[ { "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\n
Submitted - 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/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/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/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/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/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/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/qp0dq-ss803", "eprint_id": 78576, "eprint_status": "archive", "datestamp": "2023-08-19 01:36:45", "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.", "local_group": { "items": [ { "id": "SPLASH" }, { "id": "COSMOS" }, { "id": "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/56s6g-t6443", "eprint_id": 75025, "eprint_status": "archive", "datestamp": "2023-08-19 00:51:42", "lastmod": "2023-10-25 14:40:40", "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" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "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 00:51:29", "lastmod": "2023-10-25 14:40:34", "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" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "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/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.", "local_group": { "items": [ { "id": "SPLASH" }, { "id": "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 00:31:41", "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.", "local_group": { "items": [ { "id": "COSMOS" }, { "id": "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/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/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/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/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/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/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/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/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/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/a0g5q-2n888", "eprint_id": 53077, "eprint_status": "archive", "datestamp": "2023-08-22 14:25:51", "lastmod": "2023-10-19 14:31:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gilbert-K-M", "name": { "family": "Gilbert", "given": "Karoline M." }, "orcid": "0000-0003-0394-8377" }, { "id": "Kalirai-J-S", "name": { "family": "Kalirai", "given": "Jason S." }, "orcid": "0000-0001-9690-4159" }, { "id": "Guhathakurta-P", "name": { "family": "Guhathakurta", "given": "Puragra" }, "orcid": "0000-0001-8867-4234" }, { "id": "Beaton-R-L", "name": { "family": "Beaton", "given": "Rachael L." }, "orcid": "0000-0002-1691-8217" }, { "id": "Geha-M-C", "name": { "family": "Geha", "given": "Marla C." }, "orcid": "0000-0002-7007-9725" }, { "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "orcid": "0000-0001-6196-5162" }, { "id": "Majewski-S-R", "name": { "family": "Majewski", "given": "Steven R." }, "orcid": "0000-0003-2025-3147" }, { "id": "Patterson-R-J", "name": { "family": "Patterson", "given": "Richard J." } }, { "id": "Tollerud-E-J", "name": { "family": "Tollerud", "given": "Erik J." }, "orcid": "0000-0002-9599-310X" }, { "id": "Bullock-J-S", "name": { "family": "Bullock", "given": "James S." }, "orcid": "0000-0003-4298-5082" }, { "id": "Tanaka-Mikito", "name": { "family": "Tanaka", "given": "Mikito" } }, { "id": "Chiba-Masashi", "name": { "family": "Chiba", "given": "Masashi" }, "orcid": "0000-0002-9053-860X" } ] }, "title": "Global Properties of M31's Stellar Halo from the SPLASH Survey. II. Metallicity Profile", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: groups: individual (M31); galaxies: halos; stars: kinematics and dynamics; techniques: spectroscopic", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2014 April 30; accepted 2014 September 7; published 2014 November 10. \n\nSupport for this work was provided by NASA through Hubble\nFellowship grants 51273.01, and 51316.01 awarded to K.M.G.\nand E.J.T. 