[ { "id": "https://authors.library.caltech.edu/records/37san-rnc03", "eprint_id": 121650, "eprint_status": "archive", "datestamp": "2023-08-22 20:55:11", "lastmod": "2023-10-20 15:41:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zhuang-Zhuyun", "name": { "family": "Zhuang", "given": "Zhuyun" }, "orcid": "0000-0002-1945-2299" }, { "id": "Leethochawalit-Nicha", "name": { "family": "Leethochawalit", "given": "Nicha" }, "orcid": "0000-0003-4570-3159" }, { "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "orcid": "0000-0001-6196-5162" }, { "id": "Nightingale-James-W", "name": { "family": "Nightingale", "given": "J. W." }, "orcid": "0000-0002-8987-7401" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Glazebrook-Karl", "name": { "family": "Glazebrook", "given": "Karl" }, "orcid": "0000-0002-3254-9044" }, { "id": "Barone-Tania-M", "name": { "family": "Barone", "given": "Tania M." }, "orcid": "0000-0002-2784-564X" }, { "id": "Skobe-Hannah", "name": { "family": "Skobe", "given": "Hannah" }, "orcid": "0000-0003-0516-3485" }, { "id": "Sweet-Sarah-M", "name": { "family": "Sweet", "given": "Sarah M." }, "orcid": "0000-0002-1576-2505" }, { "id": "Nanayakkara-Themiya", "name": { "family": "Nanayakkara", "given": "Themiya" }, "orcid": "0000-0003-2804-0648" }, { "id": "Allen-Rebecca-J", "name": { "family": "Allen", "given": "Rebecca J." }, "orcid": "0000-0002-7278-9528" }, { "id": "G-C-Keerthi-Vasan", "name": { "family": "G. C.", "given": "Keerthi Vasan" }, "orcid": "0000-0002-2645-679X" }, { "id": "Jones-Tucker-A", "name": { "family": "Jones", "given": "Tucker" }, "orcid": "0000-0001-5860-3419" }, { "id": "Kacprzak-Glenn-G", "name": { "family": "Kacprzak", "given": "Glenn G." }, "orcid": "0000-0003-1362-9302" }, { "id": "Tran-Kim-Vy-H", "name": { "family": "Tran", "given": "Kim-Vy H." }, "orcid": "0000-0001-9208-2143" }, { "id": "Jacobs-Colin", "name": { "family": "Jacobs", "given": "Colin" }, "orcid": "0000-0003-4239-4055" } ] }, "title": "A Glimpse of the Stellar Populations and Elemental Abundances of Gravitationally Lensed, Quiescent Galaxies at z \u2273 1 with Keck Deep Spectroscopy", "ispublished": "pub", "full_text_status": "public", "keywords": "Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nThe authors acknowledge the insightful and constructive feedback of the anonymous referee, which helped us improve the manuscript. We would also like to thank Meng Gu for helpful advice on full-spectrum fitting with alf and Allison Strom for useful discussions on MOSFIRE data reduction and analysis with MOSPEC. We gratefully thank the staff at the W. M. Keck Observatory, including support astronomers Luca Rizzi, Carlos Alvarez, and Jim Lyke and telescope operators Arina Rostopchina, Julie Renauld-Kim, and Heather Hershey, for assisting in the observations. \n\nWe are grateful to the many people who have worked to make the Keck Telescope and its instruments a reality and to operate and maintain the Keck Observatory. The authors wish to extend special thanks to those of Hawaiian ancestry, on whose sacred mountain we are privileged to be guests. Without their generous hospitality, none of the observations presented herein would have been possible. \n\nThis material is based on work supported by the National Science Foundation under grant Nos. AST-2233781 (E.N.K.) and AST-2009278 (C.C.S.). Z.Z., E.N.K., and C.C.S. acknowledge financial support from National Aeronautics and Space Administration (NASA) through the FINESST program (No. 80NSSC22K1755). K.G., T.N. and C.J. acknowledge support from Australian Research Council (FL180100060). S.M.S. acknowledges funding from the Australian Research Council (DE220100003). T.J. and K.V.G.C. gratefully acknowledge financial support from NASA through grant No. HST-GO-16773, the Gordon and Betty Moore Foundation through grant No. GBMF8549, and the National Science Foundation through grant No. AST-2108515. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project No. CE170100013. \n\nThis work has made use of observations from the NASA/ESA Hubble Space Telescope obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. Support for Program No. GO-16773 was provided through a grant from the STScI under NASA contract NAS5-26555. \n\nFacilities: Keck I (LRIS - , MOSFIRE) - , HST (WFC3). - \n\nSoftware: SExtractor (Bertin & Arnouts 1996), alf (Conroy et al. 2018), dynesty (Speagle 2020), PyAutoLens (Nightingale & Dye 2015; Nightingale et al. 2018, 2021a, 2021b), BAGPIPES (Carnall et al. 2018, 2019), Astropy (Astropy Collaboration et al. 2013, 2018), NumPy (Harris et al. 2020), SciPy (Virtanen et al. 2020).\n\n
Published - Zhuang_2023_ApJ_948_132.pdf
", "abstract": "Gravitational lenses can magnify distant galaxies, allowing us to discover and characterize the stellar populations of intrinsically faint, quiescent galaxies that are otherwise extremely difficult to directly observe at high redshift from ground-based telescopes. Here, we present the spectral analysis of two lensed, quiescent galaxies at z \u2273 1 discovered by the ASTRO 3D Galaxy Evolution with Lenses survey: AGEL1323 (M_* \u223c 10^(11.1)M_\u2299, z = 1.016, \u03bc \u223c 14.6) and AGEL0014 (M_* \u223c 10^(11.5)M_\u2299, z = 1.374, \u03bc \u223c 4.3). We measured the age, [Fe/H], and [Mg/Fe] of the two lensed galaxies using deep, rest-frame-optical spectra (S/N \u2273 40 \u00c5\u207b\u00b9) obtained on the Keck I telescope. The ages of AGEL1323 and AGEL0014 are 5.6^(+0.8)_(\u22120.8) Gyr and 3.1^(+0.8)_(\u22120.3) Gyr, respectively, indicating that most of the stars in the galaxies were formed less than 2 Gyr after the Big Bang. Compared to nearby quiescent galaxies of similar masses, the lensed galaxies have lower [Fe/H] and [Mg/H]. Surprisingly, the two galaxies have comparable [Mg/Fe] to similar-mass galaxies at lower redshifts, despite their old ages. Using a simple analytic chemical evolution model connecting the instantaneously recycled element Mg with the mass-loading factors of outflows averaged over the entire star formation history, we found that the lensed galaxies may have experienced enhanced outflows during their star formation compared to lower-redshift galaxies, which may explain why they quenched