id": "Trouille-L", "name": { "family": "Trouille", "given": "L." } } ] }, "title": "An atlas of z = 5.7 and z = 6.5 Ly\u03b1 emitters", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 galaxies: distances and redshifts \u2013 galaxies: evolution \u2013 galaxies: formation\n\u2013 galaxies: high-redshift \u2013 galaxies: luminosity function, mass function", "note": "\u00a9 2010 American Astronomical Society. Received 2010 July 7; accepted 2010 August 31; published 2010 November 18. Based in part on data collected at the Subaru Telescope, which is operated\nby the National Astronomical Observatory of Japan. Based in part on data obtained at the W. M. Keck Observatory, which is\noperated as a scientific partnership among the California Institute of\nTechnology, the University of California, and NASA and was made possible\nby the generous financial support of the W. M. Keck Foundation. We are indebted to the staff of the Subaru and Keck Observatories\nfor their excellent assistance with the observations. We\nthank Yoshi Taniguchi and Masami Ouchi for useful conversations.\nWe gratefully acknowledge support from NSF grants AST\n0687850 (E.M.H.), AST 0709356 (L.L.C.), and AST 0708793\n(A.J.B.), a grant from NASA through an award issued by JPL\n1289080 (E.M.H.), the University of Wisconsin Research Committee\nwith funds granted by the Wisconsin Alumni Research\nFoundation, and the David and Lucile Packard Foundation\n(A.J.B.).\n\nPublished - Hu2010p12242Astrophys_J.pdf
", "abstract": "We present an atlas of 88 z ~ 5.7 and 30 z ~ 6.5 Ly\u03b1 emitters obtained from a wide-field narrowband survey. We\ncombined deep narrowband imaging in 120 \u00c5 bandpass filters centered at 8150 \u00c5 and 9140 \u00c5 with deep B V R I z\nbroadband imaging to select high-redshift galaxy candidates over an area of 4180 arcmin^2. The goal was to obtain\na uniform selection of comparable depth over the seven targeted fields in the two filters. For the GOODS-North\nregion of the Hubble Deep Field-North field, we also selected candidates using a 120 \u00c5 filter centered at 9210 \u00c5.\nWe made spectroscopic observations with Keck DEIMOS of nearly all the candidates to obtain the final sample of\nLy\u03b1 emitters. At the 3.3 \u00c5 resolution of the DEIMOS observations the asymmetric profile for Ly\u03b1 emission can be\nclearly seen in the spectra of nearly all the galaxies. We show that the spectral profiles are surprisingly similar for\nmany of the galaxies and that the composite spectral profiles are nearly identical at z = 5.7 and z = 6.5.We analyze\nthe distributions of line widths and Ly\u03b1 equivalent widths and find that the lines are marginally narrower at the\nhigher redshift, with median values of 0.77 \u00c5 at z = 6.5 and 0.92 \u00c5 at z = 5.7. The line widths have a dependence\non the Ly\u03b1 luminosity of the form ~L^(0.3)_\u03b1 . We compare the surface densities and the luminosity functions at the two\nredshifts and find that there is a multiplicative factor of two decrease in the number density of bright Ly\u03b1 emitters\nfrom z = 5.7 to z = 6.5, while the characteristic luminosity is unchanged.", "date": "2010-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "725", "number": "1", "publisher": "American Astronomical Society", "pagerange": "394-423", "id_number": "CaltechAUTHORS:20110112-144431112", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110112-144431112", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0687850" }, { "agency": "NSF", "grant_number": "AST-0709356" }, { "agency": "NSF", "grant_number": "AST-0708793" }, { "agency": "NASA/JPL", "grant_number": "1289080" }, { "agency": "Wisconsin Alumni Research Foundation" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/725/1/394", "primary_object": { "basename": "Hu2010p12242Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/kmrss-7yz47/files/Hu2010p12242Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Hu, E. M.; Cowie, L. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/a2ex1-s6264", "eprint_id": 21514, "eprint_status": "archive", "datestamp": "2023-08-22 01:27:31", "lastmod": "2023-10-21 00:05:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Tracking the impact of environment on the galaxy stellar mass function up to z ~ 1 in the 10 k zCOSMOS sample", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: fundamental parameters; galaxies: luminosity function, mass function", "note": "\u00a9 2010 ESO.\n\nReceived 30 June 2009; Accepted 21 September 2010; Published online 24 November 2010.\n\nBased on observations obtained at the European Southern Observatory (ESO) Very Large Telescope (VLT), Paranal, Chile, as part of the Large Program 175.A-0839 (the zCOSMOS Spectroscopic Redshift Survey).\n\nM.B. wishes to thank Preethi Nair, Alexis Finoguenov, and\nRamin Skibba for useful discussions, comments and suggestions. We thank the anonymous referee for the constructive first report, that helped improve the paper.\nM.B. is grateful to the editor, Fran\u00e7oise Combes, for her kind support. This work was partly supported by an INAF contract PRIN/2007/1.06.10.08 and an ASI grant \nASI/COFIS/WP3110 I/026/07/0.\n\nPublished - Bolzonella2010p12248Astron_Astrophys.pdf
", "abstract": "We study the impact of the environment on the evolution of galaxies in the zCOSMOS 10 k sample in the redshift range 0.1 \u2264 z \u2264 1.0 over an area of ~1.5\u2009deg^2. The considered sample of secure spectroscopic redshifts contains about 8500 galaxies, with their stellar masses estimated by SED fitting of the multiwavelength optical to near-infrared (NIR) photometry. The evolution of the galaxy stellar mass function (GSMF) in high and low density regions provides a tool to study the mass assembly evolution in different environments; moreover, the contributions to the GSMF from different galaxy types, as defined by their SEDs and their morphologies, can be quantified. At redshift z ~ 1, the GSMF is only slightly dependent on environment, but at lower redshifts the shapes of the GSMFs in high- and low-density environments become extremely different, with high density regions exhibiting a marked bimodality, not reproducible by a single Schechter function. As a result of this analysis, we infer that galaxy evolution depends on both the stellar mass and the environment, the latter setting the probability of a galaxy to have a given mass: all the galaxy properties related to the stellar mass show a dependence on environment, reflecting the difference observed in the mass functions. The shapes of the GSMFs of early- and late-type galaxies are almost identical for the extremes of the density contrast we consider, ranging from isolated galaxies to rich group members. The evolution toward z = 0 of the transition mass M_(cross), i.e., the mass at which the early- and late-type GSMFs match each other, is more rapid in high density environments, because of a difference in the evolution of the normalisation of GSMFs compared to the total one in the considered environment. The same result is found by studying the relative contributions of different galaxy types, implying that there is a more rapid evolution in overdense regions, in particular for intermediate stellar masses. The rate of evolution is different for sets of galaxy types divided on the basis of their SEDs or their morphologies, tentatively suggesting that the migration from the blue cloud to the red sequence occurs on a shorter timescale than the transformation from disc-like morphologies to ellipticals. Our analysis suggests that environmental mechanisms of galaxy transformation start to be more effective at z < 1. The comparison of the observed GSMFs to the same quantities derived from a set of mock catalogues based on semi-analytical models shows disagreement, in both low and high density environments: in particular, blue galaxies in sparse environments are overproduced in the semi-analytical models at intermediate and high masses, because of a deficit of star formation suppression, while at z < 0.5 an excess of red galaxies is present in dense environments at intermediate and low masses, because of the overquenching of satellites.", "date": "2010-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "524", "publisher": "EDP Sciences", "pagerange": "A76", "id_number": "CaltechAUTHORS:20101223-095421254", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101223-095421254", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN/2007/1.06.10.08" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110 I/026/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/200912801", "primary_object": { "basename": "Bolzonella2010p12248Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/a2ex1-s6264/files/Bolzonella2010p12248Astron_Astrophys.pdf" }, "pub_year": "2010", "author_list": "Bolzonella, M.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/2m49b-gnh92", "eprint_id": 21683, "eprint_status": "archive", "datestamp": "2023-08-19 04:32:09", "lastmod": "2023-10-21 00:14:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The zCOSMOS 10k-sample: the role of galaxy stellar mass in the colour-density relation up to z ~ 1", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: fundamental parameters \u2013 galaxies: statistics \u2013 galaxies: high-redshift \u2013 cosmology: observations \u2013\nlarge-scale structure of Universe", "note": "\u00a9 2010 ESO. Received 27 May 2009, Accepted 3 August 2010, Published online 19 November 2010. European Southern Observatory (ESO), Large Program 175.A-\n0839. We thank the referee for helpful comments. This work has\nbeen supported in part by the grant ASI/COFIS/WP3110 I/026/07/0.\n\nPublished - Cucciati2010p12244Astron_Astrophys.pdf
", "abstract": "Aims. With the first ~10 000 spectra of the flux limited zCOSMOS sample (I_(AB) \u2264 22.5) we want to study the evolution of environmental effects\non galaxy properties since z ~ 1.0, and to disentangle the dependence among galaxy colour, stellar mass and local density.\nMethods. We use our previously derived 3D local density contrast \u03b4, computed with the 5th nearest neighbour approach, to study the evolution\nwith z of the environmental effects on galaxy U-B colour, D4000 \u00c5 break and [OII]\u03bb3727 equivalent width (EW[OII]). We also analyze the implications\ndue to the use of different galaxy selections, using luminosity or stellar mass, and we disentangle the relations among colour, stellar mass\nand \u03b4 studying the colour-density relation in narrow mass bins.\nResults. We confirm that within a luminosity-limited sample (M_B \u2264 \u221220.5 \u2212 z) the fraction of red (U \u2212 B \u2265 1) galaxies depends on \u03b4 at least\nup to z ~ 1, with red galaxies residing mainly in high densities. This trend becomes weaker for increasing redshifts, and it is mirrored by the\nbehaviour of the fraction of galaxies with D4000 \u00c5 break \u22651.4. We also find that up to z ~ 1 the fraction of galaxies with log(EW[OII]) \u2265 1.15 is\nhigher for lower \u03b4, and also this dependence weakens for increasing z. Given the triple dependence among galaxy colours, stellar mass and \u03b4, the\ncolour-\u03b4 relation that we find in the luminosity-selected sample can be due to the broad range of stellar masses embedded in the sample. Thus, we\nstudy the colour-\u03b4 relation in narrow mass bins within mass complete subsamples, defining red galaxies with a colour threshold roughly parallel\nto the red sequence in the colour-mass plane. We find that once mass is fixed the colour-\u03b4 relation is globally flat up to z ~ 1 for galaxies with\nlog(M/M_\u2299) \u2273 10.7. This means that for these masses any colour-\u03b4 relation found within a luminosity-selected sample is the result of the combined\ncolour-mass and mass-\u03b4 relations. On the contrary, even at fixed mass we observe that within 0.1 \u2264 z \u2264 0.5 the fraction of red galaxies with\nlog(M/M_\u2299) \u2272 10.7 depends on \u03b4. For these mass and redshift ranges, environment affects directly also galaxy colours.\nConclusions. We suggest a scenario in which the colour depends primarily on stellar mass, but for an intermediate mass regime (10.2 \u2272 log(M/M_\u2299) \u2272 10.7) the local density modulates this dependence. These relatively low mass galaxies formed more recently, in an epoch when\nmore evolved structures were already in place, and their longer SFH allowed environment-driven physical processes to operate during longer\nperiods of time.", "date": "2010-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "524", "publisher": "EDP Sciences", "pagerange": "Art. No. A2", "id_number": "CaltechAUTHORS:20110111-090758572", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110111-090758572", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110I/026/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/200912585", "primary_object": { "basename": "Cucciati2010p12244Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/2m49b-gnh92/files/Cucciati2010p12244Astron_Astrophys.pdf" }, "pub_year": "2010", "author_list": "Cucciati, O. and Scoville, N." }, { "id": "https://authors.library.caltech.edu/records/6syph-rq478", "eprint_id": 21894, "eprint_status": "archive", "datestamp": "2023-08-19 04:32:52", "lastmod": "2023-10-23 15:28:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Doyle-T-F", "name": { "family": "Mizusawa", "given": "Trisha" }, "orcid": "0000-0001-7182-5307" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "Thomas H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "Patrick" }, "orcid": "0000-0002-3471-981X" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi" }, "orcid": "0000-0002-5619-4938" } ] }, "title": "The Spitzer Survey of Stellar Structure in Galaxies (S^4G)", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2010 The Astronomical Society of the Pacific. Received 2010 April 22; accepted 2010 October 6; published 2010 December 2. The authors thank the referee for useful comments and suggestions\nthat greatly helped improve this article. We are also\ngrateful to the dedicated staff at the Spitzer Science Center\nfor their support and help with the planning and execution of this legacy exploration program. K. S. would like to thank\nL. Armus, E. Bell, S. Carey, E. Churchwell, M. Dickinson,\nG. Helou, N. Scoville, and J. Stauffer for sharing their experiences\nin leading large teams. A. G. d. P. and J. C. M. M. are\npartially financed by the Spanish Programa Nacional de Astronom\u00eda\ny Astrof\u00edsica under grants AyA2006-02358 and\nAyA2009-10368. A. G. d. P. is also financed by the Spanish\nRam\u00f3n y Cajal program. J. C. M. M. acknowledges the receipt\nof a Formaci\u00f3n del Profesorado Universitario fellowship. E. L.\nand H. S. acknowledge support from the Academy of Finland.\nK. M. D. is supported by a National Science Foundation (NSF)\nAstronomy and Astrophysics Postdoctoral Fellowship under\naward AST-0802399. D. M. E. acknowledges support from\nthe Spitzer Science Center from NASA grant JPL RSA-1368024. R. B. acknowledges support from NSF grant AST\n05-07140. E. A. and A. B. thank the Centre National d'Etudes\nSpatiales and ANR-06-BLAN-0172 for support. K. L. M. acknowledges\nfunding from the Peter and Patricia Gruber Foundation\nas the 2008 IAU Fellow, from the University of\nPortsmouth, and from the South East Physics Network. This\nwork is based on observations and archival data obtained with\nthe Spitzer Space Telescope, which is operated by the Jet Propulsion\nLaboratory, California Institute of Technology under a\ncontract with NASA. Support for this work was provided by\nNASA. We gratefully acknowledge support from NASA JPL/Spitzer grant RSA 1374189 provided for the S^4G project.\n\nPublished - Sheth2010p12393Publ_Astron_Soc_Pac.pdf
", "abstract": "The Spitzer Survey of Stellar Structure in Galaxies (S^4G) is an Exploration Science Legacy Program\napproved for the Spitzer post\u2013cryogenic mission. It is a volume-, magnitude-, and size-limited (d < 40 Mpc,\n|b|> 30\u00b0,m_(Bcorr) < 15:5, and D_(25) > 1') survey of 2331 galaxies using the Infrared Array Camera (IRAC) at 3.6 and\n4.5 \u03bcm. Each galaxy is observed for 240 s and mapped to \u2265 1:5 \u00d7 D_(25). The final mosaicked images have a typical\n1 \u03c3 rms noise level of 0.0072 and 0:0093 MJy sr^-1 at 3.6 and 4.5 \u03bcm, respectively. Our azimuthally averaged surface\nbrightness profile typically traces isophotes at \u03bc_(3.6\u03bcm (AB)(1\u03c3) ~ 27 mag arcsec^(-2), equivalent to a stellar mass surface\ndensity of ~1 M_\u2299pc^(-2). S^4G thus provides an unprecedented data set for the study of the distribution of mass\nand stellar structures in the local universe. This large, unbiased, and extremely deep sample of all Hubble types from\ndwarfs to spirals to ellipticals will allow for detailed structural studies, not only as a function of stellar mass, but also\nas a function of the local environment. The data from this survey will serve as a vital testbed for cosmological\nsimulations predicting the stellar mass properties of present-day galaxies. This article introduces the survey and\ndescribes the sample selection, the significance of the 3.6 and 4.5 \u03bcm bands for this study, and the data collection\nand survey strategies. We describe the S^4G data analysis pipeline and present measurements for a first set of galaxies,\nobserved in both the cryogenic and warm mission phases of Spitzer. For every galaxy we tabulate the galaxy\ndiameter, position angle, axial ratio, inclination at \u03bc_(3.6\u03bcm)(AB) = 25:5, and 26:5 mag arcsec^(-2) (equivalent to\n\u2248\u03bc_B(AB) = 27:2 and 28:2 mag arcsec^(-2), respectively). These measurements will form the initial S^4G catalog\nof galaxy properties. We also measure the total magnitude and the azimuthally averaged radial profiles of ellipticity,\nposition angle, surface brightness, and color. Finally, using the galaxy-fitting code GALFIT, we deconstruct each\ngalaxy into its main constituent stellar components: the bulge/spheroid, disk, bar, and nuclear point source, where\nnecessary. Together, these data products will provide a comprehensive and definitive catalog of stellar structures,\nmass, and properties of galaxies in the nearby universe and will enable a variety of scientific investigations, some of\nwhich are highlighted in this introductory S^4G survey paper.", "date": "2010-12", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "122", "number": "898", "publisher": "Astronomical Society of the Pacific", "pagerange": "1397-1414", "id_number": "CaltechAUTHORS:20110126-084714506", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110126-084714506", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Nacional de Astronomia y Astrofisica", "grant_number": "AyA2006-02358" }, { "agency": "Nacional de Astronomia y Astrofisica", "grant_number": "AyA2009-10368" }, { "agency": "Ramon y Cajal programme" }, { "agency": "Formacion del Profesorado Universitario" }, { "agency": "Academy of Finland" }, { "agency": "NSF", "grant_number": "AST-0802399" }, { "agency": "NSF", "grant_number": "AST 05-07140" }, { "agency": "NASA", "grant_number": "RSA-1368024" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "University of Portsmouth" }, { "agency": "South East Physics Network" }, { "agency": "NASA", "grant_number": "RSA 1374189" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-06-BLAN-0172" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/657638", "primary_object": { "basename": "Sheth2010p12393Publ_Astron_Soc_Pac.pdf", "url": "https://authors.library.caltech.edu/records/6syph-rq478/files/Sheth2010p12393Publ_Astron_Soc_Pac.pdf" }, "pub_year": "2010", "author_list": "Sheth, Kartik; Mizusawa, Trisha; et el." }, { "id": "https://authors.library.caltech.edu/records/p7x0h-y8g09", "eprint_id": 21619, "eprint_status": "archive", "datestamp": "2023-08-22 01:28:28", "lastmod": "2023-10-21 00:11:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Understanding the shape of the galaxy two-point correlation function at z \u2243 1 in the COSMOS field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: statistics; cosmology: observations; large-scale structure of Universe", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS.\nAccepted 2010 July 12. Received 2010 July 7; in original form 2010 May 21.\nArticle first published online: 6 Sep. 2010.\n\n\n\nWe thank Ravi Sheth for helpful comments on the manuscript,\nand M. Kitzbichler and S. White for providing us with the\nCOSMOS mock surveys. LG thanks D. Sanders and the \nUniversity of Hawaii for hospitality at the Institute for Astronomy, where this work was initiated. Financial support from INAF and ASI through grants PRIN-INAF\u20132007 and ASI/COFIS/WP3110 I/026/07/0 is gratefully acknowledged.\nThis work is based on observations undertaken at the \nESO\u2013VLT under Large Programme 175.A-0839. Also based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under NASA contract NAS 5Y26555, with the Subaru Telescope, operated by the National Astronomical Observatory of Japan, with the telescopes\nof the National Optical Astronomy Observatory, operated\nby the Association of Universities for Research in Astronomy, Inc. (AURA), under cooperative agreement with the National Science Foundation and the Canada\u2013France\u2013Hawaii Telescope, operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France and the University of Hawaii.\n\nPublished - delaTorre2010p12121Mon_Not_R_Astron_Soc.pdf
", "abstract": "We investigate how the shape of the galaxy two-point correlation function as measured in the zCOSMOS survey depends on local environment, quantified in terms of the density contrast on scales of 5 h^(\u22121) Mpc. We show that the flat shape previously observed at redshifts between z= 0.6 and 1 can be explained by this volume being simply 10 per cent overabundant in high-density environments, with respect to a universal density probability distribution function. When galaxies corresponding to the top 10 per cent tail of the distribution are excluded, the measured w_(p)(r_(p)) steepens and becomes indistinguishable from Lambda cold dark matter (\u039bCDM) predictions on all scales. This is the same effect recognized by Abbas & Sheth in the Sloan Digital Sky Survey (SDSS) data at z \u2243 0 and explained as a natural consequence of halo\u2013environment correlations in a hierarchical scenario. Galaxies living in high-density regions trace dark matter haloes with typically higher masses, which are more correlated. If the density probability distribution function of the sample is particularly rich in high-density regions because of the variance introduced by its finite size, this produces a distorted two-point correlation function. We argue that this is the dominant effect responsible for the observed 'peculiar' clustering in the COSMOS field.", "date": "2010-12", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "867-872", "id_number": "CaltechAUTHORS:20110106-100036404", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110106-100036404", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-INAF\u20132007" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110 I/026/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1111/j.1365-2966.2010.17352.x", "primary_object": { "basename": "delaTorre2010p12121Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/p7x0h-y8g09/files/delaTorre2010p12121Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2010", "author_list": "de la Torre, S. and Scoville, N." }, { "id": "https://authors.library.caltech.edu/records/00ben-jfc49", "eprint_id": 21503, "eprint_status": "archive", "datestamp": "2023-08-22 01:27:19", "lastmod": "2023-10-21 00:05:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Moresco-M", "name": { "family": "Moresco", "given": "M." } }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "zCOSMOS 10k-bright spectroscopic sample: Exploring mass and environment dependence in early-type galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: fundamental parameters; galaxies: statistics; surveys", "note": "\u00a9 2010 ESO.\n\nReceived 12 January 2010; Accepted 8 September 2010; Published online 24 November 2010.\n\nBased on data obtained with the European Southern Observatory\nVery Large Telescope, Paranal, Chile, program 175.A-0839.\n\nWe acknowledge support from an INAF contract PRIN-\n2007/1.06.10.08 and an ASI grant ASI/COFIS/WP3110 I/026/07/0.\n\nPublished - Moresco2010p12250Astron_Astrophys.pdf
", "abstract": "Aims. We present the analysis of the U \u2013 V rest-frame color distribution and some spectral features as a function of mass and environment for a sample of early-type galaxies up to z = 1 extracted from the zCOSMOS spectroscopic survey. This analysis is used to place constraints on the relative importance of these two properties in controlling galaxy evolution. \n\nMethods. We used the zCOSMOS 10k-bright sample, limited to the AB magnitude range 15 < I < 22.5, from which we extracted two different subsamples of early-type galaxies. The first sample (\"red galaxies\") was selected using a photometric classification (2098 galaxies), while in the second case (\"ETGs\") we combined morphological, photometric, and spectroscopic properties to obtain a more reliable sample of elliptical, red, passive, early-type galaxies (981 galaxies). The analysis is performed at fixed mass to search for any dependence of the color distribution on environment, and at fixed environment to search for any mass dependence. \n\nResults. In agreement with the low redshift results of the SDSS, we find that the color distribution of red galaxies is not strongly dependent on environment for all mass bins, exhibiting only a weak trend such that galaxies in overdense regions (log_(10)(1+\u0394) ~ 1.2) are redder than galaxies in underdense regions (log_(10)(1+\u0394) ~ 0.1), \nwith a difference of <\u0394(U \u2013 V)_(rest)> = 0.027\u00b10.008 mag. On the other hand, the dependence on mass is far more significant, and we find that the average colors of massive galaxies (log_(10)(M/M_\u2609) ~ 10.8) are redder by <\u0394(U \u2013 V)_(rest)> = 0.093\u00b10.007 mag than low-mass galaxies (log_(10)(M/M_\u2609) ~ 10) \nthroughout the entire redshift range. We study the color-mass (U \u2013 V)_(rest) \u221d S_M \u00b7log_(10)(M/M_\u2609) relation, finding a mean slope = 0.12\u00b10.005, while the color-environment (U \u2013 V)_(rest) \u221d S_\u03b4 \u00b7 log_(10)(1+\u0394) relation is flatter, with a slope always smaller than S_\u03b4 \u2248 0.04. \n\nThe spectral analysis that we perform on our ETGs sample is in good agreement with our photometric results: we study the 4000 \u00c5\u2002 break and the equivalent width of the H\u03b4 Balmer line, finding for D4000 a dependence on mass (<\u0394D4000> =0.11\u00b10.02 between log_(10)(M/M_\u2609) ~ 10.2 and log_(10)(M/M_\u2609) ~ 10.8), and a much weaker dependence on environment (<\u0394D4000> = 0.05\u00b10.02 between high and low environment quartiles). The same is true for the equivalent width of H\u03b4, for which we measure a difference of \u0394EW0(H\u03b4) = 0.28\u00b10.08 \u00c5\u2002 across the same mass range and no significant dependence on environment. By analyzing the lookback time of early-type galaxies, we support the possibility of a downsizing scenario, in which massive galaxies with a stronger D4000 and an almost constant equivalent width of H\u03b4 formed their mass at higher redshift than lower mass ones. We also conclude that the main driver of galaxy evolution is the galaxy mass, the environment playing a subdominant role.", "date": "2010-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "524", "publisher": "EDP Sciences", "pagerange": "A67", "id_number": "CaltechAUTHORS:20101222-113130367", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101222-113130367", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-2007/1.06.10.08" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110 I/026/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201014044", "primary_object": { "basename": "Moresco2010p12250Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/00ben-jfc49/files/Moresco2010p12250Astron_Astrophys.pdf" }, "pub_year": "2010", "author_list": "Moresco, M.; Scarlata, C.; et el." }, { "id": "https://authors.library.caltech.edu/records/ekh1y-edp02", "eprint_id": 21362, "eprint_status": "archive", "datestamp": "2023-08-19 04:19:28", "lastmod": "2023-10-20 23:58:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kakazu-Yuko", "name": { "family": "Kakazu", "given": "Yuko" } }, { "id": "Hu-Esther-M", "name": { "family": "Hu", "given": "Esther M." } }, { "id": "Liu-Michael-C", "name": { "family": "Liu", "given": "Michael C." }, "orcid": "0000-0003-2232-7664" }, { "id": "Wang-Wei-Hao", "name": { "family": "Wang", "given": "Wei-Hao" }, "orcid": "0000-0003-2588-1265" }, { "id": "Wainscoat-R-J", "name": { "family": "Wainscoat", "given": "Richard J." }, "orcid": "0000-0002-1341-0952" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "Hawaii quasar and T dwarf survey. I. Method and discovery of faint field ultracool dwarfs", "ispublished": "pub", "full_text_status": "public", "keywords": "brown dwarfs, early universe, quasars: general, stars: low-mass, techniques: photometric", "note": "\u00a9 2010 American Astronomical Society. \n\nReceived 2009 August 7; accepted 2010 March 3; published 2010 October 8.\nBased in part on data obtained at the Subaru Telescope, which is operated by\nthe National Astronomical Observatory of Japan. Based in part on data obtained at the W. M. Keck Observatory, which is\noperated as a scientific partnership among the California Institute of\nTechnology, the University of California, and NASA and was made possible\nby the generous financial support of the W. M. Keck Foundation. We are indebted to the staff of the Subaru, Keck, and UKIRT\nobservatories for their excellent assistance with the observations.\nWe especially thank the support astronomer, Hisanori\nFurusawa, for his invaluable help in completing the observing\nrun with the Suprime-Cam. We are also grateful to the anonymous\nreferee for a helpful report.\n\nPublished - Kakazu2010p12055Astrophys_J.pdf
", "abstract": "The Hawaii Quasar and T dwarf survey (HQT Survey) is a wide-field, red optical survey carried out with the\nSuprime-Cam mosaic CCD camera on the 8.2 m Subaru telescope. The HQT survey is designed to search for\nlow-luminosity (M_(AB1450) < \u221223) quasars at high redshift (z > 5.7) as well as T dwarfs, both of which are selected\nby their very red I \u2212 z' colors. We use an optical narrowband filter NB816 to break a well-known I \u2212 z' color degeneracy between high-z quasars and foreground M and L dwarfs, which are more numerous than quasars.\nThis paper is the first in a series of papers from the HQT survey and we report on the discovery of six faint\n(19 \u2264 J \u2264 20) ultracool dwarfs found over a ~9.3 deg^2 area with a limiting magnitude of z'_(AB) \u2264 23.3. These\ndwarfs were confirmed by near-IR imaging and/or spectroscopy conducted at various facilities on Mauna Kea.\nWith estimated distances of 60\u2013170 pc, these are among the most distant spectroscopically confirmed field brown\ndwarfs to date. Limits on the proper motions of these ultracool dwarfs suggest that they are old members of the\nGalactic disk, though future follow-up observations are necessary to minimize errors. Our finding rate of ultracool\ndwarfs is within model predictions of Liu et al. However, the large brightening amplitude (~1 mag) previously\nreported for the L/T transition objects appears to overpredict the numbers. We also examine how the survey field latitude affects the survey sensitivity to the vertical scale height of ultracool dwarfs.", "date": "2010-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "723", "number": "1", "publisher": "American Astronomical Society", "pagerange": "184-196", "id_number": "CaltechAUTHORS:20101214-135434627", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101214-135434627", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/723/1/184", "primary_object": { "basename": "Kakazu2010p12055Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/ekh1y-edp02/files/Kakazu2010p12055Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Kakazu, Yuko; Hu, Esther M.; et el." }, { "id": "https://authors.library.caltech.edu/records/0m4cj-fan04", "eprint_id": 21801, "eprint_status": "archive", "datestamp": "2023-08-19 04:15:39", "lastmod": "2023-10-21 00:20:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "L." } }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "zCOSMOS \u2013 10k-bright spectroscopic sample : The bimodality in the galaxy stellar mass function: exploring\n its evolution with redshift", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: luminosity function, mass function \u2013 galaxies: statistics \u2013 galaxies: formation", "note": "\u00a9 2010 ESO. Received 30 July 2009, Accepted 31 May 2010, Published online 10 November 2010. Based on data obtained with the European Southern Observatory\nVery Large Telescope, Paranal, Chile, program 175.A-0839. L.P. wish to thank Fabio Fontanot and Gabriella De Lucia\nfor the stimulating discussions and to have provided SAM models and derived\nproperties in electronic form. L.P. thanks Micheal Brown and Ramin\nSkibba for comments. We acknowledge support from an INAF contract PRIN-\n2007/1.06.10.08 and an ASI grant ASI/COFIS/WP3110 I/026/07/0.\n\nPublished - Pozzetti2010p12367Astron_Astrophys.pdf
", "abstract": "We present the galaxy stellar mass function (GSMF) to redshift z \u2243 1, based on the analysis of about 8500 galaxies with I < 22.5 (AB mag)\nover 1.4 deg^2, which are part of the zCOSMOS-bright 10k spectroscopic sample. We investigate the total GSMF, as well as the contributions of\nearly- and late-type galaxies (ETGs and LTGs, respectively), defined by different criteria (broad-band spectral energy distribution, morphology,\nspectral properties, or star formation activities). We unveil a galaxy bimodality in the global GSMF, whose shape is more accurately represented\nby 2 Schechter functions, one linked to the ETG and the other to the LTG populations. For the global population, we confirm a mass-dependent\nevolution (\"mass-assembly downsizing\"), i.e., galaxy number density increases with cosmic time by a factor of two between z = 1 and z = 0 for\nintermediate-to-low mass (log(M/M_\u2299) ~ 10.5) galaxies but less than 15% for log(M/M_\u2299) > 11.We find that the GSMF evolution at intermediate-to-\nlow values of M(log(M/M_\u2299) < 10.6) is mostly explained by the growth in stellar mass driven by smoothly decreasing star formation activities,\ndespite the redder colours predicted in particular at low redshift. The low residual evolution is consistent, on average, with ~0.16 merger per\ngalaxy per Gyr (of which fewer than 0.1 are major), with a hint of a decrease with cosmic time but not a clear dependence on the mass. From\nthe analysis of different galaxy types, we find that ETGs, regardless of the classification method, increase in number density with cosmic time\nmore rapidly with decreasing M, i.e., follow a top-down building history, with a median \"building redshift\" increasing with mass (z > 1 for\nlog(M/M_\u2299) > 11), in contrast to hierarchical model predictions. For LTGs, we find that the number density of blue or spiral galaxies with\nlog(M/M_\u2299) > 10 remains almost constant with cosmic time from z ~ 1. Instead, the most extreme population of star-forming galaxies (with\nhigh specific star formation), at intermediate/high-mass, rapidly decreases in number density with cosmic time. Our data can be interpreted as\na combination of different effects. Firstly, we suggest a transformation, driven mainly by SFH, from blue, active, spiral galaxies of intermediate\nmass to blue quiescent and subsequently (1\u22122 Gyr after) red, passive types of low specific star formation. We find an indication that the complete\nmorphological transformation, probably driven by dynamical processes, into red spheroidal galaxies, occurred on longer timescales or followed\nafter 1\u22122 Gyr. A continuous replacement of blue galaxies is expected to be accomplished by low-mass active spirals increasing their stellar\nmass. We estimate the growth rate in number and mass density of the red galaxies at different redshifts and masses. The corresponding fraction\nof blue galaxies that, at any given time, is transforming into red galaxies per Gyr, due to the quenching of their SFR, is on average ~25% for\nlog(M/M_\u2299) < 11. We conclude that the build-up of galaxies and in particular of ETGs follows the same downsizing trend with mass (i.e. occurs\nearlier for high-mass galaxies) as the formation of their stars and follows the converse of the trend predicted by current SAMs. In this scenario, we\nexpect there to be a negligible evolution of the galaxy baryonic mass function (GBMF) for the global population at all masses and a decrease with\ncosmic time in the GBMF for the blue galaxy population at intermediate-high masses.", "date": "2010-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "523", "publisher": "EDP Sciences", "pagerange": "Art. No. A13", "id_number": "CaltechAUTHORS:20110118-162651431", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110118-162651431", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Istituto Nazionale di Astrofisica (INAF) (Italy)", "grant_number": "PRIN-2007/1.06.10.08" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110I/026/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/200913020", "primary_object": { "basename": "Pozzetti2010p12367Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/0m4cj-fan04/files/Pozzetti2010p12367Astron_Astrophys.pdf" }, "pub_year": "2010", "author_list": "Pozzetti, L.; Scarlata, C.; et el." }, { "id": "https://authors.library.caltech.edu/records/01txm-x0865", "eprint_id": 21442, "eprint_status": "archive", "datestamp": "2023-08-22 01:16:00", "lastmod": "2023-10-21 00:02:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "The Extended Chandra Deep Field-South Survey: Optical Spectroscopy of Faint X-ray Sources with the VLT and Keck", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: Seyfert; quasars: general; surveys; X-rays: galaxies", "note": "\u00a9 2010 American Astronomical Society.\n\nReceived 2010 April 13; accepted 2010 August 21; published 2010 October 26.\n\nBased on observations made with ESO Telescopes at Paranal Observatories under programme IDs 072.A-0139 and 080.A-0411.\n\n\nSome of the data presented herein were obtained at the W.M. Keck\nObservatory, which is operated as a scientific partnership among the California\nInstitute of Technology, the University of California and the National\nAeronautics and Space Administration. The Observatory was made possible\nby the generous financial support of the W.M. Keck Foundation.\n\nJ.D.S. is supported by World Premier International Research\nCenter Initiative (WPI Initiative), MEXT, Japan. The authors\nrecognize support from Michael Cooper for the use of the\nDEEP2 pipeline that was developed at UC Berkeley with\nsupport from NSF grant AST-0071048. W.N.B., B.L., and\nY.X. acknowledge support from the Chandra X-ray Center\ngrant SP8-9003A and NASA ADP grant NNX10AC99G. G.S.\nacknowledges support of the Pol\u00e1nyi Fellowship of NKTH.\nD.A. is funded by the Royal Society and Leverhulme Trust.\nM.S. and G.H. acknowledge support by the Leibniz Prize of\nthe Deutsche Forschungsgemeinschaft, DFG (HA 1850/28-1).\nA.C. is supported through ASI-INAF grants I/023/05/00 and I/\n088/06. P.T. acknowledges financial contribution from contract\nASIINAF I/088/06/0. The authors recognize and acknowledge\nthe very significant cultural role and reverence that the summit\nof Mauna Kea has always had within the indigenous Hawaiian\ncommunity. We are most fortunate to have the opportunity to\nconduct observations from this mountain.\nFacilities: VLT:Melipal(VIMOS), Keck:II(DEIMOS),\nCXO(ACIS-I)\n\nPublished - Silverman2010p12235Astrophys_J_Suppl_S.pdf
", "abstract": "We present the results of a program to acquire high-quality optical spectra of X-ray sources detected in the Extended-Chandra Deep Field-South (E-CDF-S) and its central 2 Ms area. New spectroscopic redshifts, up to z = 4, are measured for 283 counterparts to Chandra sources with deep exposures (t ~ 2-9 hr per pointing) using multi-slit facilities on both VLT (VIMOS) and Keck (DEIMOS), thus bringing the total number of spectroscopically identified X-ray sources to over 500 in this survey field. Since our new spectroscopic identifications are mainly associated with X-ray sources in the shallower 250 ks coverage, we provide a comprehensive catalog of X-ray sources detected in the E-CDF-S including the optical and near-infrared counterparts, determined by a likelihood routine, and redshifts (both spectroscopic and photometric), that incorporate published spectroscopic catalogs, thus resulting in a final sample with a high fraction (80%) of X-ray sources having secure identifications. We demonstrate the remarkable coverage of the luminosity-redshift plane now accessible from our data while emphasizing the detection of active galactic nuclei (AGNs) that contribute to the faint end of the luminosity function (L_(0.5-8 keV) ~ 10^(43)-10^(44) erg s^(\u20131)) at 1.5 \u2272 z \u2272 3 including those with and without broad emission lines. Our redshift catalog includes 17 type-2 QSOs at 1 \u2272 z \u2272 3.5 that significantly increases such samples (2\u00d7). Based on our deepest (9 hr) VLT/VIMOS observation, we identify \"elusive\" optically faint galaxies (R_(mag) ~ 25) at z ~ 2-3 based upon the detection of interstellar absorption lines (e.g., O II+Si IV, C II], C IV); we highlight one such case, an absorption-line galaxy at z = 3.208 having no obvious signs of an AGN in its optical spectrum. In addition, we determine accurate distances to eight galaxy groups with extended X-ray emission detected both by Chandra and XMM-Newton. Finally, we measure the physical extent of known large-scale structures (z ~ 0.7) evident in the CDF-S. While a thick sheet (a radial size of 67.7 Mpc) at z ~ 0.67 extends over the full field, the z ~ 0.73 structure is thin (18.8 Mpc) and filamentary as traced by both AGNs and galaxy groups. In the Appendix, we provide spectroscopic redshifts for 49 counterparts to fainter X-ray sources detected only in the 1 and 2 Ms catalogs, and 48 Very Large Array radio sources not detected in X-rays.", "date": "2010-11", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "191", "number": "1", "publisher": "American Astronomical Society", "pagerange": "124-142", "id_number": "CaltechAUTHORS:20101220-114038976", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101220-114038976", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "World Premier International Research Center Initiative (WPI Initiative)" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan" }, { "agency": "NSF", "grant_number": "AST-0071048" }, { "agency": "Chandra X-ray Center", "grant_number": "SP8-9003A" }, { "agency": "NASA ADP", "grant_number": "NNX10AC99G" }, { "agency": "Nemzeti Kutat\u00e1si \u00e9s Technol\u00f3giai Hivatal (NKTH)" }, { "agency": "Royal Society" }, { "agency": "Leverhulme Trust" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "HA 1850/28-1" }, { "agency": "Agenzia Spaziale Italiana-Istituto Nazionale di Astrofisica (ASI-INAF)", "grant_number": "I/023/05/00" }, { "agency": "Agenzia Spaziale Italiana-Istituto Nazionale di Astrofisica (ASI-INAF)", "grant_number": "I/088/06" }, { "agency": "Agenzia Spaziale Italiana-Istituto Nazionale di Astrofisica (ASI-INAF)", "grant_number": "I/088/06/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0067-0049/191/1/124", "primary_object": { "basename": "Silverman2010p12235Astrophys_J_Suppl_S.pdf", "url": "https://authors.library.caltech.edu/records/01txm-x0865/files/Silverman2010p12235Astrophys_J_Suppl_S.pdf" }, "pub_year": "2010", "author_list": "Silverman, J. D. and Capak, P." }, { "id": "https://authors.library.caltech.edu/records/a48w9-0nq14", "eprint_id": 21794, "eprint_status": "archive", "datestamp": "2023-08-19 04:15:22", "lastmod": "2023-10-21 00:20:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hildebrandt-H", "name": { "family": "Hildebrandt", "given": "H." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "PHAT: PHoto-z Accuracy Testing", "ispublished": "pub", "full_text_status": "public", "keywords": "techniques: photometric \u2013 galaxies: distances and redshifts \u2013 galaxies: photometry \u2013 cosmology: observations \u2013\nmethods: data analysis", "note": "\u00a9 2010 ESO. Received 29 April 2010, Accepted 23 July 2010, Published online 15 November 2010. Based on observations obtained with the Hubble Space Telescope,\nthe Spitzer Space Telescope, the Keck Observatory, the Kitt Peak\nNational Observatory, the Subaru Telescope, the Palomar Observatory,\nand the University of Hawaii 2.2-m telescope. We would like to thank JPL/Caltech for hospitality and support\nduring the 2008 PHAT workshop. We are grateful to the large number of colleagues\nwho made PHAT a success through discussions, criticism, and encouragement.\nA special thanks goes to Mike Hudson who came up with the acronym\n\"PHAT\". HH would like to thank in particular Catherine Heymans, Konrad\nKuijken, Ludovic van Waerbeke, and Peter Schneider for supporting the PHAT\neffort. HH was supported by the European DUEL RTN, project MRTN-CT-\n2006-036133. The work of LAM and DC was carried out at the Jet Propulsion\nLaboratory, California Institute of Technology, under a contract with NASA. LAM acknowledges support by the NASA ATFP program. CW was supported by\nan STFC Advanced Fellowship. NP acknowledges support from NKTH:Polanyi\nand KCKHA005 grants.\n\nPublished - Hildebrandt2010p12373Astron_Astrophys.pdf
", "abstract": "Context. Photometric redshifts (photo-z's) have become an essential tool in extragalactic astronomy. Many current and upcoming\nobserving programmes require great accuracy of photo-z's to reach their scientific goals.\nAims. Here we introduce PHAT, the PHoto-z Accuracy Testing programme, an international initiative to test and compare different\nmethods of photo-z estimation.\nMethods. Two different test environments are set up, one (PHAT0) based on simulations to test the basic functionality of the different\nphoto-z codes, and another one (PHAT1) based on data from the GOODS survey including 18-band photometry and ~ 2000 spectroscopic\nredshifts.\nResults. The accuracy of the different methods is expressed and ranked by the global photo-z bias, scatter, and outlier rates. While\nmost methods agree very well on PHAT0 there are differences in the handling of the Lyman-\u03b1 forest for higher redshifts. Furthermore,\ndifferent methods produce photo-z scatters that can differ by up to a factor of two even in this idealised case. A larger spread in accuracy\nis found for PHAT1. Few methods benefit from the addition of mid-IR photometry. The accuracy of the other methods is\nunaffected or suffers when IRAC data are included. Remaining biases and systematic effects can be explained by shortcomings in the\ndifferent template sets (especially in the mid-IR) and the use of priors on the one hand and an insufficient training set on the other\nhand. Some strategies to overcome these problems are identified by comparing the methods in detail. Scatters of 4\u20138% in \u0394z/(1 + z)\nwere obtained, consistent with other studies. However, somewhat larger outlier rates (>7.5% with \u0394z/(1 + z) > 0.15; >4.5% after\ncleaning) are found for all codes that can only partly be explained by AGN or issues in the photometry or the spec-z catalogue. Some\noutliers were probably missed in comparisons of photo-z's to other, less complete spectroscopic surveys in the past. There is a general\ntrend that empirical codes produce smaller biases than template-based codes.\nConclusions. The systematic, quantitative comparison of different photo-z codes presented here is a snapshot of the current state-of-the-\nart of photo-z estimation and sets a standard for the assessment of photo-z accuracy in the future. The rather large outlier rates\nreported here for PHAT1 on real data should be investigated further since they are most probably also present (and possibly hidden) in\nmany other studies. The test data sets are publicly available and can be used to compare new, upcoming methods to established ones\nand help in guiding future photo-z method development.", "date": "2010-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "523", "publisher": "EDP Sciences", "pagerange": "Art. No. A31", "id_number": "CaltechAUTHORS:20110118-134911247", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110118-134911247", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Dark Universe through Extragalactic Lensing (DUEL) Research and Training Network (RTN)", "grant_number": "MRTN-CT-2006-036133" }, { "agency": "NASA" }, { "agency": "Science and Technology Facilities Council (STFC) (UK)" }, { "agency": "NKTH: Polanyi (Hungary)", "grant_number": "KCKHA005" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/201014885", "primary_object": { "basename": "Hildebrandt2010p12373Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/a48w9-0nq14/files/Hildebrandt2010p12373Astron_Astrophys.pdf" }, "pub_year": "2010", "author_list": "Hildebrandt, H. and Capak, P." }, { "id": "https://authors.library.caltech.edu/records/4qafd-67y09", "eprint_id": 21620, "eprint_status": "archive", "datestamp": "2023-08-22 01:17:03", "lastmod": "2023-10-21 00:11:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cameron-E-M", "name": { "family": "Cameron", "given": "E." } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Aller-M-C", "name": { "family": "Aller", "given": "M. C." } }, { "id": "Bschorr-T-J", "name": { "family": "Bschorr", "given": "T." } }, { "id": "Cerulo-P", "name": { "family": "Cerulo", "given": "P." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Massey-R", "name": { "family": "Massey", "given": "R." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } } ] }, "title": "Bars in early- and late-type discs in COSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: structure", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS. \n\nAccepted 2010 July 6; Received 2010 July 6; in original form 2010 January 11. Article first published online: 30 Aug. 2010.\n\nPublished - Cameron2010p12120Mon_Not_R_Astron_Soc.pdf
", "abstract": "We investigate the (large-scale) bar fraction in a mass-complete sample of M > 10^(10.5) M_\u2299 disc galaxies at 0.2 < z < 0.6 in the Cosmological Evolution Survey (COSMOS) field. The fraction of barred discs strongly depends on mass, disc morphology and specific star formation rate (SSFR). At intermediate stellar mass (10^(10.5) < M < 10^(11) M_\u2299) the bar fraction in early-type discs is much higher, at all redshifts, by a factor of ~2, than that in late-type discs. This trend is reversed at higher stellar mass (M > 10^(11) M_\u2299), where the fraction of bars in early-type discs becomes significantly lower, at all redshifts, than that in late-type discs. The bar fractions for galaxies with low and high SSFRs closely follow those of the morphologically selected early- and late-type populations, respectively. This indicates a close correspondence between morphology and SSFR in disc galaxies at these earlier epochs. Interestingly, the total bar fraction in 10^(10.5) < M < 10^(11) M_\u2299 discs is built up by a factor of ~2 over the redshift interval explored, while for M > 10^(11) M_\u2299 discs it remains roughly constant. This indicates that, already by z ~ 0.6, spectral and morphological transformations in the most massive disc galaxies have largely converged to the familiar Hubble sequence that we observe in the local Universe, while for intermediate-mass discs this convergence is ongoing until at least z ~ 0.2. Moreover, these results highlight the importance of employing mass-limited samples for quantifying the evolution of barred galaxies. Finally, the evolution of the barred galaxy populations investigated does not depend on the large-scale environmental density (at least, on the scales which can be probed with the available photometric redshifts).", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "346-354", "id_number": "CaltechAUTHORS:20110106-100103588", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110106-100103588", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2010.17314.x", "primary_object": { "basename": "Cameron2010p12120Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/4qafd-67y09/files/Cameron2010p12120Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2010", "author_list": "Cameron, E.; Carollo, C. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/nearn-pe206", "eprint_id": 20659, "eprint_status": "archive", "datestamp": "2023-08-22 01:07:25", "lastmod": "2023-10-20 23:18:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fu-Hai", "name": { "family": "Fu", "given": "Hai" }, "orcid": "0000-0001-9608-6395" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" } ] }, "title": "Decomposing Star Formation and Active Galactic Nucleus with Spitzer Mid-infrared Spectra: Luminosity Functions and Co-evolution", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: luminosity function, mass function; infrared: galaxies; quasars: general; X-rays: galaxies", "note": "\u00a9 2010 The American Astronomical Society. Received 2010 June 15; accepted 2010 August 17; published 2010 September 22. We thank Knud Jahnke, Mark Sargent, Giovanni Zamorani, and the anonymous referee for helpful comments. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech under grant JPL-1344606.\n\nPublished - Fu2010p11726Astrophys_J.pdf
", "abstract": "We present Spitzer 7-38 \u03bcm spectra for a 24 \u03bcm flux-limited sample of galaxies at z ~ 0.7 in the COSMOS field. The detailed high-quality spectra allow us to cleanly separate star formation (SF) and active galactic nucleus (AGN) in individual galaxies. We first decompose mid-infrared luminosity functions (LFs). We find that the SF 8 \u03bcm and 15 \u03bcm LFs are well described by Schechter functions. AGNs dominate the space density at high luminosities, which leads to the shallow bright-end slope of the overall mid-infrared LFs. The total infrared (8-1000 \u03bcm) LF from 70 \u03bcm selected galaxies shows a shallower bright-end slope than the bolometrically corrected SF 15 \u03bcm LF, owing to the intrinsic dispersion in the mid-to-far-infrared spectral energy distributions. We then study the contemporary growth of galaxies and their supermassive black holes (BHs). Seven of the thirty-one luminous infrared galaxies with Spitzer spectra host luminous AGNs, implying an AGN duty cycle of 23% \u00b1 9%. The time-averaged ratio of BH accretion rate and SF rate matches the local M_(BH) \u2013 M_(bulge) relation and the M_(BH) \u2013 M_(host) relation at z ~ 1. These results favor co-evolution scenarios in which BH growth and intense SF happen in the same event but the former spans a shorter lifetime than the latter. Finally, we compare our mid-infrared spectroscopic selection with other AGN identification methods and discuss candidate Compton-thick AGNs in the sample. While only half of the mid-infrared spectroscopically selected AGNs are detected in X-ray, ~90% of them can be identified with their near-infrared spectral indices.", "date": "2010-10-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "722", "number": "1", "publisher": "American Astronomical Society", "pagerange": "653-667", "id_number": "CaltechAUTHORS:20101104-083052443", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101104-083052443", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "JPL-1344606" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/722/1/653", "primary_object": { "basename": "Fu2010p11726Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/nearn-pe206/files/Fu2010p11726Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Fu, Hai; Yan, Lin; et el." }, { "id": "https://authors.library.caltech.edu/records/vktw5-r5870", "eprint_id": 20597, "eprint_status": "archive", "datestamp": "2023-08-22 00:52:40", "lastmod": "2023-10-20 23:14:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "Jeyhan S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" } ] }, "title": "A Multiwavelength Study of a Sample of 70 \u03bcm Selected Galaxies in the COSMOS Field. II. The Role of Mergers in Galaxy Evolution", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: evolution; galaxies: high-redshift; infrared: galaxies; surveys", "note": "\u00a9 2010 American Astronomical Society.\n\nReceived 2009 August 9; accepted 2010 June 22; published 2010 August 26.\n\nBased on observations with the NASA/ESA Hubble Space Telescope,\nobtained at the Space Telescope Science Institute, which is operated by AURA\nInc, under NASA contract NAS 5-26555; also based on data collected at the\nSubaru Telescope, which is operated by the National Astronomical\nObservatory of Japan; the XMM-Newton, an ESA science mission with\ninstruments and contributions directly funded by ESA Member States and\nNASA; the European Southern Observatory under Large Program\n175.A-0839, Chile; the National Radio Astronomy Observatory which is a\nfacility of the National Science Foundation operated under cooperative\nagreement by Associated Universities, Inc; the Canada\u2013France\u2013Hawaii\nTelescope with MegaPrime/MegaCam operated as a joint project by the CFHT\nCorporation, CEA/DAPNIA, the National Research Council of Canada, the\nCanadian Astronomy Data Centre, the Centre National de la Recherche\nScientifique de France, TERAPIX and the University of Hawaii.\n\nSupport for this work was provided in part by NASA\nthrough contracts 1282612, 1298213, and 1344920 issued by\nthe Jet Propulsion Laboratory. This work was supported in\npart by a grant from The City University of New York PSCCUNY\nResearch Award Program. We would also like to recognize the contributions from all of the members of the COSMOS Team who helped in obtaining and reducing the large amount of multi-wavelength data that are now publicly available through the NASA Infrared Science Archive (IRSA) at\nhttp://irsa.ipac.caltech.edu/Missions/cosmos.html. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has also made use of data from the Sloan Digital Sky Survey (SDSS-DR7). Funding for the SDSS and SDSSII has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U. S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSSWeb site is http://www.sdss.org/. We thank the anonymous referee for their thorough comments, which\ngreatly improved the paper. We also thank Marco Barden and\nKnud Jhanke for the use of the FERENGI redshifting code as\nwell as their help with using it.\n\nPublished - Kartaltepe2010p11586Astrophys_J.pdf
", "abstract": "We analyze the morphological properties of a large sample of 1503 70 \u03bcm selected galaxies in the COSMOS field spanning the redshift range 0.01 < z < 3.5 with a median redshift of 0.5 and an infrared luminosity range of 10^8 < L_(IR)(8 \u2013 1000 \u03bcm)< 10^(14) L_\u2609 with a median luminosity of 10^(11.4) L_\u2609. In general, these galaxies are massive, with a stellar mass range of 10^(10)-10^(12) M_\u2609, and luminous, with \u201325 < M_K < \u201320. We find a strong correlation between the fraction of major mergers and L IR, with the fraction at the highest luminosity (L_(IR) > 10^(12) L_\u2609) being up to ~50%. We also find that the fraction of spirals drops dramatically with L_(IR). Minor mergers likely play a role in boosting the infrared luminosity for sources with low luminosities (L_(IR) < 10^(11.5) L_\u2609). The precise fraction of mergers in any given L(IR) bin varies by redshift due to sources at z > 1 being difficult to classify and subject to the effects of bandpass shifting; therefore, these numbers can only be considered lower limits. At z < 1, where the morphological classifications are most robust, major mergers clearly dominate the ULIRG population (~50%-80%) and are important for the LIRG population (~25%-40%). At z > 1, the fraction of major mergers is lower, but is at least 30%-40% for ULIRGs. In a comparison of our visual classifications with several automated classification techniques we find general agreement; however, the fraction of identified mergers is underestimated due to automated classification methods being sensitive to only certain timescales of a major merger. Although the general morphological trends agree with what has been observed for local (U)LIRGs, the fraction of major mergers is slightly lower than seen locally. This is in part due to the difficulty of identifying merger signatures at high redshift. The distribution of the U \u2013 V color of the galaxies in our sample peaks in the green valley (= 1.1) with a large spread at bluer and redder colors and with the major mergers peaking more strongly in the green valley than the rest of the morphological classes. We argue that, given the number of major gas-rich mergers observed and the relatively short timescale that they would be observable in the (U)LIRG phase, it is plausible for the observed red sequence of massive ellipticals (<10^(12) M_\u2609) to have been formed entirely by gas-rich major mergers.", "date": "2010-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "721", "number": "1", "publisher": "American Astronomical Society", "pagerange": "98-123", "id_number": "CaltechAUTHORS:20101029-095828614", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101029-095828614", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1282612" }, { "agency": "NASA", "grant_number": "1298213" }, { "agency": "NASA", "grant_number": "1344920" }, { "agency": "City University of New York" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/721/1/98", "primary_object": { "basename": "Kartaltepe2010p11586Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/vktw5-r5870/files/Kartaltepe2010p11586Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Kartaltepe, Jeyhan S.; Frayer, D. T.; et el." }, { "id": "https://authors.library.caltech.edu/records/nt69b-2nj74", "eprint_id": 20513, "eprint_status": "archive", "datestamp": "2023-08-19 03:51:44", "lastmod": "2023-10-20 23:08:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Feruglio-C", "name": { "family": "Feruglio", "given": "C." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Fiore-F", "name": { "family": "Fiore", "given": "F." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Ideue-Y", "name": { "family": "Ideue", "given": "Y." } } ] }, "title": "Obscured Star Formation and Environment in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general \u2013 galaxies: evolution \u2013 large-scale structure of universe \u2013 surveys", "note": "\u00a9 2010 The American Astronomical Society.\n\nReceived 2009 May 2; accepted 2010 July 7; published 2010 August 31.\nThis work is based on observations made with the Spitzer\nSpace Observatory, which is operated by the Jet Propulsion Laboratory\n(JPL), California Institute of Technology under NASA\ncontract 1407. Support for this work was provided by ANR \"DSIGALE\"\nANR-06-BLAN-0170 grant. Support for this work\nwas provided in part by NASA through contracts 1282612 and\n1298231 issued by the JPL, and grants 1289085 and 1310136.\nWe thank the anonymous referee for carefully reading and providing\nuseful suggestions that improved the paper.\n\nPublished - Feruglio2010p11583Astrophys_J.pdf
", "abstract": "We investigate the effects of the environment on star formation in a sample of massive luminous and ultra-luminous infrared galaxies (LIRGs and ULIRGs) with S(24 \u03bcm) >80 \u03bcJy and i ^+ < 24 in the COSMOS field. We exploit the accurate photometric redshifts in COSMOS to characterize the galaxy environment and study the evolution of the fraction of LIRGs and ULIRGs in different environments in the redshift range z = 0.3-1.2 and in bins of stellar mass. We find that the environment plays a role in the star formation processes and evolution of LIRGs and ULIRGs. We find an overall increase of the ULIRG+LIRG fraction in an optically selected sample with increasing redshift, as expected from the evolution of the star formation rate (SFR) density. We find that the ULIRG+LIRG fraction decreases with increasing density up to z ~ 1, and that the dependence on density flattens with increasing redshift. We do not observe the reversal of the SFR density relation up to z = 1 in massive LIRGs and ULIRGs, suggesting that such reversal might occur at higher redshift in this infrared luminosity range.", "date": "2010-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "721", "number": "1", "publisher": "American Astronomical Society", "pagerange": "607-614", "id_number": "CaltechAUTHORS:20101025-134444339", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101025-134444339", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "ANR \"DSIGALE\"", "grant_number": "ANR-06-BLAN-0170" }, { "agency": "NASA/JPL", "grant_number": "1282612" }, { "agency": "NASA/JPL", "grant_number": "1298231" }, { "agency": "NASA", "grant_number": "1289085" }, { "agency": "NASA", "grant_number": "1310136" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/721/1/607", "primary_object": { "basename": "Feruglio2010p11583Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/nt69b-2nj74/files/Feruglio2010p11583Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Feruglio, C.; Aussel, H.; et el." }, { "id": "https://authors.library.caltech.edu/records/cevp6-j7e30", "eprint_id": 20157, "eprint_status": "archive", "datestamp": "2023-08-22 00:50:00", "lastmod": "2023-10-20 22:16:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "Dominik A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "Christopher L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Cox-Pierre", "name": { "family": "Cox", "given": "Pierre" }, "orcid": "0000-0003-2027-8221" }, { "id": "Neri-Roberto", "name": { "family": "Neri", "given": "Roberto" }, "orcid": "0000-0002-7176-4046" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "Frank" }, "orcid": "0000-0002-1707-1775" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" } ] }, "title": "A Massive Molecular Gas Reservoir in the z = 5.3 Submillimeter Galaxy AzTEC-3", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: formation; galaxies: high-redshift; galaxies:\nstarburst; radio lines: galaxies", "note": "\u00a9 2010 American Astronomical Society. \n\nReceived 2010 June 28; accepted 2010 July 30; published 2010 August 16. \n\nWe thank Josh Younger for the SMA image of AzTEC-3, Christian Henkel for the original version of the LVG code, and the referee for a helpful report. D.R. acknowledges support from NASA through Hubble Fellowship grant HST-HF-51235.01 awarded by STScI, operated by AURA for NASA, under contract NAS 5-26555. The IRAM PdBI is supported by INSU/CNRS (France),MPG (Germany), and IGN (Spain). The EVLA is a facility of NRAO, operated by AUI, under a cooperative agreement with the NSF.\n\nPublished - Riechers2010p11446Astrophys_J_Lett.pdf
Accepted Version - 1008.0389.pdf
", "abstract": "We report the detection of CO J = 2\u21921, 5\u21924, and 6\u21925 emission in the highest-redshift submillimeter galaxy (SMG) AzTEC-3 at z = 5.298, using the Expanded Very Large Array and the Plateau de Bure Interferometer. These observations ultimately confirm the redshift, making AzTEC-3 the most submillimeter-luminous galaxy in a massive z \u2243 5.3 protocluster structure in the COSMOS field. The strength of the CO line emission reveals a large molecular gas reservoir with a mass of 5.3 \u00d7 10^(10)(\u03b1_(CO)/0.8) M_\u2609 sun, which can maintain the intense 1800 M_\u2609 sun yr^(\u20131) starburst in this system for at least 30 Myr, increasing the stellar mass by up to a factor of six in the process. This gas mass is comparable to \"typical\" z ~ 2 SMGs and constitutes \u227380% of the baryonic mass (gas+stars) and 30%-80% of the total (dynamical) mass in this galaxy. The molecular gas reservoir has a radius of <4 kpc and likely consists of a \"diffuse\", low-excitation component, containing (at least) 1/3 of the gas mass (depending on the relative conversion factor \u03b1CO), and a \"dense\", high-excitation component, containing ~2/3 of the mass. The likely presence of a substantial diffuse component besides highly excited gas suggests different properties between the star-forming environments in z > 4 SMGs and z > 4 quasar host galaxies, which perhaps trace different evolutionary stages. The discovery of a massive, metal-enriched gas reservoir in an SMG at the heart of a large z = 5.3 protocluster considerably enhances our understanding of early massive galaxy formation, pushing back to a cosmic epoch where the universe was less than 1/12 of its present age.", "date": "2010-09-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "720", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L131-L136", "id_number": "CaltechAUTHORS:20100927-105114318", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100927-105114318", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51235.01" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/2041-8205/720/2/L131", "primary_object": { "basename": "1008.0389.pdf", "url": "https://authors.library.caltech.edu/records/cevp6-j7e30/files/1008.0389.pdf" }, "related_objects": [ { "basename": "Riechers2010p11446Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/cevp6-j7e30/files/Riechers2010p11446Astrophys_J_Lett.pdf" } ], "pub_year": "2010", "author_list": "Riechers, Dominik A.; Capak, Peter L.; et el." }, { "id": "https://authors.library.caltech.edu/records/erk5d-z0r24", "eprint_id": 20196, "eprint_status": "archive", "datestamp": "2023-08-19 03:44:34", "lastmod": "2023-10-20 22:19:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bhattacharya-B", "name": { "family": "Bhattacharya", "given": "B." } }, { "id": "Noriega-Crespo-A", "name": { "family": "Noriega-Crespo", "given": "A." }, "orcid": "0000-0002-6296-8960" }, { "id": "Penprase-B-E", "name": { "family": "Penprase", "given": "B. E." } }, { "id": "Meadows-V-S", "name": { "family": "Meadows", "given": "V. S." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Looper-D", "name": { "family": "Looper", "given": "D." } }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Giorgini-J-D", "name": { "family": "Giorgini", "given": "J. D." } }, { "id": "Granvik-M", "name": { "family": "Granvik", "given": "M." }, "orcid": "0000-0002-5624-1888" }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "C." }, "orcid": "0000-0003-4072-169X" }, { "id": "Hagen-A", "name": { "family": "Hagen", "given": "A." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Reach-W-T", "name": { "family": "Reach", "given": "W. T." }, "orcid": "0000-0001-8362-4094" }, { "id": "Rebull-L-M", "name": { "family": "Rebull", "given": "L. M." }, "orcid": "0000-0001-6381-515X" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" } ] }, "title": "Mid-infrared Photometric Analysis of Main Belt Asteroids: A Technique for Color-Color Differentiation from Background Astrophysical Sources", "ispublished": "pub", "full_text_status": "public", "keywords": "minor planets, asteroids: general \u2013 techniques: photometric", "note": "\u00a9 2010. The American Astronomical Society. All rights reserved. Received 2009 May 12; accepted 2010 June 16; published 2010 August 6. The authors acknowledge the late S. Tyler, whose enthusiastic\npresence is missed by the FLS-EPC team. During his years\nat the Spitzer Science Center, Mr. Tyler assisted in data analysis\nfor this project. The authors also thank the anonymous referee for helpful comments. B.B. thanks Dr. Tom Jarrett for providing\nvaluable feedback, and the FLS-EPC team acknowledges\nProfessor Jim Elliot for developing the original concept of the\nsolar system First Look Survey. This work is based upon observations\nmade with the Spitzer Space Telescope, operated by JPL,\nCaltech, and funded under NASA contract 1407. Additional\nwork is funded by the NASA Herschel Science Center, operated\nby JPL, Caltech.\n\nPublished - Bhattacharya2010p11429Astrophys_J.pdf
", "abstract": "The Spitzer Space Telescope routinely detects asteroids in astrophysical observations near the ecliptic plane. For the galactic or extragalactic astronomer, these solar system bodies can introduce appreciable uncertainty into the source identification process. We discuss an infrared color discrimination tool that may be used to distinguish between solar system objects and extrasolar sources. We employ four Spitzer Legacy data sets, the First Look Survey-Ecliptic Plane Component (FLS-EPC), SCOSMOS, SWIRE, and GOODS. We use the Standard Thermal Model to derive FLS-EPC main belt asteroid (MBA) diameters of 1-4 km for the numbered asteroids in our sample and note that several of our solar system sources may have fainter absolute magnitude values than previously thought. A number of the MBAs are detected at flux densities as low as a few tens of \u03bcJy at 3.6 \u03bcm. As the FLS-EPC provides the only 3.6-24.0 \u03bcm observations of individual asteroids to date, we are able to use this data set to carry out a detailed study of asteroid color in comparison to astrophysical sources observed by SCOSMOS, SWIRE, and GOODS. Both SCOSMOS and SWIRE have identified a significant number of asteroids in their data, and we investigate the effectiveness of using relative color to distinguish between asteroids and background objects. We find a notable difference in color in the IRAC 3.6-8.0 mm and MIPS 24 \u03bcm bands between the majority of MBAs, stars, galaxies, and active galactic nuclei, though this variation is less significant when comparing fluxes in individual bands. We find median colors for the FLS-EPC asteroids to be [F(5.8/3.6), F(8.0/4.5), F(24/8)] = (4.9 \u00b1 1.8, 8.9 \u00b1 7.4, 6.4 \u00b1 2.3). Finally, we consider the utility of this technique for other mid-infrared observations that are sensitive to near-Earth objects, MBAs, and trans-Neptunian objects. We consider the potential of using color to differentiate between solar system and background sources for several space-based observatories, including Warm Spitzer, Herschel, and WISE.", "date": "2010-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "720", "number": "1", "publisher": "American Astronomical Society", "pagerange": "114-129", "id_number": "CaltechAUTHORS:20100928-115506218", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100928-115506218", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1407" }, { "agency": "NASA Herschel Science Center" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/720/1/114", "primary_object": { "basename": "Bhattacharya2010p11429Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/erk5d-z0r24/files/Bhattacharya2010p11429Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Bhattacharya, B.; Noriega-Crespo, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/8mbg2-dwn07", "eprint_id": 19748, "eprint_status": "archive", "datestamp": "2023-08-22 00:37:51", "lastmod": "2023-10-20 21:20:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bundy-K-A", "name": { "family": "Bundy", "given": "Kevin" }, "orcid": "0000-0001-9742-3138" }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "Claudia" }, "orcid": "0000-0002-9136-8876" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Drory-N", "name": { "family": "Drory", "given": "Niv" } }, { "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Murray-N-W", "name": { "family": "Murray", "given": "Norman" } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "Pascal" }, "orcid": "0000-0001-5851-6649" }, { "id": "Ma-Chung-Pei", "name": { "family": "Ma", "given": "Chung-Pei" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "Lucia" } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The Rise and Fall of Passive Disk Galaxies: Morphological Evolution Along the Red Sequence Revealed by COSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation", "note": "\u00a9 2010 The American Astronomical Society.\n\nReceived 2009 December 5; accepted 2010 June 26; published 2010 August 4.\n\nWe thank Eliot Quataert, Arjen van der Wel, Avishai Dekel,\nFr\u00e9d\u00e9ric Bournaud, Bob Nichol, Karen Masters, and Tommaso\nTreu for very useful discussions and feedback. K.B. acknowledges\nsupport for this work provided by NASA through\nHubble Fellowship grant HF-01215, awarded by the Space\nTelescope Science Institute, which is operated by the Association\nof Universities for Research in Astronomy, Inc., for\nNASA, under contract NAS 5-26555. We acknowledge the entire\nCOSMOS collaboration which has made this work possible.\nMore information on the COSMOS survey is available at\nhttp://www.astro.caltech.edu/cosmos.\n\nPublished - Bundy2010p11222Astrophys_J.pdf
", "abstract": "The increasing abundance of passive \"red-sequence\" galaxies since z ~ 1-2 is mirrored by a coincident rise in the number of galaxies with spheroidal morphologies. In this paper, however, we show in detail, that, the correspondence between galaxy morphology and color is not perfect, providing insight into the physical origin of this evolution. Using the COSMOS survey, we study a significant population of red-sequence galaxies with disk-like morphologies. These passive disks typically have Sa-Sb morphological types with large bulges, but they are not confined to dense environments. They represent nearly one-half of all red-sequence galaxies and dominate at lower masses (\u227e10^(10) M_\u2299) where they are increasingly disk-dominated. As a function of time, the abundance of passive disks with M_* \u227e10^(11) M_\u2299 increases, but not as fast as red-sequence spheroidals in the same mass range. At higher mass, the passive disk population has declined since z ~ 1, likely because they transform into spheroidals. Based on these trends, we estimate that as much as 60% of galaxies transitioning onto the red sequence evolve through a passive disk phase. The origin of passive disks therefore has broad implications for our understanding of how star formation shuts down. Because passive disks tend to be more bulge-dominated than their star-forming counterparts, a simple fading of blue disks does not fully explain their origin. We explore the strengths and weaknesses of several more sophisticated explanations, including environmental effects, internal stabilization, and disk regrowth during gas-rich mergers. While previous work has sought to explain color and morphological transformations with a single process, these observations open the way to new insight by highlighting the fact that galaxy evolution may actually proceed through several separate stages.", "date": "2010-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "719", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1969-1983", "id_number": "CaltechAUTHORS:20100831-144255846", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100831-144255846", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HF-01215" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/719/2/1969", "primary_object": { "basename": "Bundy2010p11222Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/8mbg2-dwn07/files/Bundy2010p11222Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Bundy, Kevin; Scarlata, Claudia; et el." }, { "id": "https://authors.library.caltech.edu/records/148ry-a6036", "eprint_id": 19744, "eprint_status": "archive", "datestamp": "2023-08-22 00:34:19", "lastmod": "2023-10-20 21:19:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" }, { "id": "Younger-J-D", "name": { "family": "Younger", "given": "J. D." } }, { "id": "Fazio-G-G", "name": { "family": "Fazio", "given": "G. G." }, "orcid": "0000-0002-0670-0708" }, { "id": "Gurwell-M-A", "name": { "family": "Gurwell", "given": "M." }, "orcid": "0000-0003-0685-3621" }, { "id": "Espada-D", "name": { "family": "Espada", "given": "D." } }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Wilner-D-J", "name": { "family": "Wilner", "given": "D." }, "orcid": "0000-0003-1526-7587" } ] }, "title": "Identification of Two Bright z > 3 Submillimeter Galaxy Candidates in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: starburst", "note": "\u00a9 2010 The American Astronomical Society.\n\nReceived 2010 June 6; accepted 2010 June 30; published 2010 July 19.\n\nBased on observations obtained with the SMA, which is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Also based on observations obtained, within the COSMOS Legacy Survey, with the Institut de Radioastronomie Millimetrique (IRAM) 30 m telescope, the Caltech Submillimeter Observatory (CSO), the APEX telescope, the Hubble Space Telescope (HST), the Spitzer Space Telescope, the Subaru telescope, the Kitt Peak National Observatory (KPNO), the Cerro Tololo Inter-American Observatory (CTIO), the National Optical Astronomy Observatory (NOAO), the United Kingdom IR telescope (UKIRT), and the Canada-France-Hawaii telescope (CFHT). The National Radio Astronomy Observatory (NRAO) is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nJ.D.Y. acknowledges support from NASA through Hubble\nFellowship grant HF-51266.01 awarded by the Space Telescope\nScience Institute, which is operated by the Association of\nUniversities for Research in Astronomy, Inc., for NASA, under\ncontract NAS 5-26555. D.E. was supported by a Marie Curie\nInternational Fellowship within the 6th European Community\nFramework Programme (MOIF-CT-2006-40298).\n\nPublished - Aravena2010p11219Astrophys_J_Lett.pdf