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. P.G., J.S.B., S.R.M., and R.L.B. acknowledge support from collaborative NSF grants AST-1010039, AST-1009973, AST-1009882, and AST-0607726. This project was also supported by NSF grants AST03-07842, AST03-07851, AST06-07726, AST08-07945, and AST10-09882, NASA grant ST-GO-12105.03 through STScI, NASA/JPL contract 1228235, the David and Lucile Packard Foundation, and the F. H. Levinson Fund of the Peninsula Community Foundation (S.R.M., R.J.P., and R.L.B.). E.N.K acknowledges support from the Southern California Center for Galaxy Evolution, a multicampus research program funded by the University of California Office of Research, and partial support from NSF grant AST-1009973. E.J.T. acknowledges support from a Graduate Assistance in Areas of National Need (GAANN) fellowship. R.L.B. acknowledges receipt of the Mark C. Pirrung Family Graduate Fellowship from the Jefferson Scholars Foundation and a Fellowship Enhancement for Outstanding Doctoral Candidates from the Office of the Vice President of Research at the University of Virginia. M.T. acknowledges support from Grant-in-Aid for Scientific Research (25800098) 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. The 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.\n\nPublished - 0004-637X_796_2_76.pdf
Accepted Version - 1409.3843.pdf
", "abstract": "We present the metallicity distribution of red giant branch (RGB) stars in M31's stellar halo, derived from photometric metallicity estimates for over 1500 spectroscopically confirmed RGB halo stars. The stellar sample comes from 38 halo fields observed with the Keck/DEIMOS spectrograph, ranging from 9 to 175 kpc in projected distance from M31's center, and includes 52 confirmed M31 halo stars beyond 100 kpc. While a wide range of metallicities is seen throughout the halo, the metal-rich peak of the metallicity distribution function becomes significantly less prominent with increasing radius. The metallicity profile of M31's stellar halo shows a continuous gradient from 9 to ~100 kpc, with a magnitude of ~ \u2013 0.01 dex kpc\u20131. The stellar velocity distributions in each field are used to identify stars that are likely associated with tidal debris features. The removal of tidal debris features does not significantly alter the metallicity gradient in M31's halo: a gradient is maintained in fields spanning 10-90 kpc. We analyze the halo metallicity profile, as well as the relative metallicities of stars associated with tidal debris features and the underlying halo population, in the context of current simulations of stellar halo formation. We argue that the large-scale gradient in M31's halo implies M31 accreted at least one relatively massive progenitor in the past, while the field to field variation seen in the metallicity profile indicates that multiple smaller progenitors are likely to have contributed substantially to M31's outer halo.", "date": "2014-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "796", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 76", "id_number": "CaltechAUTHORS:20141222-094115048", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141222-094115048", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "51273.01" }, { "agency": "NASA", "grant_number": "51316.01" }, { "agency": "Space Telescope Science Institute" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF", "grant_number": "AST-1010039" }, { "agency": "NSF", "grant_number": "AST-1009973" }, { "agency": "NSF", "grant_number": "AST-1009882" }, { "agency": "NSF", "grant_number": "AST-0607726" }, { "agency": "NSF", "grant_number": "AST03-07842" }, { "agency": "NSF", "grant_number": "AST03-07851" }, { "agency": "NSF", "grant_number": "AST06-07726" }, { "agency": "NSF", "grant_number": "AST08-07945" }, { "agency": "NSF", "grant_number": "AST10-09882" }, { "agency": "NASA", "grant_number": "ST-GO-12105.03" }, { "agency": "NASA/JPL", "grant_number": "1228235" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "F. H. Levinson Fund of the Peninsula Community Foundation" }, { "agency": "Southern California Center for Galaxy Evolution" }, { "agency": "University of California" }, { "agency": "NSF", "grant_number": "AST-1009973" }, { "agency": "Graduate Assistance in Areas of National Need (GAANN) fellowship" }, { "agency": "Jefferson Scholars Foundation" }, { "agency": "University of Virginia" }, { "agency": "Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan", "grant_number": "25800098" }, { "agency": "NSF", "grant_number": "AST-0071048" } ] }, "local_group": { "items": [ { "id": "SPLASH" } ] }, "doi": "10.1088/0004-637X/796/2/76", "primary_object": { "basename": "0004-637X_796_2_76.pdf", "url": "https://authors.library.caltech.edu/records/a0g5q-2n888/files/0004-637X_796_2_76.pdf" }, "related_objects": [ { "basename": "1409.3843.pdf", "url": "https://authors.library.caltech.edu/records/a0g5q-2n888/files/1409.3843.pdf" } ], "pub_year": "2014", "author_list": "Gilbert, Karoline M.; Kalirai, Jason S.; 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/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/ez0cb-hs087", "eprint_id": 17767, "eprint_status": "archive", "datestamp": "2023-08-21 23:34:32", "lastmod": "2023-10-20 00:13:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kalirai-J-S", "name": { "family": "Kalirai", "given": "Jason S." }, "orcid": "0000-0001-9690-4159" }, { "id": "Beaton-R-L", "name": { "family": "Beaton", "given": "Rachael L." }, "orcid": "0000-0002-1691-8217" }, { "id": "Geha-M-C", "name": { "family": "Geha", "given": "Marla C." }, "orcid": "0000-0002-7007-9725" }, { "id": "Gilbert-K-M", "name": { "family": "Gilbert", "given": "Karoline M." }, "orcid": "0000-0003-0394-8377" }, { "id": "Guhathakurta-P", "name": { "family": "Guhathakurta", "given": "Puragra" }, "orcid": "0000-0001-8867-4234" }, { "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "orcid": "0000-0001-6196-5162" }, { "id": "Majewski-S-R", "name": { "family": "Majewski", "given": "Steven R." }, "orcid": "0000-0003-2025-3147" }, { "id": "Ostheimer-J-C", "name": { "family": "Ostheimer", "given": "James C." } }, { "id": "Patterson-R-J", "name": { "family": "Patterson", "given": "Richard J." } }, { "id": "Wolf-J", "name": { "family": "Wolf", "given": "Joe" } } ] }, "title": "The SPLASH Survey: Internal Kinematics, Chemical Abundances, and Masses of the Andromeda I, II, III, VII, X, and XIV Dwarf Spheroidal Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "dark matter; galaxies: abundances; galaxies: dwarf; galaxies: individual (And I, And I, And I, And I, And I, And II, And II, And II, And II, And II, And III, And III, And III, And III, And III, And VII, And VII, And VII, And VII, And VII, And X, And X, And X, And X, And X, And XIV, And XIV, And XIV, And XIV, And XIV); techniques: photometric; techniques: spectroscopic", "note": "\u00a9 2010 The American Astronomical Society. \n\nIssue 2 (2010 March 10); received 2009 November 11, accepted for publication 2010 January 21; published 2010 February 17. \n\nWe thank Eva Grebel, Steve Vogt, and Dan Zucker for their valuable contribution to the And VII and X observations. J.S.K.'s research is supported in part by a grant from the STScI Director's Discretionary Research Fund, and was supported by NASA through Hubble Fellowship grant HF-01185.01-A, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This project was also supported by NSF grants AST-0307966, AST-0507483, AST-0607852, and AST-0808133 and NASA/STScI grant GO-10265.02 (J.S.K., P.G., K.M.G., and E.N.K.), an NSF Graduate Fellowship (K.M.G.), a Hubble Fellowship grant (HST-HF-01233.01) awarded by STScI (E.N.K.), and\nNSF grants AST-0307842, AST-0307851, and AST-0607726, NASA/JPL contract 1228235, the David and Lucile Packard Foundation, and The F. H. Levinson Fund of the Peninsula Community Foundation (S.R.M., R.J.P., and R.L.B.).\n\nPublished - Kalirai2010p7266Astrophys_J.pdf
Accepted Version - 0911.1998.pdf
", "abstract": "We present new Keck/DEIMOS spectroscopic observations of hundreds of individual stars along the sightline to the first three of the Andromeda (M31) dwarf spheroidal (dSph) galaxies to be discovered, And I, II, and III, and combine them with recent spectroscopic studies by our team of three additional M31 dSphs, And VII, X, and XIV, as a part of the SPLASH Survey (Spectroscopic and Photometric Landscape of Andromeda's Stellar Halo). Member stars of each dSph are isolated from foreground Milky Way dwarf stars and M31 field contamination using a variety of photometric and spectroscopic diagnostics. Our final spectroscopic sample of member stars in each dSph, for which we measure accurate radial velocities with a median uncertainty (random plus systematic errors) of 4-5 km s^(\u20131), includes 80 red giants in And I, 95 in And II, 43 in And III, 18 in And VII, 22 in And X, and 38 in And XIV. The sample of confirmed members in the six dSphs is used to derive each system's mean radial velocity, intrinsic central velocity dispersion, mean abundance, abundance spread, and dynamical mass. This combined data set presents us with a unique