early.", "date": "2023-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "948", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 132", "id_number": "CaltechAUTHORS:20230531-151922700.2", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230531-151922700.2", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-2233781" }, { "agency": "NSF", "grant_number": "AST-2009278" }, { "agency": "NASA Earth and Space Science and Technology Fellowship", "grant_number": "80NSSC22K1755" }, { "agency": "Australian Research Council", "grant_number": "FL180100060" }, { "agency": "Australian Research Council", "grant_number": "DE220100003" }, { "agency": "NASA", "grant_number": "HST-GO-16773" }, { "agency": "Gordon and Betty Moore Foundation", "grant_number": "GBMF8549" }, { "agency": "NSF", "grant_number": "AST-2108515" }, { "agency": "Australian Research Council", "grant_number": "CE170100013" }, { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/acc79b", "primary_object": { "basename": "Zhuang_2023_ApJ_948_132.pdf", "url": "https://authors.library.caltech.edu/records/37san-rnc03/files/Zhuang_2023_ApJ_948_132.pdf" }, "resource_type": "article", "pub_year": "2023", "author_list": "Zhuang, Zhuyun; Leethochawalit, Nicha; et el." }, { "id": "https://authors.library.caltech.edu/records/j0qjc-8wf35", "eprint_id": 121130, "eprint_status": "archive", "datestamp": "2023-08-22 20:46:46", "lastmod": "2023-10-18 18:09:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pahl-Anthony-J", "name": { "family": "Pahl", "given": "Anthony J." }, "orcid": "0000-0003-4464-4505" }, { "id": "Shapley-Alice-E", "name": { "family": "Shapley", "given": "Alice" }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Reddy-Naveen-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Chen-Yuguang", "name": { "family": "Chen", "given": "Yuguang" }, "orcid": "0000-0003-4520-5395" }, { "id": "Rudie-Gwen-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Strom-Allison-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" } ] }, "title": "The connection between the escape of ionizing radiation and galaxy properties at z \u223c 3 in the Keck Lyman continuum spectroscopic survey", "ispublished": "pub", "full_text_status": "public", "keywords": "Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2023 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model).\n\nWe acknowledge support from NSF AAG grants 0606912, 0908805, 1313472, 2009313, 2009085, and 2009278. Support for program HST-GO-15287.001 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. CS was supported in part by the Caltech/JPL President's and Director's program. Based in part 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 paper includes data gathered with the 6.5\u2009m Magellan Telescopes located at Las Campanas Observatory, Chile. We thank D. Kelson for the use of his FourCLift FourStar Reduction code and for his assistance with it. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain, we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible. \n\nDATA AVAILABILITY. The HST data referenced in this article are publicly available from the Mikulski Archive for Space Telescopes. The ground-based data presented here will be shared on reasonable request to the corresponding author.\n\nPublished - stad774.pdf
", "abstract": "The connection between the escape fraction of ionizing radiation (f_(esc)) and the properties of galaxies, such as stellar mass (\u2060M_\u2217\u2060), age, star-formation rate (SFR), and dust content, are key inputs for reionization models, but many of these relationships remain untested at high redshift. We present an analysis of a sample of 96 z \u223c 3 galaxies from the Keck Lyman Continuum Spectroscopic Survey (KLCS). These galaxies have both sensitive Keck/LRIS spectroscopic measurements of the Lyman continuum (LyC) region, and multiband photometry that places constraints on stellar population parameters. We construct composite spectra from subsamples binned as a function of galaxy property and quantify the ionizing-photon escape for each composite. We find a significant anti-correlation between f_(esc) and M_\u2217\u2060, consistent with predictions from cosmological zoom-in simulations. We also find significant anti-correlation between f_(esc) and E(B\u2212V), encoding the underlying physics of LyC escape in our sample. We also find no significant correlation between fesc and either stellar age or specific SFR (= SFR/M_\u2217\u2060), challenging interpretations that synchronize recent star formation and favorable conditions for ionizing escape. The galaxy properties now shown to correlate with fesc in the KLCS are Ly\u03b1 equivalent width, UV Luminosity, M_\u2217\u2060, SFR, and E(B\u2212V), but not age or sSFR. This comprehensive analysis of galaxy properties and LyC escape at high redshift will be used to guide future models and observations of the reionization epoch.", "date": "2023-05", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "521", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "3247-3259", "id_number": "CaltechAUTHORS:20230420-956212500.3", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230420-956212500.3", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "NSF", "grant_number": "AST-2009313" }, { "agency": "NSF", "grant_number": "AST-2009085" }, { "agency": "NSF", "grant_number": "AST-2009278" }, { "agency": "NASA", "grant_number": "HST-GO-15287.001" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "JPL President and Director's Fund" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/stad774", "primary_object": { "basename": "stad774.pdf", "url": "https://authors.library.caltech.edu/records/j0qjc-8wf35/files/stad774.pdf" }, "resource_type": "article", "pub_year": "2023", "author_list": "Pahl, Anthony J.; Shapley, Alice; et el." }, { "id": "https://authors.library.caltech.edu/records/z784y-84t72", "eprint_id": 121662, "eprint_status": "archive", "datestamp": "2023-08-22 20:42:44", "lastmod": "2023-10-20 