", "abstract": "We present high-resolution interferometric Submillimeter Array imaging at 890 \u03bcm (~2\" resolution) of two millimeter selected galaxies\u2014MMJ100015+021549 and MMJ100047+021021\u2014discovered with the Max-Planck Millimeter Bolometer (MAMBO) on the IRAM 30 m telescope and also detected with Bolocam on the CSO, in the COSMOS field. The first source is significantly detected at the ~11\u03c3 level, while the second source is tentatively detected at the ~4\u03c3 level, leading to a positional accuracy of ~0.\"2-0.\"3. MM100015+021549 is identified with a faint radio and K-band source. MMJ100047+021021 shows no radio emission and is tentatively identified with a very faint K-band peak which lies at ~1.\"2 from a clumpy optical source. The submillimeter-to-radio flux ratio for MM100015+021549 yields a redshift of ~4.8, consistent with the redshift implied by the UV-to-submillimeter photometry, z ~ 3.0-5.0. We find evidence for warm dust in this source with an infrared luminosity in the range ~(0.9-2.5) \u00d7 10^(13) L_\u2299, supporting the increasing evidence for a population of luminous submillimeter galaxies at z > 3. Finally, the lack of photometric data for MMJ100047+021021 does not allow us to investigate its properties in detail; however, its submillimeter-to-radio flux ratio implies z > 3.5.", "date": "2010-08-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "719", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L15-L19", "id_number": "CaltechAUTHORS:20100831-132539538", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100831-132539538", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HF-51266.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Space Telescope Science Institute" }, { "agency": "Marie Curie International Fellowship", "grant_number": "MOIF-CT-2006-40298" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/2041-8205/719/1/L15", "primary_object": { "basename": "Aravena2010p11219Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/148ry-a6036/files/Aravena2010p11219Astrophys_J_Lett.pdf" }, "pub_year": "2010", "author_list": "Aravena, M.; Younger, J. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/4b6sh-8bx19", "eprint_id": 19745, "eprint_status": "archive", "datestamp": "2023-08-22 00:34:24", "lastmod": "2023-10-20 21:19:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aspin-C", "name": { "family": "Aspin", "given": "Colin" } }, { "id": "Reipurth-B", "name": { "family": "Reipurth", "given": "Bo" }, "orcid": "0000-0001-8174-1932" }, { "id": "Herczeg-G-J", "name": { "family": "Herczeg", "given": "Gregory J." }, "orcid": "0000-0002-7154-6065" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" } ] }, "title": "The 2008 Extreme Outburst of the Young Eruptive Variable Star EX Lupi", "ispublished": "pub", "full_text_status": "public", "keywords": "circumstellar matter; stars: formation; stars: individual (EX Lupi)", "note": "\u00a9 2010 The American Astronomical Society.\n\nReceived 2010 March 13; accepted 2010 June 28; published 2010 July 22.\n\nWe warmly thank G.H. Herbig for providing access to the J23\nHIRES data on EX Lupi. We are indebted to A. Jones for alerting\nus (via G.H. Herbig) to this new outburst of EX Lup. We also\nthank A. Juhasz for providing the K-band magnitude used above.\nData were obtained at the W.M. Keck Observatory, operated as a\nscientific partnership by the California Institute of Technology,\nthe University of California, and the National Aeronautics and\nSpace Administration. B.R. acknowledges partial support from\nthe NASA Astrobiology Institute (Cooperative Agreement No.\nNNA04CC08A).\n\nPublished - Aspin2010p11226Astrophys_J_Lett.pdf
", "abstract": "In early 2008, the young low-mass star EX Lupi, the prototype of the EXor class of eruptive variables, optically brightened by over 5 mag for a period of seven months. The previous time a change of such amplitude had been observed in EX Lup was over 50 years ago. In this Letter, we present new optical and near-IR high-resolution spectroscopy of EX Lup during the 2008 outburst. We investigate the physical characteristics of the outburst both soon after it began and some four months later, and consider the observed energetics and kinematics. Emission line strengths, widths, and profiles significantly changed between the two observations. Also, modeling of the 2.2935 \u03bcm CO overtone band head emission suggests that an inner gap in the circumstellar gas disk around the star may be present and that it is from the inner edge of the gas disk that the CO overtone emission probably arises. We derive a mass accretion luminosity and rate during the extreme outburst of ~2 \u00b1 0.5 L_\u2299 and ~(2 \u00b1 0.5) \u00d7 10^(\u20137) M_\u2299 yr^(\u20131), respectively, which suggests that this outburst was indeed one of the strongest witnessed in EX Lup, yet not as strong as those observed in FU Orionis stars.", "date": "2010-08-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "719", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L50-L55", "id_number": "CaltechAUTHORS:20100831-133312246", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100831-133312246", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNA04CC08A" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/2041-8205/719/1/L50", "primary_object": { "basename": "Aspin2010p11226Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/4b6sh-8bx19/files/Aspin2010p11226Astrophys_J_Lett.pdf" }, "pub_year": "2010", "author_list": "Aspin, Colin; Reipurth, Bo; et el." }, { "id": "https://authors.library.caltech.edu/records/vkg19-kfq32", "eprint_id": 19639, "eprint_status": "archive", "datestamp": "2023-08-19 03:22:04", "lastmod": "2023-10-20 21:13:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dobke-B-M", "name": { "family": "Dobke", "given": "Benjamin M." } }, { "id": "Johnston-D-E", "name": { "family": "Johnston", "given": "David E." } }, { "id": "Massey-R", "name": { "family": "Massey", "given": "Richard" } }, { "id": "High-F-W", "name": { "family": "High", "given": "F. William" } }, { "id": "Ferry-M", "name": { "family": "Ferry", "given": "Matt" } }, { "id": "Rhodes-J", "name": { "family": "Rhodes", "given": "Jason" } }, { "id": "Vanderveld-R-A", "name": { "family": "Vanderveld", "given": "R. Ali" } } ] }, "title": "Astronomical Image Simulation for Telescope and Survey Development", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2010 The Astronomical Society of the Pacific.\n\nReceived 2009 November 2; accepted 2010 June 26; published 2010 July 22.\n\nThanks to Molly Peeples and Banaby Rowe. B. M. D. and\nJ. R. acknowledge financial support through the NASA-JPL\nAward/Project Weak Gravitational Lensing: The Ideal Probe\nof Dark Matter and Dark Energy. R. J. M. acknowledges financial\nsupport through European Union grant MIRG-CT-208994\nand STFC Advanced Fellowship PP/E006450/1. The work of\nB. M. D., J. R., and A. V. was carried out at the Jet Propulsion\nLaboratory, California Institute of Technology, under contract\nwith the National Aeronautics and Space Administration\n(NASA).\n\nPublished - Dobke2010p11105Publ_Astron_Soc_Pac.pdf
", "abstract": "We present the simage software suite for the simulation of artificial extragalactic images, based\nempirically around real observations of the Hubble Ultra Deep Field. The simulations reproduce galaxies with\nrealistic and complex morphologies via the modeling of UDF galaxies as shapelets. Images can be created in\nthe B, V, i and z bands for both space- and ground-based telescopes and instruments. The simulated images\ncan be produced for any required field size, exposure time, PSF, telescope mirror size, pixel resolution, field star\ndensity, and a variety of detector noise sources. It has the capability to create images with either a predetermined\nnumber of galaxies, or one calibrated to the number counts of preexisting data sets such as the HST COSMOS\nsurvey. In addition, simple options are included to add a known weak gravitational lensing signal (both shear\nand flexion) to the simulated images. The software is available in IDL and can be freely downloaded for scientific,\ndevelopmental, and teaching purposes.", "date": "2010-08", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "122", "number": "894", "publisher": "Astronomical Society of the Pacific", "pagerange": "947-954", "id_number": "CaltechAUTHORS:20100824-131211852", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100824-131211852", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "European Union", "grant_number": "MIRG-CT-208994" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "PP/E006450/1" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1086/656016", "primary_object": { "basename": "Dobke2010p11105Publ_Astron_Soc_Pac.pdf", "url": "https://authors.library.caltech.edu/records/vkg19-kfq32/files/Dobke2010p11105Publ_Astron_Soc_Pac.pdf" }, "pub_year": "2010", "author_list": "Dobke, Benjamin M.; Johnston, David E.; et el." }, { "id": "https://authors.library.caltech.edu/records/hkyss-67930", "eprint_id": 19047, "eprint_status": "archive", "datestamp": "2023-08-22 00:18:20", "lastmod": "2023-10-20 19:19:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "Nicholas" } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "Emeric" } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "Stephane" } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "Herve" }, "orcid": "0000-0002-1371-5705" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "Jeyhan S." }, "orcid": "0000-0001-9187-3605" } ] }, "title": "A Far-infrared Characterization of 24 \u03bcm Selected Galaxies at 0 < z < 2.5 using Stacking at 70 \u03bcm and 160 \u03bcm in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: statistics; infrared: galaxies", "note": "\u00a9 2010 The American Astronomical Society.\nReceived 2010 February 17; accepted 2010 May 7; published 2010 June 9.\n\nIt is a pleasure to acknowledge the contribution from\nall our colleagues in the COSMOS collaboration. More\ninformation on the COSMOS survey is available at\nhttp://www.astro.caltech.edu/cosmos. This work is based on\nobservations made with the Spitzer Space Telescope, a facility\noperated by NASA/JPL. Financial supports were provided\nby NASA through contracts 1289085, 1310136, 1282612,\nand 1298231 issued by the Jet Propulsion Laboratory. We are\ngrateful to Herve Dole for insightful discussions on stacking\ntechniques.\n\nPublished - Lee2010p10594Astrophys_J.pdf
", "abstract": "We present a study of the average properties of luminous infrared galaxies detected directly at 24 \u03bcm in the COSMOS field using a median stacking analysis at 70 \u03bcm and 160 \u03bcm. Over 35,000 sources spanning 0 \u2264 z \u2264 3 and 0.06 mJy \u2264 S_(24) \u2264 3.0 mJy are stacked, divided into bins of both photometric redshift and 24 \u03bcm flux. We find no correlation of S_(70)/S_(24) flux density ratio with S_(24), but find that galaxies with higher S_(24) have a lower S_(160)/S_(24) flux density ratio. These observed ratios suggest that 24 \u03bcm selected galaxies have warmer spectral energy distributions (SEDs) at higher mid-IR fluxes, and therefore have a possible higher fraction of active galactic nuclei. Comparisons of the average S_(70)/S_(24) and S_(160)/S_(24) colors with various empirical templates and theoretical models show that the galaxies detected at 24 \u03bcm are consistent with \"normal\" star-forming galaxies and warm mid-IR galaxies such as Mrk 231, but inconsistent with heavily obscured galaxies such as Arp 220. We perform a \u03c7^2 analysis to determine best-fit galactic model SEDs and total IR luminosities for each of our bins. We compare our results to previous methods of estimating L IR and find that previous methods show considerable agreement over the full redshift range, except for the brightest S_(24) sources, where they overpredict the bolometric IR luminosity at high redshift, most likely due to their warmer dust SED. We present a table that can be used as a more accurate and robust method for estimating bolometric infrared luminosity from 24 \u03bcm flux densities.", "date": "2010-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "717", "number": "1", "publisher": "American Astronomical Society", "pagerange": "175-182", "id_number": "CaltechAUTHORS:20100714-135827342", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100714-135827342", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL", "grant_number": "1289085" }, { "agency": "NASA/JPL", "grant_number": "1310136" }, { "agency": "NASA/JPL", "grant_number": "1282612" }, { "agency": "NASA/JPL", "grant_number": "1298231" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/717/1/175", "primary_object": { "basename": "Lee2010p10594Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/hkyss-67930/files/Lee2010p10594Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Lee, Nicholas; Le Floc'h, Emeric; et el." }, { "id": "https://authors.library.caltech.edu/records/nczmf-71658", "eprint_id": 19060, "eprint_status": "archive", "datestamp": "2023-08-22 00:18:49", "lastmod": "2023-10-20 19:19:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D." }, "orcid": "0000-0003-1924-1122" } ] }, "title": "A Runaway Black Hole in COSMOS: Gravitational Wave or Slingshot Recoil?", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: formation; galaxies: interactions; galaxies: nuclei; quasars: absorption lines", "note": "\u00a9 2010 The American Astronomical Society.\n\nReceived 2009 August 3; accepted 2010 May 9; published 2010 June 9.\n\nF.C. thanks E. Costantini, T. J. Cox, M. Dotti, L. Hernquist,\nand A. Sesana for useful discussion. The authors thank Chien Y.\nPeng for useful discussions about GALFIT. The authors thank\nthe anonymous referee, whose critical analysis helped improve\nthis paper, making it more interesting. This work was supported\nin part by NASA Chandra grant number GO7-8136A\n(F.C., M.E., and A.F.), NASA contract NAS8-39073 (Chandra\nX-ray Center). K.J. acknowledges support from the Emmy\nNoether Programme of the German Science Foundation (DFG)\nthrough grant number JA 1114/3-1. In Italy, this work is supported\nby ASI/INAF contracts I/023/05/0, I/024/05/0, and\nI/088/06, and by PRIN/MUR grant 2006-02-5203. In\nGermany, this project is supported by the Bundesministerium\nf\u00a8ur Bildung und Forschung/Deutsches Zentrum f\u00a8ur Luft und\nRaumfahrt and the Max Planck Society.\nFacilities: CXO (ACIS), HST (ACS), XMM (pn)\n\nPublished - Civano2010p10591Astrophys_J.pdf
", "abstract": "We present a detailed study of a peculiar source detected in the COSMOS survey at z = 0.359. Source\nCXOC J100043.1+020637, also known as CID-42, has two compact optical sources embedded in the same galaxy.\nThe distance between the two, measured in the HST/ACS image, is 0.\"495 \u00b1 0.\"005 that, at the redshift of the source,\ncorresponds to a projected separation of 2.46 \u00b1 0.02 kpc. A large (~1200 km s^(\u22121)) velocity offset between the\nnarrow and broad components of H\u03b2 has been measured in three different optical spectra from the VLT/VIMOS\nand Magellan/IMACS instruments. CID-42 is also the only X-ray source in COSMOS, having in its X-ray spectra\na strong redshifted broad absorption iron line and an iron emission line, drawing an inverted P-Cygni profile. The\nChandra and XMM-Newton data show that the absorption line is variable in energy by \u0394E = 500 eV over four years\nand that the absorber has to be highly ionized in order not to leave a signature in the soft X-ray spectrum. That\nthese features\u2014the morphology, the velocity offset, and the inverted P-Cygni profile\u2014occur in the same source\nis unlikely to be a coincidence. We envisage two possible explanations, both exceptional, for this system: (1) a\ngravitational wave (GW) recoiling black hole (BH), caught 1\u201310 Myr after merging; or (2) a Type 1/Type 2 system\nin the same galaxy where the Type 1 is recoiling due to the slingshot effect produced by a triple BH system. The first\npossibility gives us a candidate GW recoiling BH with both spectroscopic and imaging signatures. In the second\ncase, the X-ray absorption line can be explained as a BAL-like outflow from the foreground nucleus (a Type 2 AGN)\nat the rearer one (a Type 1 AGN), which illuminates the otherwise undetectable wind, giving us the first opportunity\nto show that fast winds are present in obscured active galactic nuclei (AGNs), and possibly universal in AGNs.", "date": "2010-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "717", "number": "1", "publisher": "American Astronomical Society", "pagerange": "209-222", "id_number": "CaltechAUTHORS:20100715-083232132", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100715-083232132", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Chandra", "grant_number": "GO7-8136A" }, { "agency": "NASA", "grant_number": "NAS8-39073" }, { "agency": "German Science Foundation (DFG), Emmy Noether Programme", "grant_number": "JA 1114/3-1" }, { "agency": "Agenzia Spaziale Italiana/Istituto Nazionale di Astrofisica (ASI/INAF)", "grant_number": "I/023/05/0" }, { "agency": "Agenzia Spaziale Italiana/Istituto Nazionale di Astrofisica (ASI/INAF)", "grant_number": "I/024/05/0" }, { "agency": "Agenzia Spaziale Italiana/Istituto Nazionale di Astrofisica (ASI/INAF)", "grant_number": "I/088/06" }, { "agency": "PRIN/MUR", "grant_number": "2006-02-5203" }, { "agency": "Bundesministerium f\u00fcr Bildung und Forschung/Deutsches Zentrum f\u00fcr Luft und Raumfahrt" }, { "agency": "Max Planck Society" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/717/1/209", "primary_object": { "basename": "Civano2010p10591Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/nczmf-71658/files/Civano2010p10591Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Civano, F.; Salvato, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/gyakm-rtg73", "eprint_id": 18740, "eprint_status": "archive", "datestamp": "2023-08-22 00:06:28", "lastmod": "2023-10-20 16:43:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Zamojski-M-A", "name": { "family": "Zamojski", "given": "M." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The XMM-Newton Wide-field Survey in the Cosmos Field (XMM-COSMOS): Demography and Multiwavelength Properties of Obscured and Unobscured Luminous Active Galactic Nuclei", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; surveys; X-rays: diffuse background; X-rays: galaxies; X-rays: general", "note": "\u00a9 2010 The American Astronomical Society.\nReceived 2009 December 23; accepted 2010 April 15; published 2010 May 18. \n\nBased on data collected at: the NASA/ESA Hubble Space Telescope,\nobtained at the Space Telescope Science Institute, which is operated by AURA\nInc, under NASA contract NAS 5-26555; the Subaru Telescope, which is\noperated by the National Astronomical Observatory of Japan; the European\nSouthern Observatory, Chile, under Large Program 175.A-0839; Kitt Peak\nNational Observatory, Cerro Tololo Inter-American Observatory, and the\nNational Optical Astronomy Observatory, which are operated by the\nAssociation of Universities for Research in Astronomy, Inc. (AURA) under\ncooperative agreement with the National Science Foundation; and the\nCanada\u2013France\u2013Hawaii Telescope operated by the National Research Council\nof Canada, the Centre National de la Recherche Scientifique de France and the\nUniversity of Hawaii.\n\n\n\nThis work is based on observations obtained with XMM Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). In Germany, the XMM-Newton project is supported by the Bundesministerium f\u00a8ur Wirtschaft und Technologie/Deutsches Zentrum f\u00a8ur Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OX 0001), the Max-Planck Society, and the Heidenhain-Stiftung. Part of this work was supported by the Deutsches Zentrum f\u00a8ur Luft\u2013und Raumfahrt, DLR project numbers 50 OR 0207 and 50 OR 0405. In Italy, the XMM-COSMOS project is supported by PRIN/MIUR under grant 2006-02-5203, ASI-INAF grants I/023/05/00, I/088/06 and ASI/COFIS/WP3110,I/026/07/0. This work was supported in part by NASA Chandra grant number GO7- 8136A (F.C., M.E., A.F., H.H.). T.M. acknowledges support from CONACyT 83564 DGAPA/PAPIIT IN10209 to IAUNAM as well as the NASA ADP (NNX07AT02G) grant to UCSD. G.H. and M.S. acknowledge a contribution from the Leibniz Prize of the Deutsche Forschungsgemeinschaft under the grant HA 1850/28-1. N.C. and A.F. were partially supported from a NASA grant NNX07AV03G to UMBC. K.J. is supported by the Emmy Noether-Programme of the German Science Foundation DFG. E.T. is supported by the National Aeronautics and Space Administration through Chandra Postdoctoral Fellowship Award Number PF8-90055. We thank James Aird and Jacobo Ebrero for sending us machine-readable tables of their X-ray luminosity functions, Desika Narayanan for help with his model SEDs, and Ryan Hickox for providing unpublished information about the X-Bootes survey. We gratefully thank Nick Wright for a carefully reading of the manuscript. This work is based in part on observations obtained with MegaPrime/ MegaCam, a joint project of Canada\u2013France\u2013Hawaii Telescope (CFHT) and CEA/DAPNIA, at the CFHT, and on data products produced at TERAPIX data center located at the Institut d'Astophysique de Paris. This research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. We gratefully acknowledge the contribution of the entire COSMOS collaboration; more information on the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. This research has made use of the NASA/IPAC Extragalactic Database (NED) and the SDSS spectral archive. Finally, we thank the anonymous referee for detailed and constructive comments to the first version of this paper.\n\nPublished - Brusa2010p10350Astrophys_J.pdf
", "abstract": "We report the final optical identifications of the medium-depth (~60 ks), contiguous (2 deg^2) XMM-Newton survey of the COSMOS field. XMM-Newton has detected ~1800 X-ray sources down to limiting fluxes of ~5 \u00d7 10^(\u201316), ~3 \u00d7 10^(\u201315), and ~7 \u00d7 10^(\u201315) erg cm^(\u20132) s^(\u20131) in the 0.5-2 keV, 2-10 keV, and 5-10 keV bands, respectively (~1 \u00d7 10^(\u201315), ~6 \u00d7 10^(\u201315), and ~1 \u00d7 10^(\u201314) erg cm^(\u20132) s^(\u20131), in the three bands, respectively, over 50% of the area). The work is complemented by an extensive collection of multiwavelength data from 24 \u03bcm to UV, available from the COSMOS survey, for each of the X-ray sources, including spectroscopic redshifts for \u227350% of the sample, and high-quality photometric redshifts for the rest. The XMM and multiwavelength flux limits are well matched: 1760 (98%) of the X-ray sources have optical counterparts, 1711 (~95%) have IRAC counterparts, and 1394 (~78%) have MIPS 24 \u03bcm detections. Thanks to the redshift completeness (almost 100%) we were able to constrain the high-luminosity tail of the X-ray luminosity function confirming that the peak of the number density of log L_X > 44.5 active galactic nuclei (AGNs) is at z ~ 2. Spectroscopically identified obscured and unobscured AGNs, as well as normal and star-forming galaxies, present well-defined optical and infrared properties. We devised a robust method to identify a sample of ~150 high-redshift (z > 1), obscured AGN candidates for which optical spectroscopy is not available. We were able to determine that the fraction of the obscured AGN population at the highest (L_X > 10^(44) erg s^(\u20131)) X-ray luminosity is ~15%-30% when selection effects are taken into account, providing an important observational constraint for X-ray background synthesis. We studied in detail the optical spectrum and the overall spectral energy distribution of a prototypical Type 2 QSO, caught in a stage transitioning from being starburst dominated to AGN dominated, which was possible to isolate only thanks to the combination of X-ray and infrared observations.", "date": "2010-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "716", "number": "1", "publisher": "American Astronomical Society", "pagerange": "348-369", "id_number": "CaltechAUTHORS:20100621-082509894", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100621-082509894", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsches Zentrum f\u00fcr Luft\u2013und Raumfahrt (DLR)", "grant_number": "50 OR 0207" }, { "agency": "Deutsches Zentrum f\u00fcr Luft\u2013und Raumfahrt (DLR)", "grant_number": "50 OR 0405" }, { "agency": "NASA", "grant_number": "GO7-8136A" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "83564" }, { "agency": "DGAPA/PAPIIT", "grant_number": "IN10209" }, { "agency": "NASA", "grant_number": "NNX07AT02G" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "HA 1850/28-1" }, { "agency": "NASA", "grant_number": "NNX07AV03G" }, { "agency": "NASA Chandra Fellowship", "grant_number": "PF8-90055" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/716/1/348", "primary_object": { "basename": "Brusa2010p10350Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/gyakm-rtg73/files/Brusa2010p10350Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Brusa, M.; Salvato, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/dwkpr-87m39", "eprint_id": 18963, "eprint_status": "archive", "datestamp": "2023-08-22 00:00:32", "lastmod": "2023-10-20 19:14:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M. T." }, "orcid": "0000-0003-1033-9684" }, { "id": "Bondi-M", "name": { "family": "Bondi", "given": "M." } }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." } }, { "id": "Datta-A", "name": { "family": "Datta", "given": "A." } }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Ciliegi-P", "name": { "family": "Ciliegi", "given": "P." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The VLA-COSMOS Survey. IV. Deep Data and Joint Catalog", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; radio continuum: galaxies; surveys", "note": "\u00a9 2010 American Astronomical Society.\n\nReceived 2008 December 19; accepted 2010 April 19; published 2010 May 17.\n\nThe National Radio Astronomy Observatory (NRAO) is\noperated by Associated Universities, Inc., under cooperative\nagreement with the National Science Foundation. We thank the\nNRAOfor their support during this project.We thank our referee\nJim Condon for his insightful comments for improving the paper. C.C. thanks the Max-Planck-Gesellschaft and the Humboldt-Stiftung for support through the Max-Planck-Forschungspreis. C.C. and A.D. acknowledge support through NASA grant HST-GO-09822.33-A. M.T.S. acknowledges support by the German\nDFG under grant SCHI 536/3-2 and SCHI 536/3-3. V.S. acknowledges support by the German DFG under grant SCHI\n536/3-1. This project has been (partially) funded by the DFG\nPriority Programme 1177 \"Galaxy Evolution.\"\n\nPublished - Schinnerer2010p10598Astrophys_J_Suppl_S.pdf
", "abstract": "In the context of the VLA-COSMOS Deep project, additional VLA A array observations at 1.4 GHz were obtained for the central degree of the COSMOS field and combined with the existing data from the VLA-COSMOS Large project. A newly constructed Deep mosaic with a resolution of 2\".5 was used to search for sources down to 4\u03c3 with 1\u03c3 \u2248 12 \u03bcJy beam^(\u20131) in the central 50' \u00d7 50'. This new catalog is combined with the catalog from the Large project (obtained at 1\".5 \u00d7 1\".4 resolution) to construct a new Joint catalog. All sources listed in the new Joint catalog have peak flux densities of \u22655\u03c3 at 1\".5 and/or 2\".5 resolution to account for the fact that a significant fraction of sources at these low flux levels are expected to be slightly resolved at 1\".5 resolution. All properties listed in the Joint catalog, such as peak flux density, integrated flux density, and source size, are determined in the 2\".5 resolution Deep image. In addition, the Joint catalog contains 43 newly identified multi-component sources.", "date": "2010-06", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "188", "number": "2", "publisher": "American Astronomical Society", "pagerange": "384-404", "id_number": "CaltechAUTHORS:20100709-110106023", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100709-110106023", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Radio Astronomy Observatory" }, { "agency": "Max-Planck-Forschungspreis" }, { "agency": "NASA", "grant_number": "HST-GO-09822.33-A" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "SCHI 536/3-2" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "SCHI 536/3-3" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "SCHI 536/3-1" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "Priority Programme 1177 \"Galaxy Evolution\"" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0067-0049/188/2/384", "primary_object": { "basename": "Schinnerer2010p10598Astrophys_J_Suppl_S.pdf", "url": "https://authors.library.caltech.edu/records/dwkpr-87m39/files/Schinnerer2010p10598Astrophys_J_Suppl_S.pdf" }, "pub_year": "2010", "author_list": "Schinnerer, E.; Sargent, M. T.; et el." }, { "id": "https://authors.library.caltech.edu/records/xb1fy-wbm35", "eprint_id": 18582, "eprint_status": "archive", "datestamp": "2023-08-21 23:57:22", "lastmod": "2023-10-20 16:33:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Onodera-Masato", "name": { "family": "Onodera", "given": "M." } }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "Gobat-R", "name": { "family": "Gobat", "given": "R." } }, { "id": "Cappellari-M", "name": { "family": "Cappellari", "given": "M." } }, { "id": "Arimoto-Nobuo", "name": { "family": "Arimoto", "given": "N." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Yamada-Y", "name": { "family": "Yamada", "given": "Y." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mancini-C", "name": { "family": "Mancini", "given": "C." }, "orcid": "0000-0002-4297-0561" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kong-X", "name": { "family": "Kong", "given": "X." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Motohara-Kentaro", "name": { "family": "Motohara", "given": "K." } }, { "id": "Ohta-K", "name": { "family": "Ohta", "given": "K." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Tamura-N", "name": { "family": "Tamura", "given": "N." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" } ] }, "title": "A z = 1.82 Analog of Local Ultra-massive Elliptical Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift", "note": "\u00a9 2010 American Astronomical Society. \n\nReceived 2009 December 3; accepted 2010 April 12; published 2010 April 26. \n\nBased on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan (S09A-043). \n\nWe are grateful to Tomohiro Yoshikawa for providing MCSMDP before publication. We thank the Subaru telescope staff for help with our observations. We acknowledge funding ERC-StG-UPGAL-240039, ANR-07-BLAN-0228, ANR-08-JCJC-0008 and a Grant-in-Aid for Science Research (No. 19540245) by the Japanese Ministry of Education, Culture, Sports, Science, and Technology. A.R. is grateful to the Institute of Astronomy of ETH Z\u00a8urich for its kind hospitality. M.C. acknowledges support from an STFC Advanced Fellowship\n(PP/D005574/1).\n\nPublished - Onodera2010p10085Astrophys_J_Lett.pdf
", "abstract": "We present observations of a very massive galaxy at z = 1.82 that show that its morphology, size, velocity dispersion, and stellar population properties are fully consistent with those expected for passively evolving progenitors of today's giant ellipticals. These findings are based on a deep optical rest-frame spectrum obtained with the Multi-Object InfraRed Camera and Spectrograph on the Subaru Telescope of a high-z passive galaxy candidate (pBzK) from the COSMOS field, for which we accurately measure its redshift of z = 1.8230 and obtain an upper limit on its velocity dispersion \u03c3_* < 326 km s^(\u20131). By detailed stellar population modeling of both the galaxy broadband spectral energy distribution and the rest-frame optical spectrum, we derive a star formation-weighted age and formation redshift of t_(sf) \u2243 1-2 Gyr and z_(form) \u2243 2.5-4, and a stellar mass of M_* \u2243 (3-4) \u00d7 10^(11) M_\u2609. This is in agreement with a virial mass limit of M_(vir) < 7 \u00d7 10^(11) M_\u2609, derived from the measured \u03c3_* value and stellar half-light radius, as well as with the dynamical mass limit based on the Jeans equations. In contrast to previously reported super-dense passive galaxies at z ~ 2, the present galaxy at z = 1.82 appears to have both size and velocity dispersion similar to early-type galaxies in the local universe with similar stellar mass. This suggests that z ~ 2 massive and passive galaxies may exhibit a wide range of properties, then possibly following quite different evolutionary histories from z ~ 2 to z = 0.", "date": "2010-05-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "715", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L6-L11", "id_number": "CaltechAUTHORS:20100607-120752650", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100607-120752650", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "ERC-StG-UPGAL-240039" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-07-BLAN-0228" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-08-JCJC-0008" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "19540245" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "PP/D005574/1" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/2041-8205/715/1/L6", "primary_object": { "basename": "Onodera2010p10085Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/xb1fy-wbm35/files/Onodera2010p10085Astrophys_J_Lett.pdf" }, "pub_year": "2010", "author_list": "Onodera, M.; Daddi, E.; et el." }, { "id": "https://authors.library.caltech.edu/records/jq7te-7zk10", "eprint_id": 18524, "eprint_status": "archive", "datestamp": "2023-08-21 23:54:54", "lastmod": "2023-10-20 16:29:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M. T." }, "orcid": "0000-0003-1033-9684" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C. M." }, "orcid": "0000-0002-9136-8876" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Massey-R", "name": { "family": "Massey", "given": "R." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P. A." }, "orcid": "0000-0001-5851-6649" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" } ] }, "title": "The Opacity of Galactic Disks at z ~ 0.7", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; dust, extinction; galaxies: spiral; surveys", "note": "\u00a9 2010 American Astronomical Society.\n\nReceived 2010 February 1; accepted 2010 March 17; published 2010 April 5.\n\nWe gratefully acknowledge the anonymous referee's helpful\nsuggestions and the contribution of the COSMOS collaboration\nand its more than 100 scientists worldwide. P.K., P.A.O., C.S.,\nand M.T.S. acknowledge support from the Swiss National\nScience Foundation. This research was also financed by DFG\ngrant SCHI 536/3-2. The HST COSMOS Treasury programwas\nsupported through NASA grant HST-GO-09822.\nFacilities: HST (ACS), Subaru (SuprimeCam)\n\nPublished - Sargent2010p9985Astrophys_J_Lett.pdf
", "abstract": "We compare the surface brightness-inclination relation for a sample of COSMOS pure disk galaxies at z ~ 0.7 with an artificially redshifted sample of Sloan Digital Sky Survey (SDSS) disks well matched to the COSMOS sample in terms of rest-frame photometry and morphology, as well as their selection and analysis. The offset between the average surface brightness of face-on and edge-on disks in the redshifted SDSS sample matches that predicted by measurements of the optical depth of galactic disks in the nearby universe. In contrast, large disks at z ~ 0.7 have a virtually flat surface brightness-inclination relation, suggesting that they are more opaque than their local counterparts. This could be explained by either an increased amount of optically thick material in disks at higher redshift or a different spatial distribution of the dust.", "date": "2010-05-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "714", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L113-L117", "id_number": "CaltechAUTHORS:20100602-140157782", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100602-140157782", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "SCHI 536/3-2" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/2041-8205/714/1/L113", "primary_object": { "basename": "Sargent2010p9985Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/jq7te-7zk10/files/Sargent2010p9985Astrophys_J_Lett.pdf" }, "pub_year": "2010", "author_list": "Sargent, M. T.; Carollo, C. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/e8cy3-awp35", "eprint_id": 18479, "eprint_status": "archive", "datestamp": "2023-08-21 23:54:43", "lastmod": "2023-10-20 16:25:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Giodini-S", "name": { "family": "Giodini", "given": "S." } }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Boehringer-H", "name": { "family": "Boehringer", "given": "H." } }, { "id": "B\u00eerzan-L", "name": { "family": "B\u00eerzan", "given": "L." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Oklop\u010di\u0107-A", "name": { "family": "Oklop\u010di\u0107", "given": "A." }, "orcid": "0000-0002-9584-6476" }, { "id": "Pierini-D", "name": { "family": "Pierini", "given": "D." } }, { "id": "Pratt-G-W", "name": { "family": "Pratt", "given": "G. W." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "R." }, "orcid": "0000-0002-6085-3780" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. .S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } } ] }, "title": "Radio Galaxy Feedback in X-ray-selected Groups from COSMOS: The Effect on the Intracluster Medium", "ispublished": "pub", "full_text_status": "public", "keywords": "intergalactic medium; galaxies: active; galaxies: clusters: general; radio continuum: galaxies; X-rays: galaxies: clusters", "note": "\u00a9 2010 The American Astronomical Society. Received 2009 October 30; accepted 2010 February 19; published 2010 April 8. S.G. acknowledges support by the DFG Cluster of Excellence\n\"Origin and Structure of the universe\" (http://www.universecluster.de). S.G. thanks A. Merloni for helpful comments. V.S.\nacknowledges support from the Owens Valley Radio Observatory,\nwhich is supported by the National Science Foundation\nthrough grant AST-0838260. V.S. and A.O. thank\nUnity through Knowledge Fund (http://www.ukf.hr) for collaboration\nsupport through the \"Homeland Visit\" grant. A.O.\nthanks California Institute of Technology for generous support\nthrough NASA grants 1292462 and 1344606. We acknowledge\nthe contributions of the entire COSMOS collaboration;\nmore informations on the COSMOS survey are\navailable at http://www.astro.caltech.edu/\u223ccosmos. The authors\nacknowledge the National Radio Astronomy Observatory for\nsupport. The National Radio Astronomy Observatory is a facility\nof the National Science Foundation operated under cooperative\nagreement by Associated Universities, Inc.\n\nPublished - Giodini2010p9840Astrophys_J.pdf
", "abstract": "We quantify the importance of the mechanical energy released by radio galaxies inside galaxy groups. We use\nscaling relations to estimate the mechanical energy released by 16 radio-active galactic nuclei located inside X-raydetected\ngalaxy groups in the COSMOS field. By comparing this energy output to the host groups' gravitational\nbinding energy,we find that radio galaxies produce sufficient energy to unbind a significant fraction of the intragroup\nmedium. This unbinding effect is negligible in massive galaxy clusters with deeper potential wells. Our results\ncorrectly reproduce the breaking of self-similarity observed in the scaling relation between entropy and temperature\nfor galaxy groups.", "date": "2010-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "714", "number": "1", "publisher": "American Astronomical Society", "pagerange": "218-228", "id_number": "CaltechAUTHORS:20100527-112348383", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100527-112348383", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "Owens Valley Radio Observatory" }, { "agency": "NSF", "grant_number": "AST-0838260" }, { "agency": "Unity through Knowledge Fund" }, { "agency": "Caltech/NASA", "grant_number": "1292462" }, { "agency": "Caltech/NASA", "grant_number": "1344606" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/714/1/218", "primary_object": { "basename": "Giodini2010p9840Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/e8cy3-awp35/files/Giodini2010p9840Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Giodini, S.; Smol\u010di\u0107, V.; et el." }, { "id": "https://authors.library.caltech.edu/records/kfw8g-4yc56", "eprint_id": 18565, "eprint_status": "archive", "datestamp": "2023-08-21 23:55:09", "lastmod": "2023-10-20 16:31:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P. A." }, "orcid": "0000-0001-5851-6649" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Feldmann-R", "name": { "family": "Feldmann", "given": "R." }, "orcid": "0000-0002-1109-1919" }, { "id": "Hahn-O", "name": { "family": "Hahn", "given": "O." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M. T." }, "orcid": "0000-0003-1033-9684" }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Aller-M-C", "name": { "family": "Aller", "given": "M. C." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Bschorr-T-J", "name": { "family": "Bschorr", "given": "T." } }, { "id": "Bundy-K-A", "name": { "family": "Bundy", "given": "K." }, "orcid": "0000-0001-9742-3138" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "R." }, "orcid": "0000-0002-6085-3780" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "L." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } } ] }, "title": "The Buildup of the Hubble Sequence in the Cosmos Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation; galaxies: irregular; galaxies: spiral; galaxies: structure", "note": "\u00a9 2010 American Astronomical Society.\n\nReceived 2009 November 7; accepted 2010 March 11; published 2010 April 1.\n\nWe thank the COSMOS and zCOSMOS collaborations for\nmany stimulating discussions. P.O. acknowledges support from\nthe Swiss National Foundation (SNF). This work is based on\nobservations with the NASA/ESA Hubble Space Telescope,\nobtained at the Space Telescope Science Institute, which is\noperated by AURA Inc, under NASA contract NAS 5-26555;\nalso based on data collected at: the Subaru Telescope, which is\noperated by the National Astronomical Observatory of Japan;\nthe European Southern Observatory under Large Program\n175.A-0839, Chile; Kitt Peak National Observatory, Cerro\nTololo Inter-American Observatory, and the National Optical\nAstronomy Observatory, which are operated by the Association\nof Universities for Research in Astronomy, Inc. (AURA) under\ncooperative agreement with the National Science Foundation;\nand the Canada\u2013France\u2013Hawaii Telescope with MegaPrime/\nMegaCam operated as a joint project by the CFHT Corporation,\nCEA/DAPNIA, the National Research Council of Canada, the\nCanadian Astronomy Data Centre, the Centre National de la\nRecherche Scientifique de France, TERAPIX, and the University of Hawaii.\n\nPublished - Oesch2010p9988Astrophys_J_Lett.pdf
", "abstract": "We use ~8600 COSMOS galaxies at mass scales >5 \u00d7 10^(10) M_\u2609 to study how the morphological mix of massive ellipticals, bulge-dominated disks, intermediate-bulge disks, disk-dominated galaxies, and irregular systems evolves from z = 0.2 to z = 1. The morphological evolution depends strongly on mass. At M > 3 \u00d7 10^(11) M_\u2609, no evolution is detected in the morphological mix: ellipticals dominate since z = 1, and the Hubble sequence has quantitatively settled down by this epoch. At the 10^(11) M_\u2609 mass scale, little evolution is detected, which can be entirely explained by major mergers. Most of the morphological evolution from z = 1 to z = 0.2 takes place at masses 5 \u00d7 10^(10)-10^(11) M_\u2609, where (1) the fraction of spirals substantially drops and the contribution of early types increases. This increase is mostly produced by the growth of bulge-dominated disks, which vary their contribution from ~10% at z = 1 to >30% at z = 0.2 (for comparison, the elliptical fraction grows from ~15% to ~20%). Thus, at these masses, transformations from late to early types result in diskless elliptical morphologies with a statistical frequency of only 30%-40%. Otherwise, the processes which are responsible for the transformations either retain or produce a non-negligible disk component. (2) The disk-dominated galaxies, which contribute ~15% to the intermediate-mass galaxy population at z = 1, virtually disappear by z = 0.2. The merger rate since z = 1 is too low to account for the disappearance of these massive disk-dominated systems, which most likely grow a bulge via secular evolution.", "date": "2010-05-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "714", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L47-L51", "id_number": "CaltechAUTHORS:20100604-110726916", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100604-110726916", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swiss National Science Foundation (SNSF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/2041-8205/714/1/L47", "primary_object": { "basename": "Oesch2010p9988Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/kfw8g-4yc56/files/Oesch2010p9988Astrophys_J_Lett.pdf" }, "pub_year": "2010", "author_list": "Oesch, P. A.; Carollo, C. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/fstnw-x9t73", "eprint_id": 18663, "eprint_status": "archive", "datestamp": "2023-08-21 23:47:33", "lastmod": "2023-10-20 16:38:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Robertson-B-E", "name": { "family": "Robertson", "given": "Brant E." }, "orcid": "0000-0002-4271-0364" } ] }, "title": "Estimating Luminosity Function Constraints from High-Redshift Galaxy Surveys", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: abundances; methods: statistical; surveys", "note": "\u00a9 2010 The American Astronomical Society. Received 2010 January 7; accepted 2010 March 9; published 2010 April 1. I thank Peter Capak and Nick Scoville for useful advice on\nmodeling the survey data and WFC3 observations, Richard Ellis\nfor helpful discussions, and Anatoly Klypin for permission to\nuse his cosmological simulation. I am supported by a Hubble\nFellowship grant, program number HST-HF-51262.01-A\nprovided by NASA from the Space Telescope Science Institute,\nwhich is operated by the Association of Universities for\nResearch in Astronomy, Incorporated, under NASA contract\nNAS5-26555. I also thank the Caltech Astronomy Department\nfor hosting me during my Hubble Fellowship.\n\nPublished - Robertson2010p9927Astrophys_J.pdf
", "abstract": "The installation of the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope (HST) will revolutionize the study of high-redshift galaxy populations. Initial observations of the HST Ultra Deep Field (UDF) have yielded multiple z \u2273 7 dropout candidates. Supplemented by the GOODS Early Release Science (ERS) and further UDF pointings, these data will provide crucial information about the most distant known galaxies. However, achieving tight constraints on the z ~ 7 galaxy luminosity function (LF) will require even more ambitious photometric surveys. Using a Fisher matrix approach to fully account for Poisson and cosmic sample variance, as well as covariances in the data, we estimate the uncertainties on LF parameters achieved by surveys of a given area and depth. Applying this method to WFC3 z ~ 7 dropout galaxy samples, we forecast the LF parameter uncertainties for a variety of model surveys. We demonstrate that performing a wide area (~1 deg^2) survey to H_(AB) ~ 27 depth or increasing the UDF depth to H_(AB) ~ 30 provides excellent constraints on the high-z LF when combined with the existing Ultradeep Field Guest Observation and GOODS ERS data. We also show that the shape of the matter power spectrum may limit the possible gain of splitting wide area (\u22730.5 deg^2) high-redshift surveys into multiple fields to probe statistically independent regions; the increased rms density fluctuations in smaller volumes mostly offset the improved variance gained from independent samples.", "date": "2010-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "713", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1266-1281", "id_number": "CaltechAUTHORS:20100614-075754596", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100614-075754596", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Hubble Fellowship/NASA", "grant_number": "HST-HF-51262.01-A" }, { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/713/2/1266", "primary_object": { "basename": "Robertson2010p9927Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/fstnw-x9t73/files/Robertson2010p9927Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Robertson, Brant E." }, { "id": "https://authors.library.caltech.edu/records/3ke1y-4br69", "eprint_id": 17956, "eprint_status": "archive", "datestamp": "2023-08-21 23:43:59", "lastmod": "2023-10-20 15:27:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Oklop\u010di\u0107-A", "name": { "family": "Oklop\u010di\u0107", "given": "A." }, "orcid": "0000-0002-9584-6476" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Giodini-S", "name": { "family": "Giodini", "given": "S." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "B\u00eerzan-L", "name": { "family": "B\u00eerzan", "given": "L." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Identifying Dynamically Young Galaxy Groups Via Wide-angle Tail Galaxies: A Case Study in the COSMOS Field at z = 0.53", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: evolution; galaxies: fundamental parameters; radio continuum: galaxies", "note": "\u00a9 2010 American Astronomical Society.\n\nReceived 2009 November 6; accepted 2010 February 23; published 2010 March 23.\n\nA.O. thanks California Institute of Technology for generous\nsupport through NASA grants 1292462 and 1344606. V.S.\nacknowledges support from the Owens Valley Radio Observatory,\nwhich is supported by the National Science Foundation\nthrough grant AST-0838260. The research leading to these results\nhas received funding from the European Community's\nSeventh Framework Programme (FP7/2007-2013) under grant\nagreement 229517. V.S. and A.O. thank Unity through Knowledge\nFund (www.ukf.hr) for collaboration support through the\n\"Homeland Visit\" grant. S.G. acknowledges support by the DFG\nCluster of Excellence \"Origin and Structure of the Universe\"\n(www.universe-cluster.de). C.C. acknowledges support from the\nMax-Planck Society and the Alexander von Humboldt Foundation\nthrough the Max-Planck-Forschungspreis 2005. G.Z.\nacknowledges support from an INAF contract PRIN-2007/\n1.06.10.08 and an ASI grant ASI/COFIS/WP3110 I/026/\n07/0.\n\nPublished - Oklopcic2010p7477Astrophys_J.pdf
", "abstract": "We present an analysis of a wide-angle tail (WAT) radio galaxy located in a galaxy group in the COSMOS field at a redshift of z = 0.53 (hereafter CWAT-02). We find that the host galaxy of CWAT-02 is the brightest galaxy in the group although it does not coincide with the center of mass of the system. Estimating (1) the velocity of CWAT-02, relative to the intra-cluster medium, and (2) the line-of-sight peculiar velocity of CWAT-02's host galaxy, relative to the average velocity of the group, we find that both values are higher than those expected for a dominant galaxy in a relaxed system. This suggests that CWAT-02's host group is dynamically young and likely in the process of an ongoing group merger. Our results are consistent with previous findings showing that the presence of a WAT galaxy in a galaxy group or cluster can be used as an indicator of dynamically young non-relaxed systems. Taking the unrelaxed state of CWAT-02's host group into account, we discuss the impact of radio-active galactic nucleus (AGN) heating from CWAT-02 onto its environment, in the context of the missing baryon problem in galaxy groups. Our analysis strengthens recent results suggesting that radio-AGN heating may be powerful enough to expel baryons from galaxy groups.", "date": "2010-04-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "713", "number": "1", "publisher": "American Astronomical Society", "pagerange": "484-490", "id_number": "CaltechAUTHORS:20100413-105827588", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100413-105827588", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech/NASA", "grant_number": "1292462" }, { "agency": "Caltech/NASA", "grant_number": "1344606" }, { "agency": "NSF", "grant_number": "AST-0838260" }, { "agency": "European Community's Seventh Framework Programme", "grant_number": "FP7/2007-2013" }, { "agency": "Unity through Knowledge Fund" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "Max-Planck Society" }, { "agency": "Alexander von Humboldt Foundation" }, { "agency": "IIstituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-2007/1.06.10.08" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110 I/026/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/713/1/484", "primary_object": { "basename": "Oklopcic2010p7477Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/3ke1y-4br69/files/Oklopcic2010p7477Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Oklop\u010di\u0107, A.; Smol\u010di\u0107, V.; et el." }, { "id": "https://authors.library.caltech.edu/records/jfc38-4ke53", "eprint_id": 17434, "eprint_status": "archive", "datestamp": "2023-08-21 23:20:16", "lastmod": "2023-10-19 23:53:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "Jeyhan S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "S." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K." }, "orcid": "0000-0001-8183-1460" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Faure-C", "name": { "family": "Faure", "given": "C." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "N." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Liu-Charles-T", "name": { "family": "Liu", "given": "C. T." }, "orcid": "0000-0002-4314-8713" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D-J", "name": { "family": "Thompson", "given": "D. J." } }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J." } } ] }, "title": "A Multiwavelength Study of a Sample of 70 \u03bcm Selected Galaxies in the COSMOS Field. I. Spectral Energy Distributions and Luminosities", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: evolution; galaxies: high-redshift; infrared: galaxies; surveys", "note": "\u00a9 2010 American Astronomical Society.\n\nPrint publication: Issue 2 (2010 February 1); received 2009 July 14; accepted for publication 2009 November 25; published 2010 January 6.\n\nSupport for this work was provided in part by NASA\nthrough contracts 1282612, 1298213, and 1344920 issued\nby the Jet Propulsion Laboratory. We would also like to\nrecognize the contributions from all of the members of the\nCOSMOS Team who helped in obtaining and reducing the\nlarge amount of multiwavelength data that are now publicly\navailable through theNASA Infrared Science Archive (IRSA) at\nhttp://irsa.ipac.caltech.edu/Missions/cosmos.html. The analysis\npipeline used to reduce the DEIMOS data was developed at\nUC Berkeley with support from NSF grant AST-0071048.\nThis research has made use of the NASA/IPAC Extragalactic\nDatabase (NED), which is operated by the Jet Propulsion\nLaboratory, California Institute of Technology, under contract\nwith the National Aeronautics and Space Administration. This\nresearch has also made use of data from the Sloan Digital\nSky Survey (SDSS-DR7). Funding for the SDSS and SDSSII\nhas been provided by the Alfred P. Sloan Foundation, the\nParticipating Institutions, the National Science Foundation, the\nU.S. Department of Energy, the National Aeronautics and Space\nAdministration, the JapaneseMonbukagakusho, theMax Planck\nSociety, and theHigher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/.\n\nPublished - Kartaltepe2010p6998Astrophys_J.pdf
", "abstract": "We present a large robust sample of 1503 reliable and unconfused 70 \u03bcm selected sources from the multiwavelength data set of the Cosmic Evolution Survey. Using the Spitzer IRAC and MIPS photometry, we estimate the total infrared (IR) luminosity, L_(IR) (8-1000 \u03bcm), by finding the best-fit template from several different template libraries. The long-wavelength 70 and 160 \u03bcm data allow us to obtain a reliable estimate of L_(IR), accurate to within 0.2 and 0.05 dex, respectively. The 70 \u03bcm data point enables a significant improvement over the luminosity estimates possible with only a 24 \u03bcm detection. The full sample spans a wide range in IR luminosity, L_(IR) \u2248 10^8-10^(14) L_\u2609, with a median luminosity of 10^(11.4) L_\u2609. We identify a total of 687 luminous, 303 ultraluminous, and 31 hyperluminous infrared galaxies (LIRGs, ULIRGs, and HyLIRGs) over the redshift range 0.01 < z < 3.5 with a median redshift of 0.5. Presented here are the full spectral energy distributions (SEDs) for each of the sources compiled from the extensive multiwavelength data set from the ultraviolet (UV) to the far-infrared. A catalog of the general properties of the sample (including the photometry, redshifts, and L_(IR)) is included with this paper. We find that the overall shape of the SED and trends with L_(IR) (e.g., IR color temperatures and optical-IR ratios) are similar to what has been seen in studies of local objects; however, our large sample allows us to see the extreme spread in UV to near-infrared colors spanning nearly 3 orders of magnitude. In addition, using SED fits we find possible evidence for a subset of cooler ultraluminous objects than observed locally. However, until direct observations at longer wavelengths are obtained, the peak of emission and the dust temperature cannot be well constrained. We use these SEDs, along with the deep radio and X-ray coverage of the field, to identify a large sample of candidate active galactic nuclei (AGNs). We find that the fraction of AGNs increases strongly with L_(IR), as it does in the local universe, and that nearly 70% of ULIRGs and all HyLIRGs likely host a powerful AGN.", "date": "2010-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "709", "number": "2", "publisher": "American Astronomical Society", "pagerange": "572-596", "id_number": "CaltechAUTHORS:20100209-115624086", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100209-115624086", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL", "grant_number": "1282612" }, { "agency": "NASA/JPL", "grant_number": "1298213" }, { "agency": "NASA/JPL", "grant_number": "1344920" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/709/2/572", "primary_object": { "basename": "Kartaltepe2010p6998Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/jfc38-4ke53/files/Kartaltepe2010p6998Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Kartaltepe, Jeyhan S.; Sanders, D. B.; et el." }, { "id": "https://authors.library.caltech.edu/records/he7p4-85172", "eprint_id": 17436, "eprint_status": "archive", "datestamp": "2023-08-21 23:20:21", "lastmod": "2023-10-19 23:53:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "S." } }, { "id": "Bundy-K-A", "name": { "family": "Bundy", "given": "K." }, "orcid": "0000-0001-9742-3138" }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Zamojski-M-A", "name": { "family": "Zamojski", "given": "M." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } } ] }, "title": "Galaxy Stellar Mass Assembly Between 0.2 < z < 2 from the S-COSMOS Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: luminosity function, mass function", "note": "\u00a9 2010 American Astronomical Society.\n\nPrint publication: Issue 2 (2010 February 1); received 2009 January 6; accepted for publication 2009 December 4;\npublished 2010 January 6.\n\nWe are grateful to the referee for his/her careful reading of\nthe manuscript and his/her useful suggestions.\nThis work is based on observations made with the Spitzer\nSpace Telescope, which is operated by the Jet Propulsion Laboratory,\nCalifornia Institute of Technology under NASA contract\n1407. Support for this work was provided by NASA through\nContract Number 1278386 issued by JPL. We gratefully acknowledge\nthe contributions of the entire COSMOS collaboration\nconsisting of more than 100 scientists. The HST COSMOS\nprogram was supported through NASA grant HST-GO-\n09822. More information on the COSMOS survey is available\nat http://www.astro.caltech.edu/cosmos.\n\nPublished - Ilbert2010p7000Astrophys_J.pdf
", "abstract": "We follow the galaxy stellar mass assembly by morphological and spectral type in the COSMOS 2 deg^2 field. We derive the stellar mass functions and stellar mass densities from z = 2 to z = 0.2 using 196,000 galaxies selected at F_(3.6 \u03bcm) > 1 \u03bcJy with accurate photometric redshifts (\u03c3_[(zphot\u2212zspec)]/(1+zspec) = 0.008 at i^+ < 22.5). Using a spectral classification, we find that z ~ 1 is an epoch of transition in the stellar mass assembly of quiescent galaxies. Their stellar mass density increases by 1.1 dex between z = 1.5-2 and z = 0.8-1 (\u0394t ~ 2.5 Gyr), but only by 0.3 dex between z = 0.8-1 and z ~ 0.1 (\u0394t ~ 6 Gyr). Then, we add the morphological information and find that 80%-90% of the massive quiescent galaxies (logM ~ 11) have an elliptical morphology at z < 0.8. Therefore, a dominant mechanism links the shutdown of star formation and the acquisition of an elliptical morphology in massive galaxies. Still, a significant fraction of quiescent galaxies present a Spi/Irr morphology at low mass (40%-60% at logM ~ 9.5), but this fraction is smaller than predicted by semi-analytical models using a \"halo quenching\" recipe. We also analyze the evolution of star-forming galaxies and split them into \"intermediate activity\" and \"high activity\" galaxies. We find that the most massive \"high activity\" galaxies end their high star formation rate phase first. Finally, the space density of massive star-forming galaxies becomes lower than the space density of massive elliptical galaxies at z < 1. As a consequence, the rate of \"wet mergers\" involved in the formation of the most massive ellipticals must decline very rapidly at z < 1, which could explain the observed slow down in the assembly of these quiescent and massive sources.", "date": "2010-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "709", "number": "2", "publisher": "American Astronomical Society", "pagerange": "644-663", "id_number": "CaltechAUTHORS:20100209-115745637", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100209-115745637", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL", "grant_number": "1278386" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/709/2/644", "primary_object": { "basename": "Ilbert2010p7000Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/he7p4-85172/files/Ilbert2010p7000Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Ilbert, O.; Salvato, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/hcadr-3gg75", "eprint_id": 18009, "eprint_status": "archive", "datestamp": "2023-08-19 01:34:09", "lastmod": "2023-10-20 15:30:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Lanzuisi-G", "name": { "family": "Lanzuisi", "given": "G." }, "orcid": "0000-0001-9094-0984" }, { "id": "Miyaji-Takamitsu", "name": { "family": "Miyaji", "given": "T." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J. P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K." }, "orcid": "0000-0001-8183-1460" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de-Ravel", "given": "L." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Halliday-C", "name": { "family": "Halliday", "given": "C." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J.-F." } }, { "id": "Le-Brun-V", "name": { "family": "Le-Brun", "given": "V." } }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Merloni-A", "name": { "family": "Merloni", "given": "A." } }, { "id": "Nair-P-M", "name": { "family": "Nair", "given": "P." } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "P\u00e9rez-Montero-E", "name": { "family": "P\u00e9rez-Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } }, { "id": "Abbas-U", "name": { "family": "Abbas", "given": "U." } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "D." } }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "A." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Maccagni-D", "name": { "family": "Maccagni", "given": "D." } }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Memeo-P", "name": { "family": "Memeo", "given": "P." } }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "B." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "L." } }, { "id": "Scaramella-R", "name": { "family": "Scaramella", "given": "R." } } ] }, "title": "The [O III] emission line luminosity function of optically selected type-2 AGN from zCOSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys galaxies: active", "note": "\u00a9 ESO 2010. Received 2 September 2009. Accepted 17 November 2009. A.B. wishes to thank the referee for the useful suggestions\nthat significantly improved the manuscript. A.B. also thank H. Netzer for the\nthe stimulating discussion, R. Fassbender for helping to improve the manuscript\nand S. Savaglio for sharing the expertise. This work is based on the zCOSMOS\nESO Large Program Number 175.A-0839 and was supported by an INAF contract\nPRIN/2007/1.06.10.08, and an ASI grant ASI/COFIS/WP3110 I/026/07/0,\nPartial support of this work is provided by NASA ADP NNX07AT02G,\nCONACyT 83564, and PAPIITIN110209. These results are also based in part\non observations obtained with XMM-Newton, an ESA Science Mission with instruments\nand contributions directly funded by ESA Member States and the USA\n(NASA).\n\nPublished - Bongiorno2010p7476Astron_Astrophys.pdf
", "abstract": "Aims. We present a catalog of 213 type-2 AGN selected from the zCOSMOS survey. The selected sample covers a wide redshift range (0.15 <\nz < 0.92) and is deeper than any other previous study, encompassing the luminosity range 10^(5.5) L_\u2609 < L_([O III]) < 10^(9.1) L_\u2609. We explore the intrinsic\nproperties of these AGN and the relation to their X-ray emission (derived from the XMM-COSMOS observations). We study their evolution\nby computing the [O III]\u03bb5007 \u00c5 line luminosity function (LF) and we constrain the fraction of obscured AGN as a function of luminosity and\nredshift.\nMethods. The sample was selected on the basis of the optical emission line ratios, after applying a cut to the signal-to-noise ratio (S/N) of the\nrelevant lines.We used the standard diagnostic diagrams ([O III]/H\u03b2 versus [N II]/H\u03b1 and [O III]/H\u03b2 versus [S II]/H\u03b1) to isolate AGN in the redshift\nrange 0.15 < z < 0.45 and the diagnostic diagram [O III]/H\u03b2 versus [O II]/H\u03b2 to extend the selection to higher redshift (0.5 < z < 0.92).\nResults. Combining our sample with one drawn from SDSS, we found that the best description of the evolution of type-2 AGN is a luminosity-dependent\ndensity evolution model. Moreover, using the type-1 AGN LF we were able to constrain the fraction of type-2 AGN to the total\n(type-1 + type-2) AGN population. We found that the type-2 fraction decreases with luminosity, in agreement with the most recent results, and\nshows signs of a slight increase with redshift. However, the trend with luminosity is visible only after combining the SDSS+zCOSMOS samples.\nFrom the COSMOS data points alone, the type-2 fraction seems to be quite constant with luminosity.", "date": "2010-02", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "510", "publisher": "EDP Sciences", "pagerange": "Art. No. A56", "id_number": "CaltechAUTHORS:20100416-154341585", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100416-154341585", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN/2007/1.06.10.08" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110 I/026/07/0" }, { "agency": "NASA", "grant_number": "NNX07AT02G" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "83564" }, { "agency": "Direcci\u00f3n General Asuntos del Personal (DGAPA)", "grant_number": "PAPIIT IN 110209" }, { "agency": "ESA Member States" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/200913229", "primary_object": { "basename": "Bongiorno2010p7476Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/hcadr-3gg75/files/Bongiorno2010p7476Astron_Astrophys.pdf" }, "pub_year": "2010", "author_list": "Bongiorno, A.; Mignoli, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/y1tdr-t5b04", "eprint_id": 18002, "eprint_status": "archive", "datestamp": "2023-08-19 01:33:58", "lastmod": "2023-10-20 15:30:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Halliday-C", "name": { "family": "Halliday", "given": "C." } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Ciliegi-P", "name": { "family": "Ciliegi", "given": "P." } }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K." }, "orcid": "0000-0001-8183-1460" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Bondi-M", "name": { "family": "Bondi", "given": "M." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "L." } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de-Ravel", "given": "L." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J.-F." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "P\u00e9rez-Montero-E", "name": { "family": "P\u00e9rez-Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Abbas-U", "name": { "family": "Abbas", "given": "U." } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "D." } }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "A." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Maccagni-D", "name": { "family": "Maccagni", "given": "D." } }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Memeo-P", "name": { "family": "Memeo", "given": "P." } }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "B." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Scaramella-R", "name": { "family": "Scaramella", "given": "R." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "K." }, "orcid": "0000-0003-3804-2137" } ] }, "title": "Properties and environment of radio-emitting galaxies in the VLA-zCOSMOS survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: fundamental parameters galaxies: general galaxies: luminosity function, mass function radio continuum: galaxies radio continuum: planetary systems", "note": "\u00a9 ESO 2010. Received 1 July 2009. Accepted 22 October 2009.\nWe acknowledge support from an INAF contract PRIN-\n2007/1.06.10.08 and an ASI grant ASI/COFIS/WP3110 I/026/07/0.The VLA\nis operated by the National Radio Astronomy Observatory, which is a facility\nof the National Science Foundation, operated under cooperative agreement by\nAssociated Universities, IIlC.\n\nPublished - Bardelli2010p7473Astron_Astrophys.pdf
", "abstract": "Aims. We investigate the properties and the environment of radio sources with optical counterparts from the combined VLA-COSMOS and\nzCOSMOS samples. The advantage of this sample is the availability of optical spectroscopic informations, high quality redshifts, and accurate\ndensity determination.\nMethods. By comparing the star formation rates estimated from the optical spectral energy distribution with those based on the radio luminosity,\nwe divide the radio sources in to three families passive AGN, non-passive AGN, and star-forming galaxies. These families occupy specific regions\nof the 8.0\u22124.5 \u03bcm infrared color- specific star-formation plane, from which we extract the corresponding control samples.\nResults. Only the passive AGN have a significantly different environmental distribution from their control sample. The fraction of radio-loud\npassive AGN increases from ~2% in underdense regions to ~15% for overdensities (1 + \u03b4) greater than 10. This trend is also present as a function\nof richness of the groups hosting the radio sources. Passive AGN in overdensities tend to have higher radio luminosities than those in lower density\nenvironments. Since the black hole mass distribution is similar in both environments, we speculate that, for low radio luminosities, the radio\nemission is controlled (by fuel availability or confinement of the radio jet by local gas pressure) by the interstellar medium of the host galaxy,\nwhile in other cases it is determined by the structure (group or cluster) in which the galaxy resides.", "date": "2010-02", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "511", "publisher": "EDP Sciences", "pagerange": "Art. No. A1", "id_number": "CaltechAUTHORS:20100416-132658729", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100416-132658729", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-2007/1.06.10.08" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110 I/026/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/200912809", "primary_object": { "basename": "Bardelli2010p7473Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/y1tdr-t5b04/files/Bardelli2010p7473Astron_Astrophys.pdf" }, "pub_year": "2010", "author_list": "Bardelli, S.; Schinnerer, E.; et el." }, { "id": "https://authors.library.caltech.edu/records/s813n-xzt61", "eprint_id": 17592, "eprint_status": "archive", "datestamp": "2023-08-21 23:17:47", "lastmod": "2023-10-20 00:02:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M. T." }, "orcid": "0000-0003-1033-9684" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E." }, "orcid": "0000-0001-7089-7325" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Mart\u00ednez-Sansigre-A", "name": { "family": "Mart\u00ednez-Sansigre", "given": "A." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "N." } }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The VLA-COSMOS Perspective on the Infrared-Radio Relation. I. New Constraints on Selection Biases and the Non-Evolution of the Infrared/Radio Properties of Star-Forming and Active Galactic Nucleus Galaxies at Intermediate and High Redshift", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: evolution; galaxies: high-redshift; infrared: galaxies; radio continuum: galaxies; surveys", "note": "\u00a9 2010 American Astronomical Society.\n\nPrint publication: Issue 2 (2010 February); received 2009 September 30; accepted for publication 2010 January 8;\npublished 2010 January 28.\n\nWe gratefully acknowledge the contribution of the whole\nCOSMOS collaboration and its more than 100 scientists around\nthe globe. M.T.S. thanks Ute Lisenfeld, Chris Carilli, and George\nHelou for useful discussions, as well as Marco Scodeggio for\ncomments on the manuscript. The German DFG supported\nthis research with grant SCHI 536/3-2. G.Z. acknowledges\npartial support from an INAF contract (PRIN-2007/1.06.10.08)\nand an ASI grant (ASI/COFIS/WP3110 I/026/07/0). This\nwork is partly based on observations made with the Spitzer\nSpace Telescope, which is operated by NASA/JPL/Caltech.\nThe National Radio Astronomy Observatory is a facility of\nthe National Science Foundation operated under cooperative\nagreement by Associated Universities, Inc.\n\nPublished - Sargent2010p7138Astrophys_J_Suppl_S.pdf
", "abstract": "VLA 1.4 GHz (\u03c3 ~ 0.012 mJy) and MIPS 24 and 70 \u03bcm (\u03c3 ~ 0.02 and 1.7 mJy, respectively) observations covering the 2 deg^2 COSMOS field are combined with an extensive multiwavelength data set to study the evolution of the infrared (IR)-radio relation at intermediate and high redshift. With ~4500 sources\u2014of which ~30% have spectroscopic redshifts\u2014the current sample is significantly larger than previous ones used for the same purpose. Both monochromatic IR/radio flux ratios (q_(24) and q_(70)), as well as the ratio of the total IR and the 1.4 GHz luminosity (q_(TIR)), are used as indicators for the IR/radio properties of star-forming galaxies and active galactic nuclei (AGNs). Using a sample jointly selected at IR and radio wavelengths in order to reduce selection biases, we provide firm support for previous findings that the IR-radio relation remains unchanged out to at least z ~ 1.4. Moreover, based on data from ~150 objects we also find that the local relation likely still holds at z \u2208 [2.5, 5]. At redshift z < 1.4, we observe that radio-quiet AGNs populate the locus of the IR-radio relation in similar numbers as star-forming sources. In our analysis, we employ the methods of survival analysis in order to ensure a statistically sound treatment of flux limits arising from non-detections. We determine the observed shift in average IR/radio properties of IR- and radio-selected populations and show that it can reconcile apparently discrepant measurements presented in the literature. Finally, we also investigate variations of the IR/radio ratio with IR and radio luminosity and find that it hardly varies with IR luminosity but is a decreasing function of radio luminosity.", "date": "2010-02", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "186", "number": "2", "publisher": "American Astronomical Society", "pagerange": "341-377", "id_number": "CaltechAUTHORS:20100225-094258015", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100225-094258015", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "SCHI 536/3-2" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-2007/1.06.10.08" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110 I/026/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0067-0049/186/2/341", "primary_object": { "basename": "Sargent2010p7138Astrophys_J_Suppl_S.pdf", "url": "https://authors.library.caltech.edu/records/s813n-xzt61/files/Sargent2010p7138Astrophys_J_Suppl_S.pdf" }, "pub_year": "2010", "author_list": "Sargent, M. T.; Schinnerer, E.; et el." }, { "id": "https://authors.library.caltech.edu/records/nextf-g8b20", "eprint_id": 17361, "eprint_status": "archive", "datestamp": "2023-08-21 23:15:35", "lastmod": "2023-10-19 23:49:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexei" }, "orcid": "0000-0002-3677-3617" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "Alexis" }, "orcid": "0000-0002-4606-5403" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "Jean-Paul" }, "orcid": "0000-0002-4616-4989" }, { "id": "Taylor-J-E", "name": { "family": "Taylor", "given": "James E." } }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "Richard" }, "orcid": "0000-0002-6085-3780" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Bundy-K-A", "name": { "family": "Bundy", "given": "Kevin" }, "orcid": "0000-0001-9742-3138" }, { "id": "Tinker-J-L", "name": { "family": "Tinker", "given": "Jeremy" } }, { "id": "George-M-R", "name": { "family": "George", "given": "Matthew R." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Johnston-D-E", "name": { "family": "Johnston", "given": "David E." } }, { "id": "Zhang-Yu-Ying", "name": { "family": "Zhang", "given": "Yu-Ying" } }, { "id": "Cappelluti-N", "name": { "family": "Cappelutti", "given": "Nico" } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "id": "Giodini-S", "name": { "family": "Giodini", "given": "Stefania" } }, { "id": "Heymans-C", "name": { "family": "Heymans", "given": "Catherine" } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "Olivier" }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "Simon" }, "orcid": "0000-0002-6423-3597" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "Henry J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mellier-Y", "name": { "family": "Mellier", "given": "Yannick" } }, { "id": "R\u00e9fr\u00e9gier-A", "name": { "family": "R\u00e9fr\u00e9gier", "given": "Alexandre" } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Smoot-George-F", "name": { "family": "Smoot", "given": "George" } }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "Masayuki" }, "orcid": "0000-0002-5011-5178" }, { "id": "Van-Waerbeke-L", "name": { "family": "Van Waerbeke", "given": "Ludovic" } }, { "id": "Wolk-M", "name": { "family": "Wolk", "given": "Melody" } } ] }, "title": "A Weak Lensing Study of X-ray Groups in the Cosmos Survey: Form and Evolution of the Mass-Luminosity Relation", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; gravitational lensing; large-scale structure of universe", "note": "\u00a9 2010 American Astronomical Society.\n\nPrint publication: Issue 1 (2010 January 20); received 2009 May 9; accepted for publication 2009 November 12; published 2009 December 29.\n\nWe thank Uros Seljak, Reiko Nakajima, Henk Hoekstra,\nRachel Mandelbaum, Chris Hirata, Masahiro Takada, and\nSatoshi Miyazaki for useful discussions. We thank Florian\nPacaud for providing X-ray data for this analysis. We are\nalso grateful to Eduardo Rozo and to Joel Berg\u00b4e for providing\ncomments on the manuscript and to an anonymous referee\nfor insightful comments. A.L. acknowledges support from the\nChamberlain Fellowship at LBNL and from the Berkeley Center\nfor Cosmological Physics. J.P.K. acknowledges CNRS and\nCNES for support. J.P.K. and H.J.M.C.C. acknowledge support\nfrom the research grant ANR-07-BLAN-0228. The HST\nCOSMOS Treasury program was supported through NASA\ngrant HST-GO-09822. We thank Tony Roman, Denise Taylor,\nand David Soderblom for their assistance in planning and\nscheduling of the extensive COSMOS observations. We gratefully\nacknowledge the contributions of the entire COSMOS\ncollaboration consisting of more than 70 scientists. More\ninformation on the COSMOS survey is available at\nhttp://cosmos.astro.caltech.edu/. It is a pleasure to acknowledge\nthe excellent services provided by the NASA IPAC/IRSA staff\n(Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John\nGood) in providing online archive and server capabilities for the\nCOSMOS data sets.\n\nPublished - Leauthaud2010p6900Astrophys_J.pdf