opportunity to perform the first systematic comparison of the global properties (e.g., metallicities, sizes, and dark matter masses) of one-third of Andromeda's total known dSph population with Milky Way counterparts of the same luminosity. Our overall comparisons indicate that the family of dSphs in these two hosts have both similarities and differences. For example, we find that the luminosity-metallicity relation is very similar between L ~ 10^5 and 10^7 L_\u2609, suggesting that the chemical evolution histories of each group of dSphs are similar. The lowest luminosity M31 dSphs appear to deviate from the relation, possibly suggesting tidal stripping. Previous observations have noted that the sizes of M31's brightest dSphs are systematically larger than Milky Way satellites of similar luminosity. At lower luminosities between L = 10^4 and 10^6 L_\u2609, we find that the sizes of dSphs in the two hosts significantly overlap and that four of the faintest M31 dSphs are smaller than Milky Way counterparts. The first dynamical mass measurements of six M31 dSphs over a large range in luminosity indicate similar mass-to-light ratios compared to Milky Way dSphs among the brighter satellites, and smaller mass-to-light ratios among the fainter satellites. Combined with their similar or larger sizes at these luminosities, these results hint that the M31 dSphs are systematically less dense than Milky Way dSphs. The implications of these similarities and differences for general understanding of galaxy formation and evolution are summarized.", "date": "2010-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "711", "number": "2", "publisher": "American Astronomical Society", "pagerange": "671-692", "id_number": "CaltechAUTHORS:20100317-113720269", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100317-113720269", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Space Telescope Science Institute" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HF-01185.01-A" }, { "agency": "NSF", "grant_number": "AST-0307966" }, { "agency": "NSF", "grant_number": "AST-0607852" }, { "agency": "NSF", "grant_number": "AST-0808133" }, { "agency": "NASA", "grant_number": "GO-10265.02" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-01233.01" }, { "agency": "NSF", "grant_number": "AST-0307842" }, { "agency": "NSF", "grant_number": "AST-0307851" }, { "agency": "NSF", "grant_number": "AST-0607726" }, { "agency": "NASA/JPL", "grant_number": "1228235" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Peninsula Community Foundation" } ] }, "local_group": { "items": [ { "id": "SPLASH" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/711/2/671", "primary_object": { "basename": "0911.1998.pdf", "url": "https://authors.library.caltech.edu/records/ez0cb-hs087/files/0911.1998.pdf" }, "related_objects": [ { "basename": "Kalirai2010p7266Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/ez0cb-hs087/files/Kalirai2010p7266Astrophys_J.pdf" } ], "pub_year": "2010", "author_list": "Kalirai, Jason S.; Beaton, Rachael L.; et el." }, { "id": "https://authors.library.caltech.edu/records/2bgw0-pt755", "eprint_id": 16661, "eprint_status": "archive", "datestamp": "2023-08-21 22:41:23", "lastmod": "2023-10-19 22:27:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gilbert-K-M", "name": { "family": "Gilbert", "given": "Karoline M." }, "orcid": "0000-0003-0394-8377" }, { "id": "Guhathakurta-P", "name": { "family": "Guhathakurta", "given": "Puragra" }, "orcid": "0000-0001-8867-4234" }, { "id": "Kollipara-P", "name": { "family": "Kollipara", "given": "Priya" } }, { "id": "Beaton-R-L", "name": { "family": "Beaton", "given": "Rachael L." }, "orcid": "0000-0002-1691-8217" }, { "id": "Geha-M-C", "name": { "family": "Geha", "given": "Marla C." }, "orcid": "0000-0002-7007-9725" }, { "id": "Kalirai-J-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-S-R", "name": { "family": "Majewski", "given": "Steven R." }, "orcid": "0000-0003-2025-3147" }, { "id": "Patterson-R-J", "name": { "family": "Patterson", "given": "Richard J." } } ] }, "title": "The Splash Survey: A Spectroscopic Portrait of Andromeda's Giant Southern Stream", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: halos; galaxies: individual (M31); stars: kinematics; techniques: spectroscopic", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2008 December 15; accepted 2009 September 