15:42:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kikuta-Satoshi", "name": { "family": "Kikuta", "given": "Satoshi" }, "orcid": "0000-0003-3214-9128" }, { "id": "Matsuda-Yuichi", "name": { "family": "Matsuda", "given": "Yuichi" }, "orcid": "0000-0003-1747-2891" }, { "id": "Inoue-Shigeki", "name": { "family": "Inoue", "given": "Shigeki" }, "orcid": "0000-0001-8819-6877" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Cen-Renyue", "name": { "family": "Cen", "given": "Renyue" }, "orcid": "0000-0001-8531-9536" }, { "id": "Zheng-Zheng", "name": { "family": "Zheng", "given": "Zheng" }, "orcid": "0000-0003-1887-6732" }, { "id": "Yajima-Hidenobu", "name": { "family": "Yajima", "given": "Hidenobu" }, "orcid": "0000-0002-1319-3433" }, { "id": "Momose-Rieko", "name": { "family": "Momose", "given": "Rieko" }, "orcid": "0000-0002-8857-2905" }, { "id": "Imanishi-Masatoshi", "name": { "family": "Imanishi", "given": "Masatoshi" }, "orcid": "0000-0001-6186-8792" }, { "id": "Komiyama-Yutaka", "name": { "family": "Komiyama", "given": "Yutaka" }, "orcid": "0000-0002-3852-6329" } ] }, "title": "UV and Ly\u03b1 Halos of Ly\u03b1 Emitters across Environments at z = 2.84", "ispublished": "pub", "full_text_status": "public", "keywords": "Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nThis research is based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. \n\nWe are grateful to the anonymous referee for their careful reading and constructive comments and suggestions, Chris Byrohl for providing simulation data, and Haibin Zhang, Masafumi Yagi, Masayuki Umemura, Tadafumi Takata, Kazuhiro Shimasaku, Yusei Koyama, and Kazuhiro Hada for fruitful discussions. We thank Yukie Oishi and the HSC pipeline team for their helpful comments on HSC data analyses. We would like to acknowledge all who supported our observations at the Subaru Telescope, including the staff of the National Astronomical Observatory of Japan, Maunakea Observatories, and the local Hawaiian people who have been making efforts to preserve and share the beautiful dark sky of Maunakea with us. We are honored and grateful for the opportunity of observing the universe from Maunakea, which has the cultural, historical, and natural significance in Hawaii. Data analysis was carried out on the Multi-wavelength Data Analysis System operated by the Astronomy Data Center (ADC), National Astronomical Observatory of Japan, and on analysis servers at Center for Computational Astrophysics, National Astronomical Observatory of Japan. S.K. acknowledges support from the Japan Society for the Promotion of Science (JSPS) KAKENHI grant Nos. 18J11477, 19H00697 and the Course-by-Course Education Program of SOKENDAI. Y.M. acknowledges support from the JSPS KAKENHI grant Nos. 25287043, 17H04831, 17KK0098. C.C.S. acknowledges support by US NSF grant AST-2009278. Z.Z. acknowledges support by US NSF grant AST-2007499. \n\nFacility: Subaru (HSC). - \n\nSoftware: SExtractor (Bertin & Arnouts 1996), IRAF.\n\nPublished - Kikuta_2023_ApJ_947_75.pdf
", "abstract": "We present UV and Ly\u03b1 radial surface brightness (SB) profiles of Ly\u03b1 emitters (LAEs) at z = 2.84 detected with the Hyper Suprime-Cam on the Subaru Telescope. The depth of our data, together with the wide-field coverage including a protocluster, enable us to study the dependence of Ly\u03b1 halos (LAHs) on various galaxy properties, including Mpc scale environments. UV and Ly\u03b1 images of 3490 LAEs are extracted, and stacking the images yields SB sensitivity of ~ 1 x 10\u207b\u00b2\u2070 erg s\u207b\u00b9 cm\u207b\u00b2 arcsec\u207b\u00b2 in Ly\u03b1, reaching the expected level of optically thick gas illuminated by the UV background at z \u223c 3. Fitting of the two-component exponential function gives the scale-lengths of 1.56 \u00b1 0.01 and 10.4 \u00b1 0.3 pkpc. Dividing the sample according to their photometric properties, we find that, while the dependence of halo scale-length on environment outside of the protocluster core is not clear, LAEs in the central regions of protoclusters appear to have very large LAHs, which could be caused by combined effects of source overlapping and diffuse Ly\u03b1 emission from cool intergalactic gas permeating the forming protocluster core irradiated by active members. For the first time, we identify UV halos around bright LAEs that are probably due to a few lower-mass satellite galaxies. Through comparison with recent numerical simulations, we conclude that, while scattered Ly\u03b1 photons from the host galaxies are dominant, star formation in satellites evidently contributes to LAHs, and that fluorescent Ly\u03b1 emission may be boosted within protocluster cores at cosmic noon and/or near bright QSOs.", "date": "2023-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "947", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 75", "id_number": "CaltechAUTHORS:20230601-111032400.7", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230601-111032400.7", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "18J11477" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19H00697" }, { "agency": "Graduate University for Advanced Studies (SOKENDAI)" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "25287043" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17H04831" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17KK0098" }, { "agency": "NSF", "grant_number": "AST-2009278" }, { "agency": "NSF", "grant_number": "AST-2007499" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/acbf30", "primary_object": { "basename": "Kikuta_2023_ApJ_947_75.pdf", "url": "https://authors.library.caltech.edu/records/z784y-84t72/files/Kikuta_2023_ApJ_947_75.pdf" }, "resource_type": "article", "pub_year": "2023", "author_list": "Kikuta, Satoshi; Matsuda, Yuichi; et el." }, { "id": "https://authors.library.caltech.edu/records/ah8yb-53f32", "eprint_id": 119994, "eprint_status": "archive", "datestamp": "2023-08-22 20:11:48", "lastmod": "2023-10-25 16:48:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Langen-Vivienne", "name": { "family": "Langen", "given": "Vivienne" }, "orcid": "0000-0002-9523-3880" }, { "id": "Cantalupo-Sebastiano", "name": { "family": "Cantalupo", "given": "Sebastiano" }, "orcid": "0000-0001-5804-1428" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Chen-Yuguang", "name": { "family": "Chen", "given": "Yuguang" }, "orcid": "0000-0003-4520-5395" }, { "id": "Pezzulli-Gabriele", "name": { "family": "Pezzulli", "given": "Gabriele" }, "orcid": "0000-0003-0736-7879" }, { "id": "Gallego-Sofia-G", "name": { "family": "Gallego", "given": "Sofia G." }, "orcid": "0000-0002-8825-8107" } ] }, "title": "Characterizing the circumgalactic medium of quasars at z \u223c 2.2 through H\u2009\u03b1 and Ly\u2009\u03b1 emission", "ispublished": "pub", "full_text_status": "public", "keywords": "Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model).\n\nThis project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No 864361, PI: S. Cantalupo). SC gratefully acknowledges additional support from the Swiss National Science Foundation grant PP00P2_190092 and from Fondazione Cariplo. GP acknowledges support from the Netherlands Research School for Astronomy (NOVA). SG acknowledges support from the Swiss National Science Foundation grant P2EZP2_199856. \n\nDATA AVAILABILITY. The data underlying this article will be shared on reasonable request to the corresponding author.\n\nPublished - stac3205.pdf