", "abstract": "Measurements of X-ray scaling laws are critical for improving cosmological constraints derived with the halo mass function and for understanding the physical processes that govern the heating and cooling of the intracluster medium. In this paper, we use a sample of 206 X-ray-selected galaxy groups to investigate the scaling relation between X-ray luminosity (L_X) and halo mass (M_(200)) where M_(200) is derived via stacked weak gravitational lensing. This work draws upon a broad array of multi-wavelength COSMOS observations including 1.64 degrees^2 of contiguous imaging with the Advanced Camera for Surveys to a limiting magnitude of I_(F814W) = 26.5 and deep XMM-Newton/Chandra imaging to a limiting flux of 1.0 \u00d7 10^(\u201315) erg cm6(\u20132) s^(\u20131) in the 0.5-2 keV band. The combined depth of these two data sets allows us to probe the lensing signals of X-ray-detected structures at both higher redshifts and lower masses than previously explored. Weak lensing profiles and halo masses are derived for nine sub-samples, narrowly binned in luminosity and redshift. The COSMOS data alone are well fit by a power law, M_(200) (L_X)^\u03b1, with a slope of \u03b1 = 0.66 \u00b1 0.14. These results significantly extend the dynamic range for which the halo masses of X-ray-selected structures have been measured with weak gravitational lensing. As a result, tight constraints are obtained for the slope of the M-L_X relation. The combination of our group data with previously published cluster data demonstrates that the M-L_X relation is well described by a single power law, \u03b1 = 0.64 \u00b1 0.03, over two decades in mass, M_(200) ~ 10^(13.5)-10^(15.5) h^(\u20131)_72 M_\u2609. These results are inconsistent at the 3.7\u03c3 level with the self-similar prediction of \u03b1 = 0.75. We examine the redshift dependence of the M-L_X relation and find little evidence for evolution beyond the rate predicted by self-similarity from z ~ 0.25 to z ~ 0.", "date": "2010-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "709", "number": "1", "publisher": "American Astronomical Society", "pagerange": "97-114", "id_number": "CaltechAUTHORS:20100201-100414082", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100201-100414082", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Chamberlain Fellowship" }, { "agency": "Berkeley Center for Cosmological Physics" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)", "grant_number": "ANR-07-BLAN-0228" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/709/1/97", "primary_object": { "basename": "Leauthaud2010p6900Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/nextf-g8b20/files/Leauthaud2010p6900Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Leauthaud, Alexei; Finoguenov, Alexis; et el." }, { "id": "https://authors.library.caltech.edu/records/1mpnp-esk91", "eprint_id": 17423, "eprint_status": "archive", "datestamp": "2023-08-21 23:13:39", "lastmod": "2023-10-19 23:52:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mancini-C", "name": { "family": "Mancini", "given": "C." }, "orcid": "0000-0002-4297-0561" }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Salmi-F", "name": { "family": "Salmi", "given": "F." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Onodera-Masato", "name": { "family": "Onodera", "given": "M." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Willott-C-J", "name": { "family": "Willott", "given": "C." }, "orcid": "0000-0002-4201-7367" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "High-redshift elliptical galaxies: are they (all) really compact?", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: elliptical and lenticular, cD; galaxies: high-redshift", "note": "\u00a9 2009 The Authors. Journal compilation \u00a9 2009 RAS.\nAccepted 2009 September 16; received 2009 September 7; in original form 2009 July 10.\n\nWe wish to thank Swara Ravindranath and Paolo Cassata for\nuseful discussions. This work has been supported by grants\nASI/COFIS/WP3110+WP3400 I/026/07/0. CM, ED, FS, HJM and\nMO acknowledge funding support of French ANR under contracts\nANR-07-BLAN-0228 and ANR-08-JCJC-0008, and CM thanks\nCEA Saclay for hospitality and funding at the beginning of this\nwork.\n\nPublished - Mancini2010p6981Mon_Not_R_Astron_Soc.pdf
", "abstract": "We investigate the properties of 12 ultramassive passively evolving early-type galaxies (ETGs) at z_(phot) > 1.4 in the COSMOS 2 deg^2 field. These 12 ETGs were selected as pBzKs, have accurate 1.4 \u2272 z_(phot) \u2272 1.7, high S\u00e9rsic index profiles typical of ellipticals, no detection at 24 \u03bcm, resulting in a complete ETG sample at M* > 2.5 \u00d7 10^(11) M_\u2299 (Chabrier initial mass function). Contrary to the previous claims, the half-light radii estimated in very high signal-to-noise ratio imaging data from Hubble Space Telescope+Advanced Camera for Surveys (ACS) are found to be large for most of the sample, consistent with local ellipticals. If the high-redshift ETGs with M* < 2.5 \u00d7 10^(11) M_\u2299 are really small in size and compact as reported in the previous studies, our result may suggest a 'downsizing' scenario, whereby the most massive ETGs reach their final structure earlier and faster than the lower mass ones. However, simulating galaxies with morphological properties fixed to those of local ETGs with the same stellar mass show that the few compact galaxies that we still recover in our sample can be understood in terms of fluctuations due to noise preventing the recovery of the extended low surface brightness haloes in the light profile. Such haloes, typical of S\u00e9rsic profiles, extending even up to 40 kpc, are indeed seen in our sample.", "date": "2010-01-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "401", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "933-940", "id_number": "CaltechAUTHORS:20100208-152305495", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100208-152305495", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "WP3110+WP3400 I/026/07/0" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-07-BLAN-0228" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-08-JCJC-0008" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2009.15728.x", "primary_object": { "basename": "Mancini2010p6981Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/1mpnp-esk91/files/Mancini2010p6981Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2010", "author_list": "Mancini, C.; Daddi, E.; et el." }, { "id": "https://authors.library.caltech.edu/records/cc0nd-05n57", "eprint_id": 17258, "eprint_status": "archive", "datestamp": "2023-08-21 23:12:03", "lastmod": "2023-10-19 23:42:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Merloni-A", "name": { "family": "Merloni", "given": "A." } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Fiore-F", "name": { "family": "Fiore", "given": "F." } }, { "id": "Gilli-R", "name": { "family": "Gilli", "given": "R." } }, { "id": "Hao-Heng", "name": { "family": "Hao", "given": "H." } }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "K." }, "orcid": "0000-0003-3804-2137" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Lusso-E", "name": { "family": "Lusso", "given": "E." }, "orcid": "0000-0003-0083-1157" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Miyaji-Takamitsu", "name": { "family": "Miyaji", "given": "T." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J." } }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "C." }, "orcid": "0000-0002-8853-9611" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K." }, "orcid": "0000-0001-8183-1460" }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Iwasawa-Kazushi", "name": { "family": "Iwasawa", "given": "K." }, "orcid": "0000-0002-4923-3281" }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J.-F." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "Perez-Montero-E", "name": { "family": "Perez Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L. A. M." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } } ] }, "title": "On the Cosmic Evolution of the Scaling Relations Between Black Holes and Their Host Galaxies: Broad-Line Active Galactic Nuclei in the zCOSMOS Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: evolution; quasars: emission lines", "note": "\u00a9 2010 American Astronomical Society. \n\nPrint publication: Issue 1 (2010 January 1); received 2009 July 14; accepted for publication 2009 October 30; published 2009 December 9. \n\nThis research was supported by the DFG cluster of excellence \"Origin and Structure of the Universe.\" We thank the anonymous referee for carefully reading the manuscript and providing us with insightful and constructive remarks. We also thank R. Decarli, F. Fontanot, O. Gerhard, J. Greiner, P. Hopkins, S. Komossa, N. Menci, P. Monaco, H. Netzer, R. Saglia, L. Wisotzki, J.-H. Woo for their useful comments and\nsuggestions. The HST COSMOS Treasury program was supported\nthrough NASA grant HST-GO-09822. We thank Tony\nRoman, Denise Taylor, and David Soderblom for their assistance\nin planning and scheduling of the extensive COSMOS observations.\nWe gratefully acknowledge the contributions of the\nentire COSMOS collaboration consisting of more than 80 scientists.\nMore information on the COSMOS survey is available\nat http://www.astro.caltech.edu/\u223ccosmos. It is a pleasure to acknowledge\nthe excellent services provided by the NASA IPAC/\nIRSA staff (Anastasia Laity,AnastasiaAlexov, Bruce Berriman,\nand John Good) in providing online archive and server capabilities\nfor the COSMOS data sets. In Italy, this work was partly\nsupported by an INAF contract PRIN/2007/1.06.10.08 and an\nASI grant ASI/COFIS/WP3110 I/026/07/0; in Mexico by the\nCONACyT grant program 83564 and PAPIIT IN110209; in\nGermany by the Bundesministerium f\u00fcr Bildung und\nForschung/Deutsches Zentrumf\u00fcr Luft und Raumfahrt and the\nMax Planck Society.\n\nPublished - Merloni2010p6742Astrophys_J.pdf
", "abstract": "We report on the measurement of the physical properties (rest-frame K-band luminosity and total stellar mass) of the hosts of 89 broad-line (type-1) active galactic nuclei (AGNs) detected in the zCOSMOS survey in the redshift range 1 < z < 2.2. The unprecedented multi-wavelength coverage of the survey field allows us to disentangle the emission of the host galaxy from that of the nuclear black hole in their spectral energy distributions (SEDs). We derive an estimate of black hole masses through the analysis of the broad Mg II emission lines observed in the medium-resolution spectra taken with VIMOS/VLT as part of the zCOSMOS project. We found that, as compared to the local value, the average black hole to host-galaxy mass ratio appears to evolve positively with redshift, with a best-fit evolution of the form (1 + z)^[(0.68\u00b10.12)^(+0.6)_(-0.3)], where the large asymmetric systematic errors stem from the uncertainties in the choice of initial mass function, in the calibration of the virial relation used to estimate BH masses and in the mean QSO SED adopted. On the other hand, if we consider the observed rest-frame K-band luminosity, objects tend to be brighter, for a given black hole mass, than those on the local M_(BH)-M_K relation. This fact, together with more indirect evidence from the SED fitting itself, suggests that the AGN hosts are likely actively star-forming galaxies. A thorough analysis of observational biases induced by intrinsic scatter in the scaling relations reinforces the conclusion that an evolution of the M_(BH)-M_* relation must ensue for actively growing black holes at early times: either its overall normalization, or its intrinsic scatter (or both) appear to increase with redshift. This can be interpreted as signature of either a more rapid growth of supermassive black holes at high redshift, a change of structural properties of AGN hosts at earlier times, or a significant mismatch between the typical growth times of nuclear black holes and host galaxies. In any case, our results provide important clues on the nature of the early co-evolution of black holes and galaxies and challenging tests for models of AGN feedback and self-regulated growth of structures.", "date": "2010-01-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "708", "number": "1", "publisher": "American Astronomical Society", "pagerange": "137-157", "id_number": "CaltechAUTHORS:20100121-092925225", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100121-092925225", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN/2007/1.06.10.08" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110 I/026/07/0" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "83564" }, { "agency": "Programa de Apoyo a Proyectos de Investigaci\u00f3n e Innovaci\u00f3n (PAPIIT)", "grant_number": "IN110209" }, { "agency": "Bundesministerium f\u00fcr Bildung und Forschung (BMBF)" }, { "agency": "Max Planck Society" }, { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/708/1/137", "primary_object": { "basename": "Merloni2010p6742Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/cc0nd-05n57/files/Merloni2010p6742Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Merloni, A.; Bongiorno, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/5r69p-k0915", "eprint_id": 17333, "eprint_status": "archive", "datestamp": "2023-08-21 23:12:26", "lastmod": "2023-10-19 23:46:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Menten-K-M", "name": { "family": "Menten", "given": "K. M." }, "orcid": "0000-0001-6459-0669" } ] }, "title": "Environment of MAMBO Galaxies in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general; galaxies: evolution; galaxies: high-redshift; galaxies: starburst", "note": "\u00a9 2010 The American Astronomical Society. \n\nReceived 2009 July 27; accepted 2009 November 20; published 2009 December 16. \n\nM. Aravena was partly supported for this research through a stipend from the International Max-Planck Research School (IMPRS) for Radio and Infrared Astronomy at the Universities of Bonn and Cologne. D. Riechers acknowledges support from NASA through Hubble Fellowship grant HST-HF-01212.01A awarded by the STScI, operated by AURA, under contract NAS 5-26555.\n\nPublished - Aravena2010p6914Astrophys_J_Lett.pdf
", "abstract": "Submillimeter galaxies (SMGs) represent a dust-obscured high-redshift population undergoing massive star formation activity. Their properties and space density have suggested that they may evolve into spheroidal galaxies residing in galaxy clusters. In this Letter, we report the discovery of compact (~10\"-20\") galaxy overdensities centered at the position of three SMGs detected with the Max-Planck millimeter bolometer camera in the COSMOS field. These associations are statistically significant. The photometric redshifts of galaxies in these structures are consistent with their associated SMGs; all of them are between z = 1.4 and 2.5, implying projected physical sizes of ~170 kpc for the overdensities. Our results suggest that about 30% of the radio-identified bright SMGs in that redshift range form in galaxy density peaks in the crucial epoch when most stars formed.", "date": "2010-01-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "708", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L36-L41", "id_number": "CaltechAUTHORS:20100128-093632293", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100128-093632293", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "International Max-Planck Research School (IMPRS)" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-01212.01A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/2041-8205/708/1/L36", "primary_object": { "basename": "Aravena2010p6914Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/5r69p-k0915/files/Aravena2010p6914Astrophys_J_Lett.pdf" }, "pub_year": "2010", "author_list": "Aravena, M.; Bertoldi, F.; et el." }, { "id": "https://authors.library.caltech.edu/records/21667-e3531", "eprint_id": 17259, "eprint_status": "archive", "datestamp": "2023-08-21 23:12:09", "lastmod": "2023-10-19 23:42:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Willott-C-J", "name": { "family": "Willott", "given": "C. J." }, "orcid": "0000-0002-4201-7367" }, { "id": "Mancini-C", "name": { "family": "Mancini", "given": "C." }, "orcid": "0000-0002-4297-0561" }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Cook-R-R", "name": { "family": "Cook", "given": "R." } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Mellier-Y", "name": { "family": "Mellier", "given": "Y." } }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Tanaguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" } ] }, "title": "The COSMOS-WIRCam Near-Infrared Imaging Survey. I. BzK-Selected Passive and Star-Forming Galaxy Candidates at z \u2273 1.4", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; dark matter; galaxies: evolution; galaxies: formation; large-scale structure of universe; surveys", "note": "\u00a9 2010 American Astronomical Society.\n\nPrint publication: Issue 1 (2010 January 1); received 2009 March 6; accepted for publication 2009 November 9;\npublished 2009 December 9.\n\nThis work is based in part on data products produced at\nTERAPIX at the Institut d'Astrophysique de Paris. H.J.McC.\nacknowledges the use of TERAPIX computing facilities and the\nhospitality of the IfA, Honolulu, where this paper was finished.\nM. Kilbinger is acknowledged for help with dark matter models\nin Section 6 and N.V. Asari for the stacking analysis in Section 4.\nThis research has made use of the VizieR catalog access tool\nprovided by the CDS, Strasbourg, France. This research was\nsupported by ANR grant \"ANR-07-BLAN-0228.\" E.D. and\nC.M. also acknowledge support from \"ANR-08-JCJC-0008.\"\nJ.P.K. acknowledges support from the CNRS. We thank the\nreferee for an extensive commentary on a earlier version of this\npaper.\n\nPublished - McCracken2010p6752Astrophys_J.pdf
", "abstract": "We present a new near-infrared survey covering the 2 deg^2 COSMOS field conducted using WIRCam at the Canada-France-Hawaii Telescope. By combining our near-infrared data with Subaru B and z images, we construct a deep, wide-field optical-infrared catalog. At K_s < 23 (AB magnitudes), our survey completeness is greater than 90% and 70% for stars and galaxies, respectively, and contains 143,466 galaxies and 13,254 stars. Using the BzK diagram, we divide our galaxy catalog into quiescent and star-forming galaxy candidates. At z ~ 2, our catalogs contain 3931 quiescent and 25,757 star-forming galaxies representing the largest and most secure sample at these depths and redshifts to date. Our counts of quiescent galaxies turns over at K_s ~ 22, an effect that we demonstrate cannot be due to sample incompleteness. Both the number of faint and bright quiescent objects in our catalogs exceed the predictions of a recent semi-analytic model of galaxy formation, indicating potentially the need for further refinements in the amount of merging and active galactic nucleus feedback at z ~ 2 in these models. We measure the angular correlation function for each sample and find that the slope of the field galaxy correlation function flattens to 1.5 by K_s ~ 23. At small angular scales, the angular correlation function for passive BzK galaxies is considerably in excess of the clustering of dark matter. We use precise 30-band photometric redshifts to derive the spatial correlation length and the redshift distributions for each object class. At K_s < 22, we find r^(\u03b3/1.8)_0 = 7.0 \u00b1 0.5 h^(\u20131) Mpc for the passive BzK candidates and 4.7 \u00b1 0.8 h^(\u20131) Mpc for the star-forming BzK galaxies. Our pBzK galaxies have an average photometric redshift of z_p ~ 1.4, in approximate agreement with the limited spectroscopic information currently available. The stacked K_s image will be made publicly available from IRSA.", "date": "2010-01-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "708", "number": "1", "publisher": "American Astronomical Society", "pagerange": "202-217", "id_number": "CaltechAUTHORS:20100121-092954168", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100121-092954168", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-07-BLAN-0228" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-08-JCJC-0008" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/708/1/202", "primary_object": { "basename": "McCracken2010p6752Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/21667-e3531/files/McCracken2010p6752Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "McCracken, H. J.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/9vx92-er157", "eprint_id": 17273, "eprint_status": "archive", "datestamp": "2023-08-21 23:12:21", "lastmod": "2023-10-19 23:43:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "L." } }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K." }, "orcid": "0000-0001-8183-1460" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L. A. M." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J. F." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Perez-Montero-E", "name": { "family": "Perez Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } }, { "id": "Abbas-U", "name": { "family": "Abbas", "given": "U." } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "D." } }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "A." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Fumana-Marco", "name": { "family": "Fumana", "given": "M." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Maccagni-D", "name": { "family": "Maccagni", "given": "D." } }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Memeo-P", "name": { "family": "Memeo", "given": "P." } }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "B." } }, { "id": "Scaramella-R", "name": { "family": "Scaramella", "given": "R." } } ] }, "title": "The Density Field of the 10k zCOSMOS Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; large-scale structure of universe; surveys", "note": "\u00a9 2010 American Astronomical Society.\n\nPrint publication: Issue 1 (2010 January 1); received 2008 November 28; accepted for publication 2009 November 10;\nPublished 2009 December 14.\n\nThis work has been supported in part by a grant\nfrom the Swiss National Science Foundation and by grant\nASI/COFIS/WP3110I/026/07/0. We thank M. G. Kitzbichler\nand S. D. M. White for providing themock catalogs (Kitzbichler & White 2007).\n\nPublished - Kovac2010p6759Astrophys_J.pdf
", "abstract": "We use the current sample of ~10,000 zCOSMOS spectra of sources selected with I_(AB) < 22.5 to define the density field out to z ~ 1, with much greater resolution in the radial dimension than has been possible with either photometric redshifts or weak lensing. We present the new algorithm that we have developed (ZADE) to incorporate objects not yet observed spectroscopically by modifying their photometric redshift probability distributions using the spectroscopic redshifts of nearby galaxies. We present a number of tests on mock catalogs used to justify this approach. The ZADE algorithm allows us to probe a broader range of galaxy environments and reduce the Poisson noise in the density field. The reconstructed overdensity field of the 10k zCOSMOS galaxies consists of cluster-like patterns surrounded by void-like regions, extending up to z ~ 1. Some of these structures are very large, spanning the ~50 h^(\u20131) Mpc transverse direction of the COSMOS field and extending up to \u0394z ~ 0.05 in redshift. We present the three-dimensional overdensity maps and compare the reconstructed overdensity field to the independently identified virialized groups of galaxies and clusters detected in the visible and in X-rays. The distribution of the overdense structures is in general well traced by these virialized structures. A comparison of the large-scale structures in the zCOSMOS data and in the mock catalogs reveals an excellent agreement between the fractions of the volume enclosed in structures of all sizes above a given overdensity between the data and the mocks in 0.2 < z < 1, although in the data these overdense regions are in generally larger contiguous structures.", "date": "2010-01-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "708", "number": "1", "publisher": "American Astronomical Society", "pagerange": "505-533", "id_number": "CaltechAUTHORS:20100121-141126085", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100121-141126085", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110I/026/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/708/1/505", "primary_object": { "basename": "Kovac2010p6759Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/9vx92-er157/files/Kovac2010p6759Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Kova\u010d, K.; Lilly, S. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/35qfa-b9k26", "eprint_id": 17577, "eprint_status": "archive", "datestamp": "2023-08-21 23:09:05", "lastmod": "2023-10-20 00:01:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Halliday-C", "name": { "family": "Halliday", "given": "C." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "C." }, "orcid": "0000-0002-8853-9611" }, { "id": "Ciliegi-P", "name": { "family": "Ciliegi", "given": "P." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Bondi-M", "name": { "family": "Bondi", "given": "M." } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K." }, "orcid": "0000-0001-8183-1460" }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "L." } }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J.-F." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "Perez-Montero-E", "name": { "family": "Perez Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Abbas-U", "name": { "family": "Abbas", "given": "U." } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "D." } }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "A." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Maccagni-D", "name": { "family": "Maccagni", "given": "D." } }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Memeo-P", "name": { "family": "Memeo", "given": "P." } }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "B." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Scaramella-R", "name": { "family": "Scaramella", "given": "R." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" } ] }, "title": "K+a galaxies in the zCOSMOS survey: Physical properties of systems in their post-starburst phase", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: fundamental parameters; galaxies: luminosity function, mass function; cosmology: observations; galaxies: formation", "note": "\u00a9 2010 ESO.\n\nReceived: 30 June 2009; accepted: 9 September 2009.\n\nThis work has been supported in part by the grant\nASI/COFIS/WP3110 I/026/07/0. We thank the referee for providing constructive comments.\n\nPublished - Vergani2010p7142Astron_Astrophys.pdf
", "abstract": "Aims. The identities of the main processes triggering and quenching star-formation in galaxies remain unclear. A key stage in evolution, however, appears to be represented by post-starburst galaxies. To investigate the prevalence of these galaxies and their impact on galaxy evolution in general, we initiated a multiwavelength study of galaxies with k+a\u2002spectral features in the well-studied COSMOS field.\n\nMethods. We examine a mass-selected sample of k+a\u2002galaxies in the COSMOS field at z = 0.48-1.2 using the spectroscopic zCOSMOS sample. To classify galaxies in their k+a\u2002phase, we use a spectroscopic criterion, based on the amplitude of the H\u03b4\u2002absorption line and the absence of the [OII]\u2002emission line. We develop our analysis for a well-defined sample by imposing stringent confidence levels on the spectroscopic redshifts and spectral measurements. We compare our results for two mass-selected samples of star-forming and quiescent galaxies selected using a purely spectral classification scheme from the 10\u2009000 zCOSMOS catalogue (i.e.\u2009, based on measurements of 4000 \u00c5\u2002break and EW[OII]).\n\nResults. In our mass-limited sample, k+a\u2002galaxies occupy the brightest tail of the luminosity distribution. They are as massive as quiescent galaxies and populate the green valley in the colour versus luminosity (or stellar mass) distribution. A small percentage (<8%) of these galaxies have radio and/or X-ray counterparts (implying an upper limit to the SFR of ~8 M_\u2609 \u2009yr^(-1)). Over the entire redshift range explored, the class of post-starburst\u2002galaxies is morphologically a heterogeneous population with a similar incidence of bulge-dominated and disky galaxies. This distribution does not vary with the strength of the H\u03b4\u2002absorption line but instead with stellar mass in a way reminiscent of the well-known mass-morphology relation. The results about the incidence of asymmetries and the concentration of the light distribution derived from HST/ACS images imply that this galaxy population possibly represents an intermediate stage of galaxy evolution. Although k+a\u2002galaxies are also found in underdense regions, they appear to reside typically in a similarly rich environment as quiescent galaxies on a physical scale of ~2\u20138 Mpc, and in groups they show a morphological early-to-late type ratio similar to the quiescent galaxy class. With the current data set, we do not find evidence of statistical significant evolution in either the number/mass density of k+a\u2002galaxies at intermediate redshift with respect to the local values, or the spectral properties, although more solid results on this and other aspects will be obtained following the completion of the survey.\n\nConclusions. Several mechanisms related and unrelated to the environment are at work in quenching star-formation activity in galaxies on short timescales (<1 Gyr). Those galaxies, which are affected by a sudden quenching of their star-formation activity, may increase the stellar mass of the red-sequence by up to a non-negligible level of ~10%.", "date": "2010-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "509", "publisher": "EDP Sciences", "pagerange": "A42", "id_number": "CaltechAUTHORS:20100224-111937242", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100224-111937242", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110 I/026/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/200912802", "primary_object": { "basename": "Vergani2010p7142Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/35qfa-b9k26/files/Vergani2010p7142Astron_Astrophys.pdf" }, "pub_year": "2010", "author_list": "Vergani, D.; Zamorani, G.; et el." }, { "id": "https://authors.library.caltech.edu/records/71frz-w3p67", "eprint_id": 17662, "eprint_status": "archive", "datestamp": "2023-08-21 23:10:12", "lastmod": "2023-10-20 00:07:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L. A. M." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K." }, "orcid": "0000-0001-8183-1460" }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "L." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Halliday-C", "name": { "family": "Halliday", "given": "C." } }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J.-F." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "P\u00e9rez-Montero-E", "name": { "family": "P\u00e9rez-Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Abbas-U", "name": { "family": "Abbas", "given": "U." } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "D." } }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "A." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Maccagni-D", "name": { "family": "Maccagni", "given": "D." } }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Memeo-P", "name": { "family": "Memeo", "given": "P." } }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "B." } }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Scaramella-R", "name": { "family": "Scaramella", "given": "R." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The zCOSMOS redshift survey: how group environment alters global downsizing trends", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general; galaxies: evolution; galaxies: interactions", "note": "\u00a9 ESO 2010.\n\nReceived: 22 May 2009; accepted: 8 October 2009.\n\nWe acknowledge support from an INAF contract PRIN-\n2007/1.06.10.08 and an ASI grant ASI/COFIS/WP3110 I/026/07/0.\n\nPublished - Iovino2010p7147Astron_Astrophys.pdf
", "abstract": "Context. Groups of galaxies are a common environment, bridging the gap between starforming field galaxies and quiescent cluster galaxies. Within groups secular processes could be at play, contributing to the observed strong decrease of star formation with cosmic time in the global galaxy population.\n\nAims. We took advantage of the wealth of information provided by the first ~10\u2009000 galaxies of the zCOSMOS-bright survey and its group catalogue to study in detail the complex interplay between group environment and galaxy properties. \n\nMethods. The classical indicator F_(blue), i.e.,\u2002the fraction of blue galaxies, proved to be a simple but powerful diagnostic tool. We studied its variation for different luminosity and mass selected galaxy samples, divided as to define groups/field/isolated galaxy subsamples.\n\nResults. Using rest-frame evolving B-band volume-limited samples, the groups galaxy population exhibits significant blueing as redshift increases, but maintains a systematic difference (a lower F_(blue)) with respect to the global galaxy population, and an even larger difference with respect to the isolated galaxy population. However moving to mass selected samples it becomes apparent that such differences are largely due to the biased view imposed by the B-band luminosity selection, being driven by the population of lower mass, bright blue galaxies for which we miss the redder, equally low mass, counterparts. By carefully focusing the analysis on narrow mass bins such that mass segregation becomes negligible we find that only for the lowest mass bin explored, i.e., log(M_*/M_\u2609) \u2264 10.6, does a significant residual difference in color remain as a function of environment, while this difference becomes negligible toward higher masses.\n\nConclusions. Our results indicate that red galaxies of mass log(M_*/M_\u2609) \u2265 10.8 are already in place at z ~ 1 and do not exhibit any strong environmental dependence, possibly originating from so-called nature or internal mechanisms. In contrast, for lower galaxy masses and redshifts lower than z ~ 1, we observe the emergence in groups of a population of nurture red galaxies: slightly deviating from the trend of the downsizing scenario followed by the global galaxy population, and more so with cosmic time. These galaxies exhibit signatures of group-related secular physical mechanisms directly influencing galaxy evolution. Our analysis implies that these mechanisms begin to significantly influence galaxy evolution after z ~ 1, a redshift corresponding to the emergence of structures in which these mechanisms take place.", "date": "2010-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "509", "publisher": "EDP Sciences", "pagerange": "A40", "id_number": "CaltechAUTHORS:20100304-100202867", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100304-100202867", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-2007/1.06.10.08" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110 I/026/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/200912558", "primary_object": { "basename": "Iovino2010p7147Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/71frz-w3p67/files/Iovino2010p7147Astron_Astrophys.pdf" }, "pub_year": "2010", "author_list": "Iovino, A.; Cucciati, O.; et el." }, { "id": "https://authors.library.caltech.edu/records/2tr96-xkv23", "eprint_id": 17134, "eprint_status": "archive", "datestamp": "2023-08-21 22:57:14", "lastmod": "2023-10-19 22:50:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K. I." }, "orcid": "0000-0001-8183-1460" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D." }, "orcid": "0000-0003-1924-1122" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J.-F." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "P\u00e9rez-Montero-E", "name": { "family": "P\u00e9rez-Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } }, { "id": "Abbas-U", "name": { "family": "Abbas", "given": "U." } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "D." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "A." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Maccagni-D", "name": { "family": "Maccagni", "given": "D." } }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Memeo-P", "name": { "family": "Memeo", "given": "P." } }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "B." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "L." } }, { "id": "Scaramella-R", "name": { "family": "Scaramella", "given": "R." } }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Zamojski-M-A", "name": { "family": "Zamojski", "given": "M." } } ] }, "title": "The Optical Spectra of Spitzer 24 \u03bcm Galaxies in the Cosmic Evolution Survey Field. II. Faint Infrared Sources in the zCOSMOS-Bright 10k Catalog", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: abundances; galaxies: active; galaxies: evolution; galaxies: starburst; infrared: galaxies", "note": "\u00a9 2009 The American Astronomical Society.\nReceived 2009 September 8; accepted 2009 November 2; published 2009 December 4.\nThis paper is based on observations made with the VIMOS\nspectrograph on the Melipal-VLT telescope, undertaken at the\nEuropean Southern Observatory (ESO) under Large Program\n175.A-0839. This paper is also based on observations made\nwith the Spitzer Observatory, which is operated by the Jet\nPropulsion Laboratory, California Institute ofTechnology, under\nNASA contract 1407. We thank the anonymous referee for a\nconstructive report of this paper.\n\nPublished - Caputi2009p6668Astrophys_J.pdf
", "abstract": "We have used the zCOSMOS-bright 10k sample to identify 3244 Spitzer/MIPS 24 \u03bcm-selected galaxies with 0.06 mJy < S_(24 \u03bcm) \u227e 0.50 mJy and I_(AB) < 22.5, over 1.5 deg^2 of the COSMOS field, and studied different spectral properties, depending on redshift. At 0.2 < z < 0.3, we found that different reddening laws of common use in the literature explain the dust extinction properties of ~80% of our infrared (IR) sources, within the error bars. For up to 16% of objects, instead, the H\u03b1 \u03bb6563/H\u03b2 \u03bb4861 ratios are too high for their IR/UV attenuations, which is probably a consequence of inhomogeneous dust distributions. In only a few of our galaxies at 0.2 < z < 0.3, the IR emission could be mainly produced by dust heated by old rather than young stars. Besides, the line ratios of ~22% of our galaxies suggest that they might be star-formation/nuclear-activity composite systems. At 0.5 < z < 0.7, we estimated galaxy metallicities for 301 galaxies: at least 12% of them are securely below the upper-branch mass-metallicity trend, which is consistent with the local relation. Finally, we performed a combined analysis of the H\u03b4 equivalent width versus D_n (4000) diagram for 1722 faint and bright 24 \u03bcm galaxies at 0.6 < z < 1.0, spanning two decades in mid-IR luminosity. We found that, while secondary bursts of star formation are necessary to explain the position of the most luminous IR galaxies in that diagram, quiescent, exponentially declining star formation histories can well reproduce the spectral properties of ~40% of the less luminous sources. Our results suggest a transition in the possible modes of star formation at total IR luminosities L_(TIR) \u2248 (3 \u00b1 2) \u00d7 10^(11) L_\u2299.", "date": "2009-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "707", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1387-1403", "id_number": "CaltechAUTHORS:20100111-110435619", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100111-110435619", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Southern Observatory (ESO)", "grant_number": "175.A-0839" }, { "agency": "JPL" }, { "agency": "Caltech" }, { "agency": "NASA", "grant_number": "1407" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/707/2/1387", "primary_object": { "basename": "Caputi2009p6668Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/2tr96-xkv23/files/Caputi2009p6668Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Caputi, K. I.; Lilly, S. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/c5zrr-fmx07", "eprint_id": 17064, "eprint_status": "archive", "datestamp": "2023-08-21 22:56:33", "lastmod": "2023-10-19 22:46:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Drory-N", "name": { "family": "Drory", "given": "N." } }, { "id": "Bundy-K-A", "name": { "family": "Bundy", "given": "K." }, "orcid": "0000-0001-9742-3138" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J. P." }, "orcid": "0000-0002-4616-4989" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } }, { "id": "Willott-C-J", "name": { "family": "Willott", "given": "C. J." }, "orcid": "0000-0002-4201-7367" } ] }, "title": "The Bimodal Galaxy Stellar Mass Function in the COSMOS Survey to z ~ 1: A Steep Faint End and a New Galaxy Dichotomy", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: luminosity function; mass function surveys", "note": "\u00a9 2009 The American Astronomical Society.\nReceived 2009 October 1; accepted 2009 November 4; published 2009 December 7.\nWe thank R. Angulo, R. Bender, R. Ellis, P. F. Hopkins, S.\nKhochfar, and J. Tinker for stimulating discussions. We also\nthank P. F. Hopkins for providing gas mass fractions in electronic\nform. We thank the COSMOS collaboration for granting\nus access to their catalogs; and we gratefully acknowledge\nthe contributions of the entire COSMOS team that have made\nthis work possible. More information on the COSMOS survey\nis available at http://www.astro.caltech.edu/cosmos. A.L.\nacknowledges support from the Chamberlain Fellowship at\nLBNL and from the Berkeley Center for Cosmological Physics.\nH.J.McC. is supported by ANR grant \"ANR-07-BLAN-0228.\"\n\nPublished - Drory2009p6672Astrophys_J.pdf
", "abstract": "We present a new analysis of stellar mass functions in the COSMOS field to fainter limits than has been previously probed at z \u2264 1. The increase in dynamic range reveals features in the shape of the stellar mass function that deviate from a single Schechter function. Neither the total nor the red (passive) or blue (star-forming) galaxy stellar mass functions can be well fitted with a single Schechter function once the mass completeness limit of the sample probes below ~3 \u00d7 10^9 M_\u2299. We observe a dip or plateau at masses ~10^(10) M_\u2299, just below the traditional M^*, and an upturn toward a steep faint-end slope of \u03b1 ~ \u20131.7 at lower mass at all redshifts \u2264 1. This bimodal nature of the mass function is not solely a result of the blue/red dichotomy. Indeed, the blue mass function is by itself bimodal at z ~ 1. This suggests a new dichotomy in galaxy formation that predates the appearance of the red sequence. We propose two interpretations for this bimodal distribution. If the gas fraction increases toward lower mass, galaxies with M_ (baryon) ~ 10^(10) M_\u2299 would shift to lower stellar masses, creating the observed dip. This would indicate a change in star formation efficiency, perhaps linked to supernovae feedback becoming much more efficient below ~10^(10) M_\u2299. Therefore, we investigate whether the dip is present in the baryonic (stars+gas) mass function. Alternatively, the dip could be created by an enhancement of the galaxy assembly rate at ~10^(11) M_\u2299, a phenomenon that naturally arises if the baryon fraction peaks at M_(halo) ~ 10^(12) M_\u2299. In this scenario, galaxies occupying the bump around M_* would be identified with central galaxies and the second fainter component of the mass function having a steep faint-end slope with satellite galaxies. The low-mass end of the blue and total mass functions exhibit a steeper slope than has been detected in previous work that may increasingly approach the halo mass function value of \u20132. While the dip feature is apparent in the total mass function at all redshifts, it appears to shift from the blue to the red population, likely as a result of transforming high-mass blue galaxies into red ones. At the same time, we detect a drastic upturn in the number of low-mass red galaxies. Their increase with time seems to reflect a decrease in the number of blue systems and so we tentatively associate them with satellite dwarf (spheroidal) galaxies that have undergone quenching due to environmental processes.", "date": "2009-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "707", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1595-1609", "id_number": "CaltechAUTHORS:20100105-134549561", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100105-134549561", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Chamberlain Fellowship" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-07-BLAN-0228" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/707/2/1595", "primary_object": { "basename": "Drory2009p6672Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/c5zrr-fmx07/files/Drory2009p6672Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Drory, N.; Bundy, K.; et el." }, { "id": "https://authors.library.caltech.edu/records/46cfy-xc155", "eprint_id": 16925, "eprint_status": "archive", "datestamp": "2023-08-21 22:50:55", "lastmod": "2023-10-19 22:39:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "F\u00f6rster-Schreiber-N-M", "name": { "family": "F\u00f6rster Schreiber", "given": "N. M." } }, { "id": "Genzel-Reinhard", "name": { "family": "Genzel", "given": "R." }, "orcid": "0000-0002-2767-9653" }, { "id": "Bouch\u00e9-N", "name": { "family": "Bouch\u00e9", "given": "N." } }, { "id": "Cresci-G", "name": { "family": "Cresci", "given": "G." } }, { "id": "Davies-R", "name": { "family": "Davies", "given": "R." } }, { "id": "Buschkamp-P", "name": { "family": "Buschkamp", "given": "P." } }, { "id": "Shapiro-K-L", "name": { "family": "Shapiro", "given": "K." } }, { "id": "Tacconi-Linda-J", "name": { "family": "Tacconi", "given": "L. J." }, "orcid": "0000-0002-1485-9401" }, { "id": "Hicks-E-K-S", "name": { "family": "Hicks", "given": "E. K. S." } }, { "id": "Genel-S", "name": { "family": "Genel", "given": "S." }, "orcid": "0000-0002-3185-1540" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "A. E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "D. K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Eisenhauer-F", "name": { "family": "Eisenhauer", "given": "F." } }, { "id": "Gillessen-S", "name": { "family": "Gillessen", "given": "S." } }, { "id": "Sternberg-A", "name": { "family": "Sternberg", "given": "A." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "Kurk-J", "name": { "family": "Kurk", "given": "J." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Kong-X", "name": { "family": "Kong", "given": "X." } }, { "id": "Lehnert-Matthew-D", "name": { "family": "Lehnert", "given": "M. D." }, "orcid": "0000-0003-1939-5885" }, { "id": "Nesvadba-N-P-H", "name": { "family": "Nesvadba", "given": "N." } }, { "id": "Verma-A", "name": { "family": "Verma", "given": "A." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Arimoto-Nobuo", "name": { "family": "Arimoto", "given": "N." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Onodera-Masato", "name": { "family": "Onodera", "given": "M." } } ] }, "title": "The SINS Survey: SINFONI Integral Field Spectroscopy of z ~ 2 Star-forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: kinematics and dynamics; infrared: galaxies", "note": "\u00a9 2009 American Astronomical Society. \n\nPrint publication: Issue 2 (2009 December 1); received 2009 March 10; accepted for publication 2009 October 19; published 2009 November 11. \n\nWe thank the ESO staff, and in particular at Paranal Observatory, for their helpful and enthusiastic support during the many observing runs and several years over which SINFONI GTO were carried out. We also thank the SINFONI and PARSEC teams for their hard work on the instrument and the laser, which allowed our observational program to be carried out so successfully. We thank the referee for useful comments and suggestions that helped improve the quality and presentation of the paper. This paper and the SINS survey have benefited from many constructive, insightful, and enthusiastic discussions with many colleagues whom we are very grateful to, especially Marijn Franx for numerous inspiring discussions, as well as\nAndi Burkert, Thorsten Naab, Peter Johansson, Ortwin Gerhard, Avishai Dekel, Pieter van Dokkum, Guinevere Kauffmann, Simon White, Hans-Walter Rix, St\u00b4ephane Courteau, Martin Bureau, Claudia Maraston, among many others.We are grateful to Ian Smail, Scott Chapman, and Rob Ivison for providing the necessary information and imaging data of SMGs targeted as part of our SINS survey. N.M.F.S. acknowledges support by the Schwerpunkt\nProgramme SPP1177 of the Deutsche Forschungsgemeinschaft\nand by the Minerva Program of the Max-Planck-Gesellschaft. N.A. is supported by a Grant-in-Aid for Science Research (19549245) by the Japanese Ministry of Education, Culture, Sports, Science and Technology.\n\nPublished - Schreiber2009p6523Astrophys_J_Lett.pdf
", "abstract": "We present the Spectroscopic Imaging survey in the near-infrared (near-IR) with SINFONI (SINS) of high-redshift galaxies. With 80 objects observed and 63 detected in at least one rest-frame optical nebular emission line, mainly H\u03b1, SINS represents the largest survey of spatially resolved gas kinematics, morphologies, and physical properties of star-forming galaxies at z ~ 1-3. We describe the selection of the targets, the observations, and the data reduction. We then focus on the \"SINS H\u03b1 sample,\" consisting of 62 rest-UV/optically selected sources at 1.3 < z < 2.6 for which we targeted primarily the H\u03b1 and [N II] emission lines. Only \u224830% of this sample had previous near-IR spectroscopic observations. The galaxies were drawn from various imaging surveys with different photometric criteria; as a whole, the SINS H\u03b1 sample covers a reasonable representation of massive M_* \u2273 10^(10) M_\u2609 star-forming galaxies at z \u2248 1.5-2.5, with some bias toward bluer systems compared to pure K-selected samples due to the requirement of secure optical redshift. The sample spans 2 orders of magnitude in stellar mass and in absolute and specific star formation rates, with median values \u22483 \u00d7 10^(10) M_\u2609, \u224870 M_\u2609 yr^(\u20131), and \u22483 Gyr^(\u20131). The ionized gas distribution and kinematics are spatially resolved on scales ranging from \u22481.5 kpc for adaptive optics assisted observations to typically \u22484-5 kpc for seeing-limited data. The H\u03b1 morphologies tend to be irregular and/or clumpy. About one-third of the SINS H\u03b1 sample galaxies are rotation-dominated yet turbulent disks, another one-third comprises compact and velocity dispersion-dominated objects, and the remaining galaxies are clear interacting/merging systems; the fraction of rotation-dominated systems increases among the more massive part of the sample. The H\u03b1 luminosities and equivalent widths suggest on average roughly twice higher dust attenuation toward the H II regions relative to the bulk of the stars, and comparable current and past-averaged star formation rates.", "date": "2009-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "706", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1364-1428", "id_number": "CaltechAUTHORS:20091209-112844140", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091209-112844140", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "19549245" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/706/2/1364", "primary_object": { "basename": "Schreiber2009p6523Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/46cfy-xc155/files/Schreiber2009p6523Astrophys_J_Lett.pdf" }, "pub_year": "2009", "author_list": "F\u00f6rster Schreiber, N. M.; Genzel, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/yk3d2-yym29", "eprint_id": 16963, "eprint_status": "archive", "datestamp": "2023-08-21 22:51:05", "lastmod": "2023-10-19 22:41:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Newman-A-B", "name": { "family": "Newman", "given": "Andrew B." }, "orcid": "0000-0001-7769-8660" }, { "id": "Treu-Tommaso", "name": { "family": "Treu", "given": "Tommaso" }, "orcid": "0000-0002-8460-0390" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Sand-D-J", "name": { "family": "Sand", "given": "David J." }, "orcid": "0000-0003-4102-380X" }, { "id": "Richard-Johan", "name": { "family": "Richard", "given": "Johan" }, "orcid": "0000-0001-5492-1049" }, { "id": "Marshall-P-J", "name": { "family": "Marshall", "given": "Philip J." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Miyazaki-Satoshi", "name": { "family": "Miyazaki", "given": "Satoshi" } } ] }, "title": "The Distribution of Dark Matter Over Three Decades in Radius in the Lensing Cluster Abell 611", "ispublished": "pub", "full_text_status": "public", "keywords": "dark matter; galaxies: clusters: individual (Abell 611); galaxies: elliptical and lenticular, cD; galaxies: formation; gravitational lensing", "note": "\u00a9 2009 American Astronomical Society.\n\nPrint publication: Issue 2 (2009 December 1); received 2009 May 12; accepted for publication 2009 September 21; published 2009 November 10.\nWe are grateful to Steve Allen for kindly providing X-ray\nmeasurements of the Abell 611 gas profile, and to Herv\u00b4e Aussel,\nHisanori Furusawa, and Yutaka Komiyama for assistance with\nphotometric calibration. We thank Eric Jullo, Jason Rhodes,\nJoel Berge, Jean-Paul Kneib, Graham Smith, Richard Massey,\nand Simon White for their assistance and stimulating discussion.\nWe acknowledge the anonymous referee for helpful suggestions.\nR.S.E. acknowledges financial support from the Royal Society.\nJ.R. acknowledges support from an EU Marie Curie fellowship.\nT.T. acknowledges support from the NSF through CAREER\naward NSF-0642621, by the Sloan Foundation through a Sloan\nResearch Fellowship, and by the Packard Foundation through\na Packard Fellowship. The authors wish to recognize and acknowledge the cultural role and reverence that the summit\nof Mauna Kea has always had within the indigenous Hawaiian\ncommunity. We are most fortunate to have the opportunity to\nconduct observations from this mountain. This research has\nmade use of the NASA/IPAC Extragalactic Database, which is\noperated by the Jet Propulsion Laboratory, California Institute\nof Technology, under contract with the National Aeronautics\nand Space Administration.\n\nPublished - Newman2009p6520Astrophys_J_Lett.pdf
", "abstract": "We present a detailed analysis of the baryonic and dark matter distribution in the lensing cluster Abell 611 (z = 0.288), with the goal of determining the dark matter profile over an unprecedented range of cluster-centric distance. By combining three complementary probes of the mass distribution, weak lensing from multi-color Subaru imaging, strong lensing constraints based on the identification of multiply imaged sources in Hubble Space Telescope images, and resolved stellar velocity dispersion measures for the brightest cluster galaxy secured using the Keck telescope, we extend the methodology for separating the dark and baryonic mass components introduced by Sand et al. Our resulting dark matter profile samples the cluster from ~3 kpc to 3.25 Mpc, thereby providing an excellent basis for comparisons with recent numerical models. We demonstrate that only by combining our three observational techniques can degeneracies in constraining the form of the dark matter profile be broken on scales crucial for detailed comparisons with numerical simulations. Our analysis reveals that a simple Navarro-Frenk-White (NFW) profile is an unacceptable fit to our data. We confirm earlier claims based on less extensive analyses of other clusters that the inner profile of the dark matter profile deviates significantly from the NFW form and find a inner logarithmic slope \u03b2 flatter than 0.3 (68%; where \u03c1_(DM) \u221d r^(\u2013\u03b2) at small radii). In order to reconcile our data with cluster formation in a \u039bCDM cosmology, we speculate that it may be necessary to revise our understanding of the nature of baryon-dark matter interactions in cluster cores. Comprehensive weak and strong lensing data, when coupled with kinematic information on the brightest cluster galaxy, can readily be applied to a larger sample of clusters to test the universality of these results.", "date": "2009-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "706", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1078-1094", "id_number": "CaltechAUTHORS:20091211-113430327", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091211-113430327", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" }, { "agency": "Marie Curie Fellowship" }, { "agency": "NSF", "grant_number": "AST-0642621" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "David and Lucile Packard Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/706/2/1078", "primary_object": { "basename": "Newman2009p6520Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/yk3d2-yym29/files/Newman2009p6520Astrophys_J_Lett.pdf" }, "pub_year": "2009", "author_list": "Newman, Andrew B.; Treu, Tommaso; et el." }, { "id": "https://authors.library.caltech.edu/records/aka1m-s4v04", "eprint_id": 17171, "eprint_status": "archive", "datestamp": "2023-08-21 22:47:12", "lastmod": "2023-10-19 22:51:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "L." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Halliday-C", "name": { "family": "Halliday", "given": "C." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K." }, "orcid": "0000-0001-8183-1460" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J.-F." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "P\u00e9rez-Montero-E", "name": { "family": "P\u00e9rez-Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Abbas-U", "name": { "family": "Abbas", "given": "U." } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "D." } }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "A." } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Maccagni-D", "name": { "family": "Maccagni", "given": "D." } }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Memeo-P", "name": { "family": "Memeo", "given": "P." } }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "B." } }, { "id": "Moresco-M", "name": { "family": "Moresco", "given": "M." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Scaramella-R", "name": { "family": "Scaramella", "given": "R." } }, { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "S." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } } ] }, "title": "The zCOSMOS survey: the role of the environment in the evolution of the luminosity function of different galaxy types", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: luminosity function, mass function; galaxies: statistics; Surveys", "note": "\u00a9 2009 ESO.\n\nReceived 9 June 2009; accepted 17 September 2009.\n\nWe acknowledge support from an INAF contract PRIN-\n2007/1.06.10.08 and an ASI grant ASI/COFIS/WP3110 I/026/07/0.\n\nPublished - Zucca2009p6720Astron_Astrophys.pdf
", "abstract": "Aims. An unbiased and detailed characterization of the galaxy luminosity function (LF) is a basic requirement in many astrophysical issues: it is of particular interest in assessing the role of the environment in the evolution of the LF of different galaxy types. \nMethods. We studied the evolution in the B band LF to redshift z ~ 1 in the zCOSMOS 10k sample, for which both accurate galaxy classifications (spectrophotometric and morphological) and a detailed description of the local density field are available. \nResults. The global B band LF exhibits a brightening of ~0.7 mag in M^* from z ~ 0.2 to z ~ 0.9. At low redshifts (z<0.35), spectrophotometric late types dominate at faint magnitudes (M_B_(AB) > -20), while the bright end is populated mainly by spectrophotometric early types. At higher redshift, spectrophotometric late-type galaxies evolve significantly and, at redshift z ~ 1, the contribution from the various types to the bright end of the LF is comparable. The evolution for spectrophotometric early-type galaxies is in both luminosity and normalization: M* brightens by ~0.6 mag but \u03c6^\u2217 decreases by a factor ~1.7 between the first and the last redshift bin. A similar behaviour is exhibited by spectrophotometric late-type galaxies, but with an opposite trend for the normalization: a brightening of ~0.5 mag is present in M^*, while \u03c6^\u2217 increases by a factor ~1.8.\nStudying the role of the environment, we find that the global LF of galaxies in overdense regions has always a brighter M^* and a flatter slope. In low density environments, the main contribution to the LF is from blue galaxies, while for high density environments there is an important contribution from red galaxies to the bright end.\nThe differences between the global LF in the two environments are not due to only a difference in the relative numbers of red and blue galaxies, but also to their relative luminosity distributions: the value of M^* for both types in underdense regions is always fainter than in overdense environments. These results indicate that galaxies of the same type in different environments have different properties.\nWe also detect a differential evolution in blue galaxies in different environments: the evolution in their LF is similar in underdense and overdense regions between z ~ 0.25 and z ~ 0.55, and is mainly in luminosity. In contrast, between z ~ 0.55 and z ~ 0.85 there is little luminosity evolution but there is significant evolution in \u03c6^\u2217, that is, however, different between the two environments: in overdense regions \u03c6^\u2217 increases by a factor ~1.6, while in underdense regions this increase reaches a factor ~2.8. Analyzing the blue galaxy population in more detail, we find that this evolution is driven mainly by the bluest types. \nConclusions. The \"specular\" evolution of late- and early-type galaxies is consistent with a scenario where a part of blue galaxies is transformed in red galaxies with increasing cosmic time, without significant changes in the fraction of intermediate-type galaxies. The bulk of this tranformation in overdense regions probably happened before z ~ 1, while it is still ongoing at lower redshifts in underdense environments.", "date": "2009-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "508", "number": "3", "publisher": "EDP Sciences", "pagerange": "1217-1234", "id_number": "CaltechAUTHORS:20100113-153659302", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100113-153659302", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-2007/1.06.10.08" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110 I/026/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/200912665", "primary_object": { "basename": "Zucca2009p6720Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/aka1m-s4v04/files/Zucca2009p6720Astron_Astrophys.pdf" }, "pub_year": "2009", "author_list": "Zucca, E.; Bardelli, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/ardm8-66a19", "eprint_id": 16783, "eprint_status": "archive", "datestamp": "2023-08-21 22:43:07", "lastmod": "2023-10-19 22:33:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Trump-J-R", "name": { "family": "Trump", "given": "Jonathan R." } }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "Chris D." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Yoshiaki" }, "orcid": "0000-0003-2247-3741" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "Marcella" }, "orcid": "0000-0002-5059-6848" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "Francesca" }, "orcid": "0000-0002-2115-1137" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "id": "Gabor-J-M", "name": { "family": "Gabor", "given": "Jared M." } }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "Knud" }, "orcid": "0000-0003-3804-2137" }, { "id": "Kelly-B-C", "name": { "family": "Kelly", "given": "Brandon C." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "Tohru" }, "orcid": "0000-0002-7402-5441" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Yasuhiro" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Huchra-J-P", "name": { "family": "Huchra", "given": "John P." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "Jeyhan S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Lanzuisi-G", "name": { "family": "Lanzuisi", "given": "Giorgio" }, "orcid": "0000-0001-9094-0984" }, { "id": "McCarthy-P-J", "name": { "family": "McCarthy", "given": "Patrick J." } }, { "id": "Maineri-V", "name": { "family": "Maineri", "given": "Vincenzo" } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The Nature of Optically Dull Active Galactic Nuclei in COSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; black hole physics; galaxies: active; galaxies: nuclei; X-rays: galaxies", "note": "\u00a9 2009 American Astronomical Society.\n\nPrint publication: Issue 1 (2009 November 20); received 2009 August 1; accepted for publication 2009 October 13;\npublished 2009 November 5.\n\nJ.R.T. acknowledges support from NSF ADP grant\nNNX08AJ28G, an ARCS fellowship, and an NSF-EAPSI/JSPS\nsummer research fellowship. B.C.K. acknowledges support\nfrom NASA through the Hubble Fellowship grant HF-01220.01\nawarded by the Space Telescope Science Institute, which is\noperated by the Association of Universities for Research in Astronomy,\nInc., for NASA, under contract NAS 5-26555. We\nthank J. Rigby for comments on the axis ratios of AGN host\ngalaxies, and A. Diamond-Stanic for help regarding line luminosity\nmeasurements.We additionally thank the anonymous referee\nfor several suggestions which improved the quality of this\npaper.\n\nPublished - Trump2009p6416Astrophys_J.pdf
", "abstract": "We present infrared, optical, and X-ray data of 48 X-ray bright, optically dull active galactic nuclei (AGNs) in the COSMOS field. These objects exhibit the X-ray luminosity of an AGN but lack broad and narrow emission lines in their optical spectrum. We show that despite the lack of optical emission lines, most of these optically dull AGNs are not well described by a typical passive red galaxy spectrum: instead they exhibit weak but significant blue emission like an unobscured AGN. Photometric observations over several years additionally show significant variability in the blue emission of four optically dull AGNs. The nature of the blue and infrared emission suggest that the optically inactive appearance of these AGNs cannot be caused by obscuration intrinsic to the AGNs. Instead, up to ~70% of optically dull AGNs are diluted by their hosts, with bright or simply edge-on hosts lying preferentially within the spectroscopic aperture. The remaining ~30% of optically dull AGNs have anomalously high f_X /f_O ratios and are intrinsically weak, not obscured, in the optical. These optically dull AGNs are best described as a weakly accreting AGN with a truncated accretion disk from a radiatively inefficient accretion flow.", "date": "2009-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "706", "number": "1", "publisher": "American Astronomical Society", "pagerange": "797-809", "id_number": "CaltechAUTHORS:20091123-113231390", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091123-113231390", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "NNX08AJ28G" }, { "agency": "ARCS Felllowhsip" }, { "agency": "NSF-EAPSI/JSPS" }, { "agency": "NASA", "grant_number": "HF-01220.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/706/1/797", "primary_object": { "basename": "Trump2009p6416Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/ardm8-66a19/files/Trump2009p6416Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Trump, Jonathan R.; Impey, Chris D.; et el." }, { "id": "https://authors.library.caltech.edu/records/faxy0-s2233", "eprint_id": 17266, "eprint_status": "archive", "datestamp": "2023-08-21 22:42:05", "lastmod": "2023-10-19 23:42:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "Knud" }, "orcid": "0000-0003-3804-2137" }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "Angela" } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "Marcella" }, "orcid": "0000-0002-5059-6848" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "Nico" } }, { "id": "Cisternas-M", "name": { "family": "Cisternas", "given": "Mauricio" } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "Francesca" }, "orcid": "0000-0002-2115-1137" }, { "id": "Colbert-J-W", "name": { "family": "Colbert", "given": "James" } }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "Andrea" }, "orcid": "0000-0003-3451-9970" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G\u00fcnther" }, "orcid": "0000-0002-0797-0646" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "Chris" } }, { "id": "Inskip-K-J", "name": { "family": "Inskip", "given": "Katherine" } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "Simon" }, "orcid": "0000-0002-6423-3597" }, { "id": "Maier-C", "name": { "family": "Maier", "given": "Christian" } }, { "id": "Merloni-A", "name": { "family": "Merloni", "given": "Andrea" } }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "Dominik A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "John" }, "orcid": "0000-0002-0000-6977" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Yoshi" }, "orcid": "0000-0003-2247-3741" }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "Jonathan R." } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" } ] }, "title": "Massive Galaxies in COSMOS: Evolution of Black Hole Versus Bulge Mass but not Versus Total Stellar Mass Over the Last 9 Gyr?", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: evolution; galaxies: fundamental parameters; galaxies: nuclei", "note": "\u00a9 2009. The American Astronomical Society. All rights reserved. Received 2009 July 29; accepted 2009 October 27; published 2009 November 10. K.J. thanks E. F. Bell, N. Neumayer, C. Y. Peng, and A.\nvan der Wel for very fruitful discussions, and the anonymous\nreferee for helpful suggestions. K.J. is supported through the\nEmmy Noether Programme of the German Science Foundation\n(DFG). D.R. acknowledges support from NASA through a\nHubble Fellowship.\nFacilities: ESO VLT (VIMOS), HST (ACS, NICMOS),\nMagellan (IMACS), XMM-Newton\n\nPublished - Jahnke2009p6859Astrophys_J_Lett.pdf
", "abstract": "We constrain the ratio of black hole (BH) mass to total stellar mass of type-1 active galactic nuclei (AGNs) in the COSMOS survey at 1 < z < 2. For 10 AGNs at mean redshift z ~ 1.4 with both Hubble Space Telescope (HST)/ACS and HST/NICMOS imaging data, we are able to compute the total stellar mass M_(*,total), based on rest-frame UV-to-optical host galaxy colors which constrain mass-to-light ratios. All objects have virial M_(BH) estimates available from the COSMOS Magellan/IMACS and zCOSMOS surveys. We find within errors zero difference between the M_(BH)-M_(*,total) relation at z ~ 1.4 and the M_(BH)-M_(*,bulge) relation in the local universe. Our interpretation is (1) if our objects were purely bulge-dominated, the M_(BH)-M_(*,bulge) relation has not evolved since z ~ 1.4. However, (2) since we have evidence for substantial disk components, the bulges of massive galaxies (M_(*,total) = 11.1 \u00b1 0.3 or log M_(BH) ~ 8.3 \u00b1 0.2) must have grown over the last 9 Gyr predominantly by redistribution of the disk into the bulge mass. Since all necessary stellar mass exists in galaxies at z = 1.4, no star formation or addition of external stellar material is required, but only a redistribution, e.g., induced by minor and major merging or through disk instabilities. Merging, in addition to redistributing mass in the galaxy, will add both BH and stellar/bulge mass, but does not change the overall final M_(BH)/M_(*,bulge) ratio. Since the overall cosmic stellar and BH mass buildup trace each other tightly over time, our scenario of bulge formation in massive galaxies is independent of any strong BH feedback and means that the mechanism coupling BH and bulge mass until the present is very indirect.", "date": "2009-11-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "706", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L215-L220", "id_number": "CaltechAUTHORS:20100121-101835291", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100121-101835291", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "ESA Member States" }, { "agency": "European Southern Observatory", "grant_number": "175.A-0839" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/706/2/L215", "primary_object": { "basename": "Jahnke2009p6859Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/faxy0-s2233/files/Jahnke2009p6859Astrophys_J_Lett.pdf" }, "pub_year": "2009", "author_list": "Jahnke, Knud; Bongiorno, Angela; et el." }, { "id": "https://authors.library.caltech.edu/records/2072g-qbc96", "eprint_id": 16842, "eprint_status": "archive", "datestamp": "2023-08-21 22:35:00", "lastmod": "2023-10-19 22:36:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Krick-J-E", "name": { "family": "Krick", "given": "J. E." } }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J. A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } }, { "id": "Ashby-M-L-N", "name": { "family": "Ashby", "given": "M. L. N." }, "orcid": "0000-0002-3993-0745" }, { "id": "Hora-J-L", "name": { "family": "Hora", "given": "J." }, "orcid": "0000-0002-5599-4650" }, { "id": "Gorjian-V", "name": { "family": "Gorjian", "given": "V." } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Egami-Eichi", "name": { "family": "Egami", "given": "E." } }, { "id": "Lacy-M", "name": { "family": "Lacy", "given": "M." }, "orcid": "0000-0002-3032-1783" } ] }, "title": "The Infrared Array Camera Dark Field: Far-Infrared to X-ray Data", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: photometry", "note": "\u00a9 2009. The American Astronomical Society. Received 2009 April 16; accepted 2009 September 11; published 2009 October 14. We thank the anonymous referee for useful suggestions on the\nmanuscript. This research has made use of data from the Two\nMicron All Sky Survey, which is a joint project of the University\nof Massachusetts and the Infrared Processing and Analysis\nCenter/California Institute of Technology, funded by the National\nAeronautics and Space Administration and the National\nScience Foundation. This work was based on observations obtained\nwith the Hale Telescope, Palomar Observatory as part\nof a continuing collaboration between the California Institute\nof Technology, NASA/JPL, and Cornell University, the Spitzer\nSpace Telescope, which is operated by the Jet Propulsion Laboratory California Institute of Technology under a contract with\nNASA, and the NASA/ESA Hubble Space Telescope, obtained\nat the Space Telescope Science Institute, which is operated by\nthe Association of Universities for Research in Astronomy, Inc.\nSupport for program #10521 was provided by NASA through a\ngrant from the Space Telescope Science Institute, which is operated\nby the Association of Universities for Research in Astronomy,\nInc., under NASA contract NAS 5-26555. FLAMINGOS\nwas designed and constructed by the IR instrumentation group\n(PI: R. Elston) at the University of Florida, Department of Astronomy,\nwith support from NSF grant AST97-31180 and Kitt\nPeak National Observatory. Observations reported here were\nobtained at the MMT Observatory, a joint facility of the Smithsonian\nInstitution and the University of Arizona. Support for this\nwork was provided by the National Aeronautics and Space Administration\nthrough Chandra Award Number G07-8120 issued\nby the Chandra X-ray Observatory Center, which is operated by\nthe Smithsonian Astrophysical Observatory for and on behalf of\nthe National Aeronautics Space Administration under contract\nNAS8-03060. \nFacilities: Hale (LFC, WIRC, COSMIC), MMT(Megacam,\nSWIRC), HST (ACS), Spitzer (IRAC, MIPS), Akari, CXO\n(ACIS), KPNO\n\nPublished - Krick2009p6415Astrophys_J_Suppl_S.pdf
", "abstract": "We present 20 band photometry from the far-IR to X-ray in the Spitzer Infrared Array Camera (IRAC) dark field. The bias for the near-IR camera on Spitzer is calibrated by observing a ~20' diameter \"dark\" field near the north ecliptic pole roughly every two-to-three weeks throughout the mission duration of Spitzer. The field is unique for its extreme depth, low background, high quality imaging, time-series information, and accompanying photometry including data taken with Akari, Palomar, MMT, KPNO, Hubble, and Chandra. This serendipitous survey contains the deepest mid-IR data taken to date. This data set is well suited for studies of intermediate-redshift galaxy clusters, high-redshift galaxies, the first generation of stars, and the lowest mass brown dwarfs, among others. This paper provides a summary of the data characteristics and catalog generation from all bands collected to date as well as a discussion of photometric redshifts and initial and expected science results and goals. To illustrate the scientific potential of this unique data set, we also present here IRAC color-color diagrams.", "date": "2009-11", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "185", "number": "1", "publisher": "American Astronomical Society", "pagerange": "85-97", "id_number": "CaltechAUTHORS:20091130-145956719", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091130-145956719", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "NASA/ESA Hubble Space Telescope" }, { "agency": "Space Telescope Science Institute" }, { "agency": "Association of Universities for Research in Astronomy (AURA)" }, { "agency": "NASA", "grant_number": "10521" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF", "grant_number": "AST97-31180" }, { "agency": "Kitt Peak National Observatory" }, { "agency": "NASA", "grant_number": "G07-8120" }, { "agency": "Smithsonian Astrophysical Observatory" }, { "agency": "NASA", "grant_number": "NAS8-03060" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0067-0049/185/1/85", "primary_object": { "basename": "Krick2009p6415Astrophys_J_Suppl_S.pdf", "url": "https://authors.library.caltech.edu/records/2072g-qbc96/files/Krick2009p6415Astrophys_J_Suppl_S.pdf" }, "pub_year": "2009", "author_list": "Krick, J. E.; Surace, J. A.; et el." }, { "id": "https://authors.library.caltech.edu/records/0tn0d-dv250", "eprint_id": 16561, "eprint_status": "archive", "datestamp": "2023-08-19 00:26:48", "lastmod": "2023-10-19 22:22:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J. A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Huynh-Minh-T", "name": { "family": "Huynh", "given": "M. T." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Afonso-Luis-A", "name": { "family": "Afonso-Luis", "given": "A." } }, { "id": "Bhattacharya-Bidushi", "name": { "family": "Bhattacharya", "given": "B." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Fu-Hai", "name": { "family": "Fu", "given": "H." }, "orcid": "0000-0001-9608-6395" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Lee-Nicolas", "name": { "family": "Lee", "given": "Nicholas" }, "orcid": "0000-0001-5500-1324" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E." }, "orcid": "0000-0001-7089-7325" }, { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M. T." }, "orcid": "0000-0003-1033-9684" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P. L." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" } ] }, "title": "Spitzer 70 and 160 \u03bcm Observations of the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: starburst \u2013 infrared: galaxies", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2009 February 17; accepted 2009 August 15; published 2009 September 22. \n\nWe thank our colleagues associated with the Spitzer mission who have made these observations possible. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech.\n\nPublished - Frayer2009p6233Astron_J.pdf
Accepted Version - 0902.3273.pdf