23; published 2009 October 20. \n\nThe authors thank Mark Fardal for many useful discussions. This project was supported by NSF grants AST-0307966, AST-0507483, and AST-0607852 (K.M.G., P.G., J.S.K., P.K., and E.N.K.), NSF Graduate Student Research Fellowships (K.M.G., P.K., and E.N.K.), and NSF grants AST-0307842, AST-0307851, and AST-0607726, NASA/JPL contract 1228235, the David and Lucile Packard Foundation, and The F. H. Levinson Fund of the Peninsula Community Foundation (S.R.M., R.J.P., and R.L.B.). J.S.K. was supported by NASA through Hubble Fellowship grant HF-01185.01-A, awarded by 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 - Gilbert2009p6292Astrophys_J.pdf
Accepted Version - 0909.4540.pdf
", "abstract": "The giant southern stream (GSS) is the most prominent tidal debris feature in M31's stellar halo and covers a significant fraction of its southern quadrant. The GSS is a complex structure composed of a relatively metal-rich, high-surface-brightness \"core\" and a lower metallicity, lower-surface-brightness \"envelope.\" We present spectroscopy of red giant stars in six fields in the vicinity of M31's GSS (including four new fields and improved spectroscopic reductions for two previously published fields) and one field on stream C, an arc-like feature seen in star-count maps on M31's southeast minor axis at R ~ 60 kpc. These data are part of our ongoing Spectroscopic and Photometric Landscape of Andromeda's Stellar Halo survey of M31 using the DEIMOS instrument on the Keck II 10 m telescope. Several GSS-related findings and measurements are presented here. We present the innermost kinematical detection of the GSS core to date (R = 17 kpc). This field also contains the inner continuation of a second kinematically cold component that was originally seen in a GSS core field at R ~ 21 kpc. The velocity gradients of the GSS and the second component in the combined data set are parallel over a range of \u0394R = 7 kpc, suggesting that this may represent a bifurcation in the line-of-sight velocities of GSS stars. We present the first kinematical detection of substructure in the GSS envelope (S quadrant, R ~ 58 kpc). Using kinematically identified samples, we show that the envelope debris has a ~0.7 dex lower mean photometric metallicity and possibly higher intrinsic velocity dispersion than the GSS core. The GSS is also identified in the field of the M31 dwarf spheroidal satellite And I; the GSS in this field has a metallicity distribution identical to that of the GSS core. We confirm the previous finding of two kinematically cold components in stream C, and measure intrinsic velocity dispersions of ~10 and ~4 km s^(\u20131). This compilation of the kinematical (mean velocity, intrinsic velocity dispersion) and chemical properties of stars in the GSS core and envelope, coupled with published surface-brightness measurements and wide-area star-count maps, will improve constraints on the orbit and internal structure of the dwarf satellite progenitor.", "date": "2009-11-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "705", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1275-1297", "id_number": "CaltechAUTHORS:20091111-093926622", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091111-093926622", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0307966" }, { "agency": "NSF", "grant_number": "AST-0507483" }, { "agency": "NSF", "grant_number": "AST-0607852" }, { "agency": "NSF", "grant_number": "AST-0307842" }, { "agency": "NSF", "grant_number": "AST-0307851" }, { "agency": "NSF", "grant_number": "AST-0607726" }, { "agency": "NASA/JPL", "grant_number": "1228235" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Peninsula Community Foundation" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HF-01185.01-A" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "Space Telescope Science Institute" } ] }, "local_group": { "items": [ { "id": "SPLASH" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/705/2/1275", "primary_object": { "basename": "0909.4540.pdf", "url": "https://authors.library.caltech.edu/records/2bgw0-pt755/files/0909.4540.pdf" }, "related_objects": [ { "basename": "Gilbert2009p6292Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/2bgw0-pt755/files/Gilbert2009p6292Astrophys_J.pdf" } ], "pub_year": "2009", "author_list": "Gilbert, Karoline M.; Guhathakurta, Puragra; et el." } ]