", "abstract": "The discovery of giant quasar Ly\u2009\u03b1 nebulae at z > 2 has opened up the possibility to directly study in emission the Circumgalactic and Intergalactic Medium (CGM/IGM). However, the resonant nature of the Ly\u2009\u03b1 line and its different emission mechanisms hamper the ability to constrain both the kinematics and physical properties of the CGM/IGM. Here, we present results of a pilot project aiming at the detection of CGM H\u2009\u03b1 emission, a line which does not suffer from these limitations. To this end, we first used KCWI to detect Ly\u2009\u03b1 emission around three bright quasars with 2.25 < z < 2.27, a range which is free from bright IR sky lines for H\u2009\u03b1, and then selected the most extended nebula for H\u2009\u03b1 follow-up with MOSFIRE. Within the MOSFIRE slit, we detected H\u2009\u03b1 emission extending up to 20 physical kpc with a total H\u2009\u03b1 flux of F_(H\u2009\u03b1) = (9.5\u00a0\u00b1\u00a00.9) \u00d7 10\u207b\u00b9\u2078 erg s\u207b\u00b9, cm\u207b\u00b2. Considering the Ly\u2009\u03b1 flux in the same region, we found F_(Ly\u2009\u03b1)/F_(H\u2009\u03b1) = 3.7\u00a0\u00b1\u00a00.3 consistent with that obtained for the Slug Nebula at z = 2.275 and with recombination radiation. This implies high densities or a very broad density distribution within the CGM of high-redshift quasars. Moreover, the H\u2009\u03b1 line profile suggests the presence of multiple emitting components overlapping along our line of\u00a0sight and relatively quiescent kinematics, which seems incompatible with either quasar outflows capable of escaping the potential well of the host halo or disc-like rotation in a massive halo (>10\u00b9\u00b2 M_\u2299).", "date": "2023-03", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "519", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "5099-5113", "id_number": "CaltechAUTHORS:20230314-844891400.3", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230314-844891400.3", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "864361" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "PP00P2_190092" }, { "agency": "Fondazione Cariplo" }, { "agency": "Nederlandse Onderzoekschool voor de Astronomie (NOVA)" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "P2EZP2_199856" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/stac3205", "primary_object": { "basename": "stac3205.pdf", "url": "https://authors.library.caltech.edu/records/ah8yb-53f32/files/stac3205.pdf" }, "resource_type": "article", "pub_year": "2023", "author_list": "Langen, Vivienne; Cantalupo, Sebastiano; et el." }, { "id": "https://authors.library.caltech.edu/records/eht42-gm086", "eprint_id": 117171, "eprint_status": "archive", "datestamp": "2023-08-22 17:49:59", "lastmod": "2023-10-24 22:01:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "James-Bethan-L", "name": { "family": "James", "given": "Bethan L." }, "orcid": "0000-0003-4372-2006" }, { "name": { "family": "Berg", "given": "Danielle A." }, "orcid": "0000-0002-4153-053X" }, { "name": { "family": "King", "given": "Teagan" }, "orcid": "0000-0003-0834-4150" }, { "name": { "family": "Sahnow", "given": "David J." }, "orcid": "0000-0001-9594-161X" }, { "name": { "family": "Mingozzi", "given": "Matilde" }, "orcid": "0000-0003-2589-762X" }, { "name": { "family": "Chisholm", "given": "John" }, "orcid": "0000-0002-0302-2577" }, { "name": { "family": "Heckman", "given": "Timothy" }, "orcid": "0000-0003-1127-7497" }, { "name": { "family": "Martin", "given": "Crystal L." }, "orcid": "0000-0001-9189-7818" }, { "name": { "family": "Stark", "given": "Dan P." } }, { "name": { "family": "Aloisi", "given": "Alessandra" }, "orcid": "0000-0003-4137-882X" }, { "name": { "family": "Amor\u00edn", "given": "Ricardo O." }, "orcid": "0000-0001-5758-1000" }, { "name": { "family": "Arellano-C\u00f3rdova", "given": "Karla Z." }, "orcid": "0000-0002-2644-3518" }, { "name": { "family": "Bayliss", "given": "Matthew" }, "orcid": "0000-0003-1074-4807" }, { "name": { "family": "Bordoloi", "given": "Rongmon" }, "orcid": "0000-0002-3120-7173" }, { "name": { "family": "Brinchmann", "given": "Jarle" }, "orcid": "0000-0003-4359-8797" }, { "name": { "family": "Charlot", "given": "St\u00e9phane" }, "orcid": "0000-0003-3458-2275" }, { "name": { "family": "Chen", "given": "Zuyi" }, "orcid": "0000-0002-2178-5471" }, { "name": { "family": "Chevallard", "given": "Jacopo" }, "orcid": "0000-0002-7636-0534" }, { "name": { "family": "Clark", "given": "Ilyse" }, "orcid": "0000-0003-3334-4267" }, { "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "name": { "family": "Feltre", "given": "Anna" }, "orcid": "0000-0001-6865-2871" }, { "name": { "family": "Hayes", "given": "Matthew" }, "orcid": "0000-0001-8587-218X" }, { "name": { "family": "Henry", "given": "Alaina" }, "orcid": "0000-0002-6586-4446" }, { "name": { "family": "Hernandez", "given": "Svea" }, "orcid": "0000-0003-4857-8699" }, { "name": { "family": "Jaskot", "given": "Anne" }, "orcid": "0000-0002-6790-5125" }, { "name": { "family": "Kewley", "given": "Lisa