", "abstract": "We present Spitzer 70 and 160 \u03bcm observations of the COSMOS Spitzer survey (S-COSMOS). The data processing techniques are discussed for the publicly released products consisting of images and source catalogs. We present accurate 70 and 160 \u03bcm source counts of the COSMOS field and find reasonable agreement with measurements in other fields and with model predictions. The previously reported counts for GOODS-North and the extragalactic First Look Survey are updated with the latest calibration, and counts are measured based on the large area SWIRE survey to constrain the bright source counts. We measure an extragalactic confusion noise level of \u03c3_c = 9.4 \u00b1 3.3 mJy (q = 5) for the MIPS 160 \u03bcm band based on the deep S-COSMOS data and report an updated confusion noise level of \u03c3_c = 0.35 \u00b1 0.15 mJy (q = 5) for the MIPS 70 \u03bcm band.", "date": "2009-11", "date_type": "published", "publication": "Astronomical Journal", "volume": "138", "number": "5", "publisher": "American Astronomical Society", "pagerange": "1261-1270", "id_number": "CaltechAUTHORS:20091103-130946829", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091103-130946829", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "COSMOS", "value": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)", "value": "Infrared Processing and Analysis Center (IPAC)" } ] }, "doi": "10.1088/0004-6256/138/5/1261", "primary_object": { "basename": "0902.3273.pdf", "url": "https://authors.library.caltech.edu/records/0tn0d-dv250/files/0902.3273.pdf" }, "related_objects": [ { "basename": "Frayer2009p6233Astron_J.pdf", "url": "https://authors.library.caltech.edu/records/0tn0d-dv250/files/Frayer2009p6233Astron_J.pdf" } ], "pub_year": "2009", "author_list": "Frayer, D. T.; Sanders, D. B.; et el." }, { "id": "https://authors.library.caltech.edu/records/jnj6e-g4z83", "eprint_id": 16417, "eprint_status": "archive", "datestamp": "2023-08-21 22:25:19", "lastmod": "2023-10-19 22:12:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "Simon J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "Vincent" } }, { "id": "Maier-C", "name": { "family": "Maier", "given": "Christian" } }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "Vincenzo" } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "Marco" } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "Marco" } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "Gianni" } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "Marcella C." }, "orcid": "0000-0003-1624-7609" }, { "id": "Contini-T", "name": { "family": "Contini", "given": "Thierry" } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "Jean-Paul" }, "orcid": "0000-0002-4616-4989" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "Olivier" }, "orcid": "0000-0001-5891-2596" }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "Alvio" }, "orcid": "0000-0002-7093-7355" }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "Sandro" } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "Micol" } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "Angela" } }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "Karina" }, "orcid": "0000-0001-8183-1460" }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "Graziano" } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "Olga" }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "Sylvain" }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "Loic" } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "Paolo" } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "Bianca" } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "Angela" } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "Pawel" } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "Katarina" } }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "Christian" } }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "Fabrice" } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "Jean-Francois" } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "Roser" } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Yingjie" } }, { "id": "P\u00e9rez-Montero-E", "name": { "family": "P\u00e9rez-Montero", "given": "Enrique" } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "Elena" } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "John D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "Masayuki" }, "orcid": "0000-0002-5011-5178" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "Lidia" } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "Laurence" } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "Daniela" } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "Elena" } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "Pascal A." }, "orcid": "0000-0001-5851-6649" }, { "id": "Abbas-U", "name": { "family": "Abbas", "given": "Umi" } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "Dario" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "Alberto" } }, { "id": "Cassata-Paolo", "name": { "family": "Cassata", "given": "Paolo" } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "Andrea" } }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "id": "Fumana-M", "name": { "family": "Fumana", "given": "Marco" } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "Luigi" } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G\u00fcnther" }, "orcid": "0000-0002-0797-0646" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton" }, "orcid": "0000-0002-6610-2048" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexei" }, "orcid": "0000-0002-3677-3617" }, { "id": "Maccagni-D", "name": { "family": "Maccagni", "given": "Dario" } }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "Christian" } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "Henry" }, "orcid": "0000-0002-9489-7765" }, { "id": "Memeo-P", "name": { "family": "Memeo", "given": "Pierdomenico" } }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "Baptiste" } }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "Cristiano" } }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "Lucia" } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "David" }, "orcid": "0000-0002-1233-9998" }, { "id": "Scaramella-R", "name": { "family": "Scaramella", "given": "Roberto" } }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "Claudia" }, "orcid": "0000-0002-9136-8876" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "Patrick" } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Yoshiaki" }, "orcid": "0000-0003-2247-3741" } ] }, "title": "The zCOSMOS 10k-Bright Spectroscopic Sample", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: distances and redshifts; galaxies: evolution; large-scale structure of universe; quasars: general; surveys", "note": "\u00a9 2009 The American Astronomical Society.\nReceived 2009 March 19; accepted 2009 August 21; published 2009 September 15.\nEfficient execution of such a large program in Service Mode\non the VLT requires the efforts of many individual observatory\nstaff at ESO, both in Garching and on Cerro Paranal, and we\ngratefully acknowledge the contribution of these many and\nregrettably sometimes anonymous individuals to our project.\nThe zCOSMOS program builds on many of the hardware\nand software tools built by the VIMOS/VVDS team, and we\nacknowledge here the contribution of those in the VIMOS/\nVVDS team who are not part of the zCOSMOS project. Finally,\nwe acknowledge with appreciation the contributions of those\nmany individuals not listed as authors who have worked, directly\nor indirectly, to produce the superb imaging data on which the\nCOSMOS survey is based.\n\nPublished - Lilly2009p6124Astrophys_J_Suppl_S.pdf
", "abstract": "We present spectroscopic redshifts of a large sample of galaxies with I_(AB) < 22.5 in the COSMOS field, measured from spectra of 10,644 objects that have been obtained in the first two years of observations in the zCOSMOS-bright redshift survey. These include a statistically complete subset of 10,109 objects. The average accuracy of individual redshifts is 110 km s^(\u20131), independent of redshift. The reliability of individual redshifts is described by a Confidence Class that has been empirically calibrated through repeat spectroscopic observations of over 600 galaxies. There is very good agreement between spectroscopic and photometric redshifts for the most secure Confidence Classes. For the less secure Confidence Classes, there is a good correspondence between the fraction of objects with a consistent photometric redshift and the spectroscopic repeatability, suggesting that the photometric redshifts can be used to indicate which of the less secure spectroscopic redshifts are likely right and which are probably wrong, and to give an indication of the nature of objects for which we failed to determine a redshift. Using this approach, we can construct a spectroscopic sample that is 99% reliable and which is 88% complete in the sample as a whole, and 95% complete in the redshift range 0.5 < z < 0.8. The luminosity and mass completeness levels of the zCOSMOS-bright sample of galaxies is also discussed.", "date": "2009-10", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "184", "number": "2", "publisher": "American Astronomical Society", "pagerange": "218-229", "id_number": "CaltechAUTHORS:20091021-080927611", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091021-080927611", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Southern Observatory (ESO) Very Large Telescope (VLT)", "grant_number": "175" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "National Astronomical Observatory of Japan" }, { "agency": "National Research Council of Canada" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0067-0049/184/2/218", "primary_object": { "basename": "Lilly2009p6124Astrophys_J_Suppl_S.pdf", "url": "https://authors.library.caltech.edu/records/jnj6e-g4z83/files/Lilly2009p6124Astrophys_J_Suppl_S.pdf" }, "pub_year": "2009", "author_list": "Lilly, Simon J.; Le Brun, Vincent; et el." }, { "id": "https://authors.library.caltech.edu/records/b84cf-kph90", "eprint_id": 16187, "eprint_status": "archive", "datestamp": "2023-08-21 22:22:56", "lastmod": "2023-10-19 22:01:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Giodini-S", "name": { "family": "Giodini", "given": "S." } }, { "id": "Pierini-D", "name": { "family": "Pierini", "given": "D." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Pratt-G-W", "name": { "family": "Pratt", "given": "G. W." } }, { "id": "Boehringer-H", "name": { "family": "Boehringer", "given": "H." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Massey-R", "name": { "family": "Massey", "given": "R." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S. S." } }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } } ] }, "title": "Stellar and Total Baryon Mass Fractions in Groups and Clusters Since Redshift 1", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmological parameters; cosmology: observations; diffuse radiation; galaxies: clusters: general; galaxies: stellar content; X-rays: galaxies: clusters", "note": "\u00a9 2009 American Astronomical Society. \nReceived 2008 December 16, accepted for publication 2009 July 21.\nPublished 2009 September 3. \nThe authors thank the anonymous referee for her/his valuable\ncomments, which led to a significant improvement of the\npaper. We acknowledge the contributions of the entire COSMOS\ncollaboration; more information on the COSMOS survey\nare available at http://www.astr.caltech.edu/\u223ccosmos. This research\nwas supported by the DFG Cluster of Excellence Origin\nand Structure of the Universe (http://www.universe-cluster.de).\nD.P. acknowledges support by the German Deutsches Zentrum\nf\u00fcr Luft- und Raumfahrt, DLR project number 50 OR 0405.\n\nPublished - Giodini2009p5939Astrophys_J.pdf
", "abstract": "We investigate if the discrepancy between estimates of the total baryon mass fraction obtained from observations of the cosmic microwave background (CMB) and of galaxy groups/clusters persists when a large sample of groups is considered. To this purpose, 91 candidate X-ray groups/poor clusters at redshift 0.1 \u2264 z \u2264 1 are selected from the COSMOS 2 deg^2 survey, based only on their X-ray luminosity and extent. This sample is complemented by 27 nearby clusters with a robust, analogous determination of the total and stellar mass inside R_(500). The total sample of 118 groups and clusters with z \u2264 1 spans a range in M_(500) of ~10^(13)-10^(15) M_\u2609. We find that the stellar mass fraction associated with galaxies at R_(500) decreases with increasing total mass as M^(\u20130.37 \u00b1 0.04)_(500), independent of redshift. Estimating the total gas mass fraction from a recently derived, high-quality scaling relation, the total baryon mass fraction (f^(stars+gas)_(500) = f^(stars)_(500) + f^(gas)_(500)) is found to increase by ~25%, when M_(500) increases from = 5 \u00d7 10^(13) M_\u2609 to = 7 \u00d7 10^(14) M_\u2609. After consideration of a plausible contribution due to intracluster light (11%-22% of the total stellar mass) and gas depletion through the hierarchical assembly process (10% of the gas mass), the estimated values of the total baryon mass fraction are still lower than the latest CMB measure of the same quantity (WMAP5), at a significance level of 3.3\u03c3 for groups of = 5 \u00d7 10^(13) M_\u2609. The discrepancy decreases toward higher total masses, such that it is 1\u03c3 at = 7 \u00d7 10^(14) M_\u2609. We discuss this result in terms of nongravitational processes such as feedback and filamentary heating.", "date": "2009-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "703", "number": "1", "publisher": "American Astronomical Society", "pagerange": "982-993", "id_number": "CaltechAUTHORS:20091006-134828649", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091006-134828649", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50 OR 0405" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "COSMOS Collaboration" ] }, "doi": "10.1088/0004-637X/703/1/982", "primary_object": { "basename": "Giodini2009p5939Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/b84cf-kph90/files/Giodini2009p5939Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Giodini, S.; Pierini, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/42zg4-td797", "eprint_id": 16161, "eprint_status": "archive", "datestamp": "2023-08-21 22:22:41", "lastmod": "2023-10-19 21:59:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "Emeric" } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "Herve" }, "orcid": "0000-0002-1371-5705" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Riguccini-L", "name": { "family": "Riguccini", "given": "Laurie" } }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "David T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "Stephane" } }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Feruglio-C", "name": { "family": "Feruglio", "given": "Chiara" } }, { "id": "Rodighiero-G", "name": { "family": "Rodighiero", "given": "Giulia" }, "orcid": "0000-0002-9415-2296" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "Jeyhan" }, "orcid": "0000-0001-9187-3605" }, { "id": "Heinis-S", "name": { "family": "Heinis", "given": "Sebastien" } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "Henry Joy" }, "orcid": "0000-0002-9489-7765" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "David" } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "David" }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" } ] }, "title": "Deep Spitzer 24 \u03bcm COSMOS Imaging. I. The Evolution of Luminous Dusty Galaxies\u2014Confronting the Models", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: high-redshift; infrared: galaxies", "note": "\u00a9 2009. The American Astronomical Society. Received 2009 February 25; accepted 2009 July 28; published 2009 August 26. It is a pleasure to acknowledge the contribution from\nall our colleagues of the COSMOS collaboration. More\ninformation on the COSMOS survey is available at\nhttp://www.astro.caltech.edu/cosmos. This work is based on observations\nmade with the Spitzer Space Telescope, a facility\noperated by NASA/JPL. Financial supports were provided by\nNASA through contracts nos. 1289085, 1310136, 1282612, and\n1298231 issued by the Jet Propulsion Laboratory. Our research\nproject was also supplemented with phenomenological model\npredictions from published papers or future publications and\nthat Damien Le Borgne, Carlotta Gruppioni, Francesca Pozzi,\nGuilaine Lagache, and Herv\u00b4e Dole have been willing to share\nwith us; they are greatly acknowledged for their contribution.\nWe are grateful to David Elbaz and Casey Papovich for insightful\ncomments on our results, and we also appreciated the\nhospitality of the Aspen Center for Physics where part of our\nwork was prepared. We finally acknowledge the support and\nthe contribution of the Spitzer Science Center to our research\nprogram and we warmly thank the referee for a careful reading\nof the manuscript. Support for ELF's work was provided by\nNASA/Caltech through the Spitzer Space Telescope Fellowship\nProgram (no. 1080367). Part of this work was also supported by\nthe grant ASI/COFIS/WP3110 I/026/07/0.\n\nPublished - LeFloch2009p5929Astrophys_J.pdf
", "abstract": "We present the first results obtained from the identification of ~30,000 sources in the Spitzer/24 \u03bcm observations of the COSMOS field at S_(24 \u03bcm) \u2273 80 \u03bcJy. Using accurate photometric redshifts (\u03c3_ z ~ 0.12 at z ~ 2 for 24 \u03bcm sources with i ^+ \u2273 25 mag AB) and simple extrapolations of the number counts at faint fluxes, we resolve with unprecedented detail the buildup of the mid-infrared background across cosmic ages. We find that ~50% and ~80% of the 24 \u03bcm background intensity originate from galaxies at z \u2273 1 and z \u2273 2, respectively, supporting the scenario where highly obscured sources at very high redshifts (z \u2273 2) contribute only marginally to the cosmic infrared background. Assuming flux-limited selections at optical wavelengths, we also find that the fraction of i ^+-band sources with 24 \u03bcm detection strongly increases up to z ~ 2 as a consequence of the rapid evolution that star-forming galaxies have undergone with look-back time. Nonetheless, this rising trend shows a clear break at z ~ 1.3, probably due to k-correction effects implied by the complexity of spectral energy distributions in the mid-infrared. Finally, we compare our results with the predictions from different models of galaxy formation. We note that semianalytical formalisms currently fail to reproduce the redshift distributions observed at 24 \u03bcm. Furthermore, the simulated galaxies at S _(24 \u03bcm) > 80 \u03bcJy exhibit R\u2013K colors much bluer than observed and the predicted K-band fluxes are systematically underestimated at z \u2273 0.5. Unless these discrepancies mainly result from an incorrect treatment of extinction in the models they may reflect an underestimate of the predicted density of high-redshift massive sources with strong ongoing star formation, which would point to more fundamental processes and/or parameters (e.g., initial mass function, critical density to form stars, feedback,...) that are still not fully controlled in the simulations. The most recent backward evolution scenarios reproduce reasonably well the flux/redshift distribution of 24 \u03bcm sources up to z ~ 3, although none of them is able to exactly match our results at all redshifts.", "date": "2009-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "703", "number": "1", "publisher": "American Astronomical Society", "pagerange": "222-239", "id_number": "CaltechAUTHORS:20091001-151003670", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091001-151003670", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "COSMOS collaboration" }, { "agency": "NASA", "grant_number": "1289085" }, { "agency": "NASA", "grant_number": "1310136" }, { "agency": "NASA", "grant_number": "1282612" }, { "agency": "NASA", "grant_number": "1298231" }, { "agency": "Spitzer Science Center" }, { "agency": "NASA/Caltech" }, { "agency": "Spitzer Space Telescope Fellowship", "grant_number": "1080367" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "WP3110 I/026/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/703/1/222", "primary_object": { "basename": "LeFloch2009p5929Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/42zg4-td797/files/LeFloch2009p5929Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Le Floc'h, Emeric; Aussel, Herve; et el." }, { "id": "https://authors.library.caltech.edu/records/04v0c-0sm89", "eprint_id": 16160, "eprint_status": "archive", "datestamp": "2023-08-21 22:22:36", "lastmod": "2023-10-19 21:59:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kocevski-D-D", "name": { "family": "Kocevski", "given": "Dale D." } }, { "id": "Lubin-L-M", "name": { "family": "Lubin", "given": "Lori M." } }, { "id": "Lemaux-B-C", "name": { "family": "Lemaux", "given": "Brian C." }, "orcid": "0000-0002-1428-7036" }, { "id": "Gal-R-R", "name": { "family": "Gal", "given": "Roy R." } }, { "id": "Fassnacht-C-D", "name": { "family": "Fassnacht", "given": "Christopher D." }, "orcid": "0000-0002-4030-5461" }, { "id": "Squires-G-K", "name": { "family": "Squires", "given": "Gordon K." }, "orcid": "0000-0002-1977-5717" } ] }, "title": "No Evidence of Quasar-Mode Feedback in a Four-Way Group Merger at z ~ 0.84", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: clusters: general; X-rays: galaxies: clusters", "note": "\u00a9 2009. The American Astronomical Society. Received 2009 April 9; accepted 2009 July 20; published 2009 September 1.\nThis work is supported by the Chandra General Observing Program under award number G07-8126X. The spectrographic data used herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.\n\nPublished - Kocevski2009p5942Astrophys_J_Lett.pdf
", "abstract": "We report on the results of a Chandra search for evidence of triggered nuclear activity within the Cl0023+0423 four-way group merger at z ~ 0.84. The system consists of four interacting galaxy groups in the early stages of hierarchical cluster formation and, as such, provides a unique look at the level of processing and evolution already under way in the group environment prior to cluster assembly. We present the number counts of X-ray point sources detected in a field covering the entire Cl0023 structure, as well as a cross-correlation of these sources with our extensive spectroscopic database. Both the redshift distribution and cumulative number counts of X-ray sources reveal little evidence to suggest that the system contains X-ray luminous active galactic nuclei (AGNs) in excess to what is observed in the field population. If preprocessing is under way in the Cl0023 system, our observations suggest that powerful nuclear activity is not the predominant mechanism quenching star formation and driving the evolution of Cl0023 galaxies. We speculate that this is due to a lack of sufficiently massive nuclear black holes required to power such activity, as previous observations have found a high late-type fraction among the Cl0023 population. It may be that disruptive AGN-driven outflows become an important factor in the preprocessing of galaxy populations only during a later stage in the evolution of such groups and structures when sufficiently massive galaxies (and central black holes) have built up, but prior to hydrodynamical processes stripping them of their gas reservoirs.", "date": "2009-09-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "703", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L33-L36", "id_number": "CaltechAUTHORS:20091001-145047971", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091001-145047971", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Chandra General Observing Program", "grant_number": "G07-8126X" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/703/1/L33", "primary_object": { "basename": "Kocevski2009p5942Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/04v0c-0sm89/files/Kocevski2009p5942Astrophys_J_Lett.pdf" }, "pub_year": "2009", "author_list": "Kocevski, Dale D.; Lubin, Lori M.; et el." }, { "id": "https://authors.library.caltech.edu/records/2b0j1-7ra90", "eprint_id": 16283, "eprint_status": "archive", "datestamp": "2023-08-21 22:12:25", "lastmod": "2023-10-19 22:04:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jouvel-S", "name": { "family": "Jouvel", "given": "S." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Bernstein-G-M", "name": { "family": "Bernstein", "given": "G." } }, { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "S." } }, { "id": "Dahlen-T", "name": { "family": "Dahlen", "given": "T." } }, { "id": "Ealet-A", "name": { "family": "Ealet", "given": "A." } }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "B." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Designing future dark energy space missions. I. Building realistic galaxy spectro-photometric catalogs and their first applications", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; surveys; catalogs; techniques: miscellaneous", "note": "\u00a9 ESO 2009.\nReceived 5 February 2009. Accepted 23 June 2009.\nWe acknowledge useful discussions with members of the\nCOSMOS and SNAP collaborations. Stephanie Jouvel thanks CNES and\nCNRS for her Ph.D. studentship. Jean-Paul Kneib thanks CNRS for support.\nGary Bernstein is supported by grant AST-0607667 from the National\nScience Foundation, Department of Energy grant DOE-DE-FG02-95ER40893,\nand NASA grant BEFS-04-0014-0018.\n\nPublished - Jouvel2009p6057Astron_Astrophys.pdf
", "abstract": "Context. Future dark energy space missions such as JDEM and EUCLID are being designed to survey the galaxy population to trace the geometry of the universe and the growth of structure, which both depend on the cosmological model. To reach the goal of high precision cosmology they need to evaluate the capabilities of different instrument designs based on realistic mock catalogs of the galaxy distribution. \n\nAims. The aim of this paper is to construct realistic and flexible mock catalogs based on our knowledge of galaxy populations from current deep surveys. We explore two categories of mock catalogs: (i) based on luminosity functions that we fit to observations (GOODS, UDF, COSMOS, VVDS); (ii) based on the observed COSMOS galaxy distribution. \n\nMethods. The COSMOS mock catalog benefits from all the properties of the data-rich COSMOS survey and the highly accurate photometric redshift distribution based on 30-band photometry. Nevertheless this catalog is limited by the depth of the COSMOS survey. Thus, we also evaluate a mock galaxy catalog generated from luminosity functions using the Le Phare software. For these two catalogs, we have produced simulated number counts in several bands, color diagrams and redshift distributions for validation against real observational data.\n\nResults. Using these mock catalogs we derive some basic requirements to help design future Dark Energy missions in terms of the number of galaxies available for the weak-lensing analysis as a function of the PSF size and depth of the survey. We also compute the spectroscopic success rate for future spectroscopic redshift surveys (i) aiming at measuring BAO in the case of the wide field spectroscopic redshift survey, and (ii) for the photometric redshift calibration survey which is required to achieve weak lensing tomography with great accuracy. In particular, we demonstrate that for the photometric redshift calibration, using only NIR (1\u20131.7 \u00b5m) spectroscopy, we cannot achieve a complete spectroscopic survey down to the limit of the photometric survey (I < 25.5). Extending the wavelength coverage of the spectroscopic survey to cover 0.6\u20131.7 \u00b5m will then improve the fraction of very secure spectroscopic redshifts to nearly 80% of the galaxies, making possible a very accurate photometric redshift calibration. \n\nConclusions. We have produced two realistic mock galaxy catalogs that can be used in determining the best survey strategy for future dark-energy missions in terms of photometric redshift accuracy and spectroscopic redshift surveys yield. These catalogues are publicly accessible at http://lamwws.oamp.fr/cosmowiki/RealisticSpectroPhotCat, or \nat the CDS.", "date": "2009-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "504", "number": "2", "publisher": "EDP Sciences", "pagerange": "359-371", "id_number": "CaltechAUTHORS:20091012-152454346", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091012-152454346", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "NSF", "grant_number": "AST-0607667" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-95ER40893" }, { "agency": "NASA", "grant_number": "BEFS-04-0014-0018" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/200911798", "primary_object": { "basename": "Jouvel2009p6057Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/2b0j1-7ra90/files/Jouvel2009p6057Astron_Astrophys.pdf" }, "pub_year": "2009", "author_list": "Jouvel, S.; Kneib, J.-P.; et el." }, { "id": "https://authors.library.caltech.edu/records/6jh6h-w4a05", "eprint_id": 16182, "eprint_status": "archive", "datestamp": "2023-08-21 22:12:12", "lastmod": "2023-10-19 22:00:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "Francesca" }, "orcid": "0000-0002-2115-1137" }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "Cristian" }, "orcid": "0000-0002-8853-9611" }, { "id": "Puccetti-S", "name": { "family": "Puccetti", "given": "Simonetta" }, "orcid": "0000-0002-2734-7835" }, { "id": "Fiore-F", "name": { "family": "Fiore", "given": "Fabrizio" } }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "Nico" } }, { "id": "Aldcroft-T-L", "name": { "family": "Aldcroft", "given": "T. L." } }, { "id": "Fruscione-A", "name": { "family": "Fruscione", "given": "Antonella" } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "Andrea" }, "orcid": "0000-0003-3451-9970" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "Marcella" }, "orcid": "0000-0002-5059-6848" }, { "id": "Gilli-R", "name": { "family": "Gilli", "given": "Roberto" } }, { "id": "Miyaji-Takamitsu", "name": { "family": "Miyaji", "given": "Takamitsu" } }, { "id": "Damiani-F", "name": { "family": "Damiani", "given": "Francesco" } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "Alexis" }, "orcid": "0000-0002-4606-5403" }, { "id": "Brunner-H", "name": { "family": "Brunner", "given": "Hermann" } }, { "id": "Urry-C-M", "name": { "family": "Urry", "given": "C. M." }, "orcid": "0000-0002-0745-9792" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "John" }, "orcid": "0000-0002-0000-6977" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "Vincenzo" } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "Guenther" }, "orcid": "0000-0002-0797-0646" }, { "id": "Griffiths-R-E", "name": { "family": "Griffiths", "given": "Richard" } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "Marcella C." }, "orcid": "0000-0003-1624-7609" }, { "id": "Hao-Heng", "name": { "family": "Hao", "given": "Heng" } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "Luigi" } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew" }, "orcid": "0000-0001-7489-5167" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Ettori-Stefano", "name": { "family": "Ettori", "given": "Stefano" }, "orcid": "0000-0003-4117-8617" }, { "id": "Fabbiano-G", "name": { "family": "Fabbiano", "given": "Giuseppina" }, "orcid": "0000-0002-3554-3318" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "Chris" } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "Simon" }, "orcid": "0000-0002-6423-3597" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Rich-Michael-R", "name": { "family": "Rich", "given": "Michael" } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "Patrick" } }, { "id": "Taylor-J-E", "name": { "family": "Taylor", "given": "James E." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Yoshiaki" }, "orcid": "0000-0003-2247-3741" }, { "id": "Volonteri-M", "name": { "family": "Volonteri", "given": "Marta" }, "orcid": "0000-0002-3216-1322" } ] }, "title": "The Chandra COSMOS Survey. I. Overview and Point Source Catalog", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; cosmology: observations; galaxies: evolution; quasars: general; surveys; X-rays: general", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2008 November 4, accepted for publication 2009. July 29. Published 2009 August 27. \n\nWe thank the Chandra mission planning team, especially Pat Slane and Jan Vrtilek, and the Chandra pipeline data processing team for the extraordinary efforts they put into the successful scheduling and execution of C-COSMOS. We also thank the rest of COSMOS team whose support has been invaluable in reaching this stage. We thank Bin Luo for sensitivity curves of Chandra Deep Fields. We gratefully thank the Chandra EPO team, in particular Eli Bressert, for creating the true color X-ray image. This research has made use of data obtained from the Chandra Data Archive and software provided by the Chandra X-ray Center (CXC) in the application packages CIAO and Sherpa.\nThis work was supported in part by NASA Chandra grant number GO7-8136A (M.E., C.V., M.B., A.F.), NASA contract NAS8-39073 (Chandra X-ray Center), and by NASA/ADP grant NNX07AT02G (TM at UCSD). In Italy this work is supported by ASI/INAF contracts I/023/05/0, I/024/05/0 and I/088/06, by PRIN/MUR grant 2006-02-5203. In Germany this project is supported by the Bundesministerium f\u00fcr Bildung und Forschung/Deutsches Zentrum f\u00fcr Luft und Raumfahrt and the Max Planck Society.\n\nPublished - Elvis2009p5930Astrophys_J_Suppl_S.pdf
", "abstract": "The Chandra COSMOS Survey (C-COSMOS) is a large, 1.8 Ms, Chandra program that has imaged the central 0.5 deg^2 of the COSMOS field (centered at 10 ^h , +02 ^o ) with an effective exposure of ~160 ks, and an outer 0.4 deg^2 area with an effective exposure of ~80 ks. The limiting source detection depths are 1.9 \u00d7 10^(\u201316) erg cm^(\u20132) s^(\u20131) in the soft (0.5-2 keV) band, 7.3 \u00d7 10^(\u201316) erg cm^(\u20132) s^(\u20131) in the hard (2-10 keV) band, and 5.7 \u00d7 10^(\u201316) erg cm^(\u20132) s^(\u20131) in the full (0.5-10 keV) band. Here we describe the strategy, design, and execution of the C-COSMOS survey, and present the catalog of 1761 point sources detected at a probability of being spurious of <2 \u00d7 10^(\u20135) (1655 in the full, 1340 in the soft, and 1017 in the hard bands). By using a grid of 36 heavily (~50%) overlapping pointing positions with the ACIS-I imager, a remarkably uniform (\u00b112%) exposure across the inner 0.5 deg^2 field was obtained, leading to a sharply defined lower flux limit. The widely different point-spread functions obtained in each exposure at each point in the field required a novel source detection method, because of the overlapping tiling strategy, which is described in a companion paper. This method produced reliable sources down to a 7-12 counts, as verified by the resulting logN-logS curve, with subarcsecond positions, enabling optical and infrared identifications of virtually all sources, as reported in a second companion paper. The full catalog is described here in detail and is available online.", "date": "2009-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "184", "number": "1", "publisher": "American Astronomical Society", "pagerange": "158-171", "id_number": "CaltechAUTHORS:20091006-105300882", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091006-105300882", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO7-8136A" }, { "agency": "NASA", "grant_number": "NAS8-39073" }, { "agency": "NASA", "grant_number": "NNX07AT02G" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/023/05/0" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/024/05/0" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/088/06" }, { "agency": "Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)", "grant_number": "2006-02-5203" }, { "agency": "Bundesministerium f\u00fcr Bildung und Forschung (BMBF)" }, { "agency": "Max Planck Society" }, { "agency": "Deutsches Zentrum f\u00fcr Luft und Raumfahrt (DLR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0067-0049/184/1/158", "primary_object": { "basename": "Elvis2009p5930Astrophys_J_Suppl_S.pdf", "url": "https://authors.library.caltech.edu/records/6jh6h-w4a05/files/Elvis2009p5930Astrophys_J_Suppl_S.pdf" }, "pub_year": "2009", "author_list": "Elvis, Martin; Civano, Francesca; et el." }, { "id": "https://authors.library.caltech.edu/records/yzd9r-tq959", "eprint_id": 15495, "eprint_status": "archive", "datestamp": "2023-08-21 22:06:57", "lastmod": "2023-10-19 14:30:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S. S." } }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "T." }, "orcid": "0000-0002-7402-5441" }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Saito-T", "name": { "family": "Saito", "given": "T." } }, { "id": "Ideue-Y", "name": { "family": "Ideue", "given": "Y." } }, { "id": "Nakajima-A", "name": { "family": "Nakajima", "given": "A." } }, { "id": "Matsuoka-Kenta", "name": { "family": "Matsuoka", "given": "K." }, "orcid": "0000-0002-2689-4634" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C." }, "orcid": "0000-0001-6647-3861" }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C. D." } }, { "id": "Kitzbichler-M-G", "name": { "family": "Kitzbichler", "given": "M. G." } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Tribiano-S", "name": { "family": "Tribiano", "given": "S." } }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J. R." } } ] }, "title": "Hubble Space Telescope/Advanced Camera for Surveys Morphology of Ly\u03b1 Emitters at Redshift 5.7 in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; early universe; galaxies: evolution; galaxies: formation; galaxies: high-redshift", "note": "\u00a9 2009 American Astronomical Society.\n\nPrint publication: Issue 2 (2009 August 20); received 2008 November 3, accepted for publication 2009 June 15; published 2009 July 28.\n\nWe thank both the Subaru and HST staff for their invaluable help, and all members of the COSMOS team.We also thank the anonymous referee for his/her useful comments. This work was in part financially supported by JSPS (15340059 and 17253001).\n\nPublished - Taniguchi2009p5715Astrophys_J.pdf
", "abstract": "We present detailed morphological properties of Ly\u03b1 emitters (LAEs) at z \u2248 5.7 in the COSMOS field based on Hubble Space Telescope Advanced Camera for Surveys (ACS) data. The ACS imaging in the F814W filter covered 85 LAEs of the 119 LAEs identified in the full two square degree field, and 47 LAEs of them are detected in the ACS images. Nearly half of them are spatially extended with a size larger than 0.15 arcsec (~0.88 kpc at z = 5.7) and up to 0.4 arcsec (~2.5 kpc at z = 5.7). The others are nearly unresolved compact objects. Two LAEs show double-component structures indicating interaction or merging of building components to form more massive galaxies. By stacking the ACS images of all the detected sources, we obtain a Sersic parameter of n ~ 0.7 with a half-light radius of 0.13 arcsec (0.76 kpc), suggesting that the majority of ACS detected LAEs have not spheroidal-like but disk-like or irregular light profiles. Comparing ACS F814W magnitudes (I _(814)) with Subaru/Suprime-Cam magnitudes in the NB816, i', and z' bands, we find that the ACS imaging in the F814W band mainly probes UV continuum rather than Ly\u03b1 line emission. UV continuum sizes tend to be larger for LAEs with larger Ly\u03b1 emission regions as traced by the NB816 imaging. The nondetection of 38 LAEs in the ACS images is likely due to the fact that their surface brightness is too low both in the UV continuum and Ly\u03b1 emission. Estimating I_(814) for the ACS-undetected LAEs from the z' and NB816 magnitudes, we find that 16 of these are probably LAEs with a size larger than 0.15 arcsec in UV continuum. All these results suggest that our LAE sample contains systematically larger LAEs in UV continuum size than those previously studied at z ~ 6.", "date": "2009-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "701", "number": "2", "publisher": "American Astronomical Society", "pagerange": "915-944", "id_number": "CaltechAUTHORS:20090831-141027603", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090831-141027603", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15340059" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17253001" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/701/2/915", "primary_object": { "basename": "Taniguchi2009p5715Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/yzd9r-tq959/files/Taniguchi2009p5715Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Taniguchi, Y.; Murayama, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/fdfem-1vk32", "eprint_id": 15176, "eprint_status": "archive", "datestamp": "2023-08-21 21:59:56", "lastmod": "2023-10-18 21:03:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ideue-Y", "name": { "family": "Ideue", "given": "Y." } }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "T." }, "orcid": "0000-0002-7402-5441" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Saito-T", "name": { "family": "Saito", "given": "T." } }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S." } }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J. R." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Environmental Effects on the Star Formation Activity in Galaxies at z \u2243 1.2 in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: interactions", "note": "\u00a9 2009. The American Astronomical Society. \n\nPrint publication: Issue 2 (2009 August 1) Received 2008 December 2; accepted for publication 2009 May 25; published 2009 July 7. \n\nWe would like to thank both the Subaru and HST staff for their invaluable help and acknowledge the anonymous referee for an extremely useful report. This work was financially supported in part by the Ministry of Education, Culture, Sports, Science, and Technology (nos. 10044052 and 10304013) and by JSPS (nos. 15340059, 17253001, and 19340046).\n\nPublished - Ideue2009p5228Astrophys_J.pdf
", "abstract": "We investigate the relation between the star formation activity in galaxies and environment at z \u2243 1.2 in the Cosmic Evolution Survey field, using the fraction of [O II] emitters and the local galaxy density. The fraction of [O II] emitters appears to be almost constant over the surface density of galaxies between 0.2 and 10 Mpc^(\u20132). This trend is different from that seen in the local universe where the star formation activity is weaker in higher density regions. To understand this difference between z ~ 1 and z ~ 0, we study the fraction of non-isolated galaxies as a function of local galaxy density. We find that the fraction of non-isolated galaxies increases with increasing density. Our results suggest that the star formation in galaxies at z ~ 1 is triggered by galaxy interaction and/or mergers.", "date": "2009-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "700", "number": "2", "publisher": "American Astronomical Society", "pagerange": "971-976", "id_number": "CaltechAUTHORS:20090819-140756941", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090819-140756941", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Education, Culture, Sports, Science, and Technology (MEXT)", "grant_number": "10044052" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15340059" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "10304013" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17253001" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19340046" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/700/2/971", "primary_object": { "basename": "Ideue2009p5228Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/fdfem-1vk32/files/Ideue2009p5228Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Ideue, Y.; Nagao, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/8gs1w-7ja52", "eprint_id": 15686, "eprint_status": "archive", "datestamp": "2023-08-21 21:40:02", "lastmod": "2023-10-19 14:43:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pannella-M", "name": { "family": "Pannella", "given": "M." } }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Owen-F-N", "name": { "family": "Owen", "given": "F. N." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Strazzullo-V", "name": { "family": "Strazzullo", "given": "V." } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J. P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Mellier-Y", "name": { "family": "Mellier", "given": "Y." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } }, { "id": "Willott-C-J", "name": { "family": "Willott", "given": "C. J." }, "orcid": "0000-0002-4201-7367" } ] }, "title": "Star Formation and Dust Obscuration at z \u2248 2: Galaxies at the Dawn of Downsizing", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: fundamental parameters; galaxies: ISM; galaxies: luminosity function, mass function; galaxies: statistics; surveys", "note": "\u00a9 2009 The American Astronomical Society.\nReceived 2009 February 27; accepted 2009 May 8; published 2009 June 1.\nWe thank the anonymous referee for constructive comments\nthat improved the presentation of our results. M.P., V.S.,\nand C.L.C. acknowledge partial support from the Max-Planck\nForschungspreise 2005. E.D. and H.J.Mc.C. acknowledge support\nfrom the French grants ANR-07-BLAN-0228-03 and ANR-\n08-JCJC-0008. A.R. acknowledges support from the ASI grant\nCOFIS. F. C. acknowledges support from NASA-Chandra grant\nG07-8136A. This work is based in part on data products produced\nat TERAPIX. The HST COSMOS Treasury program\nwas supported through NASA grant HST-GO-09822.We gratefully\nacknowledge the contributions of the entire COSMOS\ncollaboration. \n\nBased on observations collected, within the COSMOS Legacy Survey, at the\nHST, Chandra, XMM, Keck, NRAO-VLA, Subaru, KPNO, CTIO, CFHT, and\nESO observatories. The National Radio Astronomy Observatory is a facility of\nthe National Science Foundation operated under cooperative agreement by\nAssociated Universities, Inc.\n\nPublished - Pannella2009p4792Astrophys_J_Lett.pdf
", "abstract": "We present first results of a study aimed to constrain the star formation rate (SFR) and dust content of galaxies at z \u2248 2. We use a sample of BzK-selected star-forming galaxies, drawn from the Cosmic Evolution Survey, to perform a stacking analysis of their 1.4 GHz radio continuum as a function of different stellar population properties, after cleaning the sample from contamination by active galactic nuclei. Dust unbiased SFRs are derived from radio fluxes assuming the local radio-IR correlation. The main results of this work are: (1) specific star formation rate (SSFR)s are constant over about 1 dex in stellar mass and up to the highest stellar mass probed, (2) the dust attenuation is a strong function of galaxy stellar mass with more massive galaxies being more obscured than lower mass objects, (3) a single value of the UV extinction applied to all galaxies would lead to a gross underestimate of the SFR in massive galaxies, (4) correcting the observed UV luminosities for dust attenuation based on the Calzetti recipe provides results in very good agreement with the radio derived ones, (5) the mean SSFR of our sample steadily decreases by a factor of ~4 with decreasing redshift from z = 2.3 to 1.4 and a factor of ~40 down the local universe. These empirical SFRs would cause galaxies to dramatically overgrow in mass if maintained all the way to low redshifts; we suggest that this does not happen because star formation is progressively quenched, likely starting from the most massive galaxies.", "date": "2009-06-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "698", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L116-L120", "id_number": "CaltechAUTHORS:20090909-091902540", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090909-091902540", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Max-Planck Forschungspreise" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-07-BLAN-0228-03" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-08-JCJC-0008" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "NASA", "grant_number": "G07-8136A" }, { "agency": "NASA", "grant_number": "HST-GO-09822" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/698/2/L116", "primary_object": { "basename": "Pannella2009p4792Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/8gs1w-7ja52/files/Pannella2009p4792Astrophys_J_Lett.pdf" }, "pub_year": "2009", "author_list": "Pannella, M.; Carilli, C. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/1fn5m-06447", "eprint_id": 15425, "eprint_status": "archive", "datestamp": "2023-08-21 21:36:12", "lastmod": "2023-10-18 21:46:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Henry-A-L", "name": { "family": "Henry", "given": "Alaina L." }, "orcid": "0000-0002-6586-4446" }, { "id": "Siana-Brian-D", "name": { "family": "Siana", "given": "Brian" }, "orcid": "0000-0002-4935-9511" }, { "id": "Malkan-M-A", "name": { "family": "Malkan", "given": "Matthew A." }, "orcid": "0000-0001-6919-1237" }, { "id": "Ashby-M-L-N", "name": { "family": "Ashby", "given": "Matthew L. N." }, "orcid": "0000-0002-3993-0745" }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "Carrie R." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "Ranga-Ram" }, "orcid": "0000-0001-7583-0621" }, { "id": "Colbert-J-W", "name": { "family": "Colbert", "given": "James W." } }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "Mauro" }, "orcid": "0000-0002-7831-8751" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "Harry I." }, "orcid": "0000-0002-7064-5424" }, { "id": "McCarthy-P-J", "name": { "family": "McCarthy", "given": "Patrick J." } } ] }, "title": "Expanding the Search for Galaxies at z ~ 7-10 with New NICMOS Parallel Fields", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift", "note": "\u00a9 2009. The American Astronomical Society. \n\nReceived 2008 December 15; accepted 2009 March 19; published 2009 May 8. \n\nThis work is funded in part by the University of California\nPresident's DissertationYear Fellowship. Observations reported\nhere were obtained at the MMT Observatory, a joint facility\nof the Smithsonian Institution and the University of Arizona.\nThe authors thank S. Furlanetto for helpful discussions, and\nK. Kornei and R. Bouwens for comments that improved this\nmanuscript.\n\nPublished - Henry2009p4283Astrophys_J.pdf
", "abstract": "We have carried out a search for galaxies at z ~ 7-10 in ~14.4 arcmin^2 of new NICMOS parallel imaging taken in the Great Observatories Origins Deep Survey (5.9 arcmin^2), the Cosmic Origins Survey (7.2 arcmin^2), and SSA22 (1.3 arcmin^2). These images reach 5\u03c3 sensitivities of J_(110) = 26.0-27.5 (AB), and combined they increase the amount of deep near-infrared data by more than 60% in fields where the investment in deep optical data has already been made. We find no z > 7 candidates in our survey area, consistent with the Bouwens et al. measurements at z ~ 7 and 9 (over 23 arcmin^2), which predict 0.7 galaxies at z ~ 7 and <0.03 galaxies at z ~ 9. We estimate that 10%-20% of z > 7 galaxies are missed by this survey, due to incompleteness from foreground contamination by faint sources. For the case of luminosity evolution, assuming a Schecter parameterization with a typical \u03a6_* = 10^(\u20133) Mpc^(\u20133), we find M^*> \u2013 20.0 for z ~ 7 and M^*> \u2013 20.7 for z ~ 9 (68% confidence). This suggests that the downward luminosity evolution of Lyman break galaxies continues to z ~ 7, although our result is marginally consistent with the z ~ 6 luminosity function of Bouwens et al. In addition, we present newly acquired deep MMT/Megacam imaging of the z ~ 9 candidate JD2325+1433, first presented in Henry et al. The resulting weak but significant detection at i' indicates that this galaxy is most likely an interloper at z ~ 2.7.", "date": "2009-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "697", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1128-1137", "id_number": "CaltechAUTHORS:20090828-145425289", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090828-145425289", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "University of California" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/697/2/1128", "primary_object": { "basename": "Henry2009p4283Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/1fn5m-06447/files/Henry2009p4283Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Henry, Alaina L.; Siana, Brian; et el." }, { "id": "https://authors.library.caltech.edu/records/1gkx5-ae392", "eprint_id": 14771, "eprint_status": "archive", "datestamp": "2023-08-21 21:31:10", "lastmod": "2023-10-18 19:52:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lubin-L-M", "name": { "family": "Lubin", "given": "L. M." } }, { "id": "Gal-R-R", "name": { "family": "Gal", "given": "R. R." } }, { "id": "Lemaux-B-C", "name": { "family": "Lemaux", "given": "B. C." }, "orcid": "0000-0002-1428-7036" }, { "id": "Kocevski-D-D", "name": { "family": "Kocevski", "given": "D. D." } }, { "id": "Squires-G-K", "name": { "family": "Squires", "given": "G. K." }, "orcid": "0000-0002-1977-5717" } ] }, "title": "The Observations of Redshift Evolution in Large-Scale Environments (ORELSE) Survey. I. The Survey Design and First Results on CL 0023+0423 at z = 0.84 and RX J1821.6+6827 at z = 0.82", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: clusters: general; large-scale structure of universe; surveys", "note": "\u00a9 2009 The American Astronomical Society.\nReceived 2008 August 26; accepted 2009 March 29; published 2009 April 29.\nWe thank the anonymous referee for very constructive comments\non this manuscript. This material is based upon work supported\nby the National Aeronautics and Space Administration\nunder Award NNG05GC34ZG for the Long Term Space Astrophysics\nProgram. The spectrographic data presented herein\nwere obtained at the W. M. Keck Observatory, which is operated\nas a scientific partnership among the California Institute\nof Technology, the University of California, and the National\nAeronautics and Space Administration. The Observatory was\nmade possible by the generous financial support of the W. M.\nKeck Foundation. The authors recognize and acknowledge the\nvery significant cultural role and reverence that the summit of\nMauna Kea has always had within the indigenous Hawaiian\ncommunity. We are most fortunate to have the opportunity to\nconduct observations from this mountain. The observing staff,\ntelescope operators, and instrument scientists at Keck provided\na great deal of assistance.\n\nPublished - Lubin2009p4459Astron_J.pdf
", "abstract": "We present the Observations of Redshift Evolution in Large-Scale Environments (ORELSE) Survey, a systematic search for structure on scales greater than 10 h^(\u20131)_70 Mpc around 20 well-known clusters at redshifts of 0.6 < z < 1.3. The goal of the survey is to examine a statistical sample of dynamically active clusters and large-scale structures in order to quantify galaxy properties over the full range of local and global environments. We describe the survey design, the cluster sample, and our extensive observational data covering at least 25' around each target cluster. We use adaptively smoothed red galaxy density maps from our wide-field optical imaging to identify candidate groups/clusters and intermediate-density large-scale filaments/walls in each cluster field. Because photometric techniques (such as photometric redshifts, statistical overdensities, and richness estimates) can be highly uncertain, the crucial component of this survey is the unprecedented amount of spectroscopic coverage. We are using the wide-field, multiobject spectroscopic capabilities of the Deep Multiobject Imaging Spectrograph to obtain 100-200+ confirmed cluster members in each field. Our survey has already discovered the Cl 1604 supercluster at z \u2248 0.9, a structure which contains at least eight groups and clusters and spans 13 Mpc \u00d7 100 Mpc. Here, we present the results on the large-scale environments of two additional clusters, Cl 0023+0423 at z = 0.84 and RX J1821.6+6827 at z = 0.82, which highlight the diversity of global properties at these redshifts. The optically selected Cl 0023+0423 is a four-way group-group merger with constituent groups having measured velocity dispersions between 206 and 479 km s^\u20131. The galaxy population is dominated by blue, star-forming galaxies, with 80% of the confirmed members showing [O II] emission. The strength of the H\u03b4 line in a composite spectrum of 138 members indicates a substantial contribution from recent starbursts to the overall galaxy population. In contrast, the X-ray-selected RX J1821.6+6827 is a largely isolated, massive cluster with a measured velocity dispersion of 926 \u00b1 77 km s^(\u20131). The cluster exhibits a well-defined red sequence with a large quiescent galaxy population. The results from these two targets, along with preliminary findings on other ORELSE clusters, suggest that optical selection may be more effective than X-ray surveys at detecting less-evolved, dynamically active systems at these redshifts.", "date": "2009-06", "date_type": "published", "publication": "Astronomical Journal", "volume": "137", "number": "6", "publisher": "American Astronomical Society", "pagerange": "4867-4883", "id_number": "CaltechAUTHORS:20090803-135140038", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090803-135140038", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG05GC34ZG" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-6256/137/6/4867", "primary_object": { "basename": "Lubin2009p4459Astron_J.pdf", "url": "https://authors.library.caltech.edu/records/1gkx5-ae392/files/Lubin2009p4459Astron_J.pdf" }, "pub_year": "2009", "author_list": "Lubin, L. M.; Gal, R. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/v9hsr-35n17", "eprint_id": 15482, "eprint_status": "archive", "datestamp": "2023-08-21 21:26:18", "lastmod": "2023-10-19 14:30:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Trump-J-R", "name": { "family": "Trump", "given": "Jonathan R." } }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "Chris D." } }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "id": "McCarthy-P-J", "name": { "family": "McCarthy", "given": "Patrick J." } }, { "id": "Huchra-J-P", "name": { "family": "Huchra", "given": "John P." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "Marcella" }, "orcid": "0000-0002-5059-6848" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "Nico" } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "Francesca" }, "orcid": "0000-0002-2115-1137" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "Andrea" }, "orcid": "0000-0003-3451-9970" }, { "id": "Gabor-J-M", "name": { "family": "Gabor", "given": "Jared" } }, { "id": "Hao-Heng", "name": { "family": "Hao", "given": "Heng" } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G\u00fcnther" }, "orcid": "0000-0002-0797-0646" }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "Knud" }, "orcid": "0000-0003-3804-2137" }, { "id": "Kelly-B-C", "name": { "family": "Kelly", "given": "Brandon C." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "Simon J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "Vernesa" }, "orcid": "0000-0002-3893-8614" } ] }, "title": "The COSMOS Active Galactic Nucleus Spectroscopic Survey. I. XMM-Newton Counterparts", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: Seyfert; quasars: general; surveys; X-rays: galaxies", "note": "\u00a9 2009 The American Astronomical Society.\nReceived 2008 June 9; accepted 2009 February 25; published 2009 April 22.\nWe thank the anonymous referee for thorough and helpful\ncomments. We additionally thank A. Dressler and the IMACS\nteam for creating an excellent instrument, as well as telescope\noperators H. Nunez, F. Sanchez, G. Valladares, S. Vera,\nH. Rivera, and the Las Campanas Observatory staff for support\nwhile observing. We thank M. Westover, A. Coil, S. Burles,\nand the Carnegie queue mode scientists for help with some of\nthe IMACS observations. We thank D. Fabricant for designing\nthe excellent instrument Hectospec and thank MMT operators\nand Hectospec queue mode scientists for their help during observations.\nWe also thank the COSMOS team for their work in\ncreating the catalogs used for selecting our targets. We thank P.\nShopbell, A. Alexov, and the NASA IPAC/IRSA team for assisting\nin uploading the data and catalogs to public IRSA archives.\nObservations reported here were obtained at the Magellan Telescopes,\nwhich are operated by the Carnegie Observatories, as\nwell as the MMT Observatory, a joint facility of the University\nof Arizona and the Smithsonian Institution. The HST COSMOS\nTreasury program was supported through NASA grant\nHST-GO-09822. J.R.T. acknowledges support from an ARCS\nfoundation fellowship.\n\nPublished - Trump2009p2582Astrophys_J.pdf
", "abstract": "We present optical spectroscopy for an X-ray and optical flux-limited sample of 677 XMM-Newton selected targets covering the 2 deg^2 Cosmic Evolution Survey field, with a yield of 485 high-confidence redshifts. The majority of the spectra were obtained over three seasons (2005-2007) with the Inamori Magellan Areal Camera and Spectrograph instrument on the Magellan (Baade) telescope. We also include in the sample previously published Sloan Digital Sky Survey spectra and supplemental observations with MMT/Hectospec. We detail the observations and classification analyses. The survey is 90% complete to flux limits of f_(0.5-10 keV) > 8 \u00d7 10^(\u201316) erg cm^(-2) s^(\u20131) and i^+_(AB) < 22, where over 90% of targets have high-confidence redshifts. Making simple corrections for incompleteness due to redshift and spectral type allows for a description of the complete population to i^+_(AB) < 23. The corrected sample includes a 57% broad emission line (Type 1, unobscured) active galactic nucleus (AGN) at 0.13 < z < 4.26, 25% narrow emission line (Type 2, obscured) AGN at 0.07 < z < 1.29, and 18% absorption line (host-dominated, obscured) AGN at 0 < z < 1.22 (excluding the stars that made up 4% of the X-ray targets). We show that the survey's limits in X-ray and optical fluxes include nearly all X-ray AGNs (defined by L_(0.5-10) keV > 3 \u00d7 10^(42) erg s^(\u20131)) to z < 1, of both optically obscured and unobscured types. We find statistically significant evidence that the obscured-to-unobscured AGN ratio at z < 1 increases with redshift and decreases with luminosity.", "date": "2009-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "696", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1195-1212", "id_number": "CaltechAUTHORS:20090831-104851520", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090831-104851520", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "ARCS Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/696/2/1195", "primary_object": { "basename": "Trump2009p2582Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/v9hsr-35n17/files/Trump2009p2582Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Trump, Jonathan R.; Impey, Chris D.; et el." }, { "id": "https://authors.library.caltech.edu/records/h8dk7-s5y17", "eprint_id": 15531, "eprint_status": "archive", "datestamp": "2023-08-21 21:23:58", "lastmod": "2023-10-19 14:32:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S. S." } }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "T." }, "orcid": "0000-0002-7402-5441" }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Saito-T", "name": { "family": "Saito", "given": "T." } }, { "id": "Ideue-Y", "name": { "family": "Ideue", "given": "Y." } }, { "id": "Nakajima-A", "name": { "family": "Nakajima", "given": "A." } }, { "id": "Matsuoka-Kenta", "name": { "family": "Matsuoka", "given": "K." }, "orcid": "0000-0002-2689-4634" }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Kitzbichler-M-G", "name": { "family": "Kitzbichler", "given": "M. G." } }, { "id": "Impey-C", "name": { "family": "Impey", "given": "C." } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" } ] }, "title": "Photometric Properties of Ly\u03b1 Emitters at z \u2248 4.86 in the COSMOS 2 Square Degree Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: distances and redshifts; galaxies: evolution; galaxies: luminosity function, mass function", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2008 August 8; accepted 2009 February 2; published 2009 April 16. \n\nThe HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We greatly acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. We thank Masami Ouchi for useful discussion and the anonymous referee for valuable comments. We also thank the Subaru Telescope staff for their invaluable help. This work was financially supported in part by the JSPS (Nos. 15340059 and 17253001).\n\nPublished - Shioya2009p2247Astrophys_J.pdf
Erratum - Shioya2009p5115Astrophys_J.pdf
", "abstract": "We present results of a survey for Ly\u03b1 emitters at z \u2248 4.86 based on optical narrowband (\u03bb_c = 7126 \u00c5, \u0394\u03bb = 73 \u00c5) and broadband (B, V, r', i', and z') observations of the Cosmic Evolution Survey field using Suprime-Cam on the Subaru Telescope. We find 79 Ly\u03b1 emitter (LAE) candidates at z \u2248 4.86 over a contiguous survey area of 1.83 deg^2, down to the Ly\u03b1 line flux of 1.47 \u00d7 10^(\u201317) erg s^(-1) cm^(\u20132). We obtain the Ly\u03b1 luminosity function with a best-fit Schechter parameters of log L* = 42.9^(+0.5)_(\u20130.3) erg s^(-1) and \u0424* = 1.2^(+8.0)_(\u20131.1) \u00d7 10^(\u20134) Mpc^(-3) for \u03b1 = \u20131.5 (fixed). The two-point correlation function for our LAE sample is \u03be(r) = (r/4.4^(+5.7)_(\u20132.9) Mpc)^(\u20131.90\u00b10.22). In order to investigate the field-to-field variations of the properties of Ly\u03b1 emitters, we divide the survey area into nine tiles of 0\u00b0.5 \u00d7 0\u00b0.5 each. We find that the number density varies with a factor of \u2243 2 from field to field with high statistical significance. However, we find no significant field-to-field variance when we divide the field into four tiles with 0\u00b0.7 \u00d7 0\u00b0.7 each. We conclude that at least 0.5 deg^2 survey area is required to derive averaged properties of LAEs at z ~ 5, and our survey field is wide enough to overcome the cosmic variance.", "date": "2009-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "696", "number": "1", "publisher": "American Astronomical Society", "pagerange": "546-561", "id_number": "CaltechAUTHORS:20090901-140022019", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090901-140022019", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15340059" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17253001" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/696/1/546", "primary_object": { "basename": "Shioya2009p2247Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/h8dk7-s5y17/files/Shioya2009p2247Astrophys_J.pdf" }, "related_objects": [ { "basename": "Shioya2009p5115Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/h8dk7-s5y17/files/Shioya2009p5115Astrophys_J.pdf" } ], "pub_year": "2009", "author_list": "Shioya, Y.; Taniguchi, Y.; et el." }, { "id": "https://authors.library.caltech.edu/records/r3kqg-jz212", "eprint_id": 15491, "eprint_status": "archive", "datestamp": "2023-08-21 21:23:38", "lastmod": "2023-10-23 16:06:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Bondi-M", "name": { "family": "Bondi", "given": "M." } }, { "id": "B\u00eerzan-L", "name": { "family": "B\u00eerzan", "given": "L." } }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Ciliegi-P", "name": { "family": "Ciliegi", "given": "P." } }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C. D." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Merloni-A", "name": { "family": "Merloni", "given": "A." } }, { "id": "Paglione-T", "name": { "family": "Paglione", "given": "T." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J. R." } } ] }, "title": "Cosmic Evolution of Radio Selected Active Galactic Nuclei in the Cosmos Field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: evolution; galaxies: fundamental parameters; radio continuum: galaxies", "note": "\u00a9 2009 The American Astronomical Society.\nReceived 2008 September 25; accepted 2009 January 21; \npublished 2009 April 13.\nThe authors are grateful to P. N. Best for especially deriving\nthe SDSS/NVSS radio source fractions as a function of\nstellar mass with a radio luminosity cut that matches the VLA\u2013\nCOSMOS survey data. C.C. acknowledges support from the\nMax-Planck Society and the Alexander von Humboldt Foundation\nthrough the Max-Planck-Forschungspreis 2005. G.Z.\nand S.B. acknowledge support from an INAF contract PRIN-\n2006/1.06.10.08 and an ASI grant ASI/COFIS I/026/07/0. TP\nacknowledges support from PSC-CUNY grant no. 69612-00 38.\n\nERRATUM: \"Cosmic Evolution of Radio Selected Active Galactic Nuclei in the COSMOS Field\" (2009, ApJ, 696, 24)\nV. Smol\u010di\u0107, G. Zamorani, E. Schinnerer, S. Bardelli, M. Bondi, L. B\u00eerzan, C. L. Carilli, P. Ciliegi, M. Elvis, C. D. Impey, A. M. Koekemoer, A. Merloni, T. Paglione, M. Salvato, M. Scodeggio, N. Scoville, and J. R. Trump.\ndoi: 10.1088/0004-637X/708/1/909\n\nThe scale of the volume-averaged heating rate for the VLA-COSMOS AGN, presented in Figure 14 of the paper, requires a systematic (positive) correction due to a bug in the code used to produce this plot. The modified figure is shown below. We would like to note that the applied correction does not alter any results presented in the paper, but only strengthens the agreement between the observations and the Croton et al. (2006) cosmological model in terms of the relevance of radio mode AGN feedback in the process of massive galaxy formation.\n\nPublished 2009 December 15\n\nPublished - Smolcic2009p2253Astrophys_J.pdf
Erratum - Smolcic2010p6760Astrophys_J.pdf
", "abstract": "We explore the cosmic evolution of radio luminous active galactic nuclei (AGNs) with low radio powers (L_(1.4 GHz) \u227e 5 \u00d7 10^(25) W Hz^(\u20131)) out to z = 1.3 using to date the largest sample of ~600 low-luminosity radio AGN at intermediate redshift drawn from the VLA-COSMOS survey. We derive the radio-luminosity function for these AGNs, and its evolution with cosmic time assuming two extreme cases: (1) pure luminosity and (2) pure density evolution. The former and latter yield L_* \u03b1 (1 + z)^(0.8 \u00b1 0.1), and \u03a6_* \u03b1 (1 + z)^(1.1 \u00b1 0.1), respectively, both implying a fairly modest change in properties of low-radio-power AGNs since z = 1.3. We show that this is in stark contrast with the evolution of powerful (L_(1.4 GHz) > 5 \u00d7 10^25 W Hz^(\u20131)) radio AGN over the same cosmic time interval, constrained using the 3CRR, 6CE, and 7CRS radio surveys by Willot et al. We demonstrate that this can be explained through differences in black hole fueling and triggering mechanisms, and a dichotomy in host galaxy properties of weak and powerful AGNs. Our findings suggest that high- and low-radio-power AGN activities are triggered in different stages during the formation of massive red galaxies. We show that weak radio AGN occur in the most massive galaxies already at z ~ 1, and they may significantly contribute to the heating of their surrounding medium and thus inhibit gas accretion onto their host galaxies, as recently suggested for the \"radio mode\" in cosmological models.", "date": "2009-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "696", "number": "1", "publisher": "American Astronomical Society", "pagerange": "24-39", "id_number": "CaltechAUTHORS:20090831-135058590", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090831-135058590", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Max-Planck Society" }, { "agency": "Alexander von Humboldt Foundation" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-2006/1.06.10.08" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFISI/026/07/0" }, { "agency": "PSC-CUNY", "grant_number": "69612-00 38" }, { "agency": "Max-Planck-Forschungspreis" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/696/1/24", "primary_object": { "basename": "Smolcic2009p2253Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/r3kqg-jz212/files/Smolcic2009p2253Astrophys_J.pdf" }, "related_objects": [ { "basename": "Smolcic2010p6760Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/r3kqg-jz212/files/Smolcic2010p6760Astrophys_J.pdf" } ], "pub_year": "2009", "author_list": "Smol\u010di\u0107, V.; Zamorani, G.; et el." }, { "id": "https://authors.library.caltech.edu/records/b15j1-d2637", "eprint_id": 15493, "eprint_status": "archive", "datestamp": "2023-08-21 21:23:49", "lastmod": "2023-10-19 14:30:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "N." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "K." }, "orcid": "0000-0003-3804-2137" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Merloni-A", "name": { "family": "Merloni", "given": "A." } }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Brunner-H", "name": { "family": "Brunner", "given": "H." } }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K." }, "orcid": "0000-0001-8183-1460" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Fiore-F", "name": { "family": "Fiore", "given": "F." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Gilli-R", "name": { "family": "Gilli", "given": "R." } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J.-F." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "Perez-Montero-E", "name": { "family": "Perez Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "C." }, "orcid": "0000-0002-8853-9611" }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "D." } }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "A." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Fumana-Marco", "name": { "family": "Fumana", "given": "M." } }, { "id": "Griffiths-R-E", "name": { "family": "Griffiths", "given": "R." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Memeo-P", "name": { "family": "Memeo", "given": "P." } }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "B." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" } ] }, "title": "Ongoing and Co-Evolving Star Formation in zCOSMOS Galaxies Hosting Active Galactic Nuclei", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: evolution; quasars: emission lines; quasars: general; X-rays: galaxies", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2008 July 15; accepted 2009 January 13; published 2009 April 15. \n\nWe are most grateful to the referee for providing a critical\nreview that significantly improved the paper and to Minjin\nKim for allowing us to use his emission-line measurements\nof SDSS AGNs and fielding subsequent communications. This\nwork is fully based on observations undertaken at the European\nSouthern Observatory (ESO) Very Large Telescope (VLT) under\nthe Large Program 175.A-0839 (PI: S. Lilly).\nFacilities: XMM, VLT:Melipal (VIMOS).\n\nPublished - Silverman2009p2251Astrophys_J.pdf
", "abstract": "We present a study of the host galaxies of active galactic nucleus (AGN) selected from the zCOSMOS survey to establish if accretion onto supermassive black holes (SMBHs) and star formation are explicitly linked up to z ~ 1. We identify 152 galaxies that harbor AGN, based on their X-ray emission (L_(0.5-10 keV) > 10^(42) erg s^(\u20131)) detected by XMM-Newton observations of 7543 galaxies (i_(acs) < 22.5). Star formation rates (SFRs), including those weighted by stellar mass, of a subsample are determined using the [O II]\u03bb3727 emission-line luminosity, corrected for an AGN contribution based on the observed [O III]\u03bb5007 strength or that inferred by their hard (2-10 keV) X-ray luminosity. We find that an overwhelming majority of AGN host galaxies have significant levels of star formation with a distribution spanning ~1-100 M\u2299 yr^(\u20131); their average SFR is higher than that of galaxies with equivalent stellar mass (M_* > 4 \u00d7 10^(10) M\u2299). The close association between AGN activity and star formation is further substantiated by an increase in the fraction of galaxies hosting AGN with the youthfulness of their stars as indicated by the rest-frame color (U\u2013V) and spectral index D_n(4000); we demonstrate that a mass-selected sample is required to alleviate an artificial peak in the AGN fraction falling in the transition region due to the fact that many \"blue cloud\" galaxies have low mass-to-light ratios in luminosity-limited samples. We also find that the SFRs of AGN hosts evolve with cosmic time in a manner that closely mirrors the overall galaxy population and naturally explains the low SFRs in AGNs (z < 0.3) from the SDSS. We conclude that the conditions most conducive for AGN activity are a massive host galaxy and a large reservoir of gas. Furthermore, a direct correlation between mass-accretion rate onto SMBHs and SFR is shown to be weak although the average ratio (~10\u20132) is constant with redshift, effectively shifting the evidence for a co-evolution scenario in a statistical manner to smaller physical scales (i.e., within the same galaxies). The order-of-magnitude increase in this ratio compared to the locally measured value of M_(BH)/M_(bulge) is consistent with an AGN lifetime substantially shorter than that of star formation. Our findings illustrate an intermittent scenario with underlying complexities regarding fueling over vastly different physical (and temporal) scales yet to be firmly determined.", "date": "2009-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "696", "number": "1", "publisher": "American Astronomical Society", "pagerange": "396-410", "id_number": "CaltechAUTHORS:20090831-140313251", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090831-140313251", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/696/1/396", "primary_object": { "basename": "Silverman2009p2251Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/b15j1-d2637/files/Silverman2009p2251Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Silverman, J. D.; Lamareille, F.; et el." }, { "id": "https://authors.library.caltech.edu/records/jtw5s-46z72", "eprint_id": 15349, "eprint_status": "archive", "datestamp": "2023-08-21 21:19:52", "lastmod": "2023-10-18 21:42:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hildebrandt-H", "name": { "family": "Hildebrandt", "given": "H." } }, { "id": "Pielorz-J", "name": { "family": "Pielorz", "given": "J." } }, { "id": "Erben-T", "name": { "family": "Erben", "given": "T." } }, { "id": "van-Waerbeke-L", "name": { "family": "van Waerbeke", "given": "L." } }, { "id": "Simon-P", "name": { "family": "Simon", "given": "P." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" } ] }, "title": "CARS: the CFHTLS-Archive-Research Survey. II. Weighing dark matter halos of Lyman-break galaxies at z = 3\u20135", "ispublished": "pub", "full_text_status": "public", "keywords": "techniques: photometric; galaxies: evolution; galaxies: halos; galaxies: high-redshift", "note": "\u00a9 ESO 2009.\nReceived 26 September 2008. Accepted 18 March 2009.\nWe would like to thank Ryan Quadri for interesting discussions\nabout galaxy clustering measurements that helped to improve the paper.\nMany thanks also to Claudia Maraston and Janine Pforr for help with\ntheir template set. We are grateful to the CFHTLS survey team for conducting\nthe observations and the TERAPIX team for developing software used in this\nstudy. We acknowledge use of the Canadian Astronomy Data Centre operated\nby the Dominion Astrophysical Observatory for the National Research Council\nof Canada's Herzberg Institute of Astrophysics. This work was supported by the\nDFG priority program SPP-1177 \"Witnesses of Cosmic History: formation and\nevolution of black holes, galaxies and their environment\" (project ID ER327/2-\n2), the German Ministry for Science and Education (BMBF) through DESY under\nthe project 05AV5PDA/3 and the TR33 \"The Dark Universe\". H.H. and P.S.\nwere supported by the European DUEL RTN, project MRTN-CT-2006-036133.\nLVW was supported by the Canadian Foundation for Innovation, NSERC and\nCIfAR.\n\nPublished - Hildebrandt2009p4291Astron_Astrophys.pdf
", "abstract": "Aims. We measure the clustering properties for a large samples of u- (z ~ 3), g- (z ~ 4), and r- (z ~ 5) dropouts from the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) Deep fields.\n\nMethods. Photometric redshift distributions along with simulations allow us to de-project the angular correlation measurements and estimate physical quantities such as the correlation length, halo mass, galaxy bias, and halo occupation as a function of UV luminosity.\n\nResults. For the first time we detect a significant one-halo term in the correlation function at z ~ 5 . The comoving correlation lengths and halo masses of LBGs are found to decrease with decreasing rest-frame UV-luminosity. No significant redshift evolution is found in either quantity. The typical halo mass hosting an LBG is M \u2273 10^(12)h^(-1) M\u2299 and the halos are typically occupied by less than one galaxy. Clustering segregation with UV luminosity is clearly observed in the dropout samples, however redshift evolution cannot clearly be disentangled from systematic uncertainties introduced by the redshift distributions. We study a range of possible redshift distributions to illustrate the effect of this choice. Spectroscopy of representative subsamples is required to make high-accuracy absolute measurements of high-z halo masses.", "date": "2009-05", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "498", "number": "3", "publisher": "EDP Sciences", "pagerange": "725-736", "id_number": "CaltechAUTHORS:20090827-094216573", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090827-094216573", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "DFG priority program", "grant_number": "SPP-1177" }, { "agency": "German Ministry for Science and Education (BMBF)", "grant_number": "05AV5PDA/3" }, { "agency": "European DUEL RTN", "grant_number": "MRTN-CT-2006-036133" }, { "agency": "Canadian Foundation for Innovation" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIfAR)" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361/200811042", "primary_object": { "basename": "Hildebrandt2009p4291Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/jtw5s-46z72/files/Hildebrandt2009p4291Astron_Astrophys.pdf" }, "pub_year": "2009", "author_list": "Hildebrandt, H.; Pielorz, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/001gb-mf774", "eprint_id": 15506, "eprint_status": "archive", "datestamp": "2023-08-21 21:15:57", "lastmod": "2023-10-19 14:30:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Luo-Bin", "name": { "family": "Luo", "given": "B." }, "orcid": "0000-0002-9036-0063" }, { "id": "Brandt-W-N", "name": { "family": "Brandt", "given": "W. N." }, "orcid": "0000-0002-0167-2453" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Strateva-I-V", "name": { "family": "Strateva", "given": "I. V." } }, { "id": "Bauer-F-E", "name": { "family": "Bauer", "given": "F. E." }, "orcid": "0000-0002-8686-8737" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Lehmer-B-D", "name": { "family": "Lehmer", "given": "B. D." }, "orcid": "0000-0003-2192-3296" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Szokoly-G-P", "name": { "family": "Szokoly", "given": "G." } }, { "id": "Schneider-D-P", "name": { "family": "Schneider", "given": "D. P." } }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "C." }, "orcid": "0000-0002-8853-9611" } ] }, "title": "Discovery of the Most Distant Double-Peaked Emitter at z = 1.369", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; galaxies: active; galaxies: nuclei; line: profiles; quasars: emission lines", "note": "\u00a9 2009 The American Astronomical Society.\nReceived 2008 October 20; accepted 2009 January 19; published 2009 April 7.\nWe acknowledge financial support from NASA LTSA grant\nNAG5-13035 (B.L., W.N.B.), CXC grant SP8-9003A/B (B.L.,\nW.N.B., F.E.B.), the Polanyi Program of NKTH (G.S.), and the\nItalian Space Agency (contracts ASI\u2013INAF I/023/05/0 and ASI\nI/088/06/0) and PRIN\u2013MIUR grant 2006-02-5203 (C.V.). We\nthank M. Brusa, M. Eracleous, B. P. Miller, J. Wu, and Y. Xue\nfor helpful discussions. We also thank the referee for carefully\nreviewing the manuscript and providing helpful comments.\n\nPublished - Luo2009p2073Astrophys_J.pdf