J." }, "orcid": "0000-0001-8152-3943" }, { "name": { "family": "Kumari", "given": "Nimisha" }, "orcid": "0000-0002-5320-2568" }, { "name": { "family": "Leitherer", "given": "Claus" }, "orcid": "0000-0003-2685-4488" }, { "name": { "family": "Llerena", "given": "Mario" }, "orcid": "0000-0003-1354-4296" }, { "name": { "family": "Maseda", "given": "Michael" }, "orcid": "0000-0003-0695-4414" }, { "name": { "family": "Nanayakkara", "given": "Themiya" }, "orcid": "0000-0003-2804-0648" }, { "name": { "family": "Ouchi", "given": "Masami" }, "orcid": "0000-0002-1049-6658" }, { "name": { "family": "Plat", "given": "Adele" }, "orcid": "0000-0003-0390-0656" }, { "name": { "family": "Pogge", "given": "Richard W." }, "orcid": "0000-0003-1435-3053" }, { "name": { "family": "Ravindranath", "given": "Swara" }, "orcid": "0000-0002-5269-6527" }, { "name": { "family": "Rigby", "given": "Jane R." }, "orcid": "0000-0002-7627-6551" }, { "name": { "family": "Scarlata", "given": "Claudia" }, "orcid": "0000-0002-9136-8876" }, { "name": { "family": "Senchyna", "given": "Peter" }, "orcid": "0000-0002-9132-6561" }, { "name": { "family": "Skillman", "given": "Evan D." }, "orcid": "0000-0003-0605-8732" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0002-4834-7260" }, { "name": { "family": "Sugahara", "given": "Yuma" }, "orcid": "0000-0001-6958-7856" }, { "name": { "family": "Wilkins", "given": "Stephen M." }, "orcid": "0000-0003-3903-6935" }, { "name": { "family": "Wofford", "given": "Aida" }, "orcid": "0000-0001-8289-3428" }, { "name": { "family": "Xu", "given": "Xinfeng" }, "orcid": "0000-0002-9217-7051" } ] }, "title": "CLASSY. II. A Technical Overview of the COS Legacy Archive Spectroscopic Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "Space and Planetary Science; Astronomy and Astrophysics", "note": "B.L.J. is thankful for support from the European Space Agency (ESA). D.A.B. is grateful for the support for this program, HST-GO-15840, that was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.\n\nThe CLASSY Collaboration extends special gratitude to the Lorentz Center for useful discussions during the \"Characterizing Galaxies with Spectroscopy with a view for JWST\" 2017 workshop that led to the formation of the CLASSY Collaboration and survey. The CLASSY Collaboration thanks the COS team for all their assistance and advice in the reduction of the COS data, with particular thanks to Elaine Frazer for NUV data extraction and Christian Johnson in assisting with error analysis.", "abstract": "The COS Legacy Archive Spectroscopic SurveY (CLASSY) is designed to provide the community with a spectral atlas of 45 nearby star-forming galaxies that were chosen to cover similar properties to those seen at high z (z > 6). The prime high-level science product of CLASSY is accurately coadded UV spectra, ranging from \u223c1000 to 2000 \u00c5, derived from a combination of archival and new data obtained with HST's Cosmic Origins Spectrograph (COS). This paper details the multistage technical processes of creating this prime data product and the methodologies involved in extracting, reducing, aligning, and coadding far-ultraviolet and near-ultraviolet (NUV) spectra. We provide guidelines on how to successfully utilize COS observations of extended sources, despite COS being optimized for point sources, and best-practice recommendations for the coaddition of UV spectra in general. Moreover, we discuss the effects of our reduction and coaddition techniques in the scientific application of the CLASSY data. In particular, we find that accurately accounting for flux calibration offsets can affect the derived properties of the stellar populations, while customized extractions of NUV spectra for extended sources are essential for correctly diagnosing the metallicity of galaxies via C iii] nebular emission. Despite changes in spectral resolution of up to \u223c25% between individual data sets (due to changes in the COS line-spread function), no adverse affects were observed on the difference in velocity width and outflow velocities of isolated absorption lines when measured in the final combined data products, owing in part to our signal-to-noise regime of S/N < 20.", "date": "2022-10", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "262", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 37", "id_number": "CaltechAUTHORS:20220928-285212100.17", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220928-285212100.17", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "NASA", "grant_number": "HST-GO-15840" }, { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "CLASSY Team" ] }, "doi": "10.3847/1538-4365/ac8008", "resource_type": "article", "pub_year": "2022", "author_list": "James, Bethan L.; Berg, Danielle A.; et el." }, { "id": "https://authors.library.caltech.edu/records/kswgq-bxq72", "eprint_id": 117143, "eprint_status": "archive", "datestamp": "2023-08-22 17:49:49", "lastmod": "2023-10-24 21:58:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pahl-Anthony-J", "name": { "family": "Pahl", "given": "Anthony J." }, "orcid": "0000-0003-4464-4505" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice" }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Reddy-Naveen-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Chen-Yuguang", "name": { "family": "Chen", "given": "Yuguang" }, "orcid": "0000-0003-4520-5395" } ] }, "title": "Searching for the connection between ionizing-photon escape and the surface density of star formation at z \u223c 3", "ispublished": "pub", "full_text_status": "public", "keywords": "Space and Planetary Science; Astronomy and Astrophysics", "note": "We acknowledge support from NSF AAG grants 0606912, 0908805, 1313472 2009313, 2009085, and 2009278. Support for program HST-GO-15287.001 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. CS was supported in part by the Caltech/JPL President's and Director's program. 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 CFHT Legacy Survey, a collaborative project of NRC and CNRS. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible.", "abstract": "The connection between the escape fraction of ionizing photons (f_(esc)) and star formation rate surface density (\u03a3_(SFR)) is a key input for reionization models, but remains untested at high redshift. We analyse 35 z \u223c 3 galaxies from the Keck Lyman Continuum Survey (KLCS) covered by deep, rest far-UV spectra of the Lyman continuum (LyC) and high-resolution HST V_(606) imaging, enabling estimates of both f_(esc) and rest-UV sizes. Using S\u00e9rsic profile fits to HST images and spectral-energy distribution fits to multiband photometry, we measure effective sizes and SFRs for the galaxies in our sample, and separate the sample into two bins of \u03a3_(SFR). Based on composite spectra, we estimate \u3008f_(esc)\u3009 for both \u03a3_(SFR) subsamples, finding no significant difference in \u3008f_(esc)\u3009 between the two. To test the representativeness of the KLCS HST sample and robustness of this result, we attempt to recover the well-established correlation between f_(esc) and Ly\u03b1 equivalent width. This correlation is not significant within the KLCS HST sample, indicating that the sample is insufficient for correlating f_(esc) and galaxy properties such as \u03a3_(SFR). We perform stacking simulations using the KLCS parent sample to determine the optimal sample size for robust probes of the f_(esc)-\u03a3_(SFR) connection to inform future observing programs. For a program with a selection independent of ionizing properties, \u226590 objects are required; for one preferentially observing strongly-leaking LyC sources, \u226558 objects are required. More generally, measuring the connection between f_(esc) and \u03a3_(SFR) requires a larger, representative sample spanning a wide dynamic range in galaxies properties such as \u03a3_(SFR).", "date": "2022-10", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "516", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "2062-2073", "id_number": "CaltechAUTHORS:20220926-576554400.10", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220926-576554400.10", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "NSF", "grant_number": "AST-2009313" }, { "agency": "NSF", "grant_number": "AST-2009085" }, { "agency": "NSF", "grant_number": "AST-2009278" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "JPL President and Director's Fund" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/stac1767", "resource_type": "article", "pub_year": "2022", "author_list": "Pahl, Anthony J.; Shapley, Alice; et el." }, { "id": "https://authors.library.caltech.edu/records/q6bbq-hda57", "eprint_id": 116629, "eprint_status": "archive", "datestamp": "2023-08-22 17:14:34", "lastmod": "2023-10-24 21:08:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kubo-Mariko", "name": { "family": "Kubo", "given": "Mariko" }, "orcid": "0000-0002-7598-5292" }, { "id": "Umehata-Hideki", "name": { "family": "Umehata", "given": "Hideki" }, "orcid": "0000-0003-1937-0573" }, { "id": "Matsuda-Yuichi", "name": { "family": "Matsuda", "given": "Yuichi" }, "orcid": "0000-0003-1747-2891" }, { "id": "Kajisawa-Masaru", "name": { "family": "Kajisawa", "given": "Masaru" }, "orcid": "0000-0002-1732-6387" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Yamada-Toru", "name": { "family": "Yamada", "given": "Toru" } }, { "id": "Tanaka-Ichi", "name": { "family": "Tanaka", "given": "Ichi" }, "orcid": "0000-0002-4937-4738" }, { "id": "Hatsukade-Bunyo", "name": { "family": "Hatsukade", "given": "Bunyo" }, "orcid": "0000-0001-6469-8725" }, { "id": "Tamura-Yoichi", "name": { "family": "Tamura", "given": "Yoichi" }, "orcid": "0000-0003-4807-8117" }, { "id": "Nakanishi-Kouichiro", "name": { "family": "Nakanishi", "given": "Kouichiro" }, "orcid": "0000-0002-6939-0372" }, { "id": "Kohno-Kotaro", "name": { "family": "Kohno", "given": "Kotaro" }, "orcid": "0000-0002-4052-2394" }, { "id": "Lee-Kianhong", "name": { "family": "Lee", "given": "Kianhong" }, "orcid": "0000-0003-4814-0101" }, { "id": "Matsuda-Keiichi", "name": { "family": "Matsuda", "given": "Keiichi" } }, { "id": "Ao-Yiping", "name": { "family": "Ao", "given": "Yiping" }, "orcid": "0000-0003-3139-2724" }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "Tohru" }, "orcid": "0000-0002-7402-5441" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "Min S." }, "orcid": "0000-0001-7095-7543" } ] }, "title": "An AGN with an Ionized Gas Outflow in a Massive Quiescent Galaxy in a Protocluster at z = 3.09", "ispublished": "pub", "full_text_status": "public", "keywords": "Space and Planetary Science; Astronomy and Astrophysics", "note": "This work has been supported by JSPS KAKENHI Grant Nos. 20K14530, 21H044902 (MK), 17K14252, 20H01953 (HU), 19H00697, 20H01949 (TN), 17H06130 (YT and KK). This work has been also supported by a US National Science Foundation (NSF) grant AST-2009278 (CCS). This work has been also supported by NAOJ ALMA Scientific Research Grant Numbers 2018-09B (YT) The spectroscopic data were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The observations were carried out within the framework of the Subaru-Keck/Subaru-Gemini time exchange program, which is operated by the National Astronomical Observatory of Japan. The Ks -band image was collected with nuMOIRCS at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. We are honored and grateful for the opportunity of observing the Universe from Maunakea, which has the cultural, historical, and natural significance in Hawaii. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00162.S, ADS/JAO.ALMA#2016.1.00580.S, ADS/JAO.ALMA #2017.1.01332.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The F814W-band image is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.", "abstract": "We report the detection of an ionized gas outflow from an X-ray active galactic nucleus hosted in a massive quiescent galaxy in a protocluster at z = 3.09 (J221737.29+001823.4). It is a type-2 QSO with broad (W_80 > 1000 km s^(\u22121)) and strong (log(L[OIII]/erg s^(\u22121)) \u2248 43.4) [O III]\u03bb\u03bb 4959,5007 emission lines detected by slit spectroscopy in three-position angles using Multi-Object Infra-Red Camera and Spectrograph (MOIRCS) on the Subaru telescope and the Multi-Object Spectrometer For Infra-Red Exploration (MOSFIRE) on the Keck-I telescope. In the all slit directions, [O III] emission is extended to \u223c15 physical kpc and indicates a powerful outflow spreading over the host galaxy. The inferred ionized gas mass outflow rate is 22 \u00b1 3 M_\u2299 yr^(\u22121). Although it is a radio source, according to the line diagnostics using H\u03b2, [O II], and [O III], photoionization by the central QSO is