", "abstract": "We report the discovery of the most distant double-peaked emitter, CXOECDFS J033115.0-275518, at z = 1.369. A Keck/DEIMOS spectrum shows a clearly double-peaked broad Mg II \u03bb2799 emission line, with FWHM \u2248 11,000 km s^(\u20131) for the line complex. The line profile can be well fitted by an elliptical relativistic Keplerian disk model. This is one of a handful of double-peaked emitters known to be a luminous quasar, with excellent multiwavelength coverage and a high-quality X-ray spectrum. CXOECDFS J033115.0-275518 is a radio-loud quasar with two radio lobes (FR II morphology) and a radio loudness of f_(5 GHz)/f_(4400 \u00c5) \u2248 429. The X-ray spectrum can be modeled by a power law with photon index 1.72 and no intrinsic absorption; the rest-frame 0.5-8.0 keV luminosity is 5.0 \u00d7 10^(44) erg s^(\u20131). The spectral energy distribution (SED) of CXOECDFS J033115.0-275518 has a shape typical for radio-loud quasars and double-peaked emitters at lower redshift. The local viscous energy released from the line-emitting region of the accretion disk is probably insufficient to power the observed line flux, and external illumination of the disk appears to be required. The presence of a big blue bump in the SED along with the unexceptional X-ray spectrum suggest that the illumination cannot arise from a radiatively inefficient accretion flow.", "date": "2009-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "695", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1227-1232", "id_number": "CaltechAUTHORS:20090831-154312839", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090831-154312839", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-13035" }, { "agency": "CXC", "grant_number": "SP8-9003A/B" }, { "agency": "Polanyi Program of NKTH" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI-INAF I/023/05/0" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI I/088/06/0" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)", "grant_number": "2006-02-5203" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/695/2/1227", "primary_object": { "basename": "Luo2009p2073Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/001gb-mf774/files/Luo2009p2073Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Luo, B.; Brandt, W. N.; et el." }, { "id": "https://authors.library.caltech.edu/records/j14gv-gfx93", "eprint_id": 15877, "eprint_status": "archive", "datestamp": "2023-08-21 21:13:32", "lastmod": "2023-10-19 17:19:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "N." } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "K." }, "orcid": "0000-0003-3804-2137" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Brunner-H", "name": { "family": "Brunner", "given": "H." } }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K." }, "orcid": "0000-0001-8183-1460" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Fiore-F", "name": { "family": "Fiore", "given": "F." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Gilli-R", "name": { "family": "Gilli", "given": "R." } }, { "id": "Griffiths-R", "name": { "family": "Griffiths", "given": "R." } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J.-F." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Perez-Montero-E", "name": { "family": "Perez Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "C." }, "orcid": "0000-0002-8853-9611" }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "D." } }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "A." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Memeo-P", "name": { "family": "Memeo", "given": "P." } }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "B." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" } ] }, "title": "The Environments of Active Galactic Nuclei within the zCOSMOS Density Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; quasars: general; X-rays: galaxies", "note": "\u00a9 2009 The American Astronomical Society.\n\nReceived 2008 October 24; accepted 2009 January 2; published 2009 March 30.\nWe thank the referee and Paul Martini for constructive\ncomments that significantly improved the paper. This work\nis fully based on observations undertaken at the European\nSouthern Observatory (ESO) Very Large Telescope (VLT) under\nthe Large Program 175.A-0839 (P.I.: Simon Lilly).\nFacilities: XMM, VLT:Melipal (VIMOS).\n\nPublished - Silverman2009p1475Astrophys_J.pdf
", "abstract": "The impact of environment on active galactic nucleus (AGN) activity up to z ~ 1 is assessed by utilizing a mass-selected sample of galaxies from the 10k catalog of the zCOSMOS spectroscopic redshift survey. We identify 147 AGN by their X-ray emission as detected by XMM-Newton from a parent sample of 7234 galaxies. We measure the fraction of galaxies with stellar mass M_* > 2.5 \u00d7 10^(10) M_\u2299 that host an AGN as a function of local overdensity using the 5th, 10th, and 20th nearest neighbors that cover a range of physical scales (~1-4 Mpc). Overall, we find that AGNs prefer to reside in environments equivalent to massive galaxies with substantial levels of star formation. Specifically, AGNs with host masses between 0.25 and 1 \u00d7 10^(11) M_\u2299 span the full range of environments (i.e., field to group) exhibited by galaxies of the same mass and rest-frame color or specific star formation rate. Host galaxies having M_* > 10^(11) M_\u2299 clearly illustrate the association with star formation since they are predominantly bluer than the underlying galaxy population and exhibit a preference for lower-density regions analogous to Sloan Digital Sky Survey studies of narrow-line AGN. To probe the environment on smaller physical scales, we determine the fraction of galaxies (M_* > 2.5 \u00d7 10^(10) M _\u2299) hosting AGNs inside optically selected groups, and find no significant difference with field galaxies. We interpret our results as evidence that AGN activity requires a sufficient fuel supply; the probability of a massive galaxy to have retained some sufficient amount of gas, as evidence by its ongoing star formation, is higher in underdense regions where disruptive processes (i.e., galaxy harassment, tidal stripping) are lessened.", "date": "2009-04-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "695", "number": "1", "publisher": "American Astronomical Society", "pagerange": "171-182", "id_number": "CaltechAUTHORS:20090916-110305188", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090916-110305188", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Southern Observatory", "grant_number": "175. A-0839" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/695/1/171", "primary_object": { "basename": "Silverman2009p1475Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/j14gv-gfx93/files/Silverman2009p1475Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Silverman, J. D.; Kova\u010d, K.; et el." }, { "id": "https://authors.library.caltech.edu/records/hzmvt-r6275", "eprint_id": 15556, "eprint_status": "archive", "datestamp": "2023-08-20 01:25:07", "lastmod": "2023-10-19 14:34:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Huertas-Company-M", "name": { "family": "Huertas-Company", "given": "M." } }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Rouan-D", "name": { "family": "Rouan", "given": "D." } }, { "id": "Pelat-D", "name": { "family": "Pelat", "given": "D." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J. P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Willott-C-J", "name": { "family": "Willott", "given": "C." }, "orcid": "0000-0002-4201-7367" } ] }, "title": "A robust morphological classification of high-redshift galaxies using support vector machines on seeing limited images", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: fundamental parameters - galaxies: high-redshift", "note": "\u00a9 ESO 2009. Received 30 October 2008. Accepted 14 February 2009. The authors want to thank the anonymous referee for his\nuseful suggestions that clearly improved the paper. This work is part of a big collaboration,\nwe would like to thank as well all the people who contributed somehow\nto this paper, specially with the data reduction (H. Aussel, D. Thompson,\nO. Ilbert).\n\nPublished - HuertasCompany2009p2086Astron_Astrophys.pdf
", "abstract": "Context. Morphology is the most accessible tracer of galaxies physical structure, but its interpretation in the framework of galaxy evolution still remains problematic. Its quantification at high redshift requires deep high-angular resolution imaging, which is why space data (HST) are usually employed. At z > 1, the HST visible cameras however probe the UV flux, which is dominated by the emission of young stars, which could bias the estimated morphologies towards late-type systems.\n\nAims. In this paper we quantify the effects of this morphological k-correction at 1 < z < 2 by comparing morphologies measured in the K and I-bands in the COSMOS area. The Ks-band data indeed have the advantage of probing old stellar populations in the rest frame for z < 2, enabling determination of galaxy morphological types unaffected by recent star formation.\n\nMethods. In Paper I we presented a new non-parametric method of quantifying morphologies of galaxies on seeing-limited images based on support vector machines. Here we use this method to classify ~50\u2009000 Ks selected galaxies in the COSMOS area observed with WIRCam at CFHT. We use a 10-dimensional volume, including 5 morphological parameters, and other characteristics of galaxies such as luminosity and redshift. The obtained classification is used to investigate the redshift distributions and number counts per morphological type up to z ~ 2 and to compare them to the results obtained with HST/ACS in the I-band on the same objects. We associate to every galaxy with Ks < 21.5 and z < 2 a probability between 0 and 1 of being late-type or early-type. We use this value to assess the accuracy of our classification as a function of physical parameters of the galaxy and to correct for classification errors.\nResults. The classification is found to be reliable up to z ~ 2. The mean probability is p ~ 0.8. It decreases with redshift and with size, especially for the early-type population, but remains above p ~ 0.7. The classification globally agrees with the one obtained using HST/ACS for z < 1. Above z ~ 1, the I-band classification tends to find less early-type galaxies than the Ks-band one by a factor ~1.5, which might be a consequence of morphological k-correction effects.\n\nConclusions. We argue therefore that studies based on I-band HST/ACS classifications at z > 1 could be underestimating the elliptical population. Using our method in a K_s \u2264 21.5 magnitude-limited sample, we observe that the fraction of the early-type population is (21.9% 8%) at z ~ 1.5-2 and (32.0% 5%) at the present time. We will discuss the evolution of the fraction of galaxies in types from volume-limited samples in a forthcoming paper.", "date": "2009-04-03", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "497", "number": "3", "publisher": "EDP Sciences", "pagerange": "743-753", "id_number": "CaltechAUTHORS:20090902-144412240", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090902-144412240", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/200811255", "primary_object": { "basename": "HuertasCompany2009p2086Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/hzmvt-r6275/files/HuertasCompany2009p2086Astron_Astrophys.pdf" }, "pub_year": "2009", "author_list": "Huertas-Company, M.; Tasca, L.; et el." }, { "id": "https://authors.library.caltech.edu/records/p11zn-d3c41", "eprint_id": 15553, "eprint_status": "archive", "datestamp": "2023-08-21 21:11:19", "lastmod": "2023-10-19 14:34:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M. T." }, "orcid": "0000-0003-1033-9684" }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K." }, "orcid": "0000-0001-8183-1460" }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J. -F." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "Perez-Montero-E", "name": { "family": "Perez Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } }, { "id": "Abbas-U", "name": { "family": "Abbas", "given": "U." } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "D." } }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "A." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Fumana-M", "name": { "family": "Fumana", "given": "M." } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Halliday-C", "name": { "family": "Halliday", "given": "C." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Maccagni-D", "name": { "family": "Maccagni", "given": "D." } }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Memeo-P", "name": { "family": "Memeo", "given": "P." } }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "B." } }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "L." } }, { "id": "Scaramella-R", "name": { "family": "Scaramella", "given": "R." } } ] }, "title": "The Dependence of Star Formation Activity on Stellar Mass Surface Density and Sersic Index in zCOSMOS Galaxies at 0.5 < z < 0.9 Compared with SDSS Galaxies at 0.04 < z < 0.08", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift", "note": "\u00a9 2009 American Astronomical Society.\n\nPrint publication: Issue 2 (2009 April 1); received 2008 July 29; accepted for publication 2009 January 1; published 2009 March 23.\n\nWe would like to thank the anonymous referee for his or her\nsuggestions and comments.We also want to thank M. Ciccolini\nand M. Aller for their help for testing the reliability of COSMOS size measurements. C.M. acknowledges support from the Swiss National Science Foundation. This work has been supported in part by grant ASI/COFIS/WP3110.\n\nPublished - Maier2009p1363Astrophys_J.pdf
", "abstract": "In order to try to understand the internal evolution of galaxies and relate this to the global evolution of the galaxy population, we present a comparative study of the dependence of star formation rates on the average surface mass densities (\u03a3_(M)) of galaxies at 0.5 < z < 0.9 and 0.04 < z < 0.08, using the zCOSMOS and Sloan Digital Sky Survey (SDSS) surveys, respectively. We derive star formation rates, stellar masses, and structural parameters in a consistent way for both samples, and apply them to samples that are complete down to the same stellar mass at both redshifts. We first show that the characteristic step-function dependence of median specific star formation rate (SSFR) on \u03a3_(M) in SDSS, seen by Brinchmann et al., is due to the change over from predominantly disk galaxies to predominantly spheroidal galaxies at the surface mass density log\u03a3_(Mchar) ~ 8.5 at which the SSFR is seen to drop. Turning to zCOSMOS, we find a similar shape for the median SSFR-\u03a3_(M) relation, but with median SSFR values that are about 5-6 times higher than for SDSS, across the whole range of \u03a3_(M), and in galaxies with both high and low Sersic indices. This emphasizes that galaxies of all types are contributing, proportionally, to the global increase in star formation rate density in the Universe back to these redshifts. The \u03a3_(Mchar) \"step\" shifts to slightly higher values of \u03a3 M in zCOSMOS relative to SDSS, but this can be explained by a modest differential evolution in the size-mass relations of disk and spheroid galaxies. For low Sersic index galaxies, there is little change in the size-mass relation, as seen by Barden et al., although we suggest that this does not necessarily imply inside-out growth of disks, at least not in this redshift range. On the other hand, there is a modest evolution in the stellar mass-size relation for high Sersic index galaxies, with galaxies smaller by ~25% at z ~ 0.7. Taken together these produce a modest increase in \u03a3_(Mchar). Low Sersic index galaxies have a SSFR that is almost independent of \u03a3_(M), and the same is probably also true of high Sersic index galaxies once obvious disk systems are excluded.", "date": "2009-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "694", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1099-1114", "id_number": "CaltechAUTHORS:20090902-133644391", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090902-133644391", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/COFIS/WP3110 I/026/07/0" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/694/2/1099", "primary_object": { "basename": "Maier2009p1363Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/p11zn-d3c41/files/Maier2009p1363Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Maier, C.; Lilly, S. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/ftwa4-e0p60", "eprint_id": 14099, "eprint_status": "archive", "datestamp": "2023-08-21 20:58:59", "lastmod": "2023-10-18 16:07:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Gilli-R", "name": { "family": "Gilli", "given": "R." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Iwasawa-Kazushi", "name": { "family": "Iwasawa", "given": "K." }, "orcid": "0000-0002-4923-3281" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "N." } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Fiore-F", "name": { "family": "Fiore", "given": "F." } }, { "id": "Merloni-A", "name": { "family": "Merloni", "given": "A." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J." } }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "C." }, "orcid": "0000-0002-8853-9611" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" } ] }, "title": "High-redshift quasars in the cosmos survey: the space density of z > 3 x-ray selected QSOs", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; surveys; X-rays: galaxies", "note": "\u00a9 2009 American Astronomical Society. \n\nPrint publication: Issue 1 (2009 March 1); received 2008 May 16; accepted for publication 2008 October 28; published 2009 February 27. \n\nThis work is based on observations obtained with XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). In Germany, the XMM-Newton project is supported by the Bundesministerium f\u00fcr Wirtschaft und Technologie/Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OX 0001), and the Max-Planck Society. M.B. acknowledges support from the XMM-Newton DLR grant 50-G-0502, G.H. acknowledges the contribution from the Leibniz Prize of the Deutsche Forschungsgemeinschaft under the grant HA 1850/28-1. In Italy, the XMM-COSMOS project is supported by ASI-INAF and PRIN/MIUR under grants I/023/05/00 and 2006-02-5203. The zCOSMOS ESO Large Program Number 175.A-0839 is acknowledged. These results are also based in part on observations obtained with the Walter Baade telescope of the Magellan Consortium at Las Campanas Observatory, and with the MMT which is operated by the MMT Observatory (MMTO), a joint venture of the Smithsonian Institution and the University of Arizona. We gratefully acknowledge the contributions of the entire COSMOS collaboration; more information on the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. This research has made use of the NASA/IPAC Extragalactic Database (NED) and the SDSS spectral archive. We thank the anonymous referee for his/her useful comments and suggestions.\n\nPublished - Brusa2009p62010.10880004-637X69318.pdf
", "abstract": "We present a new measurement of the space density of high-redshift (z \u2243 3.0-4.5), X-ray-selected quasi-stellar objects (QSOs) obtained by exploiting the deep and uniform multiwavelength coverage of the COSMOS survey. We have assembled a large (40 objects), homogeneous sample of z > 3 QSOs with X-ray flux F_0.5-2 keV > 10^(\u201315) erg cm^(\u20132) s^(\u20131), and available spectroscopic (22) or photometric (18) redshifts. We discuss their optical (color-color diagrams) and X-ray properties, their number counts and space densities and compare our findings with previous works and model predictions. We find that the optical properties of X-ray-selected quasars are not significantly different from those of optically selected samples. There is evidence for substantial X-ray absorption (logN_H > 23 cm^(\u20132)) in about 20% of the sources in the sample. We find that the comoving space density of luminous (L_X \u2273 10^(44) erg s^(\u20131)) QSOs declines exponentially (by an e-folding per unit redshift) in the z ~ 3.0-4.5 range, with a behavior similar to that observed for optically bright unobscured QSOs selected in large area optical surveys. Prospects for future, large and deep X-ray surveys are also discussed.", "date": "2009-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "693", "number": "1", "publisher": "American Astronomical Society", "pagerange": "8-22", "id_number": "CaltechAUTHORS:20090428-095914449", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090428-095914449", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50-G-0502" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "HA 1850/28-1" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/023/05/00" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)", "grant_number": "2006\u201302\u20135203" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/693/1/8", "primary_object": { "basename": "Brusa2009p62010.10880004-637X69318.pdf", "url": "https://authors.library.caltech.edu/records/ftwa4-e0p60/files/Brusa2009p62010.10880004-637X69318.pdf" }, "pub_year": "2009", "author_list": "Brusa, M.; Comastri, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/xwbw2-9wz19", "eprint_id": 14364, "eprint_status": "archive", "datestamp": "2023-08-21 20:59:16", "lastmod": "2023-10-18 16:48:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fiore-F", "name": { "family": "Fiore", "given": "F." } }, { "id": "Puccetti-S", "name": { "family": "Puccetti", "given": "S." }, "orcid": "0000-0002-2734-7835" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Aldcroft-T", "name": { "family": "Aldcroft", "given": "T." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Brunner-H", "name": { "family": "Brunner", "given": "H." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "N." } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Feruglio-C", "name": { "family": "Feruglio", "given": "C." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Fruscione-A", "name": { "family": "Fruscione", "given": "A." } }, { "id": "Gilli-R", "name": { "family": "Gilli", "given": "R." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Mart\u00ednez-Sansigre-A", "name": { "family": "Mart\u00ednez-Sansigre", "given": "A." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Menci-N", "name": { "family": "Menci", "given": "N." } }, { "id": "Merloni-A", "name": { "family": "Merloni", "given": "A." } }, { "id": "Miyaji-Takamitsu", "name": { "family": "Miyaji", "given": "T." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M." }, "orcid": "0000-0003-1033-9684" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Steffen-A-T", "name": { "family": "Steffen", "given": "A." } }, { "id": "Santini-P", "name": { "family": "Santini", "given": "P." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J. R." } }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "C." }, "orcid": "0000-0002-8853-9611" }, { "id": "Urry-C-M", "name": { "family": "Urry", "given": "M." }, "orcid": "0000-0002-0745-9792" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" } ] }, "title": "Chasing highly obscured QSOs in the COSMOS field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: high-redshift; X-rays: diffuse background", "note": "\u00a9 2009 American Astronomical Society. \n\nPrint publication: Issue 1 (2009 March 1); received 2008 May 25; accepted for publication 2008 October 20; published 2009 March 2. \n\nWe acknowledge support from ASI/INAF contracts I/023/05/0 and I/024/05/0 and by PRIN/MUR grant 2006-02-5203. F.F. thanks Mari Polletta for useful comments. The zCOSMOSESO Large Program Number 175.A-0839 is also acknowledged.\n\nPublished - Fiore2009p63410.10880004-637X6931447.pdf
", "abstract": "A large population of heavily obscured, Compton-thick active galactic nuclei (AGNs) is predicted by AGN synthesis models for the cosmic X-ray background and by the \"relic\" supermassive black hole mass function measured from local bulges. However, even the deepest X-ray surveys are inefficient to search for these elusive AGNs. Alternative selection criteria, combining mid-infrared with near-infrared, and optical photometry, have instead been successful in pinpointing a large population of Compton-thick AGNs. We take advantage of the deep Chandra and Spitzer coverage of a large area (more than 10 times the area covered by the Chandra deep fields, CDFs) in the Cosmic Evolution Survey (COSMOS) field to extend the search of highly obscured, Compton-thick active nuclei to higher luminosity. These sources have low surface density, and therefore large samples can be provided only through large area surveys, like the COSMOS survey. We analyze the X-ray properties of COSMOS MIPS sources with 24 \u03bcm fluxes higher than 550 \u03bcJy. For the MIPS sources not directly detected in the Chandra images, we produce stacked images in soft and hard X-rays bands. To estimate the fraction of Compton-thick AGN in the MIPS source population, we compare the observed stacked count rates and hardness ratios to those predicted by detailed Monte Carlo simulations, including both obscured AGN and star-forming galaxies. The volume density of Compton-thick QSOs (log L(2-10 keV) = 44-45 erg s^(\u20131), or log\u03bbL_\u03bb(5.8 \u03bcm) = 44.79-46.18 erg s^(\u20131) for a typical infrared to X-ray luminosity ratio) evaluated in this way is (4.8 \u00b1 1.1) \u00d7 10^(\u20136) Mpc^(\u20133) in the redshift bin 1.2-2.2. This density is ~44% of all X-ray-selected QSOs in the same redshift and luminosity bin, and it is consistent with the expectation of the most up-to-date AGN synthesis models for the cosmic X-ray background (Gilli et al. 2007). The density of lower luminosity Compton-thick AGNs (log L(2-10 keV) = 43.5-44) at z = 0.7-1.2 is (3.7 \u00b1 1.1) \u00d7 10^(\u20135) Mpc^(\u20133), corresponding to ~67% of X-ray-selected AGNs. The comparison between the fraction of infrared-selected, Compton-thick AGNs to the X-ray selected, unobscured, and moderately obscured AGNs at high and low luminosity suggests that Compton-thick AGNs follow a luminosity dependence similar to that discovered for Compton-thin AGNs, becoming relatively rarer at high luminosities. We estimate that the fraction of AGNs (unobscured, moderately obscured, and Compton thick) to the total MIPS source population is 49 \u00b1 10%, a value significantly higher than that previously estimated at similar 24 \u03bcm fluxes. We discuss how our findings can constrain AGN feedback models.", "date": "2009-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "693", "number": "1", "publisher": "American Astronomical Society", "pagerange": "447-462", "id_number": "CaltechAUTHORS:20090604-115049653", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090604-115049653", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/023/05/0" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/024/05/0" }, { "agency": "Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)", "grant_number": "2006-02-5203" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/693/1/447", "primary_object": { "basename": "Fiore2009p63410.10880004-637X6931447.pdf", "url": "https://authors.library.caltech.edu/records/xwbw2-9wz19/files/Fiore2009p63410.10880004-637X6931447.pdf" }, "pub_year": "2009", "author_list": "Fiore, F.; Puccetti, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/ky5x0-3qw14", "eprint_id": 14154, "eprint_status": "archive", "datestamp": "2023-08-21 20:53:10", "lastmod": "2023-10-18 16:10:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Austermann-J-E", "name": { "family": "Austermann", "given": "J. E." } }, { "id": "Aretxaga-I", "name": { "family": "Aretxaga", "given": "I." }, "orcid": "0000-0002-6590-3994" }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "D. H." } }, { "id": "Kang-Y", "name": { "family": "Kang", "given": "Y." } }, { "id": "Kim-S", "name": { "family": "Kim", "given": "S." } }, { "id": "Lowenthal-J-D", "name": { "family": "Lowenthal", "given": "J. D." } }, { "id": "Perera-T-A", "name": { "family": "Perera", "given": "T. A." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scott-K-S", "name": { "family": "Scott", "given": "K. S." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G. W." } }, { "id": "Sun-M-S", "name": { "family": "Sun", "given": "M. S." } } ] }, "title": "AzTEC millimetre survey of the COSMOS field - II. Source count overdensity and correlations with large-scale structure", "ispublished": "pub", "full_text_status": "restricted", "keywords": "gravitational lensing; surveys; galaxies: evolution; cosmology: miscellaneous; infrared: galaxies; submillimeter", "note": "\u00a9 2009 RAS.\nAccepted 2008 November 21; received 2008 October 23; in original form 2008 August 9.\nWe thank the referee for their thorough reading and helpful comments. Support for this work was provided in part by NSF grant AST 05-40852 and a grant from the Korea Science & Engineering Foundation (KOSEF) under a cooperative Astrophysical Research Center of the Structure and Evolution of the Cosmos (ARCSEC). IA and DHH acknowledge partial support by CONACyT from research grants 39953-F and 39548-F.", "abstract": "We report an overdensity of bright submillimetre galaxies (SMGs) in the 0.15 deg^2 AzTEC/COSMOS survey and a spatial correlation between the SMGs and the optical-IR galaxy density at z\u2272 1.1. This portion of the COSMOS field shows a ~3\u03c3 overdensity of robust SMG detections when compared to a background, or 'blank-field', population model that is consistent with SMG surveys of fields with no extragalactic bias. The SMG overdensity is most significant in the number of very bright detections (14 sources with measured fluxes S_(1.1 mm) > 6 mJy), which is entirely incompatible with sample variance within our adopted blank-field number densities and infers an overdensity significance of \u226b 4\u03c3 . We find that the overdensity and spatial correlation to optical-IR galaxy density are most consistent with lensing of a background SMG population by foreground mass structures along the line of sight, rather than physical association of the SMGs with the z \u2272 1.1 galaxies/clusters. The SMG positions are only weakly correlated with weak-lensing maps, suggesting that the dominant sources of correlation are individual galaxies and the more tenuous structures in the survey region, and not the massive and compact clusters. These results highlight the important roles cosmic variance and large-scale structure can play in the study of SMGs.", "date": "2009-03", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "393", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "1573-1583", "id_number": "CaltechAUTHORS:20090504-151956449", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090504-151956449", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 05-40852" }, { "agency": "Korea Science and Engineering Foundation (KOSEF)" }, { "agency": "Astrophysical Research Center of the Structure and Evolution of the Cosmos (ARCSEC)" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda", "grant_number": "39953-F" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda", "grant_number": "39548-F" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1111/j.1365-2966.2008.14284.x", "pub_year": "2009", "author_list": "Austermann, J. E.; Aretxaga, I.; et el." }, { "id": "https://authors.library.caltech.edu/records/c8q16-fs457", "eprint_id": 14991, "eprint_status": "archive", "datestamp": "2023-08-20 00:52:39", "lastmod": "2023-10-18 20:26:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "N." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Gilli-R", "name": { "family": "Gilli", "given": "R." } }, { "id": "Puccetti-S", "name": { "family": "Puccetti", "given": "S." }, "orcid": "0000-0002-2734-7835" }, { "id": "Miyaji-Takamitsu", "name": { "family": "Miyaji", "given": "T." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "C." }, "orcid": "0000-0002-8853-9611" }, { "id": "Aldcroft-T", "name": { "family": "Aldcroft", "given": "T." } }, { "id": "B\u00f6hringer-H", "name": { "family": "B\u00f6hringer", "given": "H." } }, { "id": "Brunner-H", "name": { "family": "Brunner", "given": "H." } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Fiore-F", "name": { "family": "Fiore", "given": "F." } }, { "id": "Fruscione-A", "name": { "family": "Fruscione", "given": "A." } }, { "id": "Griffiths-R-E", "name": { "family": "Griffiths", "given": "R. E." } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Urry-C-M", "name": { "family": "Urry", "given": "M." }, "orcid": "0000-0002-0745-9792" } ] }, "title": "The XMM-Newton wide-field survey in the COSMOS field - The point-like X-ray source catalogue", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active large scale structure of Universe X rays: diffuse background X rays: galaxies", "note": "\u00a9 ESO 2009. Received 13 August 2008. Accepted 14 January 2009. Part of this work was supported by the German Deutsche\nForschungsgemeinschaft, DFG project number Ts 17/2\u20131.In Germany the\nXMM-Newton project is supported by the Bundesministerium f\u00fcr Wirtshaft und\nTechologie/Deutsches Zentrum f\u00fcr Luft und Raumfahrt and the Max-Planck society.\nN.C. and A.F. were partially supported from a NASA grant NNX07AV03G\nto UMBC. In Italy, the XMM-COSMOS project is supported by PRIN/MIUR\nunder grant 2006-02-5203 and ASI-INAF grants I/023/05/00, I/088/06. Part of\nthis work was supported by the German Deutsche Forschungsgemeinschaft,DFG\nLeibniz Prize (FKZ HA 1850/28-1). N.C. gratefully acknowledges Ezequiel\nTreister for providing his prediction of the XRB log N \u2212 log S. The entire\nCOSMOS collaboration is gratefully acknowledged. N.C. acknowledges\nUNAM-Ensenada for the hospitality during his visit.\n\nPublished - Cappelluti2009p1694Astron_Astrophys.pdf
", "abstract": "Context. The COSMOS survey is a multiwavelength survey aimed to study the evolution of galaxies, AGN and large scale structures. Within this\nsurvey XMM-COSMOS a powerful tool to detect AGN and galaxy clusters. The XMM-COSMOS is a deep X-ray survey over the full 2 deg^2 of\nthe COSMOS area. It consists of 55 XMM-Newton pointings for a total exposure of ~1.5 Ms with an average vignetting-corrected depth of 40 ks\nacross the field of view and a sky coverage of 2.13 deg^2.\nAims. We present the catalogue of point-like X-ray sources detected with the EPIC CCD cameras, the log N \u2212 log S relations and the X-ray\ncolour\u2013colour diagrams.\nMethods. The analysis was performed using the XMM-SAS data analysis package in the 0.5\u20132 keV, 2\u201310 keV and 5\u201310 keV energy bands.\nSource detection has been performed using a maximum likelihood technique especially designed for raster scan surveys. The completeness of the\ncatalogue as well as log N \u2212 log S and source density maps have been calibrated using Monte Carlo simulations.\nResults. The catalogs contains a total of 1887 unique sources detected in at least one band with likelihood parameter det_ml > 10. The survey,\nwhich shows unprecedented homogeneity, has a flux limit of ~1.7\u00d710^(\u221215) erg cm^(\u22122) s^(\u22121), ~9.3\u00d710^(\u221215) erg cm^(\u22122) s^(\u22121) and ~1.3\u00d710^(\u221214) erg cm^(\u22122) s^(\u22121) over\n90% of the area (1.92 deg^2) in the 0.5\u20132 keV, 2\u201310 keV and 5\u201310 keV energy band, respectively. Thanks to the rather homogeneous exposure over\na large area, the derived log N \u2212 log S relations are very well determined over the flux range sampled by XMM-COSMOS. These relations have\nbeen compared with XRB synthesis models, which reproduce the observations with an agreement of ~10% in the 5\u201310 keV and 2\u201310 keV band,\nwhile in the 0.5\u20132 keV band the agreement is of the order of ~20%. The hard X-ray colors confirmed that the majority of the extragalactic sources\nin a bright subsample are actually type I or type II AGN. About 20% of the sources have a X-ray luminosity typical of AGN (L_X > 10^(42) erg/s)\nalthough they do not show any clear signature of nuclear activity in the optical spectrum.", "date": "2009-02-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "497", "number": "2", "publisher": "EDP Sciences", "pagerange": "635-648", "id_number": "CaltechAUTHORS:20090812-132642949", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090812-132642949", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Bundesministerium f\u00fcr Wirtschaft und Technologie (BMWi)" }, { "agency": "Max-Planck Society" }, { "agency": "NASA", "grant_number": "NNX07AV03G" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)", "grant_number": "2006-02-5203" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/023/05/00" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/088/06" }, { "agency": "Deutsche Forschungsgemeinschaft", "grant_number": "1850/28-1" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/200810794", "primary_object": { "basename": "Cappelluti2009p1694Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/c8q16-fs457/files/Cappelluti2009p1694Astron_Astrophys.pdf" }, "pub_year": "2009", "author_list": "Cappelluti, N.; Brusa, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/tda7e-hq247", "eprint_id": 14007, "eprint_status": "archive", "datestamp": "2023-08-20 00:43:40", "lastmod": "2023-10-18 16:02:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K. I." }, "orcid": "0000-0001-8183-1460" }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D." }, "orcid": "0000-0003-1924-1122" }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J. -F." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "P\u00e9rez-Montero-E", "name": { "family": "P\u00e9rez-Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } }, { "id": "Abbas-U", "name": { "family": "Abbas", "given": "U." } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "D." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "A." } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Fumana-Marco", "name": { "family": "Fumana", "given": "M." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Maccagni-D", "name": { "family": "Maccagni", "given": "D." } }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Memeo-P", "name": { "family": "Memeo", "given": "P." } }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "B." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "L." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Scaramella-R", "name": { "family": "Scaramella", "given": "R." } }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" } ] }, "title": "The close environment of 24 \u03bcm galaxies at 0.6 < z < 1.0 in the cosmos field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 infrared: galaxies", "note": "\u00a9 2009.\nReceived 2008 June 6; accepted 2008 September 19; published 2009 January 7.\nThis paper is based on observations made with the VIMOS\nspectrograph on the VLT telescope, undertaken at the European Southern Observatory (ESO) under Large Program 175.A-0839, and also based on observations made with the Spitzer Observatory, which is operated under NASA contract 1407.\n\nPublished - CAPapj09.pdf
", "abstract": "We investigate the close environment of 203 Spitzer 24 \u03bcm -selected sources at 0.6 < z < 1.0 using zCOSMOS-bright redshifts and spectra of I < 22.5 AB mag galaxies, over 1.5 deg^2 of the COSMOS field. We quantify the degree of passivity of the luminous and ultra-luminous IR galaxy (LIRG and ULIRG, respectively) environments by analyzing the fraction of close neighbors with Dn(4000)>1.4. We find that LIRGs at 0.6 < z < 0.8 live in more passive environments than those of other optical galaxies that have the same stellar mass distribution. Instead, ULIRGs inhabit more active regions (e.g., LIRGs and ULIRGs at 0.6 < z < 0.8 have, respectively, (42.0 \u00b1 4.9)% and (24.5 \u00b1 5.9)% of neighbors with Dn(4000)>1.4 within 1 Mpc and \u00b1500 km s^\u20131). The contrast between the activities of the close environments of LIRGs and ULIRGs appears especially enhanced in the COSMOS field density peak at z ~ 0.67, because LIRGs on this peak have a larger fraction of passive neighbors, while ULIRGs have as active close environments as those outside the large-scale structure. The differential environmental activity is related to the differences in the distributions of stellar mass ratios between LIRGs/ULIRGs and their close neighbors, as well as in the general local density fields. At 0.8 < z < 1.0, instead, we find no differences in the environment densities of ULIRGs and other similarly massive galaxies, in spite of the differential activities. We discuss a possible scenario to explain these findings.", "date": "2009-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "691", "number": "1", "publisher": "American Astronomical Society", "pagerange": "91-97", "id_number": "CaltechAUTHORS:20090417-103246449", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090417-103246449", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1407" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/691/1/91", "primary_object": { "basename": "CAPapj09.pdf", "url": "https://authors.library.caltech.edu/records/tda7e-hq247/files/CAPapj09.pdf" }, "pub_year": "2009", "author_list": "Caputi, K. I.; Kova\u010d, K.; et el." }, { "id": "https://authors.library.caltech.edu/records/8xp1v-7nt06", "eprint_id": 13114, "eprint_status": "archive", "datestamp": "2023-08-22 14:15:19", "lastmod": "2023-10-17 21:47:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gabor-J-M", "name": { "family": "Gabor", "given": "J. M." } }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C. D." } }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "K." }, "orcid": "0000-0003-3804-2137" }, { "id": "Simmons-B-D", "name": { "family": "Simmons", "given": "B. D." }, "orcid": "0000-0001-5882-3323" }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J. R." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Cappeluti-N", "name": { "family": "Cappeluti", "given": "N." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J. D." }, "orcid": "0000-0002-4485-8549" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "R." }, "orcid": "0000-0002-6085-3780" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Active galactic nucleus host galaxy morphologies in COSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: evolution; galaxies: interactions; galaxies: structure", "note": "\u00a9 2009. The American Astronomical Society. \n\nReceived 2008 May 12; accepted 2008 August 25; published 2009 January 19. Print publication: Issue 1 (2009 January 20). \n\nWe gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. We also thank the anonymous, thorough referee for contributing to the quality of this work. J.G. would like to thank Romeel Dave, Rodger Thompson, and Ann Zabludoff for guidance and useful discussion, and St\u00e9phanie Juneau for help with K-corrections. J.D.R. was supported by internal funding at the Jet Propulsion Laboratory, California Institute of Technology, operated under a contract with NASA. K.J. acknowledges support by the German DFG under grant SCHI 536/3-1 and through the DFG Emmy Noether-Program under grant JA 1114/3-1. \n\nFacilities: HST (ACS), Magellan: Baade (IMACS), XMM, VLA, MMT (Hectospec). \n\nBased on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc, under NASA contract NAS 5-26555; also based on data collected at: the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory under Large Program 175.A-0839, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc; and the Canada-France-Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the National Research Council of Canada, the Canadian Astronomy Data Centre, the Centre National de la Recherche Scientifique de France, TERAPIX and the University of Hawaii.\n\nPublished - GABapj09.pdf
Supplemental Material - GABapj09table2.gif
", "abstract": "We use Hubble Space Telescope/Advanced Camera for Surveys images and a photometric catalog of the Cosmic Evolution Survey (COSMOS) field to analyze morphologies of the host galaxies of ~400 active galactic nucleus (AGN) candidates at redshifts 0.3 < z < 1.0. We compare the AGN hosts with a sample of nonactive galaxies drawn from the COSMOS field to match the magnitude and redshift distribution of the AGN hosts. We perform two-dimensional surface brightness modeling with GALFIT to yield host galaxy and nuclear point source magnitudes. X-ray-selected AGN host galaxy morphologies span a substantial range that peaks between those of early-type, bulge-dominated and late-type, disk-dominated systems. We also measure the asymmetry and concentration of the host galaxies. Unaccounted for, the nuclear point source can significantly bias results of these measured structural parameters, so we subtract the best-fit point source component to obtain images of the underlying host galaxies. Our concentration measurements reinforce the findings of our two-dimensional morphology fits, placing X-ray AGN hosts between early- and late-type inactive galaxies. AGN host asymmetry distributions are consistent with those of control galaxies. Combined with a lack of excess companion galaxies around AGN, the asymmetry distributions indicate that strong interactions are no more prevalent among AGN than normal galaxies. In light of recent work, these results suggest that the host galaxies of AGN at these X-ray luminosities may be in a transition from disk-dominated to bulge-dominated, but that this transition is not typically triggered by major mergers.", "date": "2009-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "691", "number": "1", "publisher": "American Astronomical Society", "pagerange": "705-722", "id_number": "CaltechAUTHORS:GABapj09", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:GABapj09", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "JPL" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "SCHI 536/3-1" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "JA 1114/3-1" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "European Space Agency" }, { "agency": "European Southern Observatory", "grant_number": "175.A-0839" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/691/1/705", "primary_object": { "basename": "small.png", "url": "https://authors.library.caltech.edu/records/8xp1v-7nt06/files/small.png" }, "related_objects": [ { "basename": "GABapj09.pdf", "url": "https://authors.library.caltech.edu/records/8xp1v-7nt06/files/GABapj09.pdf" }, { "basename": "GABapj09table2.gif", "url": "https://authors.library.caltech.edu/records/8xp1v-7nt06/files/GABapj09table2.gif" }, { "basename": "medium.png", "url": "https://authors.library.caltech.edu/records/8xp1v-7nt06/files/medium.png" } ], "pub_year": "2009", "author_list": "Gabor, J. M.; Impey, C. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/rpvv5-2g678", "eprint_id": 12515, "eprint_status": "archive", "datestamp": "2023-08-22 14:11:37", "lastmod": "2023-10-17 17:01:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Dahlen-T", "name": { "family": "Dahlen", "given": "Tomas" } }, { "id": "Hopkins-A-M", "name": { "family": "Hopkins", "given": "Andrew" }, "orcid": "0000-0002-6097-2747" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "David B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" } ] }, "title": "Relation between stellar mass and star-formation activity in galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: starburst", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2008 April 8, accepted for publication 2008 August 18. Published 2008 December 2. Print publication: Issue 2 (2009 January 10). \n\nBased on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc., under NASA contract NAS 5-26555; also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory under Large Program 175.A-0839, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; and the Canada-France-Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the National Research Council of Canada, the Canadian Astronomy Data Centre, the Centre National de la Recherche Scientifique de France, TERAPIX and the University of Hawaii. \n\nOnline-only material: color figure.\n\nPublished - MOBapj09.pdf
", "abstract": "For a mass-selected sample of 66544 galaxies with photometric redshifts (z phot) from the Cosmic Evolution Survey (COSMOS), we examine the evolution of star-formation activity as a function of stellar mass in galaxies. We estimate the cosmic star-formation rates (SFRs) over the range 0.2 < z phot < 1.2, using the rest-frame 2800 \u00c5 flux (corrected for extinction). We find the mean SFR to be a strong function of the galactic stellar mass at any given redshift, with massive systems (log(M/M\u2609) > 10.5) contributing less (by a factor of ~5) to the total star-formation rate density (SFRD). Combining data from the COSMOS and Gemini Deep Deep Survey, we extend the SFRD-z relation as a function of stellar mass to z ~ 2. For massive galaxies, we find a steep increase in the SFRD-z relation to z ~ 2; for the less-massive systems, the SFRD which also increases from z = 0 to 1 levels off at z ~ 1. This implies that the massive systems have had their major star-formation activity at earlier epochs (z > 2) than the lower-mass galaxies. We study changes in the SFRDs as a function of both redshift and stellar mass for galaxies of different spectral types. We find that the slope of the SFRD-z relation for different spectral types of galaxies is a strong function of their stellar mass. For low- and intermediate-mass systems, the main contribution to the cosmic SFRD comes from the star-forming galaxies while, for more-massive systems, the evolved galaxies are the most dominant population.", "date": "2009-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "690", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1074-1083", "id_number": "CaltechAUTHORS:MOBapj09", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:MOBapj09", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "European Southern Observatory", "grant_number": "Large Program 175.A-0839" }, { "agency": "Association of Universities for Research in Astronomy, Inc. (AURA)" }, { "agency": "NSF" }, { "agency": "Associated Universities, Inc." }, { "agency": "National Research Council of Canada" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "University of Hawaii" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "COSMOS", "value": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)", "value": "Infrared Processing and Analysis Center (IPAC)" } ] }, "doi": "10.1088/0004-637X/690/2/1074", "primary_object": { "basename": "MOBapj09.pdf", "url": "https://authors.library.caltech.edu/records/rpvv5-2g678/files/MOBapj09.pdf" }, "pub_year": "2009", "author_list": "Mobasher, Bahram; Dahlen, Tomas; et el." }, { "id": "https://authors.library.caltech.edu/records/5rr4e-eke13", "eprint_id": 14794, "eprint_status": "archive", "datestamp": "2023-08-22 14:12:44", "lastmod": "2023-10-18 19:54:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "S." } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S." } }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } }, { "id": "Zamojski-M-A", "name": { "family": "Zamojski", "given": "M." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K. I." }, "orcid": "0000-0001-8183-1460" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Cook-R", "name": { "family": "Cook", "given": "R." } }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J. F." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Looper-D", "name": { "family": "Looper", "given": "D." } }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Mellier-Y", "name": { "family": "Mellier", "given": "Y." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "P\u00e9rez-Montero-E", "name": { "family": "P\u00e9rez-Montero", "given": "E." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J. A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } } ] }, "title": "Cosmos Photometric Redshifts with 30-Bands for 2-deg^2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: distances and redshifts; galaxies: evolution; galaxies: formation", "note": "\u00a9 2009 The American Astronomical Society.\nReceived 2008 August 15, accepted for publication 2008 September 10.\nPublished 2008 December 8.\nWe gratefully acknowledge the contributions of the\nentire COSMOS collaboration consisting of more than\n100 scientists. The HST COSMOS program was supported\nthrough NASA grant HST-GO-09822. More information\non the COSMOS survey is available at Web site\nhttp://www.astro.caltech.edu/cosmos. We also greatly appreciate the hospitality provided by the Aspen Center for Physics\nwhere this manuscript was completed.\nThis article is based on observations with the NASA/ESA\nHubble Space Telescope, obtained at the Space Telescope Science\nInstitute, which is operated by AURA Inc., under NASA\ncontract NAS 5-26555. It is also based on observations made\nwith the Spitzer Space Telescope, which is operated by the Jet\nPropulsion Laboratory, California Institute of Technology, under\nNASA contract 1407. The research is also based on data\ncollected at: the Subaru Telescope, which is operated by the National\nAstronomical Observatory of Japan; the XMM-Newton, an\nESAscience mission with instruments and contributions directly\nfunded by ESAMember States and NASA; the European Southern\nObservatory under Large Program 175.A-0839, Chile; Kitt\nPeak National Observatory, Cerro Tololo Inter-American Observatory,\nand the National Optical Astronomy Observatory, which\nare operated by the Association of Universities for Research in\nAstronomy, Inc. (AURA) under cooperative agreement with the\nNational Science Foundation; and the Canada\u2013France\u2013Hawaii\nTelescope (CFHT) with MegaPrime/MegaCam operated as a\njoint project by the CFHT Corporation, CEA/DAPNIA, the\nNRC and CADC of Canada, the CNRS of France, TERAPIX,\nand the University of Hawaii.\n\nPublished - ILBapj09.pdf
", "abstract": "We present accurate photometric redshifts (photo-z) in the 2-deg^2 COSMOS field. The redshifts are computed with 30 broad, intermediate, and narrowbands covering the UV (Galaxy Evolution Explorer), visible near-IR (NIR; Subaru, Canada-France-Hawaii Telescope (CFHT), United Kingdom Infrared Telescope, and National Optical Astronomy Observatory), and mid-IR (Spitzer/IRAC). A \u03c7^2 template-fitting method (Le Phare) was used and calibrated with large spectroscopic samples from the Very Large Telescope Visible Multi-Object Spectrograph and the Keck Deep Extragalactic Imaging Multi-Object Spectrograph. We develop and implement a new method which accounts for the contributions from emission lines ([O II], H\u03b2, H\u03b1, and Ly\u03b1) to the spectral energy distributions (SEDs). The treatment of emission lines improves the photo-z accuracy by a factor of 2.5. Comparison of the derived photo-z with 4148 spectroscopic redshifts (i.e., \u0394z = z_s \u2013 z_p) indicates a dispersion of at \u03c3\u0394_z/(1+z_s) = 0.007 at i^+_(AB) < 22.5, a factor of 2-6 times more accurate than earlier photo-z in the COSMOS, CFHT Legacy Survey, and the Classifying Object by Medium-Band Observations-17 survey fields. At fainter magnitudes i^+_( AB) < 24 and z < 1.25, the accuracy is \u03c3\u0394_z/(1+z_s) = 0.012. The deep NIR and Infrared Array Camera coverage enables the photo-z to be extended to z ~ 2, albeit with a lower accuracy (\u03c3\u0394_z/(1+z_s) = 0.06 at i^+_(AB) ~ 24). The redshift distribution of large magnitude-selected samples is derived and the median redshift is found to range from z m = 0.66 at 22 < i^+_(AB) < 22.5 to z_m = 1.06 at 24.5 < i^+_(AB) < 25. At i^+_(AB) < 26.0, the multiwavelength COSMOS catalog includes approximately 607,617 objects. The COSMOS-30 photo-z enables the full exploitation of this survey for studies of galaxy and large-scale structure evolution at high redshift.", "date": "2009-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "690", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1236-1249", "id_number": "CaltechAUTHORS:20090804-134612379", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090804-134612379", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NASA", "grant_number": "1407" }, { "agency": "ESA Member States" }, { "agency": "European Southern Observatory", "grant_number": "175.A-0839" }, { "agency": "Association of Universities for Research in Astronomy (AURA)" }, { "agency": "NSF" }, { "agency": "Canada-France-Hawaii Telescope (CFHT)" }, { "agency": "National Research Council" }, { "agency": "Canadian Astronomy Data Centre" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "TERAPIX" }, { "agency": "University of Hawaii" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/690/2/1236", "primary_object": { "basename": "ILBapj09.pdf", "url": "https://authors.library.caltech.edu/records/5rr4e-eke13/files/ILBapj09.pdf" }, "pub_year": "2009", "author_list": "Ilbert, O.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/59sxz-ka128", "eprint_id": 13958, "eprint_status": "archive", "datestamp": "2023-08-22 14:12:38", "lastmod": "2023-10-18 15:59:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Rau-A", "name": { "family": "Rau", "given": "A." }, "orcid": "0000-0001-5990-6243" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "S." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Buongiorno-A", "name": { "family": "Buongiorno", "given": "A." } }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "N." } }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K." }, "orcid": "0000-0001-8183-1460" }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Cook-R-R", "name": { "family": "Cook", "given": "R." } }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Gilli-R", "name": { "family": "Gilli", "given": "R." } }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "K." }, "orcid": "0000-0003-3804-2137" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C. D." } }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "McCarthy-P-J", "name": { "family": "McCarthy", "given": "P." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J. R." } }, { "id": "Urry-C-M", "name": { "family": "Urry", "given": "M." }, "orcid": "0000-0002-0745-9792" }, { "id": "Zamojski-M-A", "name": { "family": "Zamojski", "given": "M." } } ] }, "title": "Photometric Redshift and Classification for the XMM-COSMOS Sources", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: active; methods: miscellaneous", "note": "\u00a9 2009. The American Astronomical Society. \n\nReceived 2008 August 15; accepted 2008 September 9; published 2008 December 8.\n\nBased on observations with the NASA/ESA Hubble Space Telescope,\nobtained at the Space Telescope Science Institute, which is operated by the\nAssociation of Universities for Research in Astronomy, Inc. (AURA) under\nNASA contract NAS 5-26555. Also based on observations made with the\nSpitzer Space Telescope, which is operated by the Jet Propulsion Laboratory,\nCalifornia Institute of Technology, under NASA contract 1407. Also based on\ndata collected at: the Subaru Telescope, which is operated by the National\nAstronomical Observatory of Japan; the XMM-Newton, an ESA science\nmission with instruments and contributions directly funded by ESA member\nstates and NASA; the European Southern Observatory under Large Program\n175.A-0839, Chile; Kitt Peak National Observatory, Cerro Tololo\nInter-American Observatory and the National Optical Astronomy Observatory,\nwhich are operated by AURA under cooperative agreement with the National\nScience Foundation; and the Canada\u2013France\u2013Hawaii Telescope with\nMegaPrime/MegaCam operated as a joint project by the CFHT Corporation CEA/DAPNIA, the NRC and CADC of Canada, the CNRS of France,\nTERAPIX and the University of Hawaii.\n\nWe gratefully acknowledge the contributions of the entire\nCOSMOS collaboration consisting of more than 100 scientists.\nMore information on the COSMOS survey is available\nat http://www.astro.caltech.edu/cosmos. We acknowledge\nthe anonymous referee for helpful comments that improved the\npaper. We also acknowledge the hospitality of the Institute for\nAstronomy, Hawaii, and the support of the Aspen Center for\nPhysics where the work started and the manuscript was completed.\nG.H. acknowledges support by the German Deutsche\nForschungsgemeinschaft, DFG Leibniz Prize (FKZ HA 1850/\n28-1). This work was supported in part by NASA Grant GO7-\n8136A.\n\nPublished - SALapj09.pdf
", "abstract": "We present photometric redshifts and spectral energy distribution (SED) classifications for a sample of 1542 optically identified sources detected with XMM in the COSMOS field. Our template fitting classifies 46 sources as stars and 464 as nonactive galaxies, while the remaining 1032 require templates with an active galactic nucleus (AGN) contribution. High accuracy in the derived photometric redshifts was accomplished as the result of (1) photometry in up to 30 bands with high-significance detections, (2) a new set of SED templates, including 18 hybrids covering the far-UV to mid-infrared, which have been constructed by the combination of AGNs and nonactive galaxies templates, and (3) multiepoch observations that have been used to correct for variability (most important for type 1 AGNs). The reliability of the photometric redshifts is evaluated using the subsample of 442 sources with measured spectroscopic redshifts. We achieved an accuracy of \u03c3\u0394z/(1+z_(spec)) = 0.014 for i\u2217_(AB) < 22.5 (\u03c3\u0394z/(1+z_(spec)) ~ 0.015 for i\u2217_(AB) < 24.5). The high accuracies were accomplished for both type 2 (where the SED is often dominated by the host galaxy) and type 1 AGNs and QSOs out to z = 4.5. The number of outliers is a large improvement over previous photometric redshift estimates for X-ray-selected sources (4.0% and 4.8% outliers for i\u2217_(AB) < 22.5 and i\u2217_(AB) < 24.5, respectively). We show that the intermediate band photometry is vital to achieving accurate photometric redshifts for AGNs, whereas the broad SED coverage provided by mid-infrared (Spitzer/IRAC) bands is important to reduce the number of outliers for normal galaxies.", "date": "2009-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "690", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1250-1263", "id_number": "CaltechAUTHORS:20090413-145514915", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090413-145514915", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "FKZ HA 1850/ 28-1" }, { "agency": "NASA", "grant_number": "GO7-8136A" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/690/2/1250", "primary_object": { "basename": "SALapj09.pdf", "url": "https://authors.library.caltech.edu/records/59sxz-ka128/files/SALapj09.pdf" }, "pub_year": "2009", "author_list": "Salvato, M.; Hasinger, G.; et el." }, { "id": "https://authors.library.caltech.edu/records/wg6yy-kxc88", "eprint_id": 12650, "eprint_status": "archive", "datestamp": "2023-08-22 14:09:01", "lastmod": "2023-10-17 20:24:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Bell-E-F", "name": { "family": "Bell", "given": "E. F." } }, { "id": "Bondi-M", "name": { "family": "Bondi", "given": "M." } }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Ciliegi-P", "name": { "family": "Ciliegi", "given": "P." } }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Paglione-T", "name": { "family": "Paglione", "given": "T." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The Dust-Unbiased Cosmic Star-Formation History from the 20 CM VLA-COSMOS Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: fundamental parameters; galaxies: starburst; radio continuum: galaxies", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2008 April 24, accepted for publication 2008 August 25. Published 2008 December 1. Print publication: Issue 1 (2009 January 1) \n\nC.C. acknowledges support from the Max-Planck Society and the Alexander von Humboldt Foundation through the Max-Planck-Forschungspreis 2005. G.Z. acknowledges support from two contracts PRIN-INAF 2005 and 2007. T.P. acknowledges support from PSC-CUNY grant # 69612-00 38. \n\nBased on observations with the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. \n\n[V.S was a] Fellow of the International Max Planck Research School for Astronomy and Cosmic Physics.\n\nPublished - SMOapj09.pdf
", "abstract": "We derive the cosmic star-formation history out to z = 1.3 using a sample of ~350 radio-selected star-forming (SF) galaxies, a far larger sample than those in previous, similar studies. We attempt to differentiate between radio emission from active galactic nuclei and SF galaxies, and determine an evolving 1.4 GHz luminosity function (LF) based on these VLA-COSMOS SF galaxies. We precisely measure the high-luminosity end of the SF galaxy LF (star-formation rate \u2273100 M\u2609yr^\u20131; equivalent to ultra-luminous IR galaxies) out to z = 1.3, finding a somewhat slower evolution than that previously derived from mid-infrared data. We find that more stars are forming in luminous starbursts at high redshift. We use extrapolations based on the local radio galaxy LF; assuming pure luminosity evolution, we derive L* \u221d (1 + z)^2.1\u00b10.2 or L* \u221d (1 + z)^2.5\u00b10.1, depending on the choice of the local radio galaxy LF. Thus, our radio-derived results independently confirm the ~1 order of magnitude decline in the CSFH since z ~ 1.", "date": "2009-01-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "690", "number": "1", "publisher": "American Astronomical Society", "pagerange": "610-618", "id_number": "CaltechAUTHORS:SMOapj09", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:SMOapj09", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Max Planck Society" }, { "agency": "Alexander von Humboldt Foundation" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-INAF 2005" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-INAF 2007" }, { "agency": "Professional Staff Congress, City University of New York", "grant_number": "PSC-CUNY 69612-00 38" }, { "agency": "NSF" }, { "agency": "Associated Universities, Inc." } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/690/1/610", "primary_object": { "basename": "SMOapj09.pdf", "url": "https://authors.library.caltech.edu/records/wg6yy-kxc88/files/SMOapj09.pdf" }, "pub_year": "2009", "author_list": "Smol\u010di\u0107, V.; Schinnerer, E.; et el." }, { "id": "https://authors.library.caltech.edu/records/7k45p-34640", "eprint_id": 13651, "eprint_status": "archive", "datestamp": "2023-08-22 14:06:14", "lastmod": "2023-10-18 00:03:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Halliday-C", "name": { "family": "Halliday", "given": "C." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "L." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K." }, "orcid": "0000-0001-8183-1460" }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J. -F." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "Perez-Montero-E", "name": { "family": "Perez Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } }, { "id": "Abbas-U", "name": { "family": "Abbas", "given": "U." } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "D." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "A." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Fumana-M", "name": { "family": "Fumana", "given": "M." } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Maccagni-D", "name": { "family": "Maccagni", "given": "D." } }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Memeo-P", "name": { "family": "Memeo", "given": "P." } }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "B." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Scaramella-R", "name": { "family": "Scaramella", "given": "R." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "The zCOSMOS redshift survey: the three-dimensional classification cube and bimodality in galaxy physical properties", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies-general; galaxies-evolution; galaxies-fundamental parameters", "note": "\u00a9 ESO 2008\n\nReceived 4 July 2008 Accepted 6 October 2008 \n\nBased on observations undertaken at the European Southern \nObservatory (ESO) Very Large Telescope (VLT) under Large Program 175.A-0839. Also based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, operated by AURA Inc., under NASA contract NAS 5-26555, with the Subaru Telescope, operated by the National Astronomical Observatory of Japan, with the telescopes of the National Optical Astronomy Observatory, operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation, and with the Canada-France-Hawaii Telescope, operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France, and the University of Hawaii.\n\nAcknowledgements. This work was partially supported by INAF under PRIN-2006/1.06.10.08 and by ASI under grant ASI/COFIS I/016/07/0.\n\nPublished - MIGaanda09.pdf
", "abstract": "Aims. We investigate the relationships between three main optical galaxy observables (spectral properties, colors, and morphology), exploiting the data set provided by the COSMOS/zCOSMOS survey. The purpose of this paper is to define a simple galaxy classification cube, with a carefully selected sample of \u22481000 galaxies.\n\nMethods. Using medium resolution spectra of the first 1k zCOSMOS-bright sample, optical photometry from the Subaru/COSMOS observations, and morphological measurements derived from ACS imaging, we analyze the properties of the galaxy population out to z~1. Applying three straightforward classification schemes (spectral, photometric, and morphological), we identify two main galaxy types, which appear to be linked to the bimodality of galaxy population. The three parametric classifications constitute the axes of a \"classification cube\".\n\nResults. A very good agreement exists between the classification from spectral data (quiescent/star-forming galaxies) and the one based on colors (red/blue galaxies). The third parameter (morphology) is not as well correlated with the first two; in fact, a good correlation between the spectral classification and the classification based on morphological analysis (early-/late-type galaxies) is achieved only after partially complementing the morphological classification with additional color information. Finally, analyzing the 3D-distribution of all galaxies in the sample, we find that about 85% of the galaxies show a fully concordant classification, being either quiescent, red, bulge-dominated galaxies (~20%) or star-forming, blue, disk-dominated galaxies (~65%). These results imply that the galaxy bimodality is a consistent behavior both in morphology, color, and dominant stellar population, at least out to z~1.", "date": "2009-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "493", "number": "1", "publisher": "EDP Sciences", "pagerange": "39-49", "id_number": "CaltechAUTHORS:MIGaanda09", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:MIGaanda09", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-2006/1.06.10.08" }, { "agency": "Agenzia Spaziale Italiana (Italy)", "grant_number": "ASI/COFIS I/016/07/0" }, { "agency": "European Southern Observatory Very Large Telescope", "grant_number": "Large Program 175.A-0839" }, { "agency": "National Astronomical Observatory of Japan" }, { "agency": "Association of Universities for Research in Astronomy (AURA)" }, { "agency": "National Research Council of Canada" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "University of Hawaii" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361:200810520", "primary_object": { "basename": "MIGaanda09.pdf", "url": "https://authors.library.caltech.edu/records/7k45p-34640/files/MIGaanda09.pdf" }, "pub_year": "2009", "author_list": "Mignoli, M.; Zamorani, G.; et el." }, { "id": "https://authors.library.caltech.edu/records/0ayvz-c9j39", "eprint_id": 14930, "eprint_status": "archive", "datestamp": "2023-08-22 14:07:01", "lastmod": "2023-10-18 20:23:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gilli-R", "name": { "family": "Gilli", "given": "R." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Miyaji-Takamitsu", "name": { "family": "Miyaji", "given": "T." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "N." } }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Pozzetti-L", "name": { "family": "Pozzetti", "given": "L." } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Fiore-F", "name": { "family": "Fiore", "given": "F." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "C." }, "orcid": "0000-0002-8853-9611" }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K." }, "orcid": "0000-0001-8183-1460" }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Coppa-G", "name": { "family": "Coppa", "given": "G." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J.-F." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "Peng-Yingjie", "name": { "family": "Peng", "given": "Y." } }, { "id": "Perez-Montero-E", "name": { "family": "Perez Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Tanaka-Masayuki", "name": { "family": "Tanaka", "given": "M." }, "orcid": "0000-0002-5011-5178" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } }, { "id": "Abbas-U", "name": { "family": "Abbas", "given": "U." } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "D." } }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "A." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Fumana-Marco", "name": { "family": "Fumana", "given": "M." } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Maccagni-D", "name": { "family": "Maccagni", "given": "D." } }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "C." } }, { "id": "Memeo-P", "name": { "family": "Memeo", "given": "P." } }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "B." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Scaramella-R", "name": { "family": "Scaramella", "given": "R." } }, { "id": "Walcher-J", "name": { "family": "Walcher", "given": "J." } } ] }, "title": "The spatial clustering of X-ray selected AGN in the XMM-COSMOS field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; cosmology: large-scale structure of Universe; cosmology: observations; X-rays: galaxies", "note": "\u00a9 ESO 2009.\nReceived 18 August 2008 / Accepted 22 October 2008.\nhis work is based on observations obtained with\nXMM-Newton, an ESA Science Mission with instruments and contributions\ndirectly funded by ESA Member States and the USA (NASA). We gratefully\nacknowledge the contribution of the entire COSMOS collaboration (http://\nwww.astro.caltech.edu/~cosmos). In Italy, the XMM-COSMOS projects\nis supported by ASI-INAF and PRIN/MIUR under grants I/023/05/00 and 2006-\n02-5203. The zCOSMOS ESO Large Program Number 175.A-0839 is acknowledged.\nR.G. thanks Carlo Nipoti, Federico Marulli, Enzo Branchini, and\nLauro Moscardini for stimulating discussions. The referee is acknowledged for\nproviding useful comments. The Millennium Simulation databases used in this\npaper and the web application providing online access to them were constructed\nas part of the activities of the German Astrophysical Virtual Observatory.\n\nPublished - Gilli2009p31710.10510004-6361200810821.pdf
", "abstract": "We study the spatial clustering of 538 X-ray selected AGN in the 2 deg^2 XMM-COSMOS field that are spectroscopically identified with I_(AB) < 23\nand span the redshift range z = 0.2\u22123.0. The median redshift and X-ray luminosity of the sample are z = 0.98 and L_(0.5\u221210) = 6.3 \u00d7 10^43 erg s^\u22121,\nrespectively. A strong clustering signal is detected at \u223c18\u03c3 level, which is the most significant measurement obtained to date for clustering of X-ray\nselected AGN. By fitting the projected correlation function w(r_p) with a power law on scales of r_p = 0.3\u221240 h^\u22121 Mpc, we derive a best-fit comoving\ncorrelation length of r_0 = 8.6 \u00b1 0.5 h^\u22121 Mpc and slope of \u03b3 = 1.88 \u00b1 0.07 (Poissonian errors; bootstrap errors are about a factor of 2 larger). An\nexcess signal is observed in the range r_p \u223c 5\u221215 h^\u22121 Mpc, which is due to a large-scale structure at z \u223c 0.36 containing about 40 AGN, a feature\nwhich is evident over many wavelengths in the COSMOS field. When removing the z \u223c 0.36 structure or computing w(rp) in a narrower range\naround the peak of the redshift distribution (e.g. z = 0.4\u22121.6), the correlation length decreases to r\u00ac_0 \u223c 5\u22126 h^\u22121 Mpc, which is consistent with what\nis observed for bright optical QSOs at the same redshift.\nWe investigate the clustering properties of obscured and unobscured AGN separately, adopting different definitions for the source obscuration.\nFor the first time, we are able to provide a significant measurement for the spatial clustering of obscured AGN at z \u223c 1. Within the statistical\nuncertainties, we do not find evidence that AGN with broad optical lines (BLAGN) cluster differently from AGN without broad optical lines (non-\nBLAGN). Based on these results, which are limited by object statistics, however, obscured and unobscured AGN are consistent with inhabiting\nsimilar environments.\nThe evolution of AGN clustering with redshift is also investigated. No significant difference is found between the clustering properties of\nXMM-COSMOS AGN at redshifts below or above z = 1.\nThe correlation length measured for XMM-COSMOS AGN at z \u223c 1 is similar to that of massive galaxies (stellar mass M* \u2273 3 \u00d7 10^10 M\u2299) at\nthe same redshift. This suggests that AGN at z \u223c 1 are preferentially hosted by massive galaxies, as observed both in the local and in the distant\n(z \u223c 2) Universe. According to a simple clustering evolution scenario, we find that the relics of AGN are expected to have a correlation length as\nlarge as r_0 \u223c 8 h^\u22121 Mpc by z = 0, and hence to be hosted by local bright (L \u223c L*) ellipticals.\nWe make use of dark matter halo catalogs from the Millennium simulation to determine the typical halo hosting moderately luminous z \u223c 1 AGN.\nWe find that XMM-COSMOS AGN live in halos with masses M \u2273 2.5 \u00d7 10^12 M\u2299h^\u22121. By combining the number density of XMM-COSMOS\nAGN to that of the hosting dark matter halos we estimate the AGN duty cycle and lifetimes. We find lifetimes approximately of 1 Gyr for AGN\nat z \u223c 1, which are longer than those estimated for optically bright QSOs at the same redshift. These longer lifetimes mainly reflect the higher\nnumber density of AGN selected by X-ray samples.", "date": "2009-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "494", "number": "1", "publisher": "EDP Sciences", "pagerange": "33-48", "id_number": "CaltechAUTHORS:20090810-142635312", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090810-142635312", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "ESA Member States" }, { "agency": "NASA" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)", "grant_number": "I/023/05/00" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)", "grant_number": "200602-5203" }, { "agency": "zCOSMOS ESO", "grant_number": "175" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361:200810821", "primary_object": { "basename": "Gilli2009p31710.10510004-6361200810821.pdf", "url": "https://authors.library.caltech.edu/records/0ayvz-c9j39/files/Gilli2009p31710.10510004-6361200810821.pdf" }, "pub_year": "2009", "author_list": "Gilli, R.; Zamorani, G.; et el." }, { "id": "https://authors.library.caltech.edu/records/0avfp-74513", "eprint_id": 13901, "eprint_status": "archive", "datestamp": "2023-08-22 13:54:15", "lastmod": "2023-10-18 14:33:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "Nicholas" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Lee-K-S", "name": { "family": "Lee", "given": "K.-S." } }, { "id": "McCracken-H-J", "name": { "family": "McCraken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "M. S." }, "orcid": "0000-0001-7095-7543" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Datta-A", "name": { "family": "Datta", "given": "A." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Urry-C-M", "name": { "family": "Urry", "given": "Megan C." }, "orcid": "0000-0002-0745-9792" } ] }, "title": "Star Formation Rates in Lyman Break Galaxies: Radio Stacking of LBGs in the COSMOS Field and the Sub-\u03bcJy Radio Source Population", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; surveys", "note": "\u00a9 2008. The American Astronomical Society. \n\nPrint publication: Issue 2 (2008 December 20). Received 2008 April 21; accepted 2008 August 1. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. C. C. thanks the Max-Planck-Gesellschaft and the Humboldt-Stiftung for support through the Max-Planck-Forschungspreis. We thank the referee for helpful comments.\n\nBased on observations in the COSMOS Legacy Survey including those taken on the HST, Keck, NRAO-VLA, Subaru, KPNO 4 m, CTIO 4 m, and CFHT 3.6 m. The Very Large Array of the National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nPublished - CARapj08.pdf