likely the dominant ionization mechanism rather than shocks caused by radio jets. On the other hand, the spectral energy distribution of the host galaxy is well characterized as a quiescent galaxy that has shut down star formation several hundred Myr ago. Our results suggest a scenario that QSOs are powered after the shutdown of the star formation and help complete the quenching of massive quiescent galaxies at high redshift.", "date": "2022-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "935", "number": "2", "publisher": "American Astronomical Society", "pagerange": "89", "id_number": "CaltechAUTHORS:20220908-183409314", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220908-183409314", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "MEXT \u2223 Japan Society for the Promotion of Science", "grant_number": "20K14530" }, { "agency": "MEXT \u2223 Japan Society for the Promotion of Science", "grant_number": "21H044902" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17K14252" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20H01953" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19H00697" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20H01949" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17H06130" }, { "agency": "NSF", "grant_number": "AST-2009278" }, { "agency": "National Astronomical Observatory of Japan", "grant_number": "2018-09B" }, { "agency": "W. M. Keck Observatory" }, { "agency": "Subaru-Keck/Subaru-Gemini time exchange program" }, { "agency": "Subaru Telescope" }, { "agency": "ALMA" }, { "agency": "NASA", "grant_number": "5-26555" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ac7f2d", "resource_type": "article", "pub_year": "2022", "author_list": "Kubo, Mariko; Umehata, Hideki; et el." }, { "id": "https://authors.library.caltech.edu/records/91v8z-6wm14", "eprint_id": 115943, "eprint_status": "archive", "datestamp": "2023-08-22 17:06:07", "lastmod": "2023-10-24 20:55:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Berg-Danielle-A", "name": { "family": "Berg", "given": "Danielle A." }, "orcid": "0000-0002-4153-053X" }, { "name": { "family": "James", "given": "Bethan L." }, "orcid": "0000-0003-4372-2006" }, { "name": { "family": "King", "given": "Teagan" }, "orcid": "0000-0003-0834-4150" }, { "name": { "family": "McDonald", "given": "Meaghan" }, "orcid": "0000-0003-0557-3433" }, { "name": { "family": "Chen", "given": "Zuyi" }, "orcid": "0000-0002-2178-5471" }, { "name": { "family": "Chisholm", "given": "John" }, "orcid": "0000-0002-0302-2577" }, { "name": { "family": "Heckman", "given": "Timothy" }, "orcid": "0000-0001-6670-6370" }, { "name": { "family": "Martin", "given": "Crystal L." }, "orcid": "0000-0001-9189-7818" }, { "name": { "family": "Stark", "given": "Dan P." }, "orcid": "0000-0001-6106-5172" }, { "name": { "family": "Aloisi", "given": "Alessandra" }, "orcid": "0000-0003-4137-882X" }, { "name": { "family": "Amor\u00edn", "given": "Ricardo O." }, "orcid": "0000-0001-5758-1000" }, { "name": { "family": "Arellano-C\u00f3rdova", "given": "Karla Z." }, "orcid": "0000-0003-2589-762X" }, { "name": { "family": "Bayliss", "given": "Matthew" }, "orcid": "0000-0003-1074-4807" }, { "name": { "family": "Bordoloi", "given": "Rongmon" }, "orcid": "0000-0002-3120-7173" }, { "name": { "family": "Brinchmann", "given": "Jarle" }, "orcid": "0000-0003-4359-8797" }, { "name": { "family": "Charlot", "given": "St\u00e9phane" }, "orcid": "0000-0003-3458-2275" }, { "name": { "family": "Chevallard", "given": "Jacopo" }, "orcid": "0000-0002-7636-0534" }, { "name": { "family": "Clark", "given": "Ilyse" }, "orcid": "0000-0003-3334-4267" }, { "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "name": { "family": "Feltre", "given": "Anna" }, "orcid": "0000-0001-6865-2871" }, { "name": { "family": "Gronke", "given": "Max" }, "orcid": "0000-0003-2491-060X" }, { "name": { "family": "Hayes", "given": "Matthew" }, "orcid": "0000-0001-8587-218X" }, { "name": { "family": "Henry", "given": "Alaina" }, "orcid": "0000-0002-6586-4446" }, { "name": { "family": "Hernandez", "given": "Svea" }, "orcid": "0000-0003-4857-8699" }, { "name": { "family": "Jaskot", "given": "Anne" }, "orcid": "0000-0002-6790-5125" }, { "name": { "family": "Jones", "given": "Tucker" }, "orcid": "0000-0001-5860-3419" }, { "name": { "family": "Kewley", "given": "Lisa J." }, "orcid": "0000-0001-8152-3943" }, { "name": { "family": "Kumari", "given": "Nimisha" }, "orcid": "0000-0002-5320-2568" }, { "name": { "family": "Leitherer", "given": "Claus" }, "orcid": "0000-0003-2685-4488" }, { "name": { "family": "Llerena", "given": "Mario" }, "orcid": "0000-0003-1354-4296" }, { "name": { "family": "Maseda", "given": "Michael" }, "orcid": "0000-0003-0695-4414" }, { "name": { "family": "Mingozzi", "given": "Matilde" }, "orcid": "0000-0003-2589-762X" }, { "name": { "family": "Nanayakkara", "given": "Themiya" }, "orcid": "0000-0003-2804-0648" }, { "name": { "family": "Ouchi", "given": "Masami" }, "orcid": "0000-0002-1049-6658" }, { "name": { "family": "Plat", "given": "Adele" }, "orcid": "0000-0003-0390-0656" }, { "name": { "family": "Pogge", "given": "Richard W." }, "orcid": "0000-0003-1435-3053" }, { "name": { "family": "Ravindranath", "given": "Swara" }, "orcid": "0000-0002-5269-6527" }, { "name": { "family": "Rigby", "given": "Jane R." }, "orcid": "0000-0002-7627-6551" }, { "name": { "family": "Sanders", "given": "Ryan" }, "orcid": "0000-0003-4792-9119" }, { "name": { "family": "Scarlata", "given": "Claudia" }, "orcid": "0000-0002-9136-8876" }, { "name": { "family": "Senchyna", "given": "Peter" }, "orcid": "0000-0002-9132-6561" }, { "name": { "family": "Skillman", "given": "Evan D." }, "orcid": "0000-0003-0605-8732" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "name": { "family": "Sugahara", "given": "Yuma" }, "orcid": "0000-0001-6958-7856" }, { "name": { "family": "Wilkins", "given": "Stephen M." }, "orcid": "0000-0003-3903-6935" }, { "name": { "family": "Wofford", "given": "Aida" }, "orcid": "0000-0001-8289-3428" }, { "name": { "family": "Xu", "given": "Xinfeng" }, "orcid": "0000-0002-9217-7051" } ] }, "title": "The COS Legacy Archive Spectroscopy Survey (CLASSY) Treasury Atlas", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxies; Ultraviolet surveys; Emission line galaxies; Interstellar line absorption; Lyman-alpha galaxies; High-redshift galaxies; Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 October 3; revised 2022 February 16; accepted 2022 February 17; published 2022 July 27. \n\nBased on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.