", "abstract": "We present an analysis of the radio properties of large samples of Lyman break galaxies (LBGs) at z ~ 3, 4, and 5 from the COSMOS field. The median stacking analysis yields a statistical detection of the z ~ 3 LBGs (U-band dropouts), with a 1.4 GHz flux density of 0:90 \u00b1 0:21 \u00b5Jy. The stacked emission is unresolved, with a size <1, or a physical size <8 kpc. The total star formation rate implied by this radio luminosity is 31 \u00b1 7M\u05e1\u05bc yr^(-1), based on the radio-FIR correlation in low-redshift star-forming galaxies. The star formation rate derived from a similar analysis of the UV luminosities is 17 M\u05e1\u05bc yr^(-1), without any correction for UV dust attenuation. The simplest conclusion is that the dust attenuation factor is 1.8 at UV wavelengths. However, this factor is considerably smaller than the standard attenuation factor of ~5, normally assumed for LBGs. We discuss potential reasons for this discrepancy, including the possibility that the dust attenuation factor at z \u2265 3 is smaller than at lower redshifts. Conversely, the radio luminosity for a given star formation rate may be systematically lower at very high redshift. Two possible causes for a suppressed radio luminosity are (1) increased inverse Compton cooling of the relativistic electron population due to scattering off the increasing CMB at high redshift or (2) cosmic-ray diffusion from systematically smaller galaxies. The radio detections of individual sources are consistent with a radio-loud AGN fraction of 0.3%. One source is identified as a very dusty, extreme starburst galaxy (a ''submillimeter galaxy'')", "date": "2008-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "689", "number": "2", "publisher": "American Astronomical Society", "pagerange": "883-888", "id_number": "CaltechAUTHORS:20090409-093614140", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090409-093614140", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "Max-Planck-Forschungspreis" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/592319", "primary_object": { "basename": "CARapj08.pdf", "url": "https://authors.library.caltech.edu/records/0avfp-74513/files/CARapj08.pdf" }, "pub_year": "2008", "author_list": "Carilli, C. L.; Lee, Nicholas; et el." }, { "id": "https://authors.library.caltech.edu/records/t2czq-3ya58", "eprint_id": 14649, "eprint_status": "archive", "datestamp": "2023-08-20 00:10:40", "lastmod": "2023-10-18 18:10:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Mart\u00ednez-Sansigre-A", "name": { "family": "Mart\u00ednez-Sansigre", "given": "A." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "M. S." }, "orcid": "0000-0001-7095-7543" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } } ] }, "title": "Molecular Gas in a Submillimeter Galaxy at z = 4.5: Evidence for a Major Merger at 1 Billion Years after the Big Bang", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation, galaxies: high, redshift, galaxies: ISM, galaxies: starburst, submillimeter", "note": "\u00a9 2008. The American Astronomical Society. Received 2008 September 11; accepted 2008 October 13; published 2008 October 29. E. S. would like to thank J. M. Winter and R. Neri for their\ngreat help during the visit of IRAM, Grenoble. E. S. thanks\nA. Wei\u00df and E. F. Bell for helpful discussions. E. S. acknowledges\nthe hospitality of the Aspen Center for Physics where\nthe manuscript was prepared. C. C. thanks the Max-Planck-\nGesellschaft and the Humboldt-Stiftung for support through\nthe Max-Planck-Forschungspreis. The National Radio Astronomy\nObservatory (NRAO) is operated by Associated Universities,\nInc., under cooperative agreement with the National Science\nFoundation.\n\nPublished - Schinnerer2008p407Astrophys_J_Lett.pdf
", "abstract": "We report the detection of CO molecular line emission in the z = 4.5 millimeter-detected galaxy COSMOS J100054+023436 (hereafter J1000+0234) using the IRAM Plateau de Bure interferometer (PdBI) and NRAO's Very Large Array (VLA). The^12CO(4-3) line as observed with PdBI has a full line width of ~1000 km s^(\u22121), an integrated line flux of 0.66 Jy km s\u22121, and a CO luminosity of 3.2 \u00d7 10^10 L\u2609. Comparison to the 3.3 \u03c3 detection of the CO(2-1) line emission with the VLA suggests that the molecular gas is likely thermalized to the J = 4\u20133 transition level. The corresponding molecular gas mass is 2.6 \u00d7 10^(10) M\u2609 assuming an ULIRG-like conversion factor. From the spatial offset of the red- and blueshifted line peaks and the line width a dynamical mass of 1.1 \u00d7 10^(11) M\u2609 is estimated assuming a merging scenario. The molecular gas distribution coincides with the rest-frame optical and radio position of the object while being offset by 0.5\" from the previously detected Ly\u03b1 emission. J1000+0234 exhibits very typical properties for lower redshift (z ~ 2) submillimeter galaxies (SMGs) and thus is very likely one of the long sought after high-redshift (z > 4) objects of this population. The large CO(4-3) line width taken together with its highly disturbed rest-frame UV geometry suggest an ongoing major merger about a billion years after the big bang. Given its large star formation rate (SFR) of >1000 M\u2609 yr^(\u22121) and molecular gas content this object could be the precursor of a \"red and dead\" elliptical observed at a redshift of z = 2.", "date": "2008-12-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "689", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L5-L8", "id_number": "CaltechAUTHORS:20090723-092122606", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090723-092122606", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Max-Planck-Forschungspreis" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/595680", "primary_object": { "basename": "Schinnerer2008p407Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/t2czq-3ya58/files/Schinnerer2008p407Astrophys_J_Lett.pdf" }, "pub_year": "2008", "author_list": "Schinnerer, E.; Carilli, C. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/tzwfy-bes84", "eprint_id": 12774, "eprint_status": "archive", "datestamp": "2023-08-19 23:49:41", "lastmod": "2023-10-17 20:54:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Weiss-Axel", "name": { "family": "Weiss", "given": "A." }, "orcid": "0000-0003-4678-3939" }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "K." }, "orcid": "0000-0003-3804-2137" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Henkel-Christian", "name": { "family": "Henkel", "given": "C." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Menten-K-M", "name": { "family": "Menten", "given": "K. M." }, "orcid": "0000-0001-6459-0669" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" } ] }, "title": "Properties of the molecular gas in a starbursting QSO at z = 1.83 in the COSMOS field", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 ESO 2008. Article published by EDP Sciences. \n\nReceived 17 July 2008 / Accepted 4 September 2008. \n\nManuel Aravena was supported for this research through a stipend from the International Max Planck Research School (IMPRS) for Radio and Infrared Astronomy at the Universities of Bonn and Cologne. \n\nThis work is based on observations with 30m telescope of the Institute for Radioastronomy at Millimeter Wavelengths (IRAM), which is funded by the German Max Planck Society, the French CNRS and the Spanish National Geographical Institute. Also based on observations with the Very Large Array of the National Radio Astronomy Observatory, which is a facility of the National Science Foundation, operated under cooperative agreement by Associated Univ. Inc. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc, under NASA contract NAS 5-26555; also based on data collected at: the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy Inc. (AURA) under cooperative agreement with the National Science Foundation; and the Canada-France-Hawaii Telescope operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France and the University of Hawaii.\n\nPublished - ARAaanda08.pdf
", "abstract": "Using the IRAM 30 m telescope, we have detected the 12CO J = 2\u22121, 4\u22123, 5\u22124, and 6\u22125 emission lines in the millimeter-bright, blank-field selected AGN COSMOS J100038+020822 at redshift z = 1.8275. The sub-local thermodynamic equilibrium (LTE) excitation of the J = 4 level implies that the gas is less excited than that in typical nearby starburst galaxies such as NGC 253, and in the high-redshift quasars studied to date, such as J1148+5251 or BR1202-0725. Large velocity gradient (LVG) modeling of the CO line spectral energy distribution (CO SED; flux density vs. rotational quantum number) yields H2 densities in the range 10^3.5\u221210^4.0 cm^\u22123, and kinetic temperatures between 50 K and 200 K. The H2 mass of (3.6\u22125.4) \u00d7 10^10 M\u2609 implied by the line intensities compares well with our estimate of the dynamical mass within the inner 1.5 kpc of the object. Fitting a two-component gray body spectrum, we find a dust mass of 1.2\u00d7 10^9 M\u2609, and cold and hot dust temperatures of 42\u00b15 K and 160\u00b1 25 K, respectively. The broad MgII line allows us to estimate the mass of the central black hole as 1.7 \u00d7 10^9 M\u2609. Although the optical spectrum and multi-wavelength SED matches those of an average QSO, the molecular gas content and dust properties resemble those of known submillimeter galaxies (SMGs). The optical morphology of this source shows tidal tails that suggest a recent interaction or merger. Since it shares properties of both starburst and AGN, this object appears to be in a transition from a strongly starforming submillimeter galaxy to a QSO.", "date": "2008-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "491", "number": "1", "publisher": "EDP Sciences", "pagerange": "173-181", "id_number": "CaltechAUTHORS:ARAaanda08", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:ARAaanda08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "International Max Planck Research School" }, { "agency": "Max Planck Society" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" }, { "agency": "NSF" }, { "agency": "Associated Universities, Inc." }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1051/0004-6361:200810628", "primary_object": { "basename": "ARAaanda08.pdf", "url": "https://authors.library.caltech.edu/records/tzwfy-bes84/files/ARAaanda08.pdf" }, "pub_year": "2008", "author_list": "Aravena, M.; Bertoldi, F.; et el." }, { "id": "https://authors.library.caltech.edu/records/zdg0s-1yc45", "eprint_id": 14254, "eprint_status": "archive", "datestamp": "2023-08-22 12:58:12", "lastmod": "2023-10-18 16:26:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Massey-R", "name": { "family": "Massey", "given": "Richard" } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Miyazaki-Satoshi", "name": { "family": "Miyazaki", "given": "Satoshi" } }, { "id": "Rhodes-J", "name": { "family": "Rhodes", "given": "Jason" } } ] }, "title": "A comparison of weak-lensing measurements from ground- and space-based facilities", "ispublished": "pub", "full_text_status": "public", "keywords": "atmospheric effects; cosmology: observations; gravitational lensing; instrumentation: detectors", "note": "\u00a9 2008 The American Astronomical Society.\nReceived 2007 October 18; accepted 2008 March 5.\nThis work is supported by the US Department of Energy under\ncontract DE-FG02-04ER41316. J. R.'s contribution was carried\nout at the Jet Propulsion Laboratory, California Institute of Technology,\nunder a contract with the National Aeronautics and Space\nAdministration and funded through the internal Research and\nTechnology Development program. The analysis is based on observations\nwith the NASA/ESA Hubble Space Telescope, obtained\nat the Space Telescope Science Institute, which is operated by Association\nof Universities for Research in Astronomy, Inc., under\nNASA contract NAS 5-26555. It is also based on data collected\nat the Subaru Telescope, operated by the National Astronomical\nObservatory of Japan. We acknowledge the careful comments of\na referee and also valuable input from Zeljko Ivezik, Alexandre\nRefregier, James Taylor, and Alexis Finoguenov. We particularly\nthank Alexie Leauthaud and Takashi Hamana for help with the\ntwo galaxy catalogs. We also gratefully acknowledge the contributions\nof the entire COSMOS collaboration, consisting of more\nthan 70 scientists worldwide. More information on the COSMOS\nsurvey is available from http://www.astro.caltech.edu/~cosmos.\n\nPublished - KASapj08b.pdf
", "abstract": "We assess the relative merits of weak-lensing surveys, using overlapping imaging data from the ground-based Subaru telescope and the Hubble Space Telescope (HST). Our tests complement similar studies undertaken with simulated data. From observations of 230,000 matched objects in the 2 deg^2 COSMOS field, we identify the limit at which faint galaxy shapes can be reliably measured from the ground using well-established shape-measurement techniques. Our ground-based shear catalog achieves subpercent calibration bias compared to high-resolution space-based data for galaxies brighter than i' \u2243 24.5 and with half-light radii larger than 1.8\". This selection corresponds to a surface density of 15 galaxies arcmin^(\u22122) compared to ~71 arcmin^\u22122 from space. On the other hand, the survey speed of current ground-based facilities is much faster than that of HST, although this gain is mitigated by the increased depth of space-based imaging desirable for tomographic (3D) analyses. As an independent experiment, we also reconstruct the projected mass distribution in the COSMOS field using both data sets, and compare the derived cluster catalogs with those from X-ray observations. The ground-based catalog achieves a reasonable degree of completeness, with minimal contamination and no detected bias, for massive clusters at redshifts 0.2 < z < 0.5. The space-based data provide improved precision and a greater sensitivity to clusters of lower mass or at higher redshift.", "date": "2008-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "684", "number": "1", "publisher": "American Astronomical Society", "pagerange": "34-45", "id_number": "CaltechAUTHORS:20090518-105131205", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090518-105131205", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-04ER41316" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1086/588517", "primary_object": { "basename": "KASapj08b.pdf", "url": "https://authors.library.caltech.edu/records/zdg0s-1yc45/files/KASapj08b.pdf" }, "pub_year": "2008", "author_list": "Kasliwal, Mansi M.; Massey, Richard; et el." }, { "id": "https://authors.library.caltech.edu/records/70qga-mjq47", "eprint_id": 11756, "eprint_status": "archive", "datestamp": "2023-08-22 12:50:40", "lastmod": "2023-10-17 15:45:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Berta-S", "name": { "family": "Berta", "given": "S." }, "orcid": "0000-0002-0320-1532" }, { "id": "Rubele-S", "name": { "family": "Rubele", "given": "S." } }, { "id": "Franceschini-A", "name": { "family": "Franceschini", "given": "A." } }, { "id": "Held-E-V", "name": { "family": "Held", "given": "E. V." } }, { "id": "Rizzi-L", "name": { "family": "Rizzi", "given": "L." }, "orcid": "0000-0003-0882-2327" }, { "id": "Rodighiero-G", "name": { "family": "Rodighiero", "given": "G." }, "orcid": "0000-0002-9415-2296" }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Dias-J-E", "name": { "family": "Dias", "given": "J. E." } }, { "id": "Feruglio-C", "name": { "family": "Feruglio", "given": "C." } }, { "id": "La-Franca-F", "name": { "family": "La Franca", "given": "F." } }, { "id": "Lonsdale-Carol-J", "name": { "family": "Lonsdale", "given": "C. J." }, "orcid": "0000-0003-0898-406X" }, { "id": "Maiolino-R", "name": { "family": "Maiolino", "given": "R." } }, { "id": "Matute-I", "name": { "family": "Matute", "given": "I." }, "orcid": "0000-0003-1177-3896" }, { "id": "Rowan-Robinson-M", "name": { "family": "Rowan-Robinson", "given": "M." } }, { "id": "Sacchi-N", "name": { "family": "Sacchi", "given": "N." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } } ] }, "title": "The ESO-Spitzer Imaging extragalactic Survey (ESIS)\n II. VIMOS I, z wide field imaging of ELAIS-S1 and selection of distant massive galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys \u2013 galaxies: evolution \u2013 cosmology: observations \u2013 galaxies: high-redshift \u2013 galaxies: statistics", "note": "\u00a9 ESO 2008. \n\nReceived 25 April 2008 / Accepted 21 June 2008. \n\nWe wish to thank the anonymous referee for their useful comments which improved the presentation of our results. S.B. was supported by University of Padova and INAF-OaPD grants. S.R. was supported by a University of Padova grant. We are grateful to G. Brammer for providing the EAZY code before its public release. The Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. SWIRE was supported by NASA through the Spitzer Legacy Program under contract 1407 with the Jet Propulsion Laboratory. We acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'\u00c9tudes Spatiales of France and the Korean Ministry of Science and Technology.\n\nPublished - BERaanda08.pdf
", "abstract": "Context. The ESO-Spitzer Imaging extragalactic Survey (ESIS) is the optical follow up of the Spitzer Wide-area Infra-Red Extragalactic survey (SWIRE) in the ELAIS-S1 region of the sky. \n\nAims. In the era of observational cosmology, the main efforts are focused on the study of galaxy evolution and its environmental dependence. Wide area, multiwavelength, extragalactic surveys are needed in order to probe sufficiently large volumes, minimize cosmic variance and find significant numbers of rare objects. \n\nMethods. We present VIMOS I and z band imaging belonging to the ESIS survey. A total of ~4 deg^2 was targeted in I and ~1 deg^2 in z. Accurate data processing includes removal of fringing, and mosaicking of the complex observing pattern. Completeness levels and photometric uncertainties are estimated through simulations. The multi-wavelength data available in the area are exploited to identify high-redshift galaxies, using the IR-peak technique.\nResults. More than 300 000 galaxies have been detected in the I band and ~50 000 in the z band. Object coordinates are defined within an uncertainty of ~0.2 arcsec rms, with respect to GSC 2.2. We reach a 90% average completeness at 23.1 and 22.5 mag (Vega) in the I and z bands, respectively. On the basis of IRAC colors, we identify galaxies having the 1.6 $\\mu$m stellar peak shifted to z = 1-3. The new I, z band data provide reliable constraints to help avoid low-redshift interlopers and reinforce this selection. Roughly 1000 galaxies between z = 2-3 are identified over the ESIS ~4 deg^2, at the SWIRE 5.8 $\\mu$m depth (25.8 $\\mu$Jy at 3$\\sigma$). These are the best galaxy candidates to dominate the massive tail ( M > 1011 $M_\\odot$) of the z > 2 mass function.", "date": "2008-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "488", "number": "2", "publisher": "EDP Sciences", "pagerange": "533-548", "id_number": "CaltechAUTHORS:BERaanda08", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:BERaanda08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1407" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Ministry of Science and Technology (Korea)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361:200810050", "primary_object": { "basename": "BERaanda08.pdf", "url": "https://authors.library.caltech.edu/records/70qga-mjq47/files/BERaanda08.pdf" }, "pub_year": "2008", "author_list": "Berta, S.; Rubele, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/9gds2-5e564", "eprint_id": 13813, "eprint_status": "archive", "datestamp": "2023-08-22 12:30:16", "lastmod": "2023-10-18 14:28:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "N." } }, { "id": "Aldcroft-T", "name": { "family": "Aldcroft", "given": "T." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G. W." } }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "M. S." }, "orcid": "0000-0001-7095-7543" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Lee-K-S", "name": { "family": "Lee", "given": "K.-S." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S." } }, { "id": "Scott-K-S", "name": { "family": "Scott", "given": "K. S." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Tanaguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" } ] }, "title": "Spectroscopic confirmation of an extreme starburst at redshift 4.547", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: interactions; galaxies: starburst; submillimeter", "note": "\u00a9 2008 American Astronomical Society.\nPrint publication: Issue 2 (2008 July 10); received 2008 April 4; accepted for publication 2008 June 4; published 2008 June 27.\nSupport for this work was provided by the Spitzer Science\nCenter which is operated by the Jet Propulsion Laboratory\n(JPL), California Institute of Technology, under NASA contract 1407, NASA through contract 1278386 issued by the JPL, and NASA grant HST-GO-09822. C. C. thanks the Max-Planck-Gesellschaft and the Humboldt-Stiftung for support through the Max-Planck-Forschungspreis.\n\nPublished - CAPapjl08.pdf
", "abstract": "We report the spectroscopic confirmation of a submillimeter galaxy (SMG) at z = 4.547 with an estimated LIR = (0.5\u20132.0) x 10\u00b9\u00b3 L\u2609. The spectra, mid-IR, and X-ray properties indicate the bolometric luminosity is dominated by star formation at a rate of >1000 M\u2609, yr\u207b\u00b9. Multiple, spatially separated components are visible in the Ly\u03b1 line with an observed velocity difference of up to 380 km s\u207b\u00b9 and the object morphology indicates a merger. The best-fit spectral energy distribution and spectral line indicators suggest the object is 2\u20138 Myr old and contains >10\u207b\u00b9\u2070 M\u2609 of stellar mass. This object is a likely progenitor for the massive early-type systems seen at z ~ 2.", "date": "2008-07-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "681", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L53-L56", "id_number": "CaltechAUTHORS:CAPapjl08", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:CAPapjl08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1407" }, { "agency": "NASA", "grant_number": "1278386" }, { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "Max-Planck-Forschungspreis" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/590555", "primary_object": { "basename": "CAPapjl08.pdf", "url": "https://authors.library.caltech.edu/records/9gds2-5e564/files/CAPapjl08.pdf" }, "pub_year": "2008", "author_list": "Capak, Peter; Carilli, C. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/zj9y6-2ct48", "eprint_id": 14431, "eprint_status": "archive", "datestamp": "2023-08-19 22:59:41", "lastmod": "2023-10-18 17:59:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Casey-C-M", "name": { "family": "Casey", "given": "C. M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C. D." } }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J. R." } }, { "id": "Gabor-J-M", "name": { "family": "Gabor", "given": "J." } }, { "id": "Abraham-R-G", "name": { "family": "Abraham", "given": "R. G." }, "orcid": "0000-0002-4542-921X" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" } ] }, "title": "Optical selection of faint active galactic nuclei in the COSMOS field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active, galaxies: luminosity function, mass function, quasars: general, surveys", "note": "\u00a9 2008. The American Astronomical Society. Received 2007 November 22; accepted 2008 February 18.\nWe would like to sincerely thank the COSMOS team; information\non the project is given at the public area of the team Web\nsite http://cosmos.astro.caltech.edu /. We acknowledge the staff\nat Caltech, CFHT, CTIO, KPNO, NAOJ, STSCI, Terapix, and\nthe University of Hawai'i for supporting this work and making\nthe data available. Additional thanks to Annie Robin of\nL'Observatoire de Besanc\u00b8on, Universite\u00b4 de Franche-Compte\u00b4 for\nthe use of her stellar catalog, and to Andy Marble for helpful\nadvice. This work was supported by a GO grant from STSCI.\n\nPublished - CASapjss08.pdf
", "abstract": "We outline a strategy to select faint (i_(AB)<24:5) type 1 active galactic nucleus (AGN) candidates down to the Seyfert/QSO boundary for spectroscopic targeting in the COSMOS field. Our selection process picks candidates by their nonstellar colors in uBVRizK broadband photometry from the Subaru and CFH Telescopes and morphological properties extracted from Hubble Space Telescope (HST ) ACS i-band data. Although the COSMOS field has been used extensively to survey the faint galaxy population out to z ~ 6, AGN optical color selection has not been applied to so faint a level in such a large continuous part of the sky. Hot stars are known to be the dominant contaminant for bright AGN candidate selection at z < 2, but we anticipate the highest color contamination rate at all redshifts to be from faint starburst and compact galaxies. Morphological selection via the Gini Coefficient separates most potential AGNs from these faint blue galaxies. Recent models of the quasar luminosity function (QLF) from Hopkins et al. are used to estimate quasar surface densities, and a recent study of stellar populations in the COSMOS field is applied to infer stellar surface densities and contamination.We use 292 spectroscopically confirmed type 1 broad-line AGN and quasar templates to predict AGN colors as a function of redshift, and then contrast those predictions with the colors\nof known contaminating populations. Since the number of galaxy contaminants cannot be reliably identified with respect to stellar and predicted QLF numbers, the completeness and efficiency of the selection cannot be calculated before gathering confirming spectroscopic observations. Instead we offer an upper limit estimate to selection efficiency (about 50% for low-z and 20%-40% for intermediate-z and high-z) as well as the completeness and efficiency with respect to an X-ray point source population (from the COSMOS AGN Survey), in the range 20%-50%. The motivation of this study and subsequent spectroscopic follow-up is to populate and refine the faint end of the QLF, at both low and high redshifts, where the population of type 1 AGNs is presently not well known. The anticipated AGN\nobservations will add to the ~300 already known AGNs in the COSMOS field, making COSMOS a densely packed\nfield of quasars to be used to understand supermassive black holes and probe the structure of the intergalactic medium in the intervening volume.", "date": "2008-07", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "177", "number": "1", "publisher": "American Astronomical Society", "pagerange": "131-147", "id_number": "CaltechAUTHORS:20090623-115100238", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090623-115100238", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Space Telescope Science Institute", "grant_number": "GO" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/587787", "primary_object": { "basename": "CASapjss08.pdf", "url": "https://authors.library.caltech.edu/records/zj9y6-2ct48/files/CASapjss08.pdf" }, "pub_year": "2008", "author_list": "Casey, C. M.; Impey, C. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/7wbrg-pjc02", "eprint_id": 13807, "eprint_status": "archive", "datestamp": "2023-09-14 18:48:16", "lastmod": "2023-10-23 20:45:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Bondi-M", "name": { "family": "Bondi", "given": "M." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Charlot-S", "name": { "family": "Charlot", "given": "S." } }, { "id": "Ciliegi-P", "name": { "family": "Ciliegi", "given": "P." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Ivezi\u0107-\u017d", "name": { "family": "Ivezi\u0107", "given": "\u017d." }, "orcid": "0000-0001-5250-2633" }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "K." }, "orcid": "0000-0003-3804-2137" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Obri\u0107-M", "name": { "family": "Obri\u0107", "given": "M." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J. R." } }, { "id": "Tremonti-C", "name": { "family": "Tremonti", "given": "C." } }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Walcher-C-J", "name": { "family": "Walcher", "given": "C. J." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } } ] }, "title": "A new method to separate star-forming from AGN galaxies at intermediate redshift : the submillijansky radio population in the VLA-COSMOS survey", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; radio continuum: galaxies; surveys", "note": "\u00a9 2008 The American Astronomical Society.\nPrint publication: Issue 1 (2008 July)\nReceived 2007 September 27; accepted for publication 2008 February 28.\nThe authors would like to thank M. Polletta for the spectral\ntemplate library. V. S. would like to thank E. Bell, G. Fabbiano, G. Helou, and D. Frayer for insightful discussions, as well as M. Schartmann for his help regarding FORTAN compilers. C. C., E. S., and V. S. acknowledge support from NASA grant HSTGO-09822.31-A. C. C. would like to acknowledge support from the Max Planck Society and the Alexander von Humboldt Foundation through the Max-Planck-Forschungspreis 2005. K. J. acknowledges\nsupport by theGermanDFG under grant SCHI 536/3-1. C. J. W. is supported by the MAGPOP Marie Curie EU Research\nand Training Network.\nThis work is based on observations with the National Radio\nAstronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc., the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 05-26555, and XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This work is also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan, the European Southern Observatory, Chile, Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory,\nand the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc., (AURA) under cooperative agreement with the National Science Foundation. It is based also on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products\nproduced at TERAPIX and the CanadianAstronomy Data Centre.\nFunding for the Sloan Digital Sky Survey (SDSS) and\nSDSS-II has been provided by the Alfred P. Sloan Foundation,\nthe Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University\nof Cambridge, Case Western Reserve University, the University of Chicago, Drexel University, Fermilab, the Institute forAdvanced Study, the Japan ParticipationGroup, the Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group,\nthe Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, theMax Planck Institute forAstronomy (MPIA), the Max Planck Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.\n\nPublished - SMOapjss08.pdf
", "abstract": "We explore the properties of the submillijansky radio population at 20 cm by applying a newly developed optical color-based method to separate star-forming (SF) from active galactic nucleus (AGN) galaxies at intermediate redshifts (z \u2272 1.3). Although optical rest-frame colors are used, our separation method is shown to be efficient and not biased against dusty starburst galaxies. This classification method has been calibrated and tested on a local radio-selected optical sample. Given accurate multiband photometry and redshifts, it carries the potential to be generally applicable to any galaxy sample where SF and AGN galaxies are the two dominant populations. In order to quantify the properties of the submillijansky radio population, we have analyzed ~2,400 radio sources, detected at 20 cm in the VLA-COSMOS survey; 90% of these have submillijansky flux densities. We classify the objects into (1) star candidates, (2) quasi-stellar objects, (3) AGN, (4) SF, and (5) high-redshift (z > 1.3) galaxies. We find, for the composition of the submillijansky radio population, that SF galaxies are not the dominant population at submillijansky flux levels, as previously often assumed, but that they make up an approximately constant fraction of 30%-40% in the flux density range of ~50 \u03bcJy to 0.7 mJy. In summary, based on the entire VLA-COSMOS radio population at 20 cm, we find that the radio population at these flux densities is a mixture of roughly 30%-40% of SF and 50%-60% of AGN galaxies, with a minor contribution (~10%) of QSOs.", "date": "2008-07", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "177", "number": "1", "publisher": "American Astronomical Society", "pagerange": "14-38", "id_number": "CaltechAUTHORS:SMOapjss08", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:SMOapjss08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822.31-A" }, { "agency": "Max Planck Society" }, { "agency": "Alexander von Humboldt Foundation" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "SCHI 536/3-1" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Max-Planck-Forschungspreis", "grant_number": "2005" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/588028", "primary_object": { "basename": "SMOapjss08.pdf", "url": "https://authors.library.caltech.edu/records/7wbrg-pjc02/files/SMOapjss08.pdf" }, "pub_year": "2008", "author_list": "Smol\u010di\u0107, V.; Schinnerer, E.; et el." }, { "id": "https://authors.library.caltech.edu/records/kpgsq-r7w29", "eprint_id": 13936, "eprint_status": "archive", "datestamp": "2023-09-14 18:49:23", "lastmod": "2023-10-23 20:45:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K. I." }, "orcid": "0000-0001-8183-1460" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D." }, "orcid": "0000-0003-1924-1122" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Abbas-U", "name": { "family": "Abbas", "given": "U." } }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Bottini-D", "name": { "family": "Bottini", "given": "D." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Cappi-A", "name": { "family": "Cappi", "given": "A." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "S." }, "orcid": "0000-0002-0839-2884" }, { "id": "de-Ravel-L", "name": { "family": "de Ravel", "given": "L." } }, { "id": "Franzetti-P", "name": { "family": "Franzetti", "given": "P." } }, { "id": "Fumana-Marco", "name": { "family": "Fumana", "given": "M." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Halliday-C", "name": { "family": "Halliday", "given": "C." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Kova\u010d-K", "name": { "family": "Kova\u010d", "given": "K." } }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Le-Borgne-J-F", "name": { "family": "Le Borgne", "given": "J. F." } }, { "id": "Maccagni-D", "name": { "family": "Maccagni", "given": "D." } }, { "id": "Marinoni-C", "name": { "family": "Marinoni", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Meneux-B", "name": { "family": "Meneux", "given": "B." } }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Pell\u00f2-R", "name": { "family": "Pell\u00f2", "given": "R." } }, { "id": "P\u00e9rez-Montero-E", "name": { "family": "P\u00e9rez-Montero", "given": "E." } }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Scaramella-R", "name": { "family": "Scaramella", "given": "R." } }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Vergani-D", "name": { "family": "Vergani", "given": "D." } }, { "id": "Walcher-J", "name": { "family": "Walcher", "given": "J." } }, { "id": "Zamojski-M-A", "name": { "family": "Zamojski", "given": "M." } }, { "id": "Zucca-E", "name": { "family": "Zucca", "given": "E." } } ] }, "title": "The optical spectra of 24 \u03bcm galaxies in the COSMOS field. I. Spitzer MIPS bright sources in the zCOSMOS-bright 10k catalog", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : abundances; galaxies : active; galaxies : evolution; infrared : galaxies", "note": "\u00a9 2008. The American Astronomical Society. Received 2007 December 5; accepted 2008 March 6. This paper is based on observations made with VIMOS on the Melipal-VLT telescope, undertaken at the European Southern Observatory (ESO) under Large Program175.A-0839.Also based on observations made with the Spitzer Observatory, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407.\nWe thank our referee Jonathan Gardner for useful comments and suggestions.We are grateful to Gustavo Bruzual and Stephane Charlot for making available the latest version of their synthetic SED template library.\n\nPublished - CAPapj08.pdf
", "abstract": "We study zCOSMOS-bright optical spectra for 609 Spitzer MIPS 24 \u03bcm-selected galaxies with S_(24) \u03bc m > 0.30 mJy and I < 22.5 (AB mag) over 1.5 deg^2 of the COSMOS field. From emission-line diagnostics we find the following: (1) SFRs derived from the observed H\u03b1 \u03bb6563 and H\u03b2 \u03bb4861 lines underestimate, on average, the total SFR by factors of ~5 and 10, respectively. (2) Both the Calzetti et al. and the Milky Way reddening laws are suitable to describe the extinction observed in IR sources in most cases. (3) Some IR galaxies at z < 0.3 have low abundances, but many others with similar IR luminosities and redshifts are chemically enriched. (4) The average [O III] \u03bb5007/H\u03b2 \u03bb4861 ratios of \u03bd L^(24 \u03bc m)_\u03bd > 10^(11) L\u05e1\u05bc galaxies at 0.6 < z < 0.7 are ~0.6 dex higher than the average ratio of all zCOSMOS galaxies at similar redshifts. Massive star formation and AGNs could simultaneously be present in those galaxies with the highest ionizing fluxes. (5) Roughly 1/3 of the galaxies with metallicity measurements at 0.5 < z < 0.7 lie below the general mass-metallicity relation at the corresponding redshifts. The strengths of the 4000 \u00c5 break and the H\u03b4 EW of our galaxies show that secondary bursts of star formation are needed to explain the spectral properties of most IR sources. The LIRG and ULIRG phases occur, on average, between 10^7 and 10^8 yr after the onset of a starburst on top of underlying older stellar populations. These results are valid for galaxies of different IR luminosities at 0.6 < z < 1.0 and seem independent of the mechanisms triggering star formation.", "date": "2008-06-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "680", "number": "2", "publisher": "American Astronomical Society", "pagerange": "939-961", "id_number": "CaltechAUTHORS:20090410-145516020", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090410-145516020", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1407" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/588038", "primary_object": { "basename": "CAPapj08.pdf", "url": "https://authors.library.caltech.edu/records/kpgsq-r7w29/files/CAPapj08.pdf" }, "pub_year": "2008", "author_list": "Caputi, K. I.; Lilly, S. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/9ny29-6r035", "eprint_id": 11382, "eprint_status": "archive", "datestamp": "2023-08-22 11:45:27", "lastmod": "2023-10-16 23:45:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mandelbaum-R", "name": { "family": "Mandelbaum", "given": "R." }, "orcid": "0000-0003-2271-1527" }, { "id": "Seljak-U", "name": { "family": "Seljak", "given": "U." } }, { "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "C. M." }, "orcid": "0000-0002-2951-4932" }, { "id": "Bardelli-S", "name": { "family": "Bardelli", "given": "S." } }, { "id": "Bolzonella-M", "name": { "family": "Bolzonella", "given": "M." } }, { "id": "Bongiorno-A", "name": { "family": "Bongiorno", "given": "A." } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Cunha-C-E", "name": { "family": "Cunha", "given": "C. E." } }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Knobel-C", "name": { "family": "Knobel", "given": "C." } }, { "id": "Koo-David-C", "name": { "family": "Koo", "given": "D. C." }, "orcid": "0000-0003-3385-6799" }, { "id": "Lamareille-F", "name": { "family": "Lamareille", "given": "F." } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Leborgne-J-F", "name": { "family": "Leborgne", "given": "J.-F." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Newman-J-A", "name": { "family": "Newman", "given": "J. A." }, "orcid": "0000-0001-8684-2222" }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P. A." }, "orcid": "0000-0001-5851-6649" }, { "id": "Perez-Montero-E", "name": { "family": "Perez-Montero", "given": "E." } }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } } ] }, "title": "Precision photometric redshift calibration for galaxy\u2013galaxy weak lensing", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing; redshifts", "note": "\u00a9 2008 The Authors. Journal compilation \u00a9 2008 RAS. \n\nAccepted 2008 January 10. Received 2007 December 21; in original form 2007 September 11. \n\nRM is supported by NASA through Hubble Fellowship grant #HST-HF-01199.02-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. US is supported by the Packard Foundation and NSF CAREER-0132953, and the Swiss National Science Foundation (SNF). We thank Josh Frieman, Marcos Lima, Huan Lin, Hiro Oyaizu, Nikhil Padmanabhan and Erin Sheldon for useful discussion about a variety of topics addressed in this paper. \n\nFunding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS web site is http://www.sdss.org/. \n\nThe SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington. \n\nFunding for the DEEP2 survey has been provided by NSF grants AST-0071048, AST-0071198, AST-0507428 and AST-0507483. \n\nSome of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The DEEP2 team and Keck Observatory acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community and appreciate the opportunity to conduct observations from this mountain. \n\nBased in part on observations undertaken at the European Southern Observatory (ESO) Very Large Telescope (VLT) under Large Programme 175.A-0839. \n\n[R.M. was a] Hubble Fellow.\n\nPublished - MANmnras08b.pdf
", "abstract": "Accurate photometric redshifts are among the key requirements for precision weak lensing measurements. Both the large size of the Sloan Digital Sky Survey (SDSS) and the existence of large spectroscopic redshift samples that are flux-limited beyond its depth have made it the optimal data source for developing methods to properly calibrate photometric redshifts for lensing. Here, we focus on galaxy\u2013galaxy lensing in a survey with spectroscopic lens redshifts, as in the SDSS. We develop statistics that quantify the effect of source redshift errors on the lensing calibration and on the weighting scheme, and show how they can be used in the presence of redshift failure and sampling variance. We then demonstrate their use with 2838 source galaxies with spectroscopy from DEEP2 and zCOSMOS, evaluating several public photometric redshift algorithms, in two cases including a full p(z) for each object, and find lensing calibration biases as low as <1 per cent (due to fortuitous cancellation of two types of bias) or as high as 20 per cent for methods in active use (despite the small mean photoz bias of these algorithms). Our work demonstrates that lensing-specific statistics must be used to reliably calibrate the lensing signal, due to asymmetric effects of (frequently non-Gaussian) photoz errors. We also demonstrate that large-scale structure (LSS) can strongly impact the photoz calibration and its error estimation, due to a correlation between the LSS and the photoz errors, and argue that at least two independent degree-scale spectroscopic samples are needed to suppress its effects. Given the size of our spectroscopic sample, we can reduce the galaxy\u2013galaxy lensing calibration error well below current SDSS statistical errors.", "date": "2008-05-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "386", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "781-806", "id_number": "CaltechAUTHORS:MANmnras08b", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:MANmnras08b", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-01199.02-A" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Higher Education Funding Council for England" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "Max Planck Society" }, { "agency": "NSF", "grant_number": "AST-0132953" }, { "agency": "Participating Institutions" }, { "agency": "Department of Energy (DOE)" }, { "agency": "ESO VLT Large Programme", "grant_number": "175.A-0839" }, { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "NSF", "grant_number": "AST-0071048" }, { "agency": "NSF", "grant_number": "AST-0071198" }, { "agency": "NSF", "grant_number": "AST-0507428" }, { "agency": "NSF", "grant_number": "AST-0507483" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "COSMOS" } ] }, "doi": "10.1111/j.1365-2966.2008.12947.x", "primary_object": { "basename": "MANmnras08b.pdf", "url": "https://authors.library.caltech.edu/records/9ny29-6r035/files/MANmnras08b.pdf" }, "pub_year": "2008", "author_list": "Mandelbaum, R.; Seljak, U.; et el." }, { "id": "https://authors.library.caltech.edu/records/dzx3d-6mk84", "eprint_id": 14264, "eprint_status": "archive", "datestamp": "2023-08-22 11:38:39", "lastmod": "2023-10-18 16:26:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Faure-C", "name": { "family": "Faure", "given": "Cecile" } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "Jean-Paul" }, "orcid": "0000-0002-4616-4989" }, { "id": "Covone-G", "name": { "family": "Covone", "given": "Giovanni" } }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "Lidia" } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "Knud" }, "orcid": "0000-0003-3804-2137" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "Vernesa" }, "orcid": "0000-0002-3893-8614" }, { "id": "de-la-Torre-S", "name": { "family": "de la Torre", "given": "Sylvain" }, "orcid": "0000-0002-0839-2884" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard" }, "orcid": "0000-0001-7782-7071" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "Alexis" }, "orcid": "0000-0002-4606-5403" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton" }, "orcid": "0000-0002-6610-2048" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "Oliver" }, "orcid": "0000-0001-5891-2596" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "Richard" }, "orcid": "0000-0002-6085-3780" }, { "id": "Mellier-Y", "name": { "family": "Mellier", "given": "Yannick" } }, { "id": "Refregier-A", "name": { "family": "Refregier", "given": "Alexandre" } }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Taylor-J-E", "name": { "family": "Taylor", "given": "James" } }, { "id": "Van-Waerbeke-L", "name": { "family": "Van Waerbeke", "given": "Ludovic" } }, { "id": "Walcher-J", "name": { "family": "Walcher", "given": "Jakob" } } ] }, "title": "First catalog of strong lens candidates in the COSMOS field", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: statistics; gravitational lensing", "note": "\u00a9 2008 The American Astronomical Society. \n\nReceived 2007 March 5; accepted 2007 November 2. \n\nThe HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We wish to thank Tony Roman, Denise Taylor, and David Soderblom for their assistance in the planning and scheduling of the extensive COSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy (AURA) Inc., under NASA contract NAS 05-26555; also based on data collected at the Subaru\nTelescope, which is operated by the National Astronomical Observatory of Japan; the European Southern Observatory under Large Program 175.A-0839, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by AURA, Inc., under cooperative agreement with the National Science Foundation. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope which is operated by the National Research Council of Canada, the Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS data sets. C. F. acknowledges support from the European Community's Sixth Framework Marie Curie Research Training Network Programme, contract MRTN-CT-2004-505183 \"ANGLES.\" J. P. K. acknowledges support from CNRS and Caltech. G. C. is partially supported by the Cordis ERG proposal 029159.We thank the referee for useful remarks and J. Duke for correcting the draft. \n\nFacilities: HST (ACS), Subaru (Suprime). CFHT (Megacam).\n\nPublished - FAUapjss08.pdf
", "abstract": "We present the first catalog of 67 strong galaxy-galaxy lens candidates discovered in the 1.64 deg^2 Hubble Space Telescope COSMOS survey. Twenty of these systems display multiple images or strongly curved large arcs. Our initial search is performed by visual inspection of the data and is restricted, for practical considerations, to massive early-type lens galaxies with arcs found at radii smaller than ~5\". Simple mass models are constructed for the best lens candidates, and our results are compared to the strong lensing catalogs of the SLACS survey and the CASTLES database. These new strong galaxy-galaxy lensing systems constitute a valuable sample to study the mass distribution of early-type galaxies and their associated dark matter halos. We further expect this sample to play an important role in the testing of software algorithms designed to automatically search for strong gravitational lenses. From our analysis a robust lower limit is derived for the expected occurrence of strong galaxy-galaxy systems in current and future space-based wide-field imaging surveys. We expect that such surveys should uncover a large number of strong lensing systems (more than 10 systems per square degree), which will allow for a detailed statistical analysis of galaxy properties and will likely lead to constraints on models of gravitational structure formation and cosmology.", "date": "2008-05", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "176", "number": "1", "publisher": "American Astronomical Society", "pagerange": "19-38", "id_number": "CaltechAUTHORS:20090519-093146142", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090519-093146142", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NASA", "grant_number": "NAS 05-26555" }, { "agency": "Marie Curie Fellowship", "grant_number": "MRTN-CT-2004-505183 ''ANGLES''" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Caltech" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/526426", "primary_object": { "basename": "FAUapjss08.pdf", "url": "https://authors.library.caltech.edu/records/dzx3d-6mk84/files/FAUapjss08.pdf" }, "pub_year": "2008", "author_list": "Faure, Cecile; Kneib, Jean-Paul; et el." }, { "id": "https://authors.library.caltech.edu/records/khfry-9a133", "eprint_id": 14063, "eprint_status": "archive", "datestamp": "2023-08-22 11:35:27", "lastmod": "2023-10-18 16:05:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scott-K-S", "name": { "family": "Scott", "given": "K. S." } }, { "id": "Austermann-J-E", "name": { "family": "Austermann", "given": "J. E." } }, { "id": "Perera-T-A", "name": { "family": "Perera", "given": "T. A." } }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G. W." } }, { "id": "Aretxaga-I", "name": { "family": "Aretxaga", "given": "I." }, "orcid": "0000-0002-6590-3994" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "D. H." } }, { "id": "Kang-Y", "name": { "family": "Kang", "given": "Y." } }, { "id": "Kim-S", "name": { "family": "Kim", "given": "S." } }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "M. S." }, "orcid": "0000-0001-7095-7543" } ] }, "title": "AzTEC millimetre survey of the COSMOS field \u2013 I. data reduction and source catalogue", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxes: high-redshift; galaxies: starburst; submillimetre", "note": "\u00a92008 The Authors. Journal compilation \u00a92008 RAS.\nAccepted 2008 January 17. Received 2008 January 16; in original form 2007 November 16.\nThe authors are grateful to J. Aguirre, J. Karakla, K. Souccar, I. Coulson, R. Tilanus, R. Kackley, D. Haig, S. Doyle, J. Lowenthal and the observatory staff at the JCMT who made these observations possible. Support for this work was provided in part by the NSF grant AST 05-40852 and the grant from the Korea Science & Engineering Foundation (KOSEF) under a cooperative Astrophysical Research Centre of the Structure and Evolution of the Cosmos (ARCSEC). IA and DH acknowledge partial support by CONACyT from research grants 39953-F and 39548-F. This research has made use of the NASA/IPAC Extragalactic Database which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nPublished - SCOmnras08.pdf
", "abstract": "We present a 1.1mm wavelength imaging survey covering 0.3 deg^2 in the COSMOS field. These data, obtained with the AzTEC continuum camera on the James Clerk Maxwell Telescope, were centred on a prominent large-scale structure overdensity which includes a rich X-ray cluster at z \u2248 0.73. A total of 50 mm-galaxy candidates, with a significance ranging from 3.5 to 8.5\u03c3, are extracted from the central 0.15 deg^2 area which has a uniform sensitivity of \u223c1.3 mJy beam^\u22121. 16 sources are detected with S/N \u2265 4.5, where the expected false detection rate is zero, of which a surprisingly large number (9) have intrinsic (deboosted) fluxes \u22655 mJy at 1.1 mm. Assuming the emission is dominated by radiation from dust, heated by a massive population of young, optically obscured stars, then these bright AzTEC sources have far-infrared luminosities >6 \u00d7 10^(12)L_\u2609 and star formation rates \u22651100M_\u2609 yr^(\u22121). Two of these nine bright AzTEC sources are found towards the extreme peripheral region of the X-ray cluster, whilst the remainder are distributed across the larger scale overdensity. We describe the AzTEC data reduction pipeline, the source-extraction algorithm, and the characterization of the source catalogue, including the completeness, flux deboosting correction, false-detection rate and the source positional uncertainty, through an extensive set of Monte Carlo simulations. We conclude with a preliminary comparison, via a stacked analysis, of the overlapping MIPS 24-\u03bcm data and radio data with this AzTEC map of the COSMOS field.", "date": "2008-04-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "385", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "2225-2238", "id_number": "CaltechAUTHORS:20090423-212245434", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090423-212245434", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 05-40852" }, { "agency": "Korea Science & Engineering Foundation (KOSEF)" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "39953-F" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "39548-F" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2008.12989.x", "primary_object": { "basename": "SCOmnras08.pdf", "url": "https://authors.library.caltech.edu/records/khfry-9a133/files/SCOmnras08.pdf" }, "pub_year": "2008", "author_list": "Scott, K. S.; Austermann, J. E.; et el." }, { "id": "https://authors.library.caltech.edu/records/ybwwj-4pd67", "eprint_id": 13934, "eprint_status": "archive", "datestamp": "2023-08-22 11:26:09", "lastmod": "2023-10-18 15:58:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Melbourne-J-L", "name": { "family": "Melbourne", "given": "J." } }, { "id": "Ammons-M", "name": { "family": "Ammons", "given": "M." } }, { "id": "Wright-S-A", "name": { "family": "Wright", "given": "S. A." }, "orcid": "0000-0003-1034-8054" }, { "id": "Metevier-A-J", "name": { "family": "Metevier", "given": "A." } }, { "id": "Steinbring-E", "name": { "family": "Steinbring", "given": "E." } }, { "id": "Max-C-E", "name": { "family": "Max", "given": "C." }, "orcid": "0000-0003-0682-5436" }, { "id": "Koo-David-C", "name": { "family": "Koo", "given": "D. C." }, "orcid": "0000-0003-3385-6799" }, { "id": "Larkin-J-E", "name": { "family": "Larkin", "given": "J. E." }, "orcid": "0000-0001-7687-3965" }, { "id": "Barczys-M", "name": { "family": "Barczys", "given": "M." } } ] }, "title": "Triggered or self-regulated star formation within intermediate redshift luminous infrared galaxies. I. Morphologies and spectral energy distributions", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: spiral; galaxies: starburst; galaxies: stellar content; infrared: galaxies; instrumentation: adaptive optics", "note": "\u00a9 2008 The American Astronomical Society.\nReceived 2007 August 29; accepted 2007 December 22; published 2008 March 4.\nWe would like to thank Emeric Le Floc'h for contributing\nthe 24 \u03bcm measurements of GOODS-S galaxies. This work\nhas been supported in part by the NSF Science and Technology\nCenter for Adaptive Optics, managed by the University of California\n(UC) at Santa Cruz under the cooperative agreement No.\nAST-9876783. It was also supported by the HST archival grant\nHST-AR-10965. The laser guide star adaptive optics system was\nfunded by the W.M. Keck Foundation. The artificial laser guide\nstar system was developed and integrated in a partnership between\nthe Lawrence Livermore National Labs (LLNL) and the\nW.M. Keck Observatory. The laser was integrated at Keck with\nthe help of Curtis Brown and Pamela Danforth. The NIRC2\nnear-infrared camera was developed by CalTech, UCLA and\nKeck (P.I. Keith Matthews). The data presented herein were obtained\nat the Keck Observatory, which is operated as a scientific\npartnership among the CalTech, UC and NASA. This work is\nsupported in part under the auspices of the US Department of\nEnergy, National Nuclear Security Administration and by the\nLLNL under contract W-7405-Eng-48. The authors wish to recognize\nand acknowledge the very significant cultural role and\nreverence that the summit of Mauna Kea has always had within\nthe indigenous Hawaiian community. We are most fortunate to\nhave the opportunity to conduct observations from this superb\nmountain.\n\nPublished - MELaj08a.pdf
", "abstract": "As part of the Center for Adaptive Optics (AO) Treasury Survey (CATS) we imaged a set of 15 intermediate redshift (z ~ 0.8) luminous infrared (IR) galaxies (LIRGs) with the Keck Laser Guide Star (LGS) AO facility. These galaxies were selected from the Great Observatories Origins Deep Survey (GOODS) southern field, allowing us to combine the high spatial resolution Hubble Space Telescope optical (B, V, i, and z-bands) images with our near-infrared (K'-band) images to study the LIRG morphologies and spatially resolved spectral energy distributions (SEDs). Two thirds of the LIRGs are disk galaxies, with only one third showing some evidence for interactions, minor, or major mergers. In contrast with local LIRG disks (which are primarily barred systems), only 10% of the LIRG disks in our sample contain a prominent bar. While the optical bands tend to show a significant point-like substructure, indicating distributed star formation, the AO K-band images tend to be smooth. They lack point-like structures to a K ~ 23.5 limit. This places an upper bound on the number of red super giants per blue knot at less than 4000. The SEDs of the LIRGs are consistent with distributed dusty star formation, as exhibited by optical to IR colors redder than allowed by old stellar populations alone. This effect is most pronounced in the galaxy cores, possibly indicating central star formation. We also observed a set of 11 intermediate redshift comparison galaxies, selected to be non-ellipticals with apparent K-band magnitudes comparable to the LIRGs. The \"normal\" (non-LIRG) systems tended to have lower optical luminosity, lower stellar mass, and more irregular morphology than the LIRGs. Half of the \"normal\" galaxies have SEDs consistent with intermediate aged stellar populations and minimal dust. The other half show evidence for some dusty star formation, usually concentrated in their cores. Our work suggests that the LIRG disk galaxies are similar to large disk systems today, undergoing self-regulated star formation, only at 10-20 times higher rates.", "date": "2008-04", "date_type": "published", "publication": "Astronomical Journal", "volume": "135", "number": "4", "publisher": "American Astronomical Society", "pagerange": "1207-1224", "id_number": "CaltechAUTHORS:20090410-141816524", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090410-141816524", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-9876783" }, { "agency": "Hubble Space Telescope", "grant_number": "HST-AR-10965" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "W-7405-ENG-48" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-6256/135/4/1207", "primary_object": { "basename": "MELaj08a.pdf", "url": "https://authors.library.caltech.edu/records/ybwwj-4pd67/files/MELaj08a.pdf" }, "pub_year": "2008", "author_list": "Melbourne, J.; Ammons, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/w7f6e-1ar67", "eprint_id": 14232, "eprint_status": "archive", "datestamp": "2023-08-22 11:19:18", "lastmod": "2023-10-18 16:24:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Elmegreen-D-M", "name": { "family": "Elmegreen", "given": "Debra Meloy" }, "orcid": "0000-0002-1392-3520" }, { "id": "Elmegreen-B-G", "name": { "family": "Elmegreen", "given": "Bruce G." }, "orcid": "0000-0002-1723-6330" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Abraham-R-G", "name": { "family": "Abraham", "given": "Roberto G." }, "orcid": "0000-0002-4542-921X" }, { "id": "Athanassoula-E", "name": { "family": "Athanassoula", "given": "E." } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Spalsbury-L", "name": { "family": "Spalsbury", "given": "Lori" } }, { "id": "Strubbe-L-E", "name": { "family": "Strubbe", "given": "Linda" } }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "Marcella C." }, "orcid": "0000-0003-1624-7609" }, { "id": "Rich-Michael-R", "name": { "family": "Rich", "given": "Michael R." } }, { "id": "West-A-A", "name": { "family": "West", "given": "Andrew A." } } ] }, "title": "Evolution of the bar fraction in COSMOS: quantifying the assembly of the Hubble sequence", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: general; galaxies: high-redshift; galaxies: spiral; galaxies: structure", "note": "\u00a9 2008 The American Astronomical Society. \n\nReceived 2007 July 27, accepted for publication 2007 October 23. \n\nWe are indebted to the anonymous referee for many helpful comments and suggestions that have greatly improved this paper. We are also thankful for the insightful and helpful discussions we have had with Karin Menendez-Delmestre, Neal Evans, Lee Armus, Isaac Shlosman, Wyn Evans, Donald Lynden-Bell, Mark Dickinson, David Elbaz, Francois Schweizer, Tomasso Treu, Jason Melbourne, Dan Kelson, and Luis Ho. The HST COSMOS Treasury program was supported through NASA grant HST-GO- 09822.We wish to thank Tony Roman, Denise Taylor, and David Soderblom for their assistance in planning and scheduling of the extensive COSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. It is a pleasure the acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman and John Good) in providing online archive and server capabilities for the COSMOS data sets. We also wish to acknowledge support for the COSMOS Science meeting in May 2005 which was supported in part by NSF grant OISE-0456439.\n\nPublished - SHEapj08b.pdf
", "abstract": "We have analyzed the redshift-dependent fraction of galactic bars over 0.2 < z < 0.84 in 2157 luminous face-on spiral galaxies from the COSMOS 2 deg^2 field. Our sample is an order of magnitude larger than that used in any previous investigation, and is based on substantially deeper imaging data than that available from earlier wide-area studies of high-redshift galaxy morphology. We find that the fraction of barred spirals declines rapidly with redshift. Whereas in the local universe about 65% of luminous spiral galaxies contain bars (SB+SAB), at z ~ 0.84 this fraction drops to about 20%. Over this redshift range the fraction of strong bars (SBs) drops from about 30% to under 10%. It is clear that when the universe was half its present age, the census of galaxies on the Hubble sequence was fundamentally different from that of the present day. A major clue to understanding this phenomenon has also emerged from our analysis, which shows that the bar fraction in spiral galaxies is a strong function of stellar mass, integrated color and bulge prominence. The bar fraction in very massive, luminous spirals is about constant out to z ~ 0.84, whereas for the low-mass, blue spirals it declines significantly with redshift beyond z = 0.3. There is also a slight preference for bars in bulge-dominated systems at high redshifts that may be an important clue toward the coevolution of bars, bulges, and black holes. Our results thus have important ramifications for the processes responsible for galactic downsizing, suggesting that massive galaxies matured early in a dynamical sense, and not just as a result of the regulation of their star formation rate.", "date": "2008-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "671", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1141-1155", "id_number": "CaltechAUTHORS:20090515-082515631", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090515-082515631", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NSF", "grant_number": "OISE-0456439" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/524980", "primary_object": { "basename": "SHEapj08b.pdf", "url": "https://authors.library.caltech.edu/records/w7f6e-1ar67/files/SHEapj08b.pdf" }, "pub_year": "2008", "author_list": "Sheth, Kartik; Elmegreen, Debra Meloy; et el." }, { "id": "https://authors.library.caltech.edu/records/jy4kh-3s480", "eprint_id": 14097, "eprint_status": "archive", "datestamp": "2023-08-22 10:56:41", "lastmod": "2023-10-18 16:06:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Liu-Charles-T", "name": { "family": "Liu", "given": "Charles T." }, "orcid": "0000-0002-4314-8713" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Paglione-T-A-D", "name": { "family": "Paglione", "given": "Timothy A. D." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Tribiano-S-M", "name": { "family": "Tribiano", "given": "Shana M." } }, { "id": "Tyson-N-D", "name": { "family": "Tyson", "given": "Neil D." } } ] }, "title": "The faint-end slopes of galaxy luminosity functions in the COSMOS field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: dwarf; galaxies: evolution; galaxies: fundamental parameters; galaxies: luminosity function, mass function; surveys", "note": "\u00a9 2008 The American Astronomical Society.\nReceived 2006 August 11; accepted 2007 August 9.\nThe HST COSMOS Treasury program was supported through\nNASA grant HST-GO-09822. We wish to thank Tony Roman,\nDenise Taylor, and David Soderblom for their assistance in the\nplanning and scheduling of the extensive COSMOS observations.\nWe gratefully acknowledge the contributions of the entire\nCOSMOS collaboration, which contains more than 70 scientists.\nMore information on the COSMOS survey is available at http://\nwww.astro.caltech.edu/~cosmos. It is a pleasure to acknowledge\nthe excellent services provided by the NASA IPAC/IRSA staff\n(Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John\nGood) in providing online archive and server capabilities for the\nCOSMOS data sets. The COSMOS Science meeting in 2005\nMay was supported in part by the NSF through grant OISE-\n0456439. We thank Paris Bogdanos and James Cohen for image\nprocessing and data formatting assistance. C. Liu, T. Paglione,\nand S. Tribiano gratefully acknowledge support from a City University\nof New York CCIR grant, as well as the hospitality and\nsupport of the Hayden Planetarium and Department of Astrophysics\nat the American Museum of Natural History.\nFacilities: HST (ACS), Subaru, KPNO, CTIO, CFHT.\n\nPublished - LIUapj08.pdf
", "abstract": "We examine the faint-end slope of the rest-frame V-band luminosity function (LF), with respect to galaxy spectral type, of field galaxies with redshift z < 0.5, using a sample of 80,820 galaxies with photometric redshifts in the 2 deg^2 Cosmic Evolution Survey (COSMOS) field. For all galaxy spectral types combined, the LF slope ranges from \u20131.24 to \u20131.12, from the lowest redshift bin to the highest. In the lowest redshift bin (0.02 < z < 0.1), where the magnitude limit is MV \u227e \u2212 13, the slope ranges from \u03b1 ~ \u2212 1.1 for galaxies with early-type spectral energy distributions (SEDs) to \u03b1 ~ \u2212 1.9 for galaxies with low-extinction starburst SEDs. In each galaxy SED category (early-type, Sbc, Scd+Irr, and starburst), the faint-end slopes grow shallower with increasing redshift; in the highest redshift bin (0.4 < z < 0.5), \u03b1 ~ \u2212 0.5 and \u20131.3 for early types and starbursts, respectively. The steepness of \u03b1 at lower redshifts could be qualitatively explained by LF evolution, or by large numbers of faint dwarf galaxies, perhaps of low surface brightness, that are not detected at higher redshifts.", "date": "2008-01-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "672", "number": "1", "publisher": "American Astronomical Society", "pagerange": "198-206", "id_number": "CaltechAUTHORS:20090428-091919193", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090428-091919193", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1086/522361", "primary_object": { "basename": "LIUapj08.pdf", "url": "https://authors.library.caltech.edu/records/jy4kh-3s480/files/LIUapj08.pdf" }, "pub_year": "2008", "author_list": "Liu, Charles T.; Capak, Peter; et el." }, { "id": "https://authors.library.caltech.edu/records/wyhbb-j0387", "eprint_id": 12518, "eprint_status": "archive", "datestamp": "2023-08-22 10:56:27", "lastmod": "2023-10-17 17:02:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kocevski-D-D", "name": { "family": "Kocevski", "given": "Dale D." } }, { "id": "Lubin-L-M", "name": { "family": "Lubin", "given": "Lori M." } }, { "id": "Gal-R-R", "name": { "family": "Gal", "given": "Roy" } }, { "id": "Lemaux-B-C", "name": { "family": "Lemaux", "given": "Brian C." }, "orcid": "0000-0002-1428-7036" }, { "id": "Fassnacht-C-D", "name": { "family": "Fassnacht", "given": "Christopher D." }, "orcid": "0000-0002-4030-5461" }, { "id": "Squires-G-K", "name": { "family": "Squires", "given": "Gordon K." }, "orcid": "0000-0002-1977-5717" } ] }, "title": "Chandra Observations of the cl1604 Supercluster at z = 0.9: Evidence for an Overdensity of Active Galactic Nuclei", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general; large-scale structure of universe; X-rays: galaxies: clusters", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2008 April 11, accepted for publication 2008 August 11. Published 2008 December 1. Print publication: Issue 1 (2009 January 1). \n\nWe thank Patrick Henry and Harald Ebeling for several useful discussions. This work is supported by the Chandra General Observing Program under award number GO6-7114X. Additional support for this program was provided by NASA through a grant HST-GO-11003 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. The spectrographic data used herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. \n\nOnline-only material: color figures, machine-readable tables.\n\nPublished - KOCapj09.pdf
", "abstract": "We present the results of Chandra observations of the Cl1604 supercluster at z ~ 0.9. The system is the largest structure mapped at redshifts approaching unity, containing at least eight spectroscopically confirmed galaxy clusters and groups. Using two 50 ks ACIS-I pointings we examine both the X-ray point-source population and the diffuse emission from individual clusters in the system. Over an area encompassing the entire supercluster (~0.154 deg2), we find a 2.5\u03c3 excess of point sources detected in the hard band (2-10 keV) relative to the number of sources found in blank fields observed by Chandra. No such excess is observed in the soft band (0.5-2 keV). The hard-band source density is 1.47 times greater than that of a blank field, in agreement with the previously reported correlation between overdensity amplitude and cluster redshift. Using a maximum likelihood technique, we have matched 112 of the 161 detected X-ray point sources to optical counterparts and found 15 sources that are associated with the supercluster. All 15 sources have rest-frame luminosities consistent with emission from active galactic nuclei (AGNs). We find that the supercluster AGNs largely avoid the densest regions of the system and are instead distributed on the outskirts of massive clusters or within poorer clusters and groups. We have also detected diffuse emission from two of the eight clusters and groups in the system, clusters Cl1604 + 4304 and Cl1604 + 4314. The systems have bolometric luminosities of 1.43 \u00d7 10^44 and 8.20 \u00d7 10^43 h70^\u20132 erg s^\u20131 and gas temperatures of 3.50+1.82 \u20131.08 and 1.64+0.65 \u20130.45 keV, respectively. Using updated velocity dispersions, we compare the properties of these systems with the cluster scaling relations followed by other X-rays and optically selected galaxy clusters at high redshift.", "date": "2008-01-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "690", "number": "1", "publisher": "American Astronomical Society", "pagerange": "295-318", "id_number": "CaltechAUTHORS:KOCapj09", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:KOCapj09", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Chandra General Observing Program", "grant_number": "GO6-7114X" }, { "agency": "Space Telescope Science Institute", "grant_number": "HST-GO-11003" }, { "agency": "Association of Universities for Research in Astronomy, Inc." }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "W.M. Keck Foundation" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "COSMOS", "value": "COSMOS" } ] }, "doi": "10.1088/0004-637X/690/1/295", "primary_object": { "basename": "KOCapj09.pdf", "url": "https://authors.library.caltech.edu/records/wyhbb-j0387/files/KOCapj09.pdf" }, "pub_year": "2008", "author_list": "Kocevski, Dale D.; Lubin, Lori M.; et el." }, { "id": "https://authors.library.caltech.edu/records/tpy1j-hvr23", "eprint_id": 58789, "eprint_status": "archive", "datestamp": "2023-08-19 21:56:49", "lastmod": "2023-10-23 19:43:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Spectroscopic surveys of cosmic evolution", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2007 Springer Science+Business Media B.V.\n\nReceived: 3 April 2007; Accepted: 9 October 2007; Published online: 26 October 2007.\n\nThe major COSMOS datasets become publicly available in staged releases (following calibration and validation) through the web site for IPAC/IRSA: http://irsa.ipac.caltech.edu/data/COSMOS/. I gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822.", "abstract": "ALMA will be the premier instrument for the study of galaxy evolution in the early universe\u2014enabling studies of the gas content, dynamics and dynamical masses, and star formation with unparalleled resolution and sensitivity. Galaxy evolution and AGN growth in the early universe are believed to be strongly driven by merging and dynamical interactions. Thus, a full exploration of the environmental influence is absolutely essential. The Cosmic Evolution Survey (COSMOS) is specifically designed to probe the correlated coevolution of galaxies, star formation, active galactic nuclei (AGN) and dark matter (DM) large-scale structure (LSS) over the redshift range z>0.5 to 3. In this contribution I review the characteristics of the COSMOS survey and very exciting initial results on mapping large scale structure in galaxies and dark matter. The survey includes multi-wavelength imaging and spectroscopy from X-ray to radio wavelengths covering a 2 square degree equatorial field. Given the very high sensitivity and resolution of these datasets, COSMOS will provide unprecedented samples of objects at z>3 for followup studies wit ALMA.", "date": "2008-01", "date_type": "published", "publication": "Astrophysics and Space Science", "volume": "313", "number": "1-3", "publisher": "Springer", "pagerange": "287-291", "id_number": "CaltechAUTHORS:20150707-103319097", "issn": "0004-640X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150707-103319097", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1007/s10509-007-9685-3", "pub_year": "2008", "author_list": "Scoville, Nick" }, { "id": "https://authors.library.caltech.edu/records/vj16w-nt636", "eprint_id": 17536, "eprint_status": "archive", "datestamp": "2023-08-22 09:53:17", "lastmod": "2023-10-19 23:58:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Benson-A-J", "name": { "family": "Benson", "given": "A." }, "orcid": "0000-0001-5501-6008" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "El-Zant-A", "name": { "family": "El-Zant", "given": "A." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Koda-Jin", "name": { "family": "Koda", "given": "J." }, "orcid": "0000-0002-8762-7863" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Massey-R", "name": { "family": "Massey", "given": "R." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S. S." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P. L." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Taylor-J-E", "name": { "family": "Taylor", "given": "J. E." } }, { "id": "Thompson-D-J", "name": { "family": "Thompson", "given": "D. J." } } ] }, "title": "Large Structures and Galaxy Evolution in COSMOS at z < 1.1", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; dark matter; large-scale structure of universe; surveys", "note": "\u00a9 2007 American Astronomical Society. \n\nPrint publication: Issue 1 (2007 September); received 2006 April 25; accepted for publication 2006 September 22. \n\nThe HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at http://cosmos.astro.caltech.edu. The COSMOS Science meeting in 2005 May in Kyoto, Japan was supported in part by the NSF through grant OISE-0456439. Major work on this project was done while N. Z. S. was on sabbatical at the Institute for Astronomy at the University of Hawaii and during a visit at the Aspen Center For Physics. We would also like to thank the referee for a number of suggestions which have greatly improved this paper. \n\nFacilities: HST (ACS), HST (NICMOS), HST (WFPC2), Subaru (SCAM).\n\nPublished - SCOapjss07c.pdf
", "abstract": "We present the first identification of large-scale structures (LSSs) at z < 1.1 in the Cosmic Evolution Survey (COSMOS). The structures are identified from adaptive smoothing of galaxy counts in the pseudo-3D space (\u03b1, \u03b4, z) using the COSMOS photometric redshift catalog. The technique is tested on a simulation including galaxies distributed in model clusters and a field galaxy population\u2014recovering structures on all scales from 1' to 20' without a priori assumptions for the structure size or density profile. The COSMOS photometric redshift catalog yields a sample of 1.5 \u00d7 10^5 galaxies with redshift accuracy, \u0394_z_(FWHM)/(1 + z) \u2264 0.1 at z < 1.1 down to I_(AB) \u2264 25 mag. Using this sample of galaxies, we identify 42 LSSs and clusters. Projected surface-density maps for the structures indicate multiple peaks and internal structure in many of the most massive LSSs. The stellar masses (determined from the galactic SEDs) for the LSSs range from M_* ~ 10^(11) up to ~3 \u00d7 10^(13) M_\u2609. Five LSSs have total stellar masses exceeding 10^13 M_\u2609. (Total masses including nonstellar baryons and dark matter are expected to be ~50-100 times greater.) The derived mass function for the LSSs is consistent (within the expected Poisson and cosmic variances) with those derived from optical and X-ray studies at lower redshift. To characterize structure evolution and for comparison with simulations, we compute a new statistic: the area filling factor as a function of the overdensity value compared to the mean at surface overdensity (f_A [\u03a3/\u03a3(overbar)(z)). The observationally determined f_A has less than 1% of the surface area (in each redshift slice) with overdensities exceeding 10:1, and evolution to higher overdensities is seen at later epochs (lower z); both characteristics are in good agreement with what we find using similar processing on the Millennium Simulation. Although similar variations in the filling factors as a function of overdensity and redshift are seen in the observations and simulations, we do find that the observed distributions reach higher overdensities than the simulation, perhaps indicating overmerging in the simulation. All of the LSSs show a dramatic preference for earlier SED type galaxies in the denser regions of the structures, independent of redshift. The SED types in the central 1 and 1-5 Mpc regions of each structure average about one SED type earlier than the mean type at the same redshift, corresponding to a stellar population age difference of ~2-4 Gyr at z = 0.3-1. We also investigate the evolution of key galactic properties\u2014mass, luminosity, SED, and star formation rate (SFR)\u2014with redshift and environmental density as derived from overdensities in the full pseudo-3D cube. Both the maturity of the stellar populations and the \"downsizing\" of star formation in galaxies vary strongly with redshift (epoch) and environment. For a very broad mass range (10^(10)-10^(12) M_\u2609), we find that galaxies in dense environments tend to be older; this is not just restricted to the most massive galaxies. And in low-density environments, the most massive galaxies appear to have also been formed very early (z > 2), compared to the lower mass galaxies there. Over the range z < 1.1, we do not see evolution in the mass of galaxies by more than a factor of ~2 separating active and inactive star-forming galaxy populations.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "150-181", "id_number": "CaltechAUTHORS:20100219-111725493", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100219-111725493", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516751", "primary_object": { "basename": "SCOapjss07c.pdf", "url": "https://authors.library.caltech.edu/records/vj16w-nt636/files/SCOapjss07c.pdf" }, "pub_year": "2007", "author_list": "Scoville, N.; Aussel, H.; et el." }, { "id": "https://authors.library.caltech.edu/records/f71gg-15g83", "eprint_id": 18059, "eprint_status": "archive", "datestamp": "2023-08-22 09:54:37", "lastmod": "2023-10-20 15:32:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "B\u00f6hringer-H", "name": { "family": "B\u00f6hringer", "given": "H." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "N." } }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Giodini-S", "name": { "family": "Giodini", "given": "S." } }, { "id": "Griffiths-R-E", "name": { "family": "Griffiths", "given": "R. E." } }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "R." }, "orcid": "0000-0002-6085-3780" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Peacock-J-A", "name": { "family": "Peacock", "given": "J. A." } }, { "id": "Sakelliou-I", "name": { "family": "Sakelliou", "given": "I." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J. D." }, "orcid": "0000-0002-0000-6977" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Taylor-J-E", "name": { "family": "Taylor", "given": "J. E." } }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J. R." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } } ] }, "title": "The XMM-Newton Wide-Field Survey in the COSMOS Field: Statistical Properties of Clusters of Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; dark matter; large-scale structure of universe; surveys", "note": "\u00a9 2007 American Astronomical Society.\n\nReceived 2006 April 24; accepted for publication 2006 November 23.\n\nThis research is based on observations with XMM-Newton, an\nESA science mission with instruments and contributions directly\nfunded by ESA Member States and NASA; and the NASA/ESA\nHubble Space Telescope, obtained at the Space Telescope Science\nInstitute, which is operated by the Association of Universities\nfor Research in Astronomy (AURA), Inc., under NASA\ncontract NAS5-26555; it is also based on data collected at the\nSubaru Telescope, which is operated by the National Astronomical\nObservatory of Japan; the European Southern Observatory,\nChile; Kitt Peak National Observatory, Cerro Tololo Inter-\nAmerican Observatory, and the National Optical Astronomy\nObservatory, which are operated by AURA, Inc., under cooperative\nagreement with the National Science Foundation (NSF);\nthe National Radio Astronomy Observatory, which is a facility\nof the NSF operated under cooperative agreement by Associated\nUniversities, Inc.; and the Canada-France-Hawaii Telescope,\noperated by the National Research Council of Canada, the\nCentre National de la Recherche Scientifique de France, and\nthe University of Hawaii. In Germany, the XMM-Newton project\nis supported by the Bundesministerium fuer Wirtschaft\nund Technologie/Deutsches Zentrum fuer Luft-und Raumfahrt\n(BMWI/DLR, FKZ 50 OX 0001), the Max Planck Society, and\nthe Heidenhain-Stiftung. Part of this work was supported by\nthe Deutsches Zentrum fu\u00a8 r Luft-und Raumfahrt, DLR project\nnumbers 50 OR 0207 and 50 OR 0405. The HST COSMOS\nTreasury program was supported through NASA grant HST-GO-\n09822.We gratefully acknowledge the contributions of the entire\nCOSMOS collaboration, consisting of more than 70 scientists.\nMore information on the COSMOS survey is available at http://\nwww.astro.caltech.edu/cosmos. It is a pleasure to acknowledge\nthe excellent services provided by the NASA IPAC/IRSA staff\n(Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John\nGood) in providing online archive and server capabilities for the\nCOSMOS data sets. The COSMOS Science meeting in 2005\nMay was supported in part by the NSF through grant OISE-\n0456439. A. F. acknowledges support from BMBF/DLR under\ngrant 50 OR 0207, MPG, and a partial support from NASA grant\nNNG04GF686, covering his stays at UMBC. The authors thank\nthe referee, Alastair Edge, for detailed comments, which improved\nthe content of this paper. A. F. thanks Harald Ebeling,\nTrevor Ponman, Piero Rosati, and Peter Schuecker for useful\nsuggestions at various stages of this work. I. S. acknowledges the\nsupport of the European Community under a Marie Curie Intra-European Fellowship.\n\nPublished - FINapjss07.pdf
", "abstract": "We present the results of a search for galaxy clusters in the first 36 XMM-Newton pointings on the Cosmic Evolution Survey (COSMOS) field. We reach a depth for a total cluster flux in the 0.5-2 keV band of 3 \u00d7 10^(-15) ergs cm^(-2) s^(-1), having one of the widest XMM-Newton contiguous raster surveys, covering an area of 2.1 deg^2. Cluster candidates are identified through a wavelet detection of extended X-ray emission. Verification of the cluster candidates is done based on a galaxy concentration analysis in redshift slices of thickness 0.1-0.2 in redshift, using the multiband photometric catalog of the COSMOS field and restricting the search to z < 1.3 and i_(AB) < 25. We identify 72 clusters and derive their properties based on the X-ray cluster scaling relations. A statistical description of the survey in terms of the cumulative log(N > S)-log S distribution compares well with previous results, although yielding a somewhat higher number of clusters at similar fluxes. The X-ray luminosity function of COSMOS clusters matches well the results of nearby surveys, providing a comparably tight constraint on the faint-end slope of \u03b1 = 1.93 \u00b1 0.04. For the probed luminosity range of (8 \u00d7 10^(42))-(2 \u00d7 10^(44)) ergs s^(-1), our survey is in agreement with and adds significantly to the existing data on the cluster luminosity function at high redshifts and implies no substantial evolution at these luminosities to z = 1.3.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "182-195", "id_number": "CaltechAUTHORS:20100423-135303799", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100423-135303799", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsches Zentrum f\u00fcr Luft-und Raumfahrt (DLR)", "grant_number": "50 OR 0207" }, { "agency": "Deutsches Zentrum f\u00fcr Luft-und Raumfahrt (DLR)", "grant_number": "50 OR 0405" }, { "agency": "NASA", "grant_number": "NNG04GF686" }, { "agency": "Marie Curie Fellowship" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516577", "primary_object": { "basename": "FINapjss07.pdf", "url": "https://authors.library.caltech.edu/records/f71gg-15g83/files/FINapjss07.pdf" }, "pub_year": "2007", "author_list": "Finoguenov, A.; Guzzo, L.; et el." }, { "id": "https://authors.library.caltech.edu/records/j3bw8-5bz79", "eprint_id": 17466, "eprint_status": "archive", "datestamp": "2023-08-22 09:52:58", "lastmod": "2023-10-19 23:55:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "N." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Brunner-H", "name": { "family": "Brunner", "given": "H." } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Fiore-F", "name": { "family": "Fiore", "given": "F." } }, { "id": "Gilli-R", "name": { "family": "Gilli", "given": "R." } }, { "id": "Lehmann-I", "name": { "family": "Lehmann", "given": "I." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "C." }, "orcid": "0000-0002-8853-9611" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "Griffiths-R-E", "name": { "family": "Griffiths", "given": "R. E." } }, { "id": "Miyaji-Takamitsu", "name": { "family": "Miyaji", "given": "T." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" } ] }, "title": "The XMM-Newton Wide-Field Survey in the COSMOS Field. IV. X-Ray Spectral Properties of Active Galactic Nuclei", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : active; surveys; X-rays : diffuse background; X-rays : galaxies; X-rays : general", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 April 24; accepted 2006 December 5.\nThis work is based on observations obtained with XMM-Newton,\nan ESA science mission with instruments and contributions directly\nfunded by ESA Member States and the US (NASA). In Germany,\nthe XMM-Newton project is supported by the Bundesministerium\nfu\u00a8r Wirtschaft und Technologie/Deutsches Zentrum fu\u00a8r Luft- und\nRaumfahrt (BMWI/DLR, FKZ 50 OX 0001), the Max-Planck\nSociety and the Heidenhain-Stiftung. Part of this work was supported\nby the Deutsches Zentrum fu\u00a8 r Luft- und Raumfahrt, DLR\nproject numbers 50 OR 0207 and 50 OR 0405. In Italy, the\nCOSMOS XMM-Newton project is supported by INAF and\nMIUR under grants PRIN/270/2003 and Cofin-03-02-23. Based\non observations with the NASA/ESA Hubble Space Telescope,\nobtained at the Space Telescope Science Institute, which is operated\nby AURA, Inc., under NASA contract NAS5-26555. The\nHST COSMOS Treasury program was supported through NASA\ngrant HST-GO-09822. Also based on data collected at the Subaru\nTelescope, which is operated by the National Astronomical Observatory\nof Japan; the European Southern Observatory under\nLarge Program 175.A-0839, Chile; and the National Radio Astronomy\nObservatory, which is a facility of the National Science\nFoundation operated under cooperative agreement by Associated\nUniversities, Inc. We are grateful to Paolo Tozzi, Kazushi Iwasawa,\nand Paolo Padovani for inspiring discussions. We gratefully acknowledge\nthe entire COSMOS collaboration consisting of more\nthan 70 scientists. More information on the COSMOS survey is\navailable at http://www.astro.caltech.edu/_cosmos. It is a pleasure\nthe acknowledge the excellent services provided by the NASA\nIPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce\nBerriman, and John Good) in providing online archive and server\ncapabilities for the COSMOS data sets.\n\nPublished - MAIapjss07.pdf
", "abstract": "We present a detailed spectral analysis of pointlike X-ray sources in the XMM-NewtonCOSMOS field. Our sample\nof 135 sources only includes those that have more than 100 net counts in the 0.3-10 keV energy band and have been\nidentified through optical spectroscopy. The majority of the sources are well described by a simple power-law model\nwith either no absorption (76%) or a significant intrinsic, absorbing column (20%). The remaining ~4% of the\nsources require a more complex modeling by incorporating additional components to the power law. For sourceswith\nmore than 180 net counts (bright sample), we allowed both the photon spectral index \u0393 and the equivalent hydrogen\ncolumn N_H to be free parameters. For fainter sources, we fix \u0393 to the average value and allow N_H to vary. The mean\nspectral index of the 82 sources in the bright sample is <\u0393> = 2:06 \u00b1 0:08, with an intrinsic dispersion of ~0.24.\nEach of these sources has fractional errors on the value of \u0393 below 20%. As expected, the distribution of intrinsic\nabsorbing column densities is markedly different between AGNs with or without broad optical emission lines. We\nfind within our sample four type 2 QSO candidates (L_X >10^(44) ergs s^(-1), N_H >10^(22) cm^(-2)), with a spectral energy\ndistribution well reproduced by a composite Seyfert 2 spectrum, that demonstrates the strength of the wide-field\nCOSMOS XMM-Newton survey to detect these rare and underrepresented sources. In addition, we have identified a\nCompton-thick (N_H >1:5 ; 10^(24) cm^(-)2) AGN at z = 0:1248. Its X-ray spectrum is well fitted by a pure reflection\nmodel and a significant Fe K\u03b1 line at rest-frame energy of 6.4 keV.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "368-382", "id_number": "CaltechAUTHORS:20100212-104637294", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100212-104637294", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50 OR 0207" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50 OR 0405" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN/270/2003" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerc (MIUR)", "grant_number": "Cofin-03-02-23" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NASA", "grant_number": "HST-GO-09822" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516573", "primary_object": { "basename": "MAIapjss07.pdf", "url": "https://authors.library.caltech.edu/records/j3bw8-5bz79/files/MAIapjss07.pdf" }, "pub_year": "2007", "author_list": "Mainieri, V.; Hasinger, G.; et el." }, { "id": "https://authors.library.caltech.edu/records/eb4jd-6a269", "eprint_id": 17459, "eprint_status": "archive", "datestamp": "2023-08-22 09:52:53", "lastmod": "2023-10-19 23:54:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "R." }, "orcid": "0000-0002-6085-3780" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } }, { "id": "Ajiki-M", "name": { "family": "Ajiki", "given": "M." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "B\u00f6hringer-H", "name": { "family": "B\u00f6hringer", "given": "H." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Franceschini-A", "name": { "family": "Franceschini", "given": "A." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Kitzbichler-M-G", "name": { "family": "Kitzbichler", "given": "M. G." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "T." }, "orcid": "0000-0002-7402-5441" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S." } }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Taylor-J-E", "name": { "family": "Taylor", "given": "J. E." } } ] }, "title": "The Cosmic Evolution Survey (COSMOS): A Large-Scale Structure at z = 0.73 and the Relation of Galaxy Morphologies to Local Environment", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : clusters : general; galaxies : evolution; large-scale structure of universe; surveys", "note": "\u00a9 2007 The American Astronomical Society. \n\nReceived 2006 April 27; accepted 2007 January 12. \n\nWe gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. The COSMOS Science Meeting in 2005 May was supported in part by the NSF through grant OISE-0456439. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the US (NASA). In Italy, the COSMOS project is supported by INAF under PRIN-2005/1.06.08.10 and XMM-COSMOS is supported by INAF and MIUR under grants PRIN/270/2003 and Cofin-03-02-23 and by ASI under grant ASI/INAF I/023/05/0. In Germany, the XMM\u2013Newton project is supported by the Bundesministerium f\u00fcr Bildung und Forschung/Deutsches Zentrum f\u00fcr Luft und Raumfahrt, the Max-Planck Society, and the Heidenhain-Stiftung. Part of this work was supported by the Deutsches Zentrum f\u00fcr Luft- und Raumfahrt, DLR project Nos. 50 OR 0207 and 50 OR 0405. L. G. thanks Claudio Firmani and Marco Scodeggio for enlightening discussions on galaxy evolution, Davide Lazzati for invaluable help with IDL routines, and Stefania Giodini for help with the mock samples.\n\nPublished - GUZapjss07.pdf
", "abstract": "We have identified a large-scale structure at z \u2243 0.73 in the COSMOS field, coherently described by the distribution of galaxy photometric redshifts, an ACS weak-lensing convergence map, and the distribution of extended X-ray sources in a mosaic of XMM-Newton observations. The main peak seen in these maps corresponds to a rich cluster with T_X = 3.51^(+0.60)_(-0.46) keV and L_X = (1.56 \u00b1 0.04) \u00d7 10^(44) ergs s^(-1) (0.1-2.4 keV band). We estimate an X-ray mass within r_(500) corresponding to M_(500) \u2243 1.6 \u00d7 10^(14) M_\u2299 and a total lensing mass (extrapolated by fitting a NFW profile) M_(NFW) = (6 \u00b1 3) \u00d7 10^(15) M_\u2299. We use an automated morphological classification of all galaxies brighter than I_(AB) = 24 over the structure area to measure the fraction of early-type objects as a function of local projected density \u03a3_(10), based on photometric redshifts derived from ground-based deep multiband photometry. We recover a robust morphology-density relation at this redshift, indicating, for comparable local densities, a smaller fraction of early-type galaxies than today. Interestingly, this difference is less strong at the highest densities and becomes more severe in intermediate environments. We also find, however, local \"inversions\" of the observed global relation, possibly driven by the large-scale environment. In particular, we find direct correspondence of a large concentration of disk galaxies to (the colder side of) a possible shock region detected in the X-ray temperature map and surface brightness distribution of the dominant cluster. We interpret this as potential evidence of shock-induced star formation in existing galaxy disks, during the ongoing merger between two subclusters. Our analysis reveals the value of combining various measures of the projected mass density to locate distant structures and their potential for elucidating the physical processes at work in the transformation of galaxy morphologies.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "254-269", "id_number": "CaltechAUTHORS:20100211-142816176", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100211-142816176", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NSF", "grant_number": "OISE-0456439" }, { "agency": "Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)", "grant_number": "PRIN-2005/1.06.08.10" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN/270/2003" }, { "agency": "Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)", "grant_number": "Cofin-03-02-23" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "ASI/INAF I/023/05/0" }, { "agency": "Bundesministerium f\u00fcr Bildung und Forschung (BMBF)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50 OR 0207" }, { "agency": "Max-Planck Society" }, { "agency": "Heidenhain-Stiftung" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50 OR 0405" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516588", "primary_object": { "basename": "GUZapjss07.pdf", "url": "https://authors.library.caltech.edu/records/eb4jd-6a269/files/GUZapjss07.pdf" }, "pub_year": "2007", "author_list": "Guzzo, L.; Cassata, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/7m8py-qs867", "eprint_id": 18054, "eprint_status": "archive", "datestamp": "2023-08-22 09:54:32", "lastmod": "2023-10-20 15:32:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Ajiki-M", "name": { "family": "Ajiki", "given": "M." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } }, { "id": "Tribiano-S", "name": { "family": "Tribiano", "given": "S." } }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C." }, "orcid": "0000-0001-6647-3861" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Colbert-J-W", "name": { "family": "Colbert", "given": "J." } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Green-W", "name": { "family": "Green", "given": "W." } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "K." }, "orcid": "0000-0003-3804-2137" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Koda-Jin", "name": { "family": "Koda", "given": "J." }, "orcid": "0000-0002-8762-7863" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Komiyama-Yutaka", "name": { "family": "Komiyama", "given": "Y." } }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Liu-Charles-T", "name": { "family": "Liu", "given": "C." }, "orcid": "0000-0002-4314-8713" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "R." }, "orcid": "0000-0002-6085-3780" }, { "id": "Miyazaki-Satoshi", "name": { "family": "Miyazaki", "given": "S." } }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "T." }, "orcid": "0000-0002-7402-5441" }, { "id": "Peacock-J-A", "name": { "family": "Peacock", "given": "J. A." } }, { "id": "Pickles-A-J", "name": { "family": "Pickles", "given": "A." } }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Rich-M", "name": { "family": "Rich", "given": "M." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L. A. M." } }, { "id": "Taylor-J-E", "name": { "family": "Taylor", "given": "J. E." } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } } ] }, "title": "The First Release COSMOS Optical and Near-IR Data and Catalog", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; large-scale structure of universe; surveys", "note": "\u00a9 2007 American Astronomical Society. \n\nReceived 2006 September 23; accepted 2007 April 6. \n\nWe would like to thank the COSMOS team (http://cosmos.astro.caltech.edu), the staff at Caltech, CFHT, CTIO, KPNO, NAOJ, STSCI, TERAPIX, and the University of Hawaii for supporting this work and making it possible. Support for this work was provided by NASA grant HST-GO-09822 and NSF grant OISE-0456439. FLAMINGOS was designed and constructed by the IR instrumentation group (PI: R. Elston) at the University of Florida, Department of Astronomy, with support from NSF grant AST 97-31180 and Kitt Peak National Observatory. Funding for the Sloan Digital Sky Survey (SDSS) has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the US Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is at http://www.sdss.org. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, the Johns Hopkins University, Los Alamos National Laboratory, the Max Planck Institute for Astronomy, the Max Planck Institute for Astrophysics, New Mexico State University, the University of Pittsburgh, Princeton University, the United States Naval Observatory, and the University of Washington. D. T. acknowledges support from NASA through a Long Term Space Astrophysics grant (NAG5-10955, NRA-00-01-LTSA-064). This work is based (in part) on data products produced at the TERAPIX data center located at the Institut d'Astrophysique de Paris.\n\nPublished - CAPapjss07a.pdf
", "abstract": "We present imaging data and photometry for the COSMOS survey in 15 photometric bands between 0.3 and 2.4 \u03bcm. These include data taken on the Subaru 8.3 m telescope, the KPNO and CTIO 4 m telescopes, and the CFHT 3.6 m telescope. Special techniques are used to ensure that the relative photometric calibration is better than 1% across the field of view. The absolute photometric accuracy from standard-star measurements is found to be 6%. The absolute calibration is corrected using galaxy spectra, providing colors accurate to 2% or better. Stellar and galaxy colors and counts agree well with the expected values. Finally, as the first step in the scientific analysis of these data we construct panchromatic number counts which confirm that both the geometry of the universe and the galaxy population are evolving.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "99-116", "id_number": "CaltechAUTHORS:20100423-094539850", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100423-094539850", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NSF", "grant_number": "OISE-0456439" }, { "agency": "NASA", "grant_number": "NAG5-10955" }, { "agency": "NASA", "grant_number": "NRA-00-01-LTSA-064" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/519081", "primary_object": { "basename": "CAPapjss07a.pdf", "url": "https://authors.library.caltech.edu/records/7m8py-qs867/files/CAPapjss07a.pdf" }, "pub_year": "2007", "author_list": "Capak, P.; Aussel, H.; et el." }, { "id": "https://authors.library.caltech.edu/records/jdsqa-jhe38", "eprint_id": 17712, "eprint_status": "archive", "datestamp": "2023-08-22 09:53:34", "lastmod": "2023-10-20 00:10:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M. T." }, "orcid": "0000-0003-1033-9684" }, { "id": "Feldmann-R", "name": { "family": "Feldmann", "given": "R." }, "orcid": "0000-0002-1109-1919" }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "R." }, "orcid": "0000-0002-6085-3780" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Maier-C", "name": { "family": "Maier", "given": "C." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Ajiki-M", "name": { "family": "Ajiki", "given": "M." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S." } }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Takahashi-M", "name": { "family": "Takahashi", "given": "M." } } ] }, "title": "COSMOS Morphological Classification with the Zurich Estimator of Structural Types (ZEST) and the Evolution Since z = 1 of the Luminosity Function of Early, Disk, and Irregular Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; dark matter; galaxies: evolution; galaxies: formation; large-scale structure of universe; surveys", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 1 (2007 September); received 2006 April 25, accepted for publication 2006 November 5.\n\nThe HST COSMOS Treasury program was supported through\nNASA grant HST-GO-09822.We gratefully acknowledge the contributions\nof the entire COSMOS collaboration. More information\non the COSMOS survey is available at http://cosmos.astro\n.caltech.edu.We thank the NASA IPAC/IRSA staff for providing\nonline archive and server capabilities for the COSMOS data sets.\nC. S. acknowledges support from the Swiss National Science\nFoundation.\nFacilities: HST (ACS)\n\nPublished - SCAapjss07.pdf
", "abstract": "Motivated by the desire to reliably and automatically classify structure of thousands of COSMOS galaxies, we present ZEST, the Zurich Estimator of Structural Types. To classify galaxy structure, ZEST uses (1) five nonparametric diagnostics: asymmetry, concentration, Gini coefficient, second-order moment of the brightest 20% of galaxy pixels, and ellipticity; and (2) the exponent n of single-S\u00e9rsic fits to the two-dimensional surface brightness distributions. To fully exploit the wealth of information while reducing the redundancy present in these diagnostics, ZEST performs a principal component (PC) analysis. We use a sample of ~56,000 I_(AB) \u2264 24 COSMOS galaxies to show that the first three PCs fully describe the key aspects of the galaxy structure, i.e., to calibrate a three-dimensional classification grid of axes PC_1, PC_2, and PC_3. We demonstrate the robustness of the ZEST grid on the z = 0 sample of Frei et al. The ZEST classification breaks most of the degeneracy between different galaxy populations that affects morphological classifications based on only some of the diagnostics included in ZEST. As a first application, we present the evolution since z ~ 1 of the luminosity functions (LFs) of COSMOS galaxies of early, disk, and irregular galaxies and, for disk galaxies, of different bulge-to-disk ratios. Overall, we find that the LF up to a redshift z = 1 is consistent with a pure luminosity evolution (of about 0.95 mag at z ~ 0.7). We highlight, however, two trends that are in general agreement with a downsizing scenario for galaxy formation, i.e., (1) a deficit of a factor of about 2 at z ~ 0.7 of M_B > -20.5 structurally classified early-type galaxies and (2) an excess of a factor of about 3, at a similar redshift, of irregular galaxies.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "406-433", "id_number": "CaltechAUTHORS:20100309-143207444", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100309-143207444", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "Swiss National Science Foundation (SNSF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516582", "primary_object": { "basename": "SCAapjss07.pdf", "url": "https://authors.library.caltech.edu/records/jdsqa-jhe38/files/SCAapjss07.pdf" }, "pub_year": "2007", "author_list": "Scarlata, C.; Carollo, C. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/xcv6q-j4v13", "eprint_id": 16705, "eprint_status": "archive", "datestamp": "2023-08-22 09:52:16", "lastmod": "2023-10-19 22:29:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zamojski-M-A", "name": { "family": "Zamojski", "given": "M. A." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. M." }, "orcid": "0000-0003-0427-8387" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S. S." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mellier-Y", "name": { "family": "Mellier", "given": "Y." } }, { "id": "Bertin-E", "name": { "family": "Bertin", "given": "E." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Thompson-D-J", "name": { "family": "Thompson", "given": "D. J." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "T. A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "P. G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "P." }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "S G." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "M." }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T", "name": { "family": "Small", "given": "T." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "T. K." } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "L." } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "J." } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "T. M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Y.-W." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "B. F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "B." } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "A. S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "B. Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "S. K." } } ] }, "title": "Deep GALEX Imaging of the COSMOS HST Field: A First Look at the Morphology of z ~ 0.7 Star-forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: fundamental parameters; surveys", "note": "\u00a9 2009 American Astronomical Society. \n\nReceived 2006 July 28; accepted 2007 January 9. \n\nThe COSMOS HST Treasury program was supported through NASA grant HST-GO-09822. We wish to thank Tony Roman, Denise Taylor, and David Soderblom for their assistance in planning and scheduling of the extensive COSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/~cosmos. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS data sets. The COSMOS Science meeting in 2005 May was supported in part by the NSF through grant OISE-0456439.\n\n GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. \n\nFacilities: HST(ACS), GALEX, Subaru, CFHT, KPNO:2.1m, CTIO:1.5m \n\nBased on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by Association of Universities for Research in Astronomy, Inc. (AURA), under NASA contract NAS 5-26555; and with the NASA Galaxy Evolution Explorer (GALEX); also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under cooperative agreement with the National Science Foundation; the Canada-France-Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the National Research Council of Canada, the Canadian Astronomy Data Centre, the Centre National de la Recherche Scientifique de France, TERAPIX, and the University of Hawaii.\n\nPublished - ZAMapjss07.pdf
", "abstract": "We present a study of the morphological nature of redshift z ~ 0.7 star-forming galaxies using a combination of HST ACS, GALEX, and ground-based images of the COSMOS field. Our sample consists of 8146 galaxies, 5777 of which are detected in the GALEX near-ultraviolet band (2310 \u00c5 or ~1360 \u00c5 rest frame) down to a limiting magnitude of 25.5 (AB), and all of which have a brightness of F814W(HST) < 23 mag and photometric redshifts in the range 0.55 < z < 0.8. We make use of the UV to estimate star formation rates, correcting for the effect of dust using the UV slope, and of the ground-based multiband data to calculate masses. For all galaxies in our sample, we compute, from the ACS F814W images, their concentration (C), asymmetry (A), and clumpiness (S), as well as their Gini coefficient (G) and the second moment of the brightest 20% of their light (M_20). We observe a bimodality in the galaxy population in asymmetry and in clumpiness, although the separation is most evident when either of those parameters is combined with a concentration-like parameter (C, G, or M_20). We further show that this morphological bimodality has a strong correspondence with the FUV-g color bimodality and conclude that UV-optical color predominantly evolves concurrently with morphology. We observe many of the most star-forming galaxies to have morphologies approaching that of early-type galaxies, and we interpret this as evidence that strong starburst events are linked to bulge growth and constitute a process through which galaxies can be brought from the blue to the red sequence while simultaneously modifying their morphology accordingly. We conclude that the red sequence has continued growing at z \u2272 0.7. We also observe z ~ 0.7 galaxies to have physical properties similar to that of local galaxies, except for higher star formation rates. Whence we infer that the dimming of star-forming galaxies is responsible for most of the evolution in star formation rate density since that redshift, although our data are also consistent with a mild number evolution.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "468-493", "id_number": "CaltechAUTHORS:20091113-115202257", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091113-115202257", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NSF", "grant_number": "OISE-0456439" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516593", "primary_object": { "basename": "ZAMapjss07.pdf", "url": "https://authors.library.caltech.edu/records/xcv6q-j4v13/files/ZAMapjss07.pdf" }, "pub_year": "2007", "author_list": "Zamojski, M. A.; Schiminovich, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/g69gf-n2f73", "eprint_id": 17458, "eprint_status": "archive", "datestamp": "2023-08-22 09:52:47", "lastmod": "2023-10-19 23:54:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Massey-R-J", "name": { "family": "Massey", "given": "Richard" }, "orcid": "0000-0002-6085-3780" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard" }, "orcid": "0000-0001-7782-7071" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton" }, "orcid": "0000-0002-6610-2048" }, { "id": "Refregier-A", "name": { "family": "Refregier", "given": "Alexandre" } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Taylor-J-E", "name": { "family": "Taylor", "given": "James E." } }, { "id": "Albert-J", "name": { "family": "Albert", "given": "Justin" } }, { "id": "Berg\u00e9-J", "name": { "family": "Berg\u00e9", "given": "Joel" } }, { "id": "Heymans-C", "name": { "family": "Heymans", "given": "Catherine" } }, { "id": "Johnston-D", "name": { "family": "Johnston", "given": "David" } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "Jean-Paul" }, "orcid": "0000-0002-4616-4989" }, { "id": "Mellier-Y", "name": { "family": "Mellier", "given": "Yannick" } }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Semboloni-E", "name": { "family": "Semboloni", "given": "Elisabetta" } }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "Patrick" } }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "Lidia" } }, { "id": "Van-Waerbeke-L", "name": { "family": "Van Waerbeke", "given": "Ludovic" } } ] }, "title": "COSMOS: Three-dimensional Weak Lensing and the Growth of Structure", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology : observations; gravitational lensing; large-scale structure of universe", "note": "\u00a9 2007 The American Astronomical Society.\n\nReceived 2006 September 22; accepted 2007 January 24.\nThe HST COSMOS Treasury program was supported through\nNASA grant HST-GO-09822. The HST ACS CTE calibration\nprogram is supported through NASA grant HST-AR-10964. A. L.,\nA. R., E. S., J. P. K., L. T., and Y. M. were partly funded by the\nCNRS Programme National de Cosmologie. C. H. is supported\nby a CITA national fellowship. We thank Alan Heavens, Tom\nKitching, John Peacock, Andy Taylor, and Peter Schneider for\nilluminating discussions. We thank Tony Roman, Denise Taylor,\nand David Soderblom for their assistance in planning and scheduling\nthe extensive COSMOS observations. We thank the NASA\nIPAC/ IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce\nBerriman, and John Good) for providing online archive and server\ncapabilities for the COSMOS data sets. It is also our pleasure to\ngratefully acknowledge the contributions of the entire COSMOS\ncollaboration, consisting of more than 70 scientists. More information\non the COSMOS survey is available at http://www.astro\n.caltech.edu /~cosmos.\nFacilities:HST(ACS), Subaru (Suprime-Cam),CFHT(Megacam).\n\nPublished - MASapjss07.pdf
", "abstract": "We present a three-dimensional cosmic shear analysis of the Hubble Space Telescope COSMOS survey, the largest ever optical imaging program performed in space. We have measured the shapes of galaxies for the telltale distortions caused by weak gravitational lensing and traced the growth of that signal as a function of redshift. Using both 2D and 3D analyses, we measure cosmological parameters \u03a9_m, the density of matter in the universe, and \u03c3_8, the normalization of the matter power spectrum. The introduction of redshift information tightens the constraints by a factor of 3 and also reduces the relative sampling (or \"cosmic\") variance compared to recent surveys that may be larger but are only two-dimensional. From the 3D analysis, we find that \u03c3_8(\u03a9_m/0.3)^(0.44) = 0.866^(+0.085)_(-0.068) at 68% confidence limits, including both statistical and potential systematic sources of error in the total budget. Indeed, the absolute calibration of shear measurement methods is now the dominant source of uncertainty. Assuming instead a baseline cosmology to fix the geometry of the universe, we have measured the growth of structure on both linear and nonlinear physical scales. Our results thus demonstrate a proof of concept for tomographic analysis techniques that have been proposed for future weak-lensing surveys by a dedicated wide-field telescope in space.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "239-253", "id_number": "CaltechAUTHORS:20100211-134522689", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100211-134522689", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NASA", "grant_number": "HST-AR-10964" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Canadian Institute for Theoretical Astrophysics" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1086/516599", "primary_object": { "basename": "MASapjss07.pdf", "url": "https://authors.library.caltech.edu/records/g69gf-n2f73/files/MASapjss07.pdf" }, "pub_year": "2007", "author_list": "Massey, Richard; Rhodes, Jason; et el." }, { "id": "https://authors.library.caltech.edu/records/j2778-dwq53", "eprint_id": 17544, "eprint_status": "archive", "datestamp": "2023-08-22 09:53:23", "lastmod": "2023-10-19 23:59:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Bondi-M", "name": { "family": "Bondi", "given": "M." } }, { "id": "Ciliegi-P", "name": { "family": "Ciliegi", "given": "P." } }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "K." }, "orcid": "0000-0003-3804-2137" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C. D." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Urry-C-M", "name": { "family": "Urry", "given": "C. M." }, "orcid": "0000-0002-0745-9792" } ] }, "title": "The VLA-COSMOS Survey. II. Source Catalog of the Large Project", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; radio continuum: galaxies; surveys", "note": "\u00a9 2007 American Astronomical Society. \n\nPrint publication: Issue 1 (2007 September); received 2006 April 27; accepted for publication 2006 August 1. \n\nThe National Radio Astronomy Observatory (NRAO) is operated by Associated Universities, Inc., under cooperative agreement with the National Science Foundation. We would like to thank the NRAO for their support during this project with special thanks to Barry Clark and Joan Wrobel. For fruitful discussions we thank Frazer Owen, Jim Condon, Bill Cotton, Andrew Hopkins, and Jos\u00e9 Afonso. We thank the anonymous referee for constructive comments that helped improve the paper. V. S.'s visit to NRAO was supported by HST-GO-09822.31-A. C. C. thanks the Max-Planck-Gesellschaft and the Humboldt-Stiftung for support through the Max-Planck-Forschungspreis. C. C. acknowledges support through NASA grant HST-GO-09822.33-A. K. J. acknowledges support by the German DFG under grant SCHI 536/3-1. The COSMOS Science meeting in 2005 May was supported in part by the NSF through grant OISE-0456439. The Digitized Sky Survey was produced at the Space Telescope Science Institute under US government grant NAG W-2166. \n\nFacilities: VLA\n\nPublished - SCHIapjss07a.pdf
", "abstract": "The VLA-COSMOS Large Project is described and its scientific objective is discussed. We present a catalog of ~3600 radio sources found in the 2 deg^2 COSMOS field at 1.4 GHz. The observations in the VLA A and C configuration resulted in a resolution of 1.5\" \u00d7 1.4\" and a mean rms noise of ~10.5 (15) \u03bcJy beam^(-1) in the central 1 (2) deg^2. Eighty radio sources are clearly extended consisting of multiple components, and most of them appear to be double-lobed radio galaxies. The astrometry of the catalog has been thoroughly tested, and the uncertainty in the relative and absolute astrometry are 130 and <55 mas, respectively.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "46-69", "id_number": "CaltechAUTHORS:20100222-095053360", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100222-095053360", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Radio Astronomy Observatory (NRAO)" }, { "agency": "Max-Planck-Forschungspreis" }, { "agency": "NASA", "grant_number": "HST-GO-09822.33" }, { "agency": "NSF", "grant_number": "OISE-0456439" }, { "agency": "NASA", "grant_number": "HST-GO-09822.31-A" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "SCHI 536/3-1" }, { "agency": "Alexander von Humboldt Stiftung" }, { "agency": "NASA", "grant_number": "HST-GO-09822.33-A" }, { "agency": "NASA", "grant_number": "NAG W-2166" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1086/516587", "primary_object": { "basename": "SCHIapjss07a.pdf", "url": "https://authors.library.caltech.edu/records/j2778-dwq53/files/SCHIapjss07a.pdf" }, "pub_year": "2007", "author_list": "Schinnerer, E.; Smol\u010di\u0107, V.; et el." }, { "id": "https://authors.library.caltech.edu/records/mwmav-c7q94", "eprint_id": 16879, "eprint_status": "archive", "datestamp": "2023-08-22 09:52:27", "lastmod": "2023-10-19 22:37:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Ajiki-M", "name": { "family": "Ajiki", "given": "M." } }, { "id": "Miyazaki-Satoshi", "name": { "family": "Miyazaki", "given": "S." } }, { "id": "Komiyama-Yutaka", "name": { "family": "Komiyama", "given": "Y." } }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "T." }, "orcid": "0000-0002-7402-5441" }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S. S." } }, { "id": "Koda-Jin", "name": { "family": "Koda", "given": "J." }, "orcid": "0000-0002-8762-7863" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C." }, "orcid": "0000-0001-6647-3861" }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Rich-M", "name": { "family": "Rich", "given": "M." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P." } }, { "id": "Kaifu-Norio", "name": { "family": "Kaifu", "given": "N." } }, { "id": "Karoji-Hiroshi", "name": { "family": "Karoji", "given": "H." } }, { "id": "Arimoto-Nobuo", "name": { "family": "Arimoto", "given": "N." } }, { "id": "Okamura-Sadanori", "name": { "family": "Okamura", "given": "S." } }, { "id": "Ohta-K", "name": { "family": "Ohta", "given": "K." } } ] }, "title": "The Cosmic Evolution Survey (COSMOS): Subaru Observations of the HST Cosmos Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: interactions", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 1 (2007 September); received 2006 September 19; accepted for publication 2006 November 30. \n\nThe HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at http://cosmos.astro.caltech.edu. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, AnastasiaAlexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS data sets. The COSMOS Science meeting in 2005 May was supported in part by the NSF through grant OISE-0456439. We would also like to thank the staff at the Subaru Telescope for their invaluable help. In particular, we would like to thank Hisanori Furusawa because his professional help as a support scientist made our Suprime-Cam observations successful. This work was financially supported in part by the Ministry of Education, Culture, Sports, Science, and Technology (10044052 and 10304013), and by JSPS (15340059 and 17253001). S. S. S. and T. N. are JSPS fellows.\n\nPublished - TANapjss07.pdf
", "abstract": "We present deep optical imaging observations of 2 square degree area, covered by the Cosmic Evolution Survey (COSMOS), made by the prime-focus camera (Supreme-Cam) on the 8.2 m Subaru Telescope. Observations were done in six broadband [B (4459.7 \u00c5), g' (4723.1 \u00c5), V (5483.8 \u00c5), r' (6213.0 \u00c5), i' (7640.8 \u00c5), z' (8855.0 \u00c5)] and one narrowband (NB816) filters. A total of 106 galaxies were detected to i' ~ 26.5 mag. These data, combined with observations at u* and K-band are used to construct the photometric catalogs for the COSMOS, to measure their photometric redshifts, multiband spectral energy distributions, and stellar masses, and to identify high-redshift candidates. This catalog provides multi-wave band data for scientific analysis of the COSMOS survey.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "9-28", "id_number": "CaltechAUTHORS:20091204-122759314", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091204-122759314", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Education, Culture, Sports, Science, and Technology (MEXT)", "grant_number": "10044052" }, { "agency": "Ministry of Education, Culture, Sports, Science, and Technology (MEXT)", "grant_number": "10304013" }, { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NSF", "grant_number": "OISE-0456439" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15340059" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17253001" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516596", "primary_object": { "basename": "TANapjss07.pdf", "url": "https://authors.library.caltech.edu/records/mwmav-c7q94/files/TANapjss07.pdf" }, "pub_year": "2007", "author_list": "Taniguchi, Y.; Scoville, N.; et el." }, { "id": "https://authors.library.caltech.edu/records/2ytpm-qb430", "eprint_id": 17471, "eprint_status": "archive", "datestamp": "2023-08-22 09:53:03", "lastmod": "2023-10-19 23:55:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cassata-P", "name": { "family": "Cassata", "given": "P." } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Franceschini-A", "name": { "family": "Franceschini", "given": "A." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Ricciardelli-E", "name": { "family": "Ricciardelli", "given": "E." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } } ] }, "title": "The Cosmic Evolution Survey (COSMOS): The Morphological Content and Environmental Dependence of the Galaxy Color-Magnitude Relation at z ~ 0.7", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : clusters : general; galaxies : evolution; galaxies : general; galaxies : structure; large-scale structure of universe", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 June 9; accepted 2007 January 18.\nP. C. thanks the Osservatorio Astronomico di Brera for hospitality\nduring the development of this work. L. G. thanks C. Firmani\nand A. Boselli for useful discussions. We thank T. Kodama for\nproviding us with his model red sequences in electronic form.\nP. C. thanks P. Franzetti for providing Bruzual&Charlot models.\nWe thank Marcella Carollo and Simon Lilly for suggesting the\nKormendy relation analysis.\n\nPublished - CASapjss07.pdf
", "abstract": "We study the environmental dependence and the morphological composition of the galaxy color-magnitude diagram at z ~ 0.7, using a pilot subsample of COSMOS. The sample includes ~2000 galaxies with I_(AB) < 24 and photometric redshift within 0.61 < z < 0.85, covering an area of 270 arcmin^2. Galaxy morphologies are estimated via a nonparametric automatic technique. The (V - z') versus z' color-magnitude diagram shows a clear red sequence dominated by early-type galaxies and a remarkably well-defined \"blue sequence\" described by late-type objects. While the percentage of objects populating the two sequences is a function of environment, also following a clear morphology/color-density relation at this redshift, we establish that their normalization and slope are independent of local density. We identify and study a number of objects with \"anomalous\" colors, given their morphology, polluting the two sequences. Red late-type galaxies are found to be mostly highly inclined or edge-on spiral galaxies for which colors are dominated by internal reddening by dust. In a sample of color-selected red galaxies, these would represent 33% contamination with respect to truly passive spheroidals. Conversely, the population of blue early-type galaxies is composed of objects of moderate luminosity and mass, concurring to only ~5% of the mass in spheroidal galaxies. The majority of them (~70%) occupy a position in the \u03bc_B-r_(50) plane not consistent with their being precursors of current-epoch elliptical galaxies. Their fraction with respect to the whole galaxy population does not depend on the environment, at variance with the general early-type class. In a color-mass diagram, color sequences are even better defined, with red galaxies covering in general a wider range of masses at nearly constant color, and blue galaxies showing a more pronounced dependence of color on mass. While the red sequence is adequately reproduced by models of passive evolution, the blue sequence is better interpreted as a specific star formation sequence. The substantial invariance of its slope and normalization with respect to local density suggests that the overall \"secular\" star formation is driven more by galaxy mass than by environment.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "270-283", "id_number": "CaltechAUTHORS:20100212-132252052", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100212-132252052", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1086/516591", "primary_object": { "basename": "CASapjss07.pdf", "url": "https://authors.library.caltech.edu/records/2ytpm-qb430/files/CASapjss07.pdf" }, "pub_year": "2007", "author_list": "Cassata, P.; Guzzo, L.; et el." }, { "id": "https://authors.library.caltech.edu/records/kyjth-xca96", "eprint_id": 20101, "eprint_status": "archive", "datestamp": "2023-08-22 09:54:47", "lastmod": "2023-10-20 22:13:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Peacock-J-A", "name": { "family": "Peacock", "given": "J. A." } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "James-J-B", "name": { "family": "James", "given": "J. B." } }, { "id": "Kitzbichler-M-G", "name": { "family": "Kitzbichler", "given": "M. G." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Massey-R", "name": { "family": "Massey", "given": "R." } }, { "id": "Mellier-Y", "name": { "family": "Mellier", "given": "Y." } }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Norberg-P", "name": { "family": "Norberg", "given": "P." }, "orcid": "0000-0002-5875-0440" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S. S." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D-J", "name": { "family": "Thompson", "given": "D. J." } }, { "id": "White-S-D-M", "name": { "family": "White", "given": "S. D. M." } }, { "id": "El-Zant-A", "name": { "family": "El-Zant", "given": "A." } } ] }, "title": "The Angular Correlations of Galaxies in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; dark matter; galaxies: evolution; galaxies: formation; large-scale structure of universe; surveys", "note": "\u00a9 2007 American Astronomical Society.\n\nReceived 2006 November 10; accepted 2007 April 3.\n\nBased on observations with the NASA/ESA Hubble Space Telescope, obtained\nat the Space Telescope Science Institute, which is operated by the Association of\nUniversities for Research in Astronomy (AURA), Inc., under NASA contract NAS\n5-26555; also based on data collected at: the Subaru Telescope, which is operated by\nThe National Astronomical Observatory of Japan; the XMM-Newton, an ESA science\nMission with instruments and contributions directly funded by ESA Member States\nand NASA; the European Southern Observatory under Large Program175.A-0839,\nChile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory,\nand the National Optical Astronomy Observatory, which are operated by AURA\nunder cooperative agreement with the National Science Foundation; the National\nRadio Astronomy Observatory, which is a facility of the National Science Foundation,\noperated under cooperative agreement by Associated Universities, Inc.; and\nthe Canada-France-Hawaii Telescope (CFHT) with MegaPrime/MegaCam, operated\nas a joint project by the CFHT Corporation, CEA/DAPNIA, the National Research\nCouncil of Canada, the Canadian Astronomy Data Centre, the Centre National de\nla Recherche Scientifique de France, TERAPIX, and the University of Hawaii.\n\n\nThe HST COSMOS Treasury program was supported through\nNASA grant HST-GO-09822. We wish to thank Tony Roman,\nDenise Taylor, and David Soderblom for their assistance in planning and scheduling the extensive COSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration, consisting of more than 70 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/~cosmos. It is a pleasure to acknowledge the excellent\nservices provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS data sets.\n\nPublished - MCCapjss07.pdf
", "abstract": "We present measurements of the two-point galaxy angular correlation function w(\u03b8) in the COSMOS field. Independent determinations of w(\u03b8) as a function of magnitude limit are presented for both the Hubble Space Telescope (HST) ACS catalog and also the ground-based data from Subaru and the Canada-France-Hawaii Telescope. Despite having significantly different masks, these three determinations agree well. At bright magnitudes (I_(AB) < 22), our data generally match very well with existing measurements and with mock catalogs based on the semianalytic galaxy formation calculations of Kitzbichler & White (2007) from the Millennium Simulation. The exception is that our result is at the upper end of the expected cosmic variance scatter for \u03b8 > 10', which we attribute to a particularly rich structure known to exist at z \u2243 0.8. For fainter samples, however, the level of clustering is somewhat higher than reported by some previous studies; in all three catalogs we find w(\u03b8 = 1') \u2243 0.014 at a median I_(AB) magnitude of 24. At these very faintest magnitudes, our measurements agree well with the latest determinations from the Canada-France Legacy Survey. This level of clustering is approximately double what is predicted by the semianalytic catalogs (at all angles). The semianalytic results allow an estimate of cosmic variance, which is too small to account for the discrepancy. We therefore conclude that the mean amplitude of clustering at this level is higher than previously estimated.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "314-319", "id_number": "CaltechAUTHORS:20100923-112026685", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100923-112026685", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/518693", "primary_object": { "basename": "MCCapjss07.pdf", "url": "https://authors.library.caltech.edu/records/kyjth-xca96/files/MCCapjss07.pdf" }, "pub_year": "2007", "author_list": "McCracken, H. J.; Peacock, J. A.; et el." }, { "id": "https://authors.library.caltech.edu/records/hatj7-1ay25", "eprint_id": 17450, "eprint_status": "archive", "datestamp": "2023-08-22 09:52:37", "lastmod": "2023-10-19 23:54:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "Richard" }, "orcid": "0000-0002-6085-3780" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "Jean-Paul" }, "orcid": "0000-0002-4616-4989" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" }, { "id": "Johnston-D-E", "name": { "family": "Johnston", "given": "David E." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Heymans-C", "name": { "family": "Heymans", "given": "Catherine" } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "Oliver" }, "orcid": "0000-0001-5891-2596" }, { "id": "Mellier-Y", "name": { "family": "Mellier", "given": "Yannick" } }, { "id": "R\u00e9fr\u00e9gier-A", "name": { "family": "R\u00e9fr\u00e9gier", "given": "Alexandre" } }, { "id": "Robin-A-C", "name": { "family": "Robin", "given": "Annie C." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "Lidia" } }, { "id": "Taylor-J-E", "name": { "family": "Taylor", "given": "James E." } }, { "id": "Van-Waerbeke-L", "name": { "family": "Van Waerbeke", "given": "Ludovic" } } ] }, "title": "Weak Gravitational Lensing with COSMOS: Galaxy Selection and Shape Measurements", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology : observations; gravitational lensing; large-scale structure of universe", "note": "\u00a9 2007 The American Astronomical Society. \n\nReceived 2006 September 21; accepted 2007 February 11. \n\nThe HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We wish to thank our referee for useful comments and Kevin Bundy for carefully reading the manuscript. We also thank Tony Roman, Denise Taylor, and David Soderblom for their assistance in planning and scheduling of the extensive COSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration, consisting of more than 70 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/~cosmos . It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS data sets. The COSMOS Science meeting in 2005 May was supported in part by the NSF through grant OISE-0456439. C. H. is supported by a CITA National fellowship and, along with L. V. W., acknowledges support from NSERC and CIAR. In France, the COSMOS project is supported by CNES and the Programme National de Cosmologie. J. P. K. acknowledges support from CNRS.\n\nPublished - LEAapjss07.pdf
", "abstract": "With a primary goal of conducting precision weak-lensing measurements from space, the COSMOS survey has imaged the largest contiguous area observed by Hubble Space Telescope to date, using the Advanced Camera for Surveys (ACS). This is the first paper in a series in which we describe our strategy for addressing the various technical challenges in the production of weak-lensing measurements from COSMOS data. We first construct a source catalog from 575 ACS/WFC tiles (1.64 deg^2) subsampled at a pixel scale of 0.03\". Defects and diffraction spikes are carefully removed, leaving a total of 1.2 \u00d7 10^6 objects to a limiting magnitude of F814W = 26.5. This catalog is made publicly available. Multiwavelength follow-up observations of the COSMOS field provide photometric redshifts for 73% of the source galaxies in the lensing catalog. We analyze and discuss the COSMOS redshift distribution and show broad agreement with other surveys to z ~ 1. Our next step is to measure the shapes of galaxies and correct them for the distortion induced by the time-varying ACS point-spread function and for charge transfer efficiency (CTE) effects. Simulated images are used to derive the shear susceptibility factors that are necessary in transforming shape measurements into unbiased shear estimators. For every galaxy we derive a shape measurement error and utilize this quantity to extract the intrinsic shape noise of the galaxy sample. Interestingly, our results indicate that intrinsic shape noise varies little with size, magnitude, or redshift. Representing a number density of 66 galaxies per arcmin^2, the final COSMOS weak-lensing catalog contains 3.9 \u00d7 10^5 galaxies with accurate shape measurements. The properties of the COSMOS weak-lensing catalog described throughout this paper will provide key input numbers for the preparation and design of next-generation wide field space missions.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "219-238", "id_number": "CaltechAUTHORS:20100211-091709818", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100211-091709818", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NSF", "grant_number": "OISE-0456439" }, { "agency": "Canadian Institute for Theoretical Astrophysics" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIAR)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1086/516598", "primary_object": { "basename": "LEAapjss07.pdf", "url": "https://authors.library.caltech.edu/records/hatj7-1ay25/files/LEAapjss07.pdf" }, "pub_year": "2007", "author_list": "Leauthaud, Alexie; Massey, Richard; et el." }, { "id": "https://authors.library.caltech.edu/records/jqqh3-b1w36", "eprint_id": 18037, "eprint_status": "archive", "datestamp": "2023-08-22 09:54:00", "lastmod": "2023-10-20 15:31:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Cappelluti-N", "name": { "family": "Cappelluti", "given": "N." } }, { "id": "Civano-Francesca", "name": { "family": "Civano", "given": "F." }, "orcid": "0000-0002-2115-1137" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Vignali-C", "name": { "family": "Vignali", "given": "C." }, "orcid": "0000-0002-8853-9611" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Fiore-F", "name": { "family": "Fiore", "given": "F." } }, { "id": "Gilli-R", "name": { "family": "Gilli", "given": "R." } }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C. D." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J." } }, { "id": "Urry-C-M", "name": { "family": "Urry", "given": "C. M." }, "orcid": "0000-0002-0745-9792" }, { "id": "Bender-R", "name": { "family": "Bender", "given": "R." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Huchra-J-P", "name": { "family": "Huchra", "given": "J. P." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J. P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Lehmann-I", "name": { "family": "Lehmann", "given": "I." } }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "R." }, "orcid": "0000-0002-6085-3780" }, { "id": "Matute-I", "name": { "family": "Matute", "given": "I." }, "orcid": "0000-0003-1177-3896" }, { "id": "McCarthy-P-J", "name": { "family": "McCarthy", "given": "P. J." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } } ] }, "title": "The XMM-Newton Wide-Field Survey in the COSMOS Field. III. Optical Identification and Multiwavelength Properties of a Large Sample of X-Ray-Selected Sources", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; surveys; X-rays: diffuse background; X-rays: galaxies; X-rays: general", "note": "\u00a9 2007 American Astronomical Society.\n\nReceived 2006 April 24; accepted 2006 November 21.\n\nThis work is based on observations obtained with XMM-Newton,\nan ESA Science Mission with instruments and contributions\ndirectly funded by ESA Member States and the USA\n(NASA). In Germany, the XMM-Newton project is supported by\nthe Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OX 0001), the Max-Planck Society, and the Heidenhain-Stiftung. Part of this work was supported by the Deutsches Zentrum fur Luft und Raumfahrt, DLR project numbers 50 OR 0207 and 50OR 0405. In Italy, the COSMOS XMM-Newton project is supported by ASI-INAF and MIUR under grants I/023/05/00 and Cofin-03-02-23. This work is based in part on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), and on data products produced at TERAPIX data center, located at the Institute d'Astrophysique de Paris. M. B. and G. Z. gratefully\nacknowledge useful discussion with G. Micela and S. Sciortino. We thank the anonymous referee for her /his useful comments on this manuscript. We gratefully acknowledge the contributions of the entire COSMOS collaboration; more information on the COSMOS survey is available at http://www.astro.caltech.edu/~cosmos. This\nresearch has made use of the NASA/IPAC Extragalactic Database (NED) and the SDSS spectral archive.\n\nPublished - BRUapjss07.pdf
", "abstract": "We present the optical identification of a sample of 695 X-ray sources detected in the first 1.3 deg^2 of the COSMOS XMM-Newton survey, down to a 0.5-2 keV (2-10 keV) limiting flux of ~10^(-15) erg cm^(-2) s^(-1) (~5 \u00d7 10^(-15) erg cm^(-2) s^(-1)). In order to identify the correct optical counterparts and to assess the statistical significance of the X-ray-to-optical associations we have used the \"likelihood ratio technique.\" Here we present the identification method and its application to the CFHT I-band and photometric catalogs. We were able to associate a candidate optical counterpart to ~90% (626) of the X-ray sources, while for the remaining ~10% of the sources we were not able to provide a unique optical association due to the faintness of the possible optical counterparts (I_(AB) > 25) or to the presence of multiple optical sources, with similar likelihoods of being the correct identification, within the XMM-Newton error circles. We also cross-correlated the candidate optical counterparts with the Subaru multicolor and ACS catalogs and with the Magellan/IMACS, zCOSMOS, and literature spectroscopic data; the spectroscopic sample comprises 248 objects (~40% of the full sample). Our analysis of this statistically meaningful sample of X-ray sources reveals that for ~80% of the counterparts there is a very good agreement between the spectroscopic classification, the morphological parameters as derived from ACS data, and the optical-to-near-infrared colors: the large majority of spectroscopically identified broad-line active galactic nuclei (BL AGNs) have a pointlike morphology on ACS data, blue optical colors in color-color diagrams, and an X-ray-to-optical flux ratio typical of optically selected quasars. Conversely, sources classified as narrow line AGNs or normal galaxies are on average associated with extended optical sources, have significantly redder optical-to-near-infrared colors, and span a larger range of X-ray-to-optical flux ratios. However, about 20% of the sources show an apparent mismatch between the morphological and spectroscopic classifications. All the \"extended\" BL AGNs lie at redshift <1.5, while the redshift distribution of the full BL AGN population peaks at z ~ 1.5. The most likely explanation is that in these objects the nuclear emission is not dominant with respect to the host galaxy emission in the observed ACS band. Our analysis also suggests that the type 2/type 1 ratio decreases toward high luminosities, in qualitative agreement with the results from X-ray spectral analysis and the most recent modeling of the X-ray luminosity function evolution.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "353-367", "id_number": "CaltechAUTHORS:20100421-095358500", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100421-095358500", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516575", "primary_object": { "basename": "BRUapjss07.pdf", "url": "https://authors.library.caltech.edu/records/jqqh3-b1w36/files/BRUapjss07.pdf" }, "pub_year": "2007", "author_list": "Brusa, M.; Zamorani, G.; et el." }, { "id": "https://authors.library.caltech.edu/records/shcx8-cs213", "eprint_id": 16381, "eprint_status": "archive", "datestamp": "2023-08-22 09:52:10", "lastmod": "2023-10-19 22:10:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Voss-H", "name": { "family": "Voss", "given": "H." } }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "K." }, "orcid": "0000-0003-3804-2137" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Menten-K-M", "name": { "family": "Menten", "given": "K. M." }, "orcid": "0000-0001-6459-0669" }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Kreysa-E", "name": { "family": "Kreysa", "given": "E." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Aguirre-J-E", "name": { "family": "Aguirre", "given": "J." }, "orcid": "0000-0002-4810-666X" }, { "id": "Schlaerth-J-A", "name": { "family": "Schlaerth", "given": "J." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" } ] }, "title": "COSBO: The MAMBO 1.2 Millimeter Imaging Survey of the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "submillimeter; infrared : galaxies; surveys", "note": "\u00a9 2007 The American Astronomical Society. \n\nReceived 2006 September 22; accepted 2007 April 25. \n\nThe research of the Bonn-Heidelberg group was supported through a grant from the Deutsche Forschungsgemeischaft within the focus program SPP1177. K. J. acknowledges support by the German DFG under grant SCHI 536/3-1. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/~cosmos. We thank Mara Salvato and the anonymous referee for helpful comments. \n\nFacilities: IRAM (30 m), HST (ACS), VLA, Subaru, XMM, CSO (Bolocam), KPNO (FLAMINGOS)\n\nPublished - BERapjss07.pdf
", "abstract": "The inner 20 \u00d7 20 arcmin^2 of the COSMOS field was imaged at 250 GHz (1.2 mm) to an rms noise level of ~1 mJy per 11\" beam using the Max-Planck Millimeter Bolometer Array (MAMBO-2) at the IRAM 30 m telescope. We detect 15 sources at significance between 4 and 7 \u03c3, 11 of which are also detected at 1.4 GHz with the VLA with a flux density >24 \u03bcJy (3 \u03c3). We identify 12 more lower significance mm sources based on their association with faint radio sources. We present the multifrequency identifications of the MAMBO sources, including VLA radio flux densities, optical and near-infrared identifications, as well as the XMM-Newton X-ray detection for two of the mm sources. We compare radio and optical photometric redshifts and briefly describe the host galaxy morphologies. The colors of the identified optical counterparts suggest most of them to be high-redshift (z ~ 2-3) star-forming galaxies. At least three sources appear lensed by a foreground galaxy. We highlight some MAMBO sources that do not show obvious radio counterparts. These sources could be dusty starburst galaxies at redshifts >3.5. The 250 GHz source areal density in the COSMOS field is comparable to that seen in other deep mm fields.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "132-149", "id_number": "CaltechAUTHORS:20091019-113011828", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091019-113011828", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeischaft (DFG)", "grant_number": "SCHI 536/3-1" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/520511", "primary_object": { "basename": "BERapjss07.pdf", "url": "https://authors.library.caltech.edu/records/shcx8-cs213/files/BERapjss07.pdf" }, "pub_year": "2007", "author_list": "Bertoldi, F.; Carilli, C. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/ymx2b-dcd35", "eprint_id": 17534, "eprint_status": "archive", "datestamp": "2023-08-22 09:53:12", "lastmod": "2023-10-19 23:58:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Abraham-R-G", "name": { "family": "Abraham", "given": "R. G." }, "orcid": "0000-0002-4542-921X" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Barnes-J-E", "name": { "family": "Barnes", "given": "J. E." } }, { "id": "Benson-A-J", "name": { "family": "Benson", "given": "A." }, "orcid": "0000-0001-5501-6008" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C." }, "orcid": "0000-0001-6647-3861" }, { "id": "Carlstrom-J-E", "name": { "family": "Carlstrom", "given": "J. E." }, "orcid": "0000-0002-2044-7665" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Colbert-J-W", "name": { "family": "Colbert", "given": "J." } }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Ewald-S-P", "name": { "family": "Ewald", "given": "S. P." }, "orcid": "0000-0002-1567-9154" }, { "id": "Fall-M", "name": { "family": "Fall", "given": "M." } }, { "id": "Franceschini-A", "name": { "family": "Franceschini", "given": "A." } }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Green-W", "name": { "family": "Green", "given": "W." } }, { "id": "Griffiths-R-E", "name": { "family": "Griffiths", "given": "R. E." } }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Koda-Jin", "name": { "family": "Koda", "given": "J." }, "orcid": "0000-0002-8762-7863" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Liu-Charles-T", "name": { "family": "Liu", "given": "C. T." }, "orcid": "0000-0002-4314-8713" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "R." }, "orcid": "0000-0002-6085-3780" }, { "id": "Mellier-Y", "name": { "family": "Mellier", "given": "Y." } }, { "id": "Miyazaki-Satoshi", "name": { "family": "Miyazaki", "given": "S." } }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Mould-J-R", "name": { "family": "Mould", "given": "J." }, "orcid": "0000-0003-3820-1740" }, { "id": "Norman-C", "name": { "family": "Norman", "given": "C." } }, { "id": "Refregier-A", "name": { "family": "Refregier", "given": "A." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Rich-M", "name": { "family": "Rich", "given": "M." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P. L." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Tyson-N-D", "name": { "family": "Tyson", "given": "N. D." } }, { "id": "Urry-C-M", "name": { "family": "Urry", "given": "C. M." }, "orcid": "0000-0002-0745-9792" }, { "id": "van-Waerbeke-L", "name": { "family": "van Waerbeke", "given": "L." } }, { "id": "Vettolani-P", "name": { "family": "Vettolani", "given": "P." } }, { "id": "White-S-D-M", "name": { "family": "White", "given": "S. D. M." } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" } ] }, "title": "COSMOS: Hubble Space Telescope Observations", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; dark matter; galaxies: evolution; galaxies: formation; large-scale structure of universe; surveys", "note": "\u00a9 2007 American Astronomical Society. \n\nPrint publication: Issue 1 (2007 September); received 2006 April 24; accepted for publication 2006 June 28. \n\nThe HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We wish to thank Tony Roman, Denise Taylor, and David Soderblom for their assistance in the planning and scheduling of the extensive COSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration, consisting of more than 70 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS data sets. The COSMOS Science meeting in 2005 May was supported in part by the NSF through grant OISE-0456439. We thank Rob Kennicutt for suggestions on the manuscript. \n\nFacilities: HST (ACS), HST (NICMOS), HST (WFPC2)\n\nPublished - SCOapjss07b.pdf
", "abstract": "The Cosmic Evolution Survey (COSMOS) was initiated with an extensive allocation (590 orbits in Cycles 12-13) using the Hubble Space Telescope (HST) for high-resolution imaging. Here we review the characteristics of the HST imaging with the Advanced Camera for Surveys (ACS) and parallel observations with NICMOS and WFPC2. A square field (1.8 deg^2) has been imaged with single-orbit ACS I-band F814W exposures with 50% completeness for sources 0.5\" in diameter at I_(AB) = 26.0 mag. The ACS is a key part of the COSMOS survey, providing very high sensitivity and high-resolution (0.09\" FWHM and 0.05\" pixels) imaging and detecting a million objects. These images yield resolved morphologies for several hundred thousand galaxies. The small HST PSF also provides greatly enhanced sensitivity for weak-lensing investigations of the dark matter distribution.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "38-45", "id_number": "CaltechAUTHORS:20100219-111648129", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100219-111648129", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NSF", "grant_number": "OISE-0456439" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516580", "primary_object": { "basename": "SCOapjss07b.pdf", "url": "https://authors.library.caltech.edu/records/ymx2b-dcd35/files/SCOapjss07b.pdf" }, "pub_year": "2007", "author_list": "Scoville, N.; Abraham, R. G.; et el." }, { "id": "https://authors.library.caltech.edu/records/bx0g5-3dc70", "eprint_id": 17146, "eprint_status": "archive", "datestamp": "2023-08-22 09:52:31", "lastmod": "2023-10-19 22:50:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Takahashi-M-I", "name": { "family": "Takahashi", "given": "M. I." } }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Ajiki-M", "name": { "family": "Ajiki", "given": "M." } }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S. S." } }, { "id": "Koizumi-O", "name": { "family": "Koizumi", "given": "O." } }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "T." }, "orcid": "0000-0002-7402-5441" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C." }, "orcid": "0000-0001-6647-3861" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Garilli-B", "name": { "family": "Garilli", "given": "B." } }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Kitzbichler-M-G", "name": { "family": "Kitzbichler", "given": "M. G." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Maccagni-D", "name": { "family": "Maccagni", "given": "D." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Rich-M", "name": { "family": "Rich", "given": "M." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P." } }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Tribiano-S", "name": { "family": "Tribiano", "given": "S." } }, { "id": "Ideue-Y", "name": { "family": "Ideue", "given": "Y." } }, { "id": "Mihara-S", "name": { "family": "Mihara", "given": "S." } } ] }, "title": "The [O II] \u03bb3727 Luminosity Function and Star Formation Rate at z \u2248 1.2 in the COSMOS 2 Square Degree Field and the Subaru Deep Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: distances and redshifts; galaxies: evolution; galaxies: luminosity function, mass function", "note": "\u00a9 2007 American Astronomical Society . \n\nPrint publication: Issue 1 (2007 September); received 2006 September 15; accepted for publication 2007 March 3. \n\nThe HST COSMOS treasury program was supported through NASA grant HST-GO-09822. We greatly acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. The COSMOS science meeting in 2005 May was supported by in part by the NSF through grant OISE-0456439. We would also like to thank the Subaru Telescope staff for their invaluable help. This work was financially supported in part by the JSPS (grants 15340059 and 17253001). S. S. S. and T. N. are JSPS fellows.\n\nPublished - TAKapjss07.pdf
", "abstract": "We have carried out a wide-field imaging survey for [O II] \u03bb3727 emitting galaxies at z \u2248 1.2 in the HST COSMOS 2 square degree field using the Suprime-Cam on the Subaru Telescope. The survey covers a sky area of 6700 arcmin^2 in the COSMOS field, and a redshift range between 1.17 and 1.20 (\u0394z = 0.03), corresponding to a survey volume of 5.56 \u00d7 10^5 Mpc^3. We obtain a sample of 3176 [O II] emitting galaxies with observed emission-line equivalent widths greater than 26 \u00c5. Since our survey tends to sample brighter [O II] emitting galaxies, we also analyze a sample of fainter [O II] emitting galaxies found in the Subaru Deep Field (SDF). We find an extinction-corrected [O II] luminosity density of 10^(40.35)^(+0.08)_(-0.06) ergs s^(-1) Mpc^(-3), corresponding to star formation rate density of 0.32^(+0.06)_(-0.04) M_\u2609 yr^(-1) Mpc^(-3) in the COSMOS field at z \u2248 1.2. This is the largest survey for [O II] emitters beyond z = 1 currently available.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "456-467", "id_number": "CaltechAUTHORS:20100112-113531217", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100112-113531217", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NSF", "grant_number": "OISE-0456439" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15340059" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17253001" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1086/518037", "primary_object": { "basename": "TAKapjss07.pdf", "url": "https://authors.library.caltech.edu/records/bx0g5-3dc70/files/TAKapjss07.pdf" }, "pub_year": "2007", "author_list": "Takahashi, M. I.; Shioya, Y.; et el." }, { "id": "https://authors.library.caltech.edu/records/q942r-hah07", "eprint_id": 16855, "eprint_status": "archive", "datestamp": "2023-08-22 09:52:21", "lastmod": "2023-10-19 22:36:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Trump-J-R", "name": { "family": "Trump", "given": "Jonathan R." } }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "Chris D." } }, { "id": "McCarthy-P-J", "name": { "family": "McCarthy", "given": "Patrick J." } }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "id": "Huchra-J-P", "name": { "family": "Huchra", "given": "John P." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "Marcella" }, "orcid": "0000-0002-5059-6848" }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G\u00fcnther" }, "orcid": "0000-0002-0797-0646" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "Simon J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Magellan Spectroscopy of AGN Candidates in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; quasars: general; surveys", "note": "\u00a9 2009 American Astronomical Society.\n\nPrint publication: Issue 1 (2007 September); received 2006 April 24; accepted for publication 2006 May 26.\n\nWe would like to thank Alan Dressler and the IMACS team for\ncreating an excellent instrument, as well as telescope operators\nHernan Nu\u00f1ez and Felipe Sanchez and the Las Campanas Observatory\nstaff for support while observing. We thank Mike\nWestover for help with the January observations.We also thank\nthe COSMOS team for their work in creating the catalogs used\nfor selecting our targets. The HST COSMOS Treasury program\nwas supported through NASA grant HST-GO-09822.\n\nPublished - TRUapjss07.pdf
", "abstract": "We present spectroscopic redshifts for the first 466 X-ray- and radio-selected AGN targets in the 2 deg^2 COSMOS field. Spectra were obtained with the IMACS instrument on the Magellan (Baade) telescope, using the nod-and-shuffle technique. We identify a variety of type 1 and type 2 AGNs, as well as red galaxies with no emission lines. Our redshift yield is 72% down to i_(AB) = 24, although the yield is >90% for i_(AB) < 22. We expect the completeness to increase as the survey continues. When our survey is complete and additional redshifts from the zCOSMOS project are included, we anticipate ~1100 AGNs with redshifts over the entire COSMOS field. Our redshift survey is consistent with an obscured AGN population that peaks at z ~ 0.7, although further work is necessary to disentangle the selection effects.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "383-395", "id_number": "CaltechAUTHORS:20091202-100349927", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091202-100349927", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516578", "primary_object": { "basename": "TRUapjss07.pdf", "url": "https://authors.library.caltech.edu/records/q942r-hah07/files/TRUapjss07.pdf" }, "pub_year": "2007", "author_list": "Trump, Jonathan R.; Impey, Chris D.; et el." }, { "id": "https://authors.library.caltech.edu/records/yc736-n4k55", "eprint_id": 17452, "eprint_status": "archive", "datestamp": "2023-08-22 09:52:42", "lastmod": "2023-10-19 23:54:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Sakelliou-I", "name": { "family": "Sakelliou", "given": "I." } }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Botzler-C-S", "name": { "family": "Botzler", "given": "C. S." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Ajiki-M", "name": { "family": "Ajiki", "given": "M." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Jahnke-K", "name": { "family": "Jahnke", "given": "K." }, "orcid": "0000-0003-3804-2137" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S. S." } }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Trump-J-R", "name": { "family": "Trump", "given": "J. R." } } ] }, "title": "A Wide-Angle Tail Radio Galaxy in the COSMOS Field: Evidence for Cluster Formation", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: individual (CWAT-01); galaxies: jets; radio continuum: galaxies; surveys; X-rays: galaxies: clusters", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 1 (2007 September); received 2006 April 25; accepted for publication 2006 August 15.\n\nV. S. thanks Rachel Somerville and Klaus Meisenheimer for\ninsightful discussions. C. C., E. S., and V. S. acknowledge\nsupport from NASA grant HST GO-09822.31-A; C. C. would\nlike to acknowledge support from the Max Planck Society and\nthe Alexander von Humboldt Foundation through the Max-\nPlanck-Forschungspreis 2005. A. F. acknowledges support\nfrom BMBF/DLR under grant 50 OR 0207, MPG and a partial\nsupport from NASA grant NNG04GF686. I. S. acknowledges\nthe support of the European Community under a Marie Curie\nIntra-European Fellowship. C. S. B. acknowledges funding by\nthe Deutsche Forschungsgemeinschaft. K. J. acknowledges support\nby the German DFG under grant SCHI 536/3-1.\nThe XMM-Newton project is an ESA Science Mission with\ninstruments and contributions directly funded by ESA member\nstates and the USA (NASA). The XMM-Newton project is supported\nby the Bundesministeriumfu\u00a8rWirtschaft und Technologie/\nDeutsches Zentrum fu\u00a8r Luft- und Raumfahrt (BMWI/DLR,\nFKZ 50 OX 0001), theMax Planck Society, and the Heidenhain-\nStiftung, and also by PPARC, CEA, CNES, and ASI. Part of\nthis work was also supported by the Deutsches Zentrum fu\u00a8 r Luftund\nRaumfahrt, DLR project numbers 50 OR 0207 and 50 OR\n0405.\nFunding for the Sloan Digital Sky Survey (SDSS) has been\nprovided by the Alfred P. Sloan Foundation, the Participating\nInstitutions, the National Aeronautics and Space Administration,\nthe National Science Foundation, the US Department of Energy,\nthe JapaneseMonbukagakusho, and theMax Planck Society. The\nSDSS Web site is http://www.sdss.org.\nThe SDSS is managed by the Astrophysical Research Consortium\n(ARC) for the Participating Institutions. The Participating\nInstitutions are the University of Chicago, Fermilab, the Institute\nfor Advanced Study, the Japan Participation Group, the Johns\nHopkinsUniversity, the Korean Scientist Group, Los AlamosNa-\n2tional Laboratory, the Max Planck Institute for Astronomy, the\nMax Planck Institute for Astrophysics, New Mexico State University,\ntheUniversity of Pittsburgh, theUniversity of Portsmouth,\nPrinceton University, the US Naval Observatory, and the University of Washington.\n\nPublished - SMOapjss07.pdf
", "abstract": "We have identified a complex galaxy cluster system in the COSMOS field via a wide-angle tail (WAT) radio galaxy, consistent with the idea that WAT galaxies can be used as tracers of clusters. The WAT galaxy, CWAT-01, is coincident with an elliptical galaxy resolved in the HST ACS image. Using the COSMOS multiwavelength data set, we derive the radio properties of CWAT-01 and use the optical and X-ray data to investigate its host environment. The cluster hosting CWAT-01 is part of a larger assembly consisting of a minimum of four X-ray luminous clusters within ~2 Mpc distance. We apply hydrodynamic models that combine ram pressure and buoyancy forces on CWAT-01. These models explain the shape of the radio jets only if the galaxy's velocity relative to the intracluster medium (ICM) is in the range of about 300-550 km s^(-1), which is higher than expected for brightest cluster galaxies (BCGs) in relaxed systems. This indicates that the CWAT-01 host cluster is not relaxed but is possibly dynamically young. We argue that such a velocity could have been induced through subcluster merger within the CWAT-01 parent cluster and/or cluster-cluster interactions. Our results strongly indicate that we are witnessing the formation of a large cluster from an assembly of multiple clusters, consistent with the hierarchical scenario of structure formation. We estimate the total mass of the final cluster to be approximately 20% of the mass of the Coma Cluster.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "295-313", "id_number": "CaltechAUTHORS:20100211-104043723", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100211-104043723", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST GO-09822.31" }, { "agency": "Max Planck Society" }, { "agency": "Alexander von Humboldt Foundation" }, { "agency": "Bundesministerium f\u00fcr Bildung und Forschung (BMBF)", "grant_number": "50 OR 0207" }, { "agency": "NASA", "grant_number": "NNG04GF686" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "SCHI 536/3-1" }, { "agency": "Max-Planck-Forschungspreis", "grant_number": "2005" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1086/516583", "primary_object": { "basename": "SMOapjss07.pdf", "url": "https://authors.library.caltech.edu/records/yc736-n4k55/files/SMOapjss07.pdf" }, "pub_year": "2007", "author_list": "Smol\u010di\u0107, V.; Schinnerer, E.; et el." }, { "id": "https://authors.library.caltech.edu/records/j3mst-5bg40", "eprint_id": 17714, "eprint_status": "archive", "datestamp": "2023-08-22 09:53:39", "lastmod": "2023-10-20 00:10:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M. T." }, "orcid": "0000-0003-1033-9684" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Feldmann-R", "name": { "family": "Feldmann", "given": "R." }, "orcid": "0000-0002-1109-1919" }, { "id": "Kampczyk-P", "name": { "family": "Kampczyk", "given": "P." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A." }, "orcid": "0000-0002-3677-3617" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "R." }, "orcid": "0000-0002-6085-3780" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L. A. M." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D-J", "name": { "family": "Thompson", "given": "D. J." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" } ] }, "title": "The Evolution of the Number Density of Large Disk Galaxies in COSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: formation; large-scale structure of universe; surveys", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 1 (2007 September); received 2006 April 25; accepted for publication 2006 July 25.\n\nWe thank the anonymous referee for his valuable comments\nand suggested improvements to the original manuscript. The HST\nCOSMOS Treasury program was supported through NASA grant\nHST-GO-09822. We wish to thank Tony Roman, Denise Taylor,\nand David Soderblom for their assistance in planning and scheduling\nof the extensive COSMOS observations. We gratefully acknowledge\nthe contributions of the entire COSMOS collaboration\nconsisting of more than 70 scientists. More information on the\nCOSMOS survey is available at http://www.astro.caltech.edu/\n~cosmos. We acknowledge the services provided by the NASA\nIPAC/IRSA staff in providing online archive and server capabilities\nfor the COSMOS data sets. P. Kampczyk, C. Scarlata,\nand M. T. Sargent acknowledge support from the Swiss National\nScience Foundation.\nFacilities: HST (ACS).\n\nPublished - SARapjss07.pdf
", "abstract": "We study a sample of approximately 16,500 galaxies with I_(ACS,AB) \u2264 22.5 in the central 38% of the COSMOS field, which are extracted from a catalog constructed from the Cycle 12 ACS F814W COSMOS data set. Structural information on the galaxies is derived by fitting single S\u00e9rsic models to their two-dimensional surface brightness distributions. In this paper we focus on the disk galaxy population (as classified by the Zurich Estimator of Structural Types), and investigate the evolution of the number density of disk galaxies larger than approximately 5 kpc between redshift z ~ 1 and the present epoch. Specifically, we use the measurements of the half-light radii derived from the S\u00e9rsic fits to construct, as a function of redshift, the size function \u03a6(r_(1/2), z) of both the total disk galaxy population and of disk galaxies split in four bins of bulge-to-disk ratio. In each redshift bin, the size function specifies the number of galaxies per unit comoving volume and per unit half-light radius r_(1/2). Furthermore, we use a selected sample of roughly 1800 SDSS galaxies to calibrate our results with respect to the local universe. We find the following: (1) The number density of disk galaxies with intermediate sizes (r_(1/2) ~ 5-7 kpc) remains nearly constant from z ~ 1 to today. Unless the growth and destruction of such systems exactly balanced in the last eight billion years, they must have neither grown nor been destroyed over this period. (2) The number density of the largest disks (r_(1/2) > 7 kpc) decreases by a factor of about 2 out to z ~ 1. (3) There is a constancy\u2014or even slight increase\u2014in the number density of large bulgeless disks out to z ~ 1; the deficit of large disks at early epochs seems to arise from a smaller number of bulged disks. Our results indicate that the bulk of the large disk galaxy population has completed its growth by z ~ 1 and support the theory that secular evolution processes produce\u2014or at least add stellar mass to\u2014the bulge components of disk galaxies.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "434-455", "id_number": "CaltechAUTHORS:20100310-103310241", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100310-103310241", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swiss National Science Foundation (SNSF)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516584", "primary_object": { "basename": "SARapjss07.pdf", "url": "https://authors.library.caltech.edu/records/j3mst-5bg40/files/SARapjss07.pdf" }, "pub_year": "2007", "author_list": "Sargent, M. T.; Carollo, C. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/3ngdz-djz92", "eprint_id": 18089, "eprint_status": "archive", "datestamp": "2023-08-22 09:54:42", "lastmod": "2023-10-20 15:34:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Cappeluti-N", "name": { "family": "Cappeluti", "given": "N." } }, { "id": "Brunner-H", "name": { "family": "Brunner", "given": "H." } }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "A." }, "orcid": "0000-0002-4606-5403" }, { "id": "Fiore-F", "name": { "family": "Fiore", "given": "F." } }, { "id": "Franceschini-A", "name": { "family": "Franceschini", "given": "A." } }, { "id": "Gilli-R", "name": { "family": "Gilli", "given": "R." } }, { "id": "Griffiths-R-E", "name": { "family": "Griffiths", "given": "R. E." } }, { "id": "Lehmann-I", "name": { "family": "Lehmann", "given": "I." } }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Matt-G", "name": { "family": "Matt", "given": "G." }, "orcid": "0000-0002-2152-0916" }, { "id": "Matute-I", "name": { "family": "Matute", "given": "I." }, "orcid": "0000-0003-1177-3896" }, { "id": "Miyaji-Takamitsu", "name": { "family": "Miyaji", "given": "T." } }, { "id": "Molendi-S", "name": { "family": "Molendi", "given": "S." } }, { "id": "Paltani-S", "name": { "family": "Paltani", "given": "S." }, "orcid": "0000-0002-8108-9179" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Urry-C-M", "name": { "family": "Urry", "given": "C. M." }, "orcid": "0000-0002-0745-9792" }, { "id": "Vettolani-P", "name": { "family": "Vettolani", "given": "P." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } } ] }, "title": "The XMM-Newton Wide-Field Survey in the COSMOS Field. I. Survey Description", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; large-scale structure of universe; dark matter; galaxies: formation; galaxies: evolution; X-rays: galaxies", "note": "\u00a9 2007 American Astronomical Society. \n\nReceived 2006 April 24; accepted 2006 September 28. \n\nThis work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions\ndirectly funded by ESA Member States and the US\n(NASA). In Germany, the XMM-Newton project is supported by\nthe Bundesministerium fur Bildung und Forschung/Deutsches\nZentrum fur Luft und Raumfahrt, and the Max-Planck Society. Part of this work was supported by the Deutsches Zentrum fur Luft- und Raumfahrt, DLR project numbers 50 OR 0207 and 50 OR 0405. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu /cosmos. This research\nhas made use of the NASA/IPAC Extragalactic Database\n(NED) and the SDSS spectral archive. We thank Guinevere\nKauffmann and Jarle Brinchmann for help with the object No.\n2608. We acknowledge helpful comments from an anonymous\nreferee.\n\nPublished - HASapjss07.pdf
", "abstract": "We present the first set of XMM-Newton EPIC observations in the 2 deg^2 COSMOS field. The strength of the COSMOS project is the unprecedented combination of a large solid angle and sensitivity over the whole multiwavelength spectrum. The XMM-Newton observations are very efficient in localizing and identifying active galactic nuclei (AGNs) and clusters, as well as groups of galaxies. One of the primary goals of the XMM-Newton Cosmos survey is to study the coevolution of active galactic nuclei as a function of their environment in the cosmic web. Here we present the log of observations, images, and a summary of first research highlights for the first pass of 25 XMM-Newton pointings across the field. In the existing data set we have detected 1416 new X-ray sources in the 0.5-2, 2-4.5, and 4.5-10 keV bands to an equivalent 0.5-2 keV flux limit of 7 \u00d7 10^(-16) erg cm^(-2) s^(-1). The number of sources is expected to grow to almost 2000 in the final coverage of the survey. From an X-ray color-color analysis we identify a population of heavily obscured, partially leaky or reflecting absorbers, most of which are likely to be nearby, Compton-thick AGNs.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "29-37", "id_number": "CaltechAUTHORS:20100430-103501056", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100430-103501056", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50 OR 0207" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50 OR 0405" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1086/516576", "primary_object": { "basename": "HASapjss07.pdf", "url": "https://authors.library.caltech.edu/records/3ngdz-djz92/files/HASapjss07.pdf" }, "pub_year": "2007", "author_list": "Hasinger, G.; Cappeluti, N.; et el." }, { "id": "https://authors.library.caltech.edu/records/9q60g-wxg89", "eprint_id": 58788, "eprint_status": "archive", "datestamp": "2023-08-19 20:52:45", "lastmod": "2023-10-23 19:42:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S. S." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Ajiki-M", "name": { "family": "Ajiki", "given": "M." } }, { "id": "Komiyama-Yutaka", "name": { "family": "Komiyama", "given": "Y." } }, { "id": "Miyazaki-Satoshi", "name": { "family": "Miyazaki", "given": "S." } }, { "id": "Kaifu-Norio", "name": { "family": "Kaifu", "given": "N." } }, { "id": "Karoji-Hiroshi", "name": { "family": "Karoji", "given": "H." } }, { "id": "Okamura-Sadanori", "name": { "family": "Okamura", "given": "S." } }, { "id": "Arimoto-Nobuo", "name": { "family": "Arimoto", "given": "N." } }, { "id": "Ohta-K", "name": { "family": "Ohta", "given": "K." } }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "T." }, "orcid": "0000-0002-7402-5441" }, { "id": "Koda-Jin", "name": { "family": "Koda", "given": "J." }, "orcid": "0000-0002-8762-7863" }, { "id": "Hainline-L-J", "name": { "family": "Hainline", "given": "L." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Rich-M", "name": { "family": "Rich", "given": "M." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" } ] }, "title": "A Potential Galaxy Threshing System in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2007 The American Astronomical Society. \n\nReceived 2006 April 24; accepted 2006 November 5. \n\nBased on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. \n\nThe HST COSMOS Treasury program was supported through\nNASA grant HST-GO-09822. We wish to thank Tony Roman,\nDenise Taylor, and David Soderblom for their assistance in\nplanning and scheduling of the extensive COSMOS observations.\nWe gratefully acknowledge the contributions of the entire\nCOSMOS collaboration consisting of more than 70 scientists.\nMore information on the COSMOS survey is available at http://\nwww.astro.caltech.edu/~cosmos. It is a pleasure the acknowledge\nthe excellent services provided by the NASA IPAC/IRSA\nstaff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and\nJohn Good) in providing on-line archive and server capabilities\nfor the COSMOS data sets. The COSMOS Science meeting in\n2005 May was supported in part by the NSF through grant OISE-\n0456439. We would like to thank the Subaru Telescope staff for\ntheir invaluable assistance. IRAF (Image Reduction and Analysis\nFacility) is distributed by the National Optical Astronomy\nObservatory, which is operated by the Association of Universities\nfor Research in Astronomy, Inc., under cooperative agreement\nwith the National Science Foundation. This work was financially\nsupported in part by the Ministry of Education, Culture, Sports,\nScience, and Technology (Nos. 10044052 and 10304013), and by\nthe Japan Society for the Promotion of Science (15340059 and\n17253001). S. S. S. and T. N. are financially supported by the\nJapan Society for the Promotion of Science (JSPS) through JSPS\nResearch Fellowship for Young Scientists.\n\nPublished - 0067-0049_172_1_511.pdf
", "abstract": "We report on the discovery of a new potential galaxy threshing system in the COSMOS 2 square degree field using the prime-focus camera, Suprime-Cam, on the 8.2 m Subaru Telescope. This system consists of a giant elliptical galaxy with M_V \u2248 -21.6 and a tidally disrupted satellite galaxy with M_V \u2248 -17.7 at a photometric redshift of z \u2248 0.08. This redshift is consistent with the spectroscopic redshift of 0.079 for the giant elliptical galaxy obtained from the Sloan Digital Sky Survey (SDSS) archive. The luminosity masses of the two galaxies are 3.7 \u00d7 10^(12) and 3.1 \u00d7 10^9 M\u2609, respectively. The distance between the two galaxies is greater than 100 kpc. The two tidal tails emanating from the satellite galaxy extend over 150 kpc. This system would be the second well-defined galaxy threshing system found so far.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "511-517", "id_number": "CaltechAUTHORS:20150707-101935485", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150707-101935485", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NSF", "grant_number": "OISE-0456439" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "10044052" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "10304013" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15340059" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17253001" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516581", "primary_object": { "basename": "0067-0049_172_1_511.pdf", "url": "https://authors.library.caltech.edu/records/9q60g-wxg89/files/0067-0049_172_1_511.pdf" }, "pub_year": "2007", "author_list": "Sasaki, S. S.; Taniguchi, Y.; et el." }, { "id": "https://authors.library.caltech.edu/records/4akyt-ke840", "eprint_id": 20674, "eprint_status": "archive", "datestamp": "2023-08-22 09:54:56", "lastmod": "2023-10-20 23:19:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P." } }, { "id": "Thompson-D", "name": { "family": "Thompson", "given": "D." } } ] }, "title": "zCOSMOS: A large VLT/VIMOS redshift survey covering 0 < z < 3 in the COSMOS field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: distances and redshifts; galaxies: evolution; large-scale structure of universe; quasars: general; surveys", "note": "\u00a9 2007 The American Astronomical Society. Received 2006 April 28; accepted 2006 November 21. \n\nBased on observations undertaken at the European Southern Observatory\n(ESO) Very Large Telescope (VLT) under Large Program 175.A-0839. Also based\non observations with the NASA/ESA Hubble Space Telescope, obtained at the Space\nTelescope Science Institute, operated by the Association of Universities for Research\nin Astronomy, Inc. (AURA), under NASA contract NAS 5Y26555, with the Subaru\nTelescope, operated by the National Astronomical Observatory of Japan, with the\ntelescopes of the National Optical Astronomy Observatory, operated by the Association\nof Universities for Research in Astronomy, Inc. (AURA), under cooperative\nagreement with the National Science Foundation, and with the Canada-France-\nHawaii Telescope, operated by the National Research Council of Canada, the Centre\nNational de la Recherche Scientifique de France, and the University of Hawaii.\n\n\nEfficient execution of such a large program in Service Mode\non the VLT requires the efforts of many individual observatory\nstaff at ESO, both in Garching and on Cerro Paranal, and we gratefully\nacknowledge the contribution of these many and regrettably\nsometimes anonymous individuals to our project. The zCOSMOS\nprogram builds on many of the hardware and software tools built\nby the VIMOS/VVDS team, and we gratefully acknowledge here\nthe contribution of those in the VIMOS/VVDS team who are not\npart of the zCOSMOS project. Finally, we acknowledge with appreciation\nthe contributions of those individuals not listed as authors\nwho have worked, directly or indirectly, to produce the\nsuperb imaging data on which the COSMOS survey is based.\n\nPublished - LILapjss07.pdf
", "abstract": "zCOSMOS is a large-redshift survey that is being undertaken in the COSMOS field using 600 hr of observation\nwith the VIMOS spectrograph on the 8 m VLT. The survey is designed to characterize the environments of COSMOS\ngalaxies from the 100 kpc scales of galaxy groups up to the 100 Mpc scale of the cosmic web and to produce diagnostic\ninformation on galaxies and active galactic nuclei. The zCOSMOS survey consists of two parts: (1) zCOSMOSbright,\na magnitude-limited I-band I_(AB) < 22.5 sample of about 20,000 galaxies with 0.1 < z < 1.2 covering the whole\n1.7 deg^2 COSMOS ACS field, for which the survey parameters at z ~ 0.7 are designed to be directly comparable to\nthose of the 2dFGRS at z ~ 0.1; and (2) zCOSMOS-deep, a survey of approximately 10,000 galaxies selected through\ncolor-selection criteria to have 1.4 < z < 3.0, within the central 1 deg^2. This paper describes the survey design and the\nconstruction of the target catalogs and briefly outlines the observational program and the data pipeline. In the first\nobserving season, spectra of 1303 zCOSMOS-bright targets and 977 zCOSMOS-deep targets have been obtained.\nThese are briefly analyzed to demonstrate the characteristics that may be expected from zCOSMOS, and particularly\nzCOSMOS-bright, when it is finally completed between 2008 and 2009. The power of combining spectroscopic and\nphotometric redshifts is demonstrated, especially in correctly identifying the emission line in single-line spectra and in\ndetermining which of the less reliable spectroscopic redshifts are correct and which are incorrect. These techniques\nbring the overall success rate in the zCOSMOS-bright so far to almost 90% and to above 97% in the 0.5 < z < 0.8\nredshift range. Our zCOSMOS-deep spectra demonstrate the power of our selection techniques to isolate high-redshift\ngalaxies at 1.4 < z < 3.0 and of VIMOS to measure their redshifts using ultraviolet absorption lines.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "70-85", "id_number": "CaltechAUTHORS:20101104-124938229", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101104-124938229", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1086/516589", "primary_object": { "basename": "LILapjss07.pdf", "url": "https://authors.library.caltech.edu/records/4akyt-ke840/files/LILapjss07.pdf" }, "pub_year": "2007", "author_list": "Lilly, S. J.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/cgfz3-qr528", "eprint_id": 17533, "eprint_status": "archive", "datestamp": "2023-08-22 09:53:07", "lastmod": "2023-10-19 23:58:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Brusa-Marcella", "name": { "family": "Brusa", "given": "M." }, "orcid": "0000-0002-5059-6848" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Guzzo-L", "name": { "family": "Guzzo", "given": "L." } }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. M." }, "orcid": "0000-0003-0427-8387" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Tyson-N-D", "name": { "family": "Tyson", "given": "N. D." } } ] }, "title": "The Cosmic Evolution Survey (COSMOS): Overview", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; dark matter; galaxies: evolution; galaxies: formation; large-scale structure of universe; surveys", "note": "\u00a9 2007 American Astronomical Society. \n\nPrint publication: Issue 1 (2007 September); received 2006 April 25; accepted for publication 2006 June 28. \n\nWe gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. The COSMOS Science meeting in 2005 May was supported in part by the NSF through grant OISE-0456439. \n\nFacilities: HST (ACS), HST (NICMOS), HST (WFPC2), Subaru (Scam), NRAO (VLA), XMM, GALEX, Spitzer (IRAC), Spitzer (MIPS), CFHT, UKIRT, CSO, IRAM (30m). \n\nBased on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555; also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory under Large Program 175.A-0839, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the AURA, Inc., under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; and the Canada-France-Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the NRC and CADC of Canada, the CNRS of France, TERAPIX, and the University of Hawaii.\n\nPublished - SCOapjss07.pdf
", "abstract": "The Cosmic Evolution Survey (COSMOS) is designed to probe the correlated evolution of galaxies, star formation, active galactic nuclei (AGNs), and dark matter (DM) with large-scale structure (LSS) over the redshift range z > 0.5-6. The survey includes multiwavelength imaging and spectroscopy from X-ray-to-radio wavelengths covering a 2 deg^2 area, including HST imaging. Given the very high sensitivity and resolution of these data sets, COSMOS also provides unprecedented samples of objects at high redshift with greatly reduced cosmic variance, compared to earlier surveys. Here we provide a brief overview of the survey strategy, the characteristics of the major COSMOS data sets, and a summary the science goals.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "1-8", "id_number": "CaltechAUTHORS:20100219-111628660", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100219-111628660", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NSF", "grant_number": "OISE-0456439" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516585", "primary_object": { "basename": "SCOapjss07.pdf", "url": "https://authors.library.caltech.edu/records/cgfz3-qr528/files/SCOapjss07.pdf" }, "pub_year": "2007", "author_list": "Scoville, N.; Aussel, H.; et el." }, { "id": "https://authors.library.caltech.edu/records/rzhjp-de478", "eprint_id": 17715, "eprint_status": "archive", "datestamp": "2023-08-22 09:53:44", "lastmod": "2023-10-20 00:10:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J. A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D." }, "orcid": "0000-0003-1924-1122" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Brooke-T", "name": { "family": "Brooke", "given": "T." } }, { "id": "Bhattacharya-B", "name": { "family": "Bhattacharya", "given": "B." } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Barnes-J-E", "name": { "family": "Barnes", "given": "J. E." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C." }, "orcid": "0000-0001-6647-3861" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Fall-S-M", "name": { "family": "Fall", "given": "S. M." } }, { "id": "Franceschini-A", "name": { "family": "Franceschini", "given": "A." } }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Liu-Michael-C", "name": { "family": "Liu", "given": "M. C." }, "orcid": "0000-0003-2232-7664" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Rich-M", "name": { "family": "Rich", "given": "M." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P. L." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D-J", "name": { "family": "Thompson", "given": "D. J." } }, { "id": "Urry-C-M", "name": { "family": "Urry", "given": "C. M." }, "orcid": "0000-0002-0745-9792" }, { "id": "Williams-J-P", "name": { "family": "Williams", "given": "J. P." }, "orcid": "0000-0001-5058-695X" } ] }, "title": "S-COSMOS: The Spitzer Legacy Survey of the Hubble Space Telescope ACS 2 deg^2 COSMOS Field I: Survey Strategy and First Analysis", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: formation; infrared: galaxies; large-scale structure of universe; surveys", "note": "\u00a9 2007 American Astronomical Society. \n\nPrint publication: Issue 1 (2007 September); received 2006 August 28; accepted for publication 2007 January 9. \n\nThis work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology under NASA contract 1407. Support for this work was provided by NASA through contract 1278386 issued by the JPL. It is a pleasure to acknowledge the hospitality provided by the Aspen Center for Physics where the majority of this paper was written. Additional information on the S-COSMOS Legacy Survey is available from the main COSMOSWeb site at http://www.astro.caltech.edu/cosmos. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS data sets. We thank Guilaine Lagache for useful comments on power spectra measurements. We would also like to thank the referee for comments and suggestions which helped clarify our presentation. \n\nFacilities: HST (ACS), Spitzer (IRAC), Spitzer (MIPS)\n\nPublished - SANapjss07.pdf
", "abstract": "The COSMOS Spitzer survey (S-COSMOS) is a Legacy program (Cycles 2+3) designed to carry out a uniform deep survey of the full 2 deg^2 COSMOS field in all seven Spitzer bands (3.6, 4.5, 5.6, 8.0, 24.0, 70.0, and 160.0 \u03bcm). This paper describes the survey parameters, mapping strategy, data reduction procedures, achieved sensitivities to date, and the complete data set for future reference. We show that the observed infrared backgrounds in the S-COSMOS field are within 10% of the predicted background levels. The fluctuations in the background at 24 \u03bcm have been measured and do not show any significant contribution from cirrus, as expected. In addition, we report on the number of asteroid detections in the low Galactic latitude COSMOS field. We use the Cycle 2 S-COSMOS data to determine preliminary number counts, and compare our results with those from previous Spitzer Legacy surveys (e.g., SWIRE, GOODS). The results from this \"first analysis\" confirm that the S-COSMOS survey will have sufficient sensitivity with IRAC to detect ~L^* disks and spheroids out to z \u2273 3, and with MIPS to detect ultraluminous starbursts and AGNs out to z ~ 3 at 24 \u03bcm and out to z ~ 1.5-2 at 70 and 160 \u03bcm.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "86-98", "id_number": "CaltechAUTHORS:20100310-103340276", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100310-103340276", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL", "grant_number": "1278386" }, { "agency": "NASA/JPL/Caltech", "grant_number": "1407" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/517885", "primary_object": { "basename": "SANapjss07.pdf", "url": "https://authors.library.caltech.edu/records/rzhjp-de478/files/SANapjss07.pdf" }, "pub_year": "2007", "author_list": "Sanders, D. B.; Salvato, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/y0v3a-xp940", "eprint_id": 17730, "eprint_status": "archive", "datestamp": "2023-08-22 09:53:49", "lastmod": "2023-10-20 00:11:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason D." }, "orcid": "0000-0002-4485-8549" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "Richard J." }, "orcid": "0000-0002-6085-3780" }, { "id": "Albert-J", "name": { "family": "Albert", "given": "Justin" } }, { "id": "Collins-N", "name": { "family": "Collins", "given": "Nicholas" } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Heymans-C", "name": { "family": "Heymans", "given": "Catherine" } }, { "id": "Gardner-J-P", "name": { "family": "Gardner", "given": "Jonathan P." } }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "Jean-Paul" }, "orcid": "0000-0002-4616-4989" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton" }, "orcid": "0000-0002-6610-2048" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "Mellier-Y", "name": { "family": "Mellier", "given": "Yannick" } }, { "id": "Refregier-A", "name": { "family": "Refregier", "given": "Alexander" } }, { "id": "Taylor-J-E", "name": { "family": "Taylor", "given": "James E." } }, { "id": "Van-Waerbeke-L", "name": { "family": "Van Waerbeke", "given": "Ludovic" } } ] }, "title": "The Stability of the Point-Spread Function of the Advanced Camera for Surveys on the Hubble Space Telescope and Implications for Weak Gravitational Lensing", "ispublished": "pub", "full_text_status": "public", "keywords": "instrumentation: detectors; surveys; techniques: image processing", "note": "\u00a9 2007 American Astronomical Society. \n\nPrint publication: Issue 1 (2007 September); received 2006 September 21; accepted for publication 2007 January 10. \n\nWe thank Stefano Casertano and Andy Fruchter for useful discussions on the ACS PSF and how it is affected by drizzle. Our use of the Tiny Tim software would not have been possible without the help of John Krist. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We wish to thank Tony Roman, Denise Taylor, and David Soderblom for their assistance in the planning and scheduling of the extensive COSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration, consisting of more than 70 scientists, and of the COSMOS PI Nick Scoville in particular. More information on the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. It is a pleasure to acknowledge the excellent services provided by the NASA/IPAC Infrared Science Archive staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS data sets. The COSMOS Science meeting in 2005 May was supported in part by the NSF through grant OISE-0456439. We thank the anonymous referee for useful comments that improved the paper immensely. We also thank Matthew Lallo and Russell Makidon for providing focus data for the HST during the time the COSMOS observations were made. R. M. was supported in part by grant HST-AR-10964. This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA and finded through the internal Research and Technology Development program. \n\nFacilities: HST(ACS) \n\nBased on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555; also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and NASA; the European Southern Observatory, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; and the Canada-France-Hawaii Telescope, operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France, and the University of Hawaii.\n\nPublished - RHOapjss07.pdf
", "abstract": "We examine the spatial and temporal stability of the Hubble Space Telescope's Advanced Camera for Surveys (ACS) Wide Field Camera (WFC) point-spread function (PSF) using the 2 deg^2 COSMOS survey. This is important for studies of weak gravitational lensing, where the ability to deconvolve the PSF from galaxy shapes is of paramount importance. We show that stochastic aliasing of the PSF necessarily occurs during \"drizzling.\" This aliasing is maximal if the output-pixel scale is equal to the input-pixel scale. This source of PSF variation can be significantly reduced by choosing a Gaussian drizzle kernel with a size of 0.8 input pixels and by reducing the output-pixel scale. We show that the PSF is temporally unstable, resulting in an overall slow periodic focus change in the COSMOS images. Using a modified version of the Tiny Tim PSF modeling software, we create grids of undistorted stars over a range of telescope focus values. We then use the approximately 10 well-measured stars in each COSMOS field to pick the best-fit focus value for each field. The Tiny Tim model stars can then be used to perform PSF corrections for weak lensing. We derive a parametric correction for the effect of charge transfer efficiency (CTE) degradation on the shapes of objects in the COSMOS field as a function of observation date, position within the ACS WFC field, and object flux. Finally, we discuss future plans to improve the CTE correction.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "203-218", "id_number": "CaltechAUTHORS:20100312-120236909", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100312-120236909", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NSF", "grant_number": "OISE-0456439" }, { "agency": "NASA", "grant_number": "HST-AR-10964" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516592", "primary_object": { "basename": "RHOapjss07.pdf", "url": "https://authors.library.caltech.edu/records/y0v3a-xp940/files/RHOapjss07.pdf" }, "pub_year": "2007", "author_list": "Rhodes, Jason D.; Massey, Richard J.; et el." }, { "id": "https://authors.library.caltech.edu/records/qkqjk-a6239", "eprint_id": 17563, "eprint_status": "archive", "datestamp": "2023-08-22 09:53:29", "lastmod": "2023-10-20 00:00:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "J.-P." }, "orcid": "0000-0002-4616-4989" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "A" }, "orcid": "0000-0002-3677-3617" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Massey-R-J", "name": { "family": "Massey", "given": "R." }, "orcid": "0000-0002-6085-3780" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B" } }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P. L." } } ] }, "title": "The COSMOS Survey: Hubble Space Telescope Advanced Camera for Surveys Observations and Data Processing", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology : observations; dark matter; galaxies : evolution; galaxies : formation; large-scale structure of universe; surveys", "note": "\u00a9 2007 The American Astronomical Society. \n\nReceived 2006 November 30; accepted 2007 March 5. \n\nThe COSMOS HST Treasury program was supported through NASA grant HST-GO-09822. We wish to thank Tony Roman, Denise Taylor, and David Soderblom for their assistance in the planning and scheduling of the extensive COSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration, consisting of more than 70 scientists. More information on COSMOS is available at http://cosmos.astro.caltech.edu/. We acknowledge the services provided by the staff at the NASA IPAC/IRSA, as well as the STScI MAST Archive for providing online archive and server capabilities for the COSMOS data sets. The COSMOS Science meeting in 2005 May was supported in part by the NSF through grant OISE-0456439.\n\nPublished - KOEapjss07.pdf
Accepted Version - 0703095.pdf
", "abstract": "We describe the details of the Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) Wide Field Channel (WFC) observations of the COSMOS field, including the data calibration and processing procedures. We obtained a total of 583 orbits of HST ACS/WFC imaging in the F814W filter, covering a field that is 1.64 deg^2 in area, the largest contiguous field ever imaged with HST. The median exposure depth across the field is 2028 s (one HST orbit), achieving a limiting point-source depth AB(F814W) = 27.2 (5 \u03c3). We also present details of the astrometric image registration and distortion removal and image combination using MultiDrizzle, motivating the choice of our final pixel scale (30 mas pixel^(-1)), based on the requirements for weak-lensing science. The final set of images are publicly available through the archive sites at IPAC and STScI, along with further documentation on how they were produced.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "196-202", "id_number": "CaltechAUTHORS:20100223-104415226", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100223-104415226", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NSF", "grant_number": "OISE-0456439" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/520086", "primary_object": { "basename": "0703095.pdf", "url": "https://authors.library.caltech.edu/records/qkqjk-a6239/files/0703095.pdf" }, "related_objects": [ { "basename": "KOEapjss07.pdf", "url": "https://authors.library.caltech.edu/records/qkqjk-a6239/files/KOEapjss07.pdf" } ], "pub_year": "2007", "author_list": "Koekemoer, A. M.; Aussel, H.; et el." }, { "id": "https://authors.library.caltech.edu/records/k0ne6-v9e08", "eprint_id": 18047, "eprint_status": "archive", "datestamp": "2023-08-22 09:54:26", "lastmod": "2023-10-20 15:32:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Abraham-R-G", "name": { "family": "Abraham", "given": "Roberto G." }, "orcid": "0000-0002-4542-921X" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton" }, "orcid": "0000-0002-6610-2048" } ] }, "title": "The Effects of Environment on Morphological Evolution at 0 < z < 1.2 in the COSMOS Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: clusters: general; galaxies: evolution; galaxies: formation; galaxies: structure; large-scale structure of universe", "note": "\u00a9 2007 American Astronomical Society. \n\nReceived 2006 September 22; accepted 2007 March 23. \n\nBased in part on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under NASA contract NAS5-26555; the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; theMegaPrime/MegaCam, a joint project of the Canada-France-Hawaii Telescope (CFHT) and CEA/DAPNIA, at the CFHT, which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche, and the University of Hawaii; and Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which is operated by AURA under cooperative agreement with the National Science Foundation. We would like to thank Mauro Giavalisco, Jin Koda, and Mara Salvato for their excellent suggestions, feedback, and proofreading; Marc Postman and Graham Smith for providing early preprints of their papers and feedback on this work; Tomotsugu Goto and Andrew Benson for providing data from their figures; and the contributions of the COSMOS team (http://www.astro.caltech.edu/cosmos/). Support for this work was provided by NASA grant HST-GO-09822 and NSF grant OISE-0456439.\n\nPublished - CAPapjss07b.pdf
Accepted Version - 0703668.pdf
", "abstract": "We explore the evolution of the morphology-density relation using the COSMOS Advanced Camera for Surveys (ACS) and previous cluster studies. The Gini parameter measured in a Petrosian aperture is found to be an effective way of selecting early-type galaxies free from systematic effects with redshift. We find that galaxies are transformed from late- (spiral and irregular) to early-type (E+S0) galaxies more rapidly in dense than in sparse regions. At a given density, the early-type fraction grows constantly with cosmic time, but the growth rate increases with density as a power law of index 0.29 \u00b1 0.02. However, at densities below 100 galaxies Mpc^(-2), no evolution is found at z > 0.4. In contrast, the star formation-density relation shows strong evolution at all densities and redshifts, suggesting that different physical mechanisms are responsible for the morphological and star formation transformation. We show that photometric redshifts can measure local galaxy environment, but that the present results are limited by photometric redshift error to densities above \u03a3 = 3 galaxies Mpc^(-2).", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "284-294", "id_number": "CaltechAUTHORS:20100422-095203095", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100422-095203095", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NSF", "grant_number": "OISE-0456439" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/518424", "primary_object": { "basename": "0703668.pdf", "url": "https://authors.library.caltech.edu/records/k0ne6-v9e08/files/0703668.pdf" }, "related_objects": [ { "basename": "CAPapjss07b.pdf", "url": "https://authors.library.caltech.edu/records/k0ne6-v9e08/files/CAPapjss07b.pdf" } ], "pub_year": "2007", "author_list": "Capak, Peter; Abraham, Roberto G.; et el." }, { "id": "https://authors.library.caltech.edu/records/bsxbs-04t14", "eprint_id": 18024, "eprint_status": "archive", "datestamp": "2023-08-22 09:53:54", "lastmod": "2023-10-20 15:31:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Dahlen-T", "name": { "family": "Dahlen", "given": "T." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Thompson-D-J", "name": { "family": "Thompson", "given": "D. J." } }, { "id": "Feldmann-R", "name": { "family": "Feldmann", "given": "R." }, "orcid": "0000-0002-1109-1919" }, { "id": "Tasca-L-A-M", "name": { "family": "Tasca", "given": "L." } }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mould-J-R", "name": { "family": "Mould", "given": "J." }, "orcid": "0000-0003-3820-1740" }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P. L." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Ajiki-M", "name": { "family": "Ajiki", "given": "M." } }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Iovino-A", "name": { "family": "Iovino", "given": "A." } }, { "id": "Le-Brun-V", "name": { "family": "Le Brun", "given": "V." } }, { "id": "Mainieri-V", "name": { "family": "Mainieri", "given": "V." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } } ] }, "title": "Photometric Redshifts of Galaxies in COSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: distances and redshifts; galaxies: evolution; galaxies: starburst; surveys", "note": "\u00a9 2007 American Astronomical Society.\n\nReceived 2006 June 5; accepted 2006 October 6.\n\nBased on observations with the NASA/ESA Hubble Space Telescope, obtained\nat the Space Telescope Science Institute, which is operated by AURA, Inc., under\nNASA contract NAS 5-26555; also based on data collected at the Subaru Telescope,\nwhich is operated by the National Astronomical Observatory of Japan; XMM Newton,\nan ESA science mission with instruments and contributions directly funded\nby ESA Member States and NASA; the European Southern Observatory under\nLarge Program 175.A-0839, Chile; Kitt Peak National Observatory, Cerro Tololo\nInter-American Observatory, and the National Optical Astronomy Observatory,\nwhich are operated by the AURA, Inc., under cooperative agreement with the\nNational Science Foundation; the National Radio Astronomy Observatory, which\nis a facility of the National Science Foundation operated under cooperative agreement\nby Associated Universities, Inc.; and the Canada-France-Hawaii Telescope\nwith MegaPrime/MegaCam operated as a joint project by the CFHT Corporation,\nCEA/DAPNIA, the National Research Council of Canada, the Canadian Astronomy\nData Centre, the Centre National de la Recherche Scientifique de France, TERAPIX,\nand the University of Hawaii.\n\nPublished - MOBapjss07.pdf
", "abstract": "We present photometric redshifts for the COSMOS survey derived from a new code, optimized to yield accurate and reliable redshifts and spectral types of galaxies down to faint magnitudes and redshifts out to z ~ 1.2. The technique uses \u03c7^2 template fitting, combined with luminosity function priors and with the option to estimate the internal extinction [or E(B - V)]. The median most probable redshift, best-fit spectral type and reddening, absolute magnitude, and stellar mass are derived in addition to the full redshift probability distributions. Using simulations with sampling and noise similar to those in COSMOS, the accuracy and reliability is estimated for the photometric redshifts as a function of the magnitude limits of the sample, S/N ratios, and the number of bands used. We find from the simulations that the ratio of derived 95% confidence interval in the \u03c7^2 probability distribution to the estimated photometric redshift (D_(95)) can be used to identify and exclude the catastrophic failures in the photometric redshift estimates. To evaluate the reliability of the photometric redshifts, we compare the derived redshifts with high-reliability spectroscopic redshifts for a sample of 868 normal galaxies with z < 1.2 from zCOSMOS. Considering different scenarios, depending on using prior, no prior, and/or extinction, we compare the photometric and spectroscopic redshifts for this sample. The rms scatter between the estimated photometric redshifts and known spectroscopic redshifts is \u03c3(\u0394(z)) = 0.031, where \u0394(z) = (z_(phot) - z_(spec))/(1 + z_(spec)) with a small fraction of outliers (<2.5%) [outliers are defined as objects with \u0394(z) > 3\u03c3(\u0394(z)), where \u03c3(\u0394(z)) is the rms scatter in \u0394(z)]. We also find good agreement [\u03c3(\u0394(z)) = 0.10] between photometric and spectroscopic redshifts for type II AGNs. We compare results from our photometric redshift procedure with three other independent codes and find them in excellent agreement. We show preliminary results, based on photometric redshifts for the entire COSMOS sample (to i < 25 mag).", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "117-131", "id_number": "CaltechAUTHORS:20100420-110053369", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100420-110053369", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516590", "primary_object": { "basename": "MOBapjss07.pdf", "url": "https://authors.library.caltech.edu/records/bsxbs-04t14/files/MOBapjss07.pdf" }, "pub_year": "2007", "author_list": "Mobasher, B.; Capak, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/e0beg-5qb30", "eprint_id": 16754, "eprint_status": "archive", "datestamp": "2023-08-22 09:24:06", "lastmod": "2023-10-19 22:32:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Meurer-G-R", "name": { "family": "Meurer", "given": "Gerhardt R." }, "orcid": "0000-0002-0163-2507" }, { "id": "Tsvetanov-Z-I", "name": { "family": "Tsvetanov", "given": "Z. I." } }, { "id": "Gronwall-C", "name": { "family": "Gronwall", "given": "C." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Blakeslee-J-P", "name": { "family": "Blakeslee", "given": "J. P." } }, { "id": "Ben\u00edtez-N", "name": { "family": "Ben\u00edtez", "given": "N." } }, { "id": "Ford-H-C", "name": { "family": "Ford", "given": "H. C." } }, { "id": "Illingworth-G-D", "name": { "family": "Illingworth", "given": "G. D." }, "orcid": "0000-0002-8096-2837" }, { "id": "Bradley-L-D", "name": { "family": "Bradley", "given": "L. D." } }, { "id": "Pirzkal-Nor", "name": { "family": "Pirzkal", "given": "N." }, "orcid": "0000-0003-3382-5941" }, { "id": "Walsh-J", "name": { "family": "Walsh", "given": "J." } }, { "id": "Bouwens-R-J", "name": { "family": "Bouwens", "given": "R. J." }, "orcid": "0000-0002-4989-2471" }, { "id": "Srinivasan-S", "name": { "family": "Srinivasan", "given": "S." } } ] }, "title": "Automated Selection and Characterization of Emission-Line Sources in Advanced Camera for Surveys Wide Field Camera Grism Data", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : distances and redshifts; galaxies : high-redshift; methods : data analysis; surveys; techniques : spectroscopic", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 May 30; accepted 2007 March 9.\nACS was developed under NASA contract NAS 5-32865, and\nthis research has been supported by NASA grant NAG5-7697 and\nby an equipment grant from Sun Microsystems, Inc. The Space\nTelescope Science Institute is operated by Association of Universities\nfor Research in Astronomy (AURA), Inc., under NASA\ncontract NAS5-26555.We are grateful to K. Anderson, J. McCann,\nS. Busching, A. Framarini, S. Barkhouser, and T. Allen for their\ninvaluable contributions to the ACS project at Johns Hopkins University.\nG. R. M. acknowledges useful conversations with Anna\nPasquali, Marco Sirianni, James Rhoads, Sangeeta Malhotra, Chun\nXu, and S\u00f8ren Larsen. We thank the anonymous referee for suggestions\nthat improved the science and readability of this paper.\n\nPublished - MEUaj07.pdf
", "abstract": "We present complementary techniques to find emission-line targets and measure their properties in a semi-automated fashion from grism observations obtained with the Advanced Camera for Surveys aboard the Hubble Space Telescope (HST). The first technique is to find all likely sources in a direct image, extract their spectra, and search them for emission lines. The second method is to look for emission-line sources as compact structures in an unsharp masked version of the grism image. Using these methods we identify 46 emission-line targets in the Hubble Deep Field-North using a modest (three-orbit) expenditure of HST observing time. Grism spectroscopy is a powerful tool for efficiently identifying interesting low-luminosity, moderate-redshift emission-line field galaxies. The sources found here have a median i-band (F775W) flux 1.5 mag fainter than the spectroscopic redshift catalog of Cohen et al. They have redshift z \u2264 1.42, and high equivalent widths (typically >100 \u00c5) and are usually less luminous than the characteristic luminosity at the same redshift. The chief obstacle in interpreting the results is line identification, since the majority of sources have a single emission line and the spectral resolution is low. Photometric redshifts are useful for providing a first-guess redshift. However, even at the depth of the state-of-the-art ground-based and HST data used here, photometric errors can result in uncertainties in line identifications, especially for sources with i magnitudes fainter than 24.5 ABmag. Reliable line identification for the faintest emission-line galaxies requires additional ground-based spectroscopy for confirmation. Of particular concern are the faint high-EW [O II] emitters, which could represent a strongly evolving galaxy population if the possibility that they are misidentified lower redshift interlopers can be ruled out.", "date": "2007-07", "date_type": "published", "publication": "Astronomical Journal", "volume": "134", "number": "1", "publisher": "American Astronomical Society", "pagerange": "77-95", "id_number": "CaltechAUTHORS:20091118-152456295", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091118-152456295", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-32865" }, { "agency": "NASA", "grant_number": "NAG5-7697" }, { "agency": "Sun Microsystems, Inc" }, { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/518228", "primary_object": { "basename": "MEUaj07.pdf", "url": "https://authors.library.caltech.edu/records/e0beg-5qb30/files/MEUaj07.pdf" }, "pub_year": "2007", "author_list": "Meurer, Gerhardt R.; Tsvetanov, Z. I.; et el." }, { "id": "https://authors.library.caltech.edu/records/ayqqy-dr212", "eprint_id": 55867, "eprint_status": "archive", "datestamp": "2023-08-19 20:13:39", "lastmod": "2023-10-20 23:19:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Rau-A", "name": { "family": "Rau", "given": "A." }, "orcid": "0000-0001-5990-6243" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Soderberg-A-M", "name": { "family": "Soderberg", "given": "A. M." } }, { "id": "Fox-D-B", "name": { "family": "Fox", "given": "D. B." }, "orcid": "0000-0002-3714-672X" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Moon-Dae-Sik", "name": { "family": "Moon", "given": "D.-S." }, "orcid": "0000-0003-4200-5064" }, { "id": "Li-Weidong", "name": { "family": "Li", "given": "W." } }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Egami-Eichi", "name": { "family": "Egami", "given": "E." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" } ] }, "title": "An unusually brilliant transient in the galaxy M85", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2007 Macmillan Publishers Limited. \n\nReceived 2 June 2006; accepted 30 March 2007. \n\nWe thank D. Frail for discussion and constructive criticism. We also thank the astronomers who maintain the NED database at IPAC and the data archives of the Hubble Space Telescope, the Spitzer Space Telescope and the Chandra X-ray Telescope. Our work has been funded in part by NASA, NSF, the Sylvia and Jim Katz Foundation and the TABASGO Foundation.\n\nAccepted Version - 0705.3668.pdf
Supplemental Material - nature05822-s1.pdf
", "abstract": "Historically, variable and transient sources have both surprised astronomers and provided new views of the heavens. Here we report the discovery of an optical transient in the outskirts of the lenticular galaxy Messier 85 in the Virgo cluster. With a peak absolute R magnitude of -12, this event is distinctly brighter than novae, but fainter than type\u2009Ia supernovae (which are expected in a population of old stars in lenticular galaxies). Archival images of the field do not show a luminous star at that position with an upper limit in the g filter of about -4.1\u2009mag, so it is unlikely to be a giant eruption from a luminous blue variable star. Over a two-month period, the transient source emitted radiation energy of almost 10^47\u2009erg and subsequently faded in the optical sky. It is similar to, but six times more luminous at peak than, an enigmatic transient in the galaxy M31 (ref. 1). A possible origin of M85\u2009OT2006-1 is a stellar merger. If so, searches for similar events in nearby galaxies will not only allow study of the physics of hyper-Eddington sources, but also probe an important phase in the evolution of stellar binary systems.", "date": "2007-05-24", "date_type": "published", "publication": "Nature", "volume": "447", "number": "7143", "publisher": "Nature Publishing Group", "pagerange": "458-460", "id_number": "CaltechAUTHORS:20150317-154247587", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150317-154247587", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "NSF" }, { "agency": "Sylvia and Jim Katz Foundation" }, { "agency": "TABASGO Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1038/nature05822", "primary_object": { "basename": "0705.3668.pdf", "url": "https://authors.library.caltech.edu/records/ayqqy-dr212/files/0705.3668.pdf" }, "related_objects": [ { "basename": "nature05822-s1.pdf", "url": "https://authors.library.caltech.edu/records/ayqqy-dr212/files/nature05822-s1.pdf" } ], "pub_year": "2007", "author_list": "Kulkarni, S. R.; Ofek, E. O.; et el." }, { "id": "https://authors.library.caltech.edu/records/ktyxj-nwk06", "eprint_id": 55878, "eprint_status": "archive", "datestamp": "2023-08-19 19:33:14", "lastmod": "2023-10-20 23:21:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Massey-R-J", "name": { "family": "Massey", "given": "Richard" }, "orcid": "0000-0002-6085-3780" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick" }, "orcid": "0000-0002-0438-3323" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "Finoguenov-A", "name": { "family": "Finoguenov", "given": "Alexis" }, "orcid": "0000-0002-4606-5403" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Bacon-D-J", "name": { "family": "Bacon", "given": "David J." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "Herve" }, "orcid": "0000-0002-1371-5705" }, { "id": "Kneib-J-P", "name": { "family": "Kneib", "given": "Jean-Paul" }, "orcid": "0000-0002-4616-4989" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "Henry" }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Pires-S", "name": { "family": "Pires", "given": "Sandrine" } }, { "id": "Refregier-A", "name": { "family": "Refregier", "given": "Alexandre" } }, { "id": "Sasaki-Shunji", "name": { "family": "Sasaki", "given": "Shunji" } }, { "id": "Starck-J-L", "name": { "family": "Starck", "given": "Jean-Luc" } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Yoshi" }, "orcid": "0000-0003-2247-3741" }, { "id": "Taylor-A", "name": { "family": "Taylor", "given": "Andy" } }, { "id": "Taylor-J-E", "name": { "family": "Taylor", "given": "James" } } ] }, "title": "Dark matter maps reveal cosmic scaffolding", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2007 Macmillan Publishers Limited.\n\nReceived 14 November; accepted 30 November 2006; published online 7 January 2007.\n\nThis work was based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA). We also used data collected from: the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and NASA; the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the European Southern Observatory, Chile;\nthe Kitt Peak National Observatory, the Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by AURA under cooperative agreement with the American National Science Foundation; the National Radio Astronomy Observatory, which is a facility of the American National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; and the Canada-France-Hawaii Telescope operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France and the University of Hawaii. The photometric redshifts used here were validated using spectra from the European Southern Observatory Very Large Telescope zCOSMOS survey. We gratefully acknowledge the contributions of the entire COSMOS collaboration, consisting of more than 70 scientists. We thank T. Roman, D. Taylor and D. Soderblom for help scheduling the extensive COSMOS observations; and A. Laity, A. Alexov, B. Berriman and J. Good for managing online archives and servers for the COSMOS data sets at NASA IPAC/IRSA. This work was supported by grants from NASA (to N.S. and R.M.). \nA.K. processed the raw HST data, and J.-P.K. masked defects in the image. A.L., J.R. and R.M. catalogued the positions and shapes o galaxies. Y.T. and S.S. obtained multicolour follow-up data, which was processed and calibrated by S.S., P.C., H.McC. and H.A. P.C. determined galaxies' redshifts, and B.M. their stellar mass. N.S. constructed maps of stellar mass and galaxy density. A.F. processed the X-ray image and removed point sources. R.M. and A.R. produced the two-dimensional and tomographic mass maps; J.-L.S. and S.P. developed the wavelet filtering technique. D.B. and A.T. produced the three-dimensional mass reconstruction. J.T., A.F., R.E. and R.M. compared the various tracers of large-scale structure.\n\nSubmitted - 0701594.pdf
Supplemental Material - nature05497-s1.pdf
", "abstract": "Ordinary baryonic particles (such as protons and neutrons) account for only one-sixth of the total matter in the Universe. The remainder is a mysterious 'dark matter' component, which does not interact via electromagnetism and thus neither emits nor reflects light. As dark matter cannot be seen directly using traditional observations, very little is currently known about its properties. It does interact via gravity, and is most effectively probed through gravitational lensing: the deflection of light from distant galaxies by the gravitational attraction of foreground mass concentrations. This is a purely geometrical effect that is free of astrophysical assumptions and sensitive to all matter\u2014whether baryonic or dark. Here we show high-fidelity maps of the large-scale distribution of dark matter, resolved in both angle and depth. We find a loose network of filaments, growing over time, which intersect in massive structures at the locations of clusters of galaxies. Our results are consistent with predictions of gravitationally induced structure formation, in which the initial, smooth distribution of dark matter collapses into filaments then into clusters, forming a gravitational scaffold into which gas can accumulate, and stars can be built.", "date": "2007-01-18", "date_type": "published", "publication": "Nature", "volume": "445", "number": "7125", "publisher": "Nature Publishing Group", "pagerange": "286-290", "id_number": "CaltechAUTHORS:20150318-085101988", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150318-085101988", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "ESA member states" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1038/nature05497", "primary_object": { "basename": "0701594.pdf", "url": "https://authors.library.caltech.edu/records/ktyxj-nwk06/files/0701594.pdf" }, "related_objects": [ { "basename": "nature05497-s1.pdf", "url": "https://authors.library.caltech.edu/records/ktyxj-nwk06/files/nature05497-s1.pdf" } ], "pub_year": "2007", "author_list": "Massey, Richard; Rhodes, Jason; et el." }, { "id": "https://authors.library.caltech.edu/records/3y7gx-43p67", "eprint_id": 13756, "eprint_status": "archive", "datestamp": "2023-08-22 07:02:10", "lastmod": "2023-10-18 00:07:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Feldmann-R", "name": { "family": "Feldmann", "given": "R." }, "orcid": "0000-0002-1109-1919" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Porciani-C", "name": { "family": "Porciani", "given": "C." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Ajiki-M", "name": { "family": "Ajiki", "given": "M." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Contini-T", "name": { "family": "Contini", "given": "T." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Murayama-Takashi", "name": { "family": "Murayama", "given": "T." } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D." }, "orcid": "0000-0002-1233-9998" }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S." } }, { "id": "Scarlata-C-M", "name": { "family": "Scarlata", "given": "C." }, "orcid": "0000-0002-9136-8876" }, { "id": "Scodeggio-M", "name": { "family": "Scodeggio", "given": "M." } }, { "id": "Shioya-Yasuhiro", "name": { "family": "Shioya", "given": "Y." } }, { "id": "Silverman-J-D", "name": { "family": "Silverman", "given": "J." }, "orcid": "0000-0002-0000-6977" }, { "id": "Takahashi-M", "name": { "family": "Takahashi", "given": "M." } }, { "id": "Thompson-D-J", "name": { "family": "Thompson", "given": "D." } }, { "id": "Zamorani-G", "name": { "family": "Zamorani", "given": "G." } } ] }, "title": "The Zurich Extragalactic Bayesian Redshift Analyzer and its first application: COSMOS", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: statistical; galaxies: distances and redshifts; galaxies: evolution; galaxies: formation; galaxies: photometry", "note": "\u00a9 2006 The Authors. Journal compilation \u00a9 2006 RAS. \n\nAccepted 2006 August 2. Received 2006 July 1; in original form 2006 May 8.\n\nWe thank the anonymous referee for the helpful comments, which\nhave improved the presentation of this paper, and Manfred Kitzbichler\nfor making available to the COSMOS collaboration the mock\ncatalogue used in this work.\nThis work is based on observations taken with the following.\n(i) The NASA/ESA Hubble Space Telescope, obtained at the\nSpace Telescope Science Institute, which is operated by AURA,\nInc., under NASA contract NAS 5-26555.\n(ii) The Subaru Telescope, which is operated by the National\nAstronomical Observatory of Japan.\n(iii) Facilities at the European Southern Observatory, Chile.\n(iv) Facilities at the Cerro Tololo Inter-American Observatory\nand at the National Optical Astronomy Observatory, which are operated\nby the Association of Universities for Research in Astronomy,\nInc. (AURA) under cooperative agreement with the National Science\nFoundation.\n(v) The CFHT operated by the National Research Council of\nCanada, the Centre National de la Recherche Scientifique de France\nand the University of Hawaii.\nT. Lisker is acknowledged for helping with a preliminary reduction\nof a fraction of the ground-based near-IR data.\n\nPublished - FELmnras06.pdf
", "abstract": "We present the Zurich Extragalactic Bayesian Redshift Analyzer (ZEBRA). The current version of ZEBRA combines and extends several of the classical approaches to produce accurate photometric redshifts down to faint magnitudes. In particular, ZEBRA uses the template-fitting approach to produce Maximum Likelihood and Bayesian redshift estimates based on the following points.\n\n(i) An automatic iterative technique to correct the original set of galaxy templates to best represent the Spectral Energy Distributions (SEDs) of real galaxies at different redshifts.\n\n(ii) A training set of spectroscopic redshifts for a small fraction of the photometric sample to improve the robustness of the photometric redshift estimates.\n\n(iii) An iterative technique for Bayesian redshift estimates, which extracts the full two-dimensional redshift and template probability function for each galaxy.\n\nWe demonstrate the performance of ZEBRA by applying it to a sample of 866 I_AB \u2a7d 22.5 COSMOS galaxies with available u*, B, V, g', r', i', z' and K_s photometry and zCOSMOS spectroscopic redshifts in the range 0 < z < 1.3 . Adopting a 5\u03c3 clipping that excludes \u2a7d10 galaxies, both the Maximum Likelihood and Bayesian ZEBRA estimates for this sample have an accuracy \u03c3_(\u0394z/(1+z)) smaller than 0.03. Similar accuracies are recovered using mock galaxies.", "date": "2006-10-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "372", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "565-577", "id_number": "CaltechAUTHORS:FELmnras06", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:FELmnras06", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2006.10930.x", "primary_object": { "basename": "FELmnras06.pdf", "url": "https://authors.library.caltech.edu/records/3y7gx-43p67/files/FELmnras06.pdf" }, "pub_year": "2006", "author_list": "Feldmann, R.; Carollo, C. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/baf0f-cmy06", "eprint_id": 86298, "eprint_status": "archive", "datestamp": "2023-08-22 00:53:13", "lastmod": "2023-10-18 19:27:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Coker-R-F", "name": { "family": "Coker", "given": "Robert F." } }, { "id": "Christopher-M-H", "name": { "family": "Christopher", "given": "Michol H." } }, { "id": "Stolovy-S-R", "name": { "family": "Stolovy", "given": "Susan R." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Simple hydrodynamical Simulations of the Circumnuclear Disk", "ispublished": "pub", "full_text_status": "public", "keywords": "GMC; simulation; Sgr A", "note": "\u00a9 2003 Wiley\u2010VCH Verlag GmbH & Co. KGaA, Weinheim. \n\nIssue Online: 20 October 2003; Version of Record online: 20 October 2003. \n\nThis work was supported in part by UK PPARC and DOE. Some of the calculations reported here were carried out using UKAFF, a high-performance computing facility funded by UK PPARC.\n\nPublished - Coker_et_al-2003-Astronomische_Nachrichten.pdf
", "abstract": "The \"circumnuclear disk\" (CND) is a dense, clumpy, asymmetric ring\u2010like feature centered on Sgr A*. The outer edge of the CND is not distinct but the disk extends for more than 7 pc; the distinct inner edge, at a radius of \u22431.5 pc, surrounds the \"mini\u2010spiral\" of the HII region, Sgr A West. We present simple 3D hydrodynamical models of the formation and evolution of the CND from multiple selfgravitating infalling clouds and compare the results with recent observations. We assume the clouds are initially Bonner\u2010Ebert spheres, in equilibrium with a hot confining inter\u2010cloud medium. We include the gravitational potential due to the point\u2010mass of Sgr A* as well as the extended mass distribution of the underlying stellar population. We also include the effects of the ram pressure due to the stellar winds from the central cluster of early\u2010type stars.\n\nA single spherically symmetric cloud cannot reproduce the clumpy morphology of the CND; multiple clouds on diverse trajectories are required so that cloud\u2010cloud collisions can circularize the clouds' orbits while maintaining a clumpy morphology. Collisions also serve to compress the clouds, delaying tidal disruption while potentially hastening gravitational collapse. Low density clumps are disrupted before reaching the inner CND radius, forming short\u2010lived arcs. The outer parts of more massive clumps get tidally stripped, forming long\u2010lived low\u2010density wide\u2010angle arcs, while their cores potentially undergo gravitational collapse. The fine balance between resisting tidal disruption and preventing gravitational collapse implies that most if not all clumps are not stable for much more than an orbit. Thus, in order for the CND to be a long\u2010lived clumpy object, it must be continually fed by additional in\u2010falling clouds. Clouds that survive to small radii are likely to be the sites of present or future star formation. However, within a few parsecs of Sgr A*, the stellar winds decelerate any in\u2010falling cloud so that the wind\u2010cloud interface becomes Rayleigh\u2010Taylor unstable, potentially disrupting the cloud and inhibiting star formation.", "date": "2003-09", "date_type": "published", "publication": "Astronomische Nachrichten", "volume": "324", "number": "S1", "publisher": "Wiley", "pagerange": "629-634", "id_number": "CaltechAUTHORS:20180508-155748418", "issn": "0004-6337", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180508-155748418", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1002/asna.200385057", "primary_object": { "basename": "Coker_et_al-2003-Astronomische_Nachrichten.pdf", "url": "https://authors.library.caltech.edu/records/baf0f-cmy06/files/Coker_et_al-2003-Astronomische_Nachrichten.pdf" }, "pub_year": "2003", "author_list": "Coker, Robert F.; Christopher, Michol H.; et el." }, { "id": "https://authors.library.caltech.edu/records/82jsp-0pr87", "eprint_id": 74574, "eprint_status": "archive", "datestamp": "2023-08-21 21:00:52", "lastmod": "2023-10-24 22:46:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Becklin-E-E", "name": { "family": "Becklin", "given": "E. E." } }, { "id": "Evans-A-S", "name": { "family": "Evans", "given": "A. S." }, "orcid": "0000-0003-2638-1334" }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "G." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Matthews-K", "name": { "family": "Matthews", "given": "K." } }, { "id": "Ressler-M-E", "name": { "family": "Ressler", "given": "M. E." } } ] }, "title": "High-Resolution Infrared Imaging of the Compact Nuclear Source in NGC 4258", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; galaxies: individual (NGC 4258); galaxies: nuclei; infrared: general; radiation mechanisms: non-thermal", "note": "\u00a9 2000 American Astronomical Society. \n\nReceived 1999 May 5; accepted 1999 October 26. \n\nThis work is based on observations made at the W. M. Keck Observatory, the Palomar Observatory, and with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. We wish to acknowledge the contributions made by members of the NICMOS Instrument Definition Team to this project. We are grateful to Steve Willner for his help with clarifying the discussion in the Appendix. We would also like to thank the staffs of the respective observatories for their assistance. The W. M. Keck Observatory is a scientific partnership between the University of California and the California Institute of Technology.\n\nPublished - Chary_2000_ApJ_531_756.pdf
Submitted - 9910557.pdf
", "abstract": "We present high-resolution imaging of the nucleus of NGC 4258 from 1 to 18 \u03bcm. Our observations reveal that the previously discovered compact source of emission is unresolved even at the near-infrared resolution of ~0.\"2 FWHM, which corresponds to about 7 pc at the distance of the galaxy. This is consistent with the source of emission being the region in the neighborhood of the purported 3.5 \u00d7 10^7 M\u2609 black hole. After correcting for about 18 mag of visual extinction, the infrared data are consistent with an F_\u03bd \u221d \u03bd^(-1.4\u00b10.1) spectrum from 1.1 to 18 \u03bcm, implying a nonthermal origin. Based on this spectrum, the total extinction-corrected infrared luminosity (1-20 \u03bcm) of the central source is 2 \u00d7 10^8 L\u2609. We argue that the infrared spectrum and luminosity of the central source obviates the need for a substantial contribution from a standard, thin accretion disk at these wavelengths and calculate the accretion rate through an advection-dominated accretion flow to be M ~ 10^(-3) M\u2609 yr^(-1). The agreement between these observations and the theoretical spectral energy distribution for advection-dominated flows provides evidence for the existence of an advection-dominated flow in this low-luminosity active galactic nucleus.", "date": "2000-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "531", "number": "2", "publisher": "American Astronomical Society", "pagerange": "756-763", "id_number": "CaltechAUTHORS:20170228-075334335", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170228-075334335", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1086/308486", "primary_object": { "basename": "9910557.pdf", "url": "https://authors.library.caltech.edu/records/82jsp-0pr87/files/9910557.pdf" }, "related_objects": [ { "basename": "Chary_2000_ApJ_531_756.pdf", "url": "https://authors.library.caltech.edu/records/82jsp-0pr87/files/Chary_2000_ApJ_531_756.pdf" } ], "pub_year": "2000", "author_list": "Chary, R.; Becklin, E. E.; et el." }, { "id": "https://authors.library.caltech.edu/records/y75ns-1kt12", "eprint_id": 74642, "eprint_status": "archive", "datestamp": "2023-08-19 20:24:35", "lastmod": "2023-10-24 22:49:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Elias-J-H", "name": { "family": "Elias", "given": "J. H." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "B. F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Matthews-K", "name": { "family": "Matthews", "given": "K." } }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "G." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Ultraluminous infrared galaxies and the origin of quasars", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution - galaxies: photometry - infrared: sources - quasars", "note": "\u00a9 1998 American Astronomical Society.\n\nReceived 1987 May 7; accepted 1987 July 1.\n\nWe thank G. E. Danielson, Carol J. Lonsdale, and S. E.\nPersson for help in reducing the data, and M. Schmidt and J.\nPringle for useful discussions. We also thank J. Carasco, S.\nStaples, and J. Wright for assistance at the Palomar 5 m and\n1.5 m telescopes. Ground-based infrared astronomy at Caltech\nis supported by a grant from the NSF. J. H. E., G. X. N., D. B. S., and B. T. S. were also supported by NASA through the IRAS extended mission program. B. F. M. was supported by a Killam Fellowship from the Canada Council and a grant from the Natural Sciences and Engineering Research Council of Canada. N. Z. S. was supported by NSF grant AST84-12473.\nThe Palomar 1.5 m telescope is operated jointly by the California Institute of Technology and the Carnegie Institution of Washington.\n\nPublished - 1988ApJ___325___74S.pdf
", "abstract": "An evolutionary connection between ultraluminous infrared galaxies and quasars is deduced from the observations\nof all 10 infrared galaxies with luminosities L(8-1000 \u03bcm) \u2265 10^(12) L\u2299, taken from a flux-limited sample of infrared bright galaxies. Images of the infrared galaxies show that nearly all are strongly interacting merger systems with exceptionally luminous nuclei. Millimeter-wave CO observations show that these objects typically contain 0.5-2 x 10^(10) M\u2299 of H_2. Optical spectra indicate a mixture of starburst and active galactic nucleus (AGN) energy sources, both of which are apparently fueled by the tremendous reservoir of molecular gas. It is proposed that these ultraluminous infrared galaxies represent the initial, dust-enshrouded stages of quasars. Once these nuclei shed their obscuring dust, allowing the AGN to visually dominate the decaying starburst, they become optically selected quasars. The origin of quasars through the merger of molecular gas-rich spiral galaxies can account for both the increased number of high-luminosity quasars at large redshift, when the universe was smaller and gas supplies less depleted, and the observed \"redshift-cutoff\" of quasars which represents the epoch after galaxy formation when the first collisions occur.", "date": "1988-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "325", "number": "1", "publisher": "American Astronomical Society", "pagerange": "74-91", "id_number": "CaltechAUTHORS:20170301-103148522", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170301-103148522", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "Canada Council" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "NSF", "grant_number": "AST84-12473" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1086/165983", "primary_object": { "basename": "1988ApJ___325___74S.pdf", "url": "https://authors.library.caltech.edu/records/y75ns-1kt12/files/1988ApJ___325___74S.pdf" }, "pub_year": "1988", "author_list": "Sanders, D. B.; Soifer, B. T.; et el." } ]