\n\nThe CLASSY team thanks the referee for thoughtful feedback that significantly improved both the paper and the HLSPs. D.A.B. is grateful for the support for this program, HST-GO-15840, that was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. B.L.J. is grateful for support from the European Space Agency (ESA). The CLASSY collaboration extends special gratitude to the Lorentz Center for useful discussions during the \"Characterizing Galaxies with Spectroscopy with a view for JWST\" 2017 workshop that led to the formation of the CLASSY collaboration and survey. \n\nFunding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/. \n\nSDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. \n\nThis work also uses the services of the ESO Science Archive Facility, observations collected at the European Southern Observatory under ESO programmes 096.B-0690, 0103.B-0531, 0103.D-0705, and 0104.D-0503, and observations obtained with the Large Binocular Telescope (LBT). The LBT is an international collaboration among institutions in the United States, Italy, and Germany. LBT Corporation partners are as follows: The University of Arizona on behalf of the Arizona Board of Regents; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max-Planck Society, The Leibniz Institute for Astrophysics Potsdam, and Heidelberg University; The Ohio State University, University of Notre Dame, University of Minnesota, and University of Virginia. \n\nThis paper made use of the modsIDL spectral data reduction pipeline developed in part with funds provided by NSF grant AST-1108693 and a generous gift from OSU Astronomy alumnus David G. Price through the Price Fellowship in Astronomical Instrumentation. This research has made use of the HSLA database, developed and maintained at STScI, Baltimore, USA. \n\nFacilities: HST (COS) - , LBT (MODS) - , Astrophysical Observatory of the Smithsonian Institution (APO;SDSS) - , KECK (ESI) - , Very Large Telescope (MUSE - , VIMOS). - \n\nSoftware: astropy (The Astropy Collaboration 2013, 2018); BEAGLE (Chevallard & Charlot 2016); CalCOS (STScI); dustmaps (Green 2018); jupyter (Kluyver et al. 2016); LINMIX (Kelly 2007); MPFIT (Markwardt 2009); MODS reduction Pipeline, Photutils (Bradley et al. 2021); PYNEB (Luridiana et al. 2012, 2015); python, pysynphot (STScI Development Team et al. 2013); RASCAS (Michel-Dansac et al. 2020); SALT (Scarlata & Panagia 2015); STARLIGHT (Fernandes 2005); tlac (Gronke & Dijkstra 2014); XIDL.\n\nPublished - Berg_2022_ApJS_261_31.pdf
Accepted Version - 2203.07357.pdf
", "abstract": "Far-ultraviolet (FUV; \u223c1200\u20132000 \u00c5) spectra are fundamental to our understanding of star-forming galaxies, providing a unique window on massive stellar populations, chemical evolution, feedback processes, and reionization. The launch of the James Webb Space Telescope will soon usher in a new era, pushing the UV spectroscopic frontier to higher redshifts than ever before; however, its success hinges on a comprehensive understanding of the massive star populations and gas conditions that power the observed UV spectral features. This requires a level of detail that is only possible with a combination of ample wavelength coverage, signal-to-noise, spectral-resolution, and sample diversity that has not yet been achieved by any FUV spectral database. We present the Cosmic Origins Spectrograph Legacy Spectroscopic Survey (CLASSY) treasury and its first high-level science product, the CLASSY atlas. CLASSY builds on the Hubble Space Telescope (HST) archive to construct the first high-quality (S/N_(1500 \u00c5) \u2273 5/resel), high-resolution (R \u223c 15,000) FUV spectral database of 45 nearby (0.002 z M_\u22c6(M_\u2299)) M_\u2299 yr\u207b\u00b9) < +1.6), direct gas-phase metallicity (7.0 < 12 + log(O/H) < 8.8), ionization (0.5 < O\u2083\u2082 < 38.0), reddening (0.02 < E(B \u2212 V) < 0.67), and nebular density (10 < n\u2091 (cm\u207b\u00b3) < 1120). CLASSY is biased to UV-bright star-forming galaxies, resulting in a sample that is consistent with the z \u223c 0 mass\u2013metallicity relationship, but is offset to higher star formation rates by roughly 2 dex, similar to z \u2273 2 galaxies. This unique set of properties makes the CLASSY atlas the benchmark training set for star-forming galaxies across cosmic time.", "date": "2022-08", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "261", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 31", "id_number": "CaltechAUTHORS:20220728-730128000", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220728-730128000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-15840" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NSF", "grant_number": "AST-1108693" }, { "agency": "David G. Price Fellowship" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "CLASSY Team" ] }, "doi": "10.3847/1538-4365/ac6c03", "primary_object": { "basename": "2203.07357.pdf", "url": "https://authors.library.caltech.edu/records/91v8z-6wm14/files/2203.07357.pdf" }, "related_objects": [ { "basename": "Berg_2022_ApJS_261_31.pdf", "url": "https://authors.library.caltech.edu/records/91v8z-6wm14/files/Berg_2022_ApJS_261_31.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Berg, Danielle A.; James, Bethan L.; et el." }, { "id": "https://authors.library.caltech.edu/records/2wdj2-v8v82", "eprint_id": 115909, "eprint_status": "archive", "datestamp": "2023-08-22 16:50:15", "lastmod": "2023-10-24 20:54:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Xu-Xinfeng", "name": { "family": "Xu", "given": "Xinfeng" }, "orcid": "0000-0002-9217-7051" }, { "id": "Heckman-Timothy-M", "name": { "family": "Heckman", "given": "Timothy" }, "orcid": "0000-0001-6670-6370" }, { "id": "Henry-Alaina-L", "name": { "family": "Henry", "given": "Alaina" }, "orcid": "0000-0002-6586-4446" }, { "id": "Berg-Danielle-A", "name": { "family": "Berg", "given": "Danielle A." }, "orcid": "0000-0002-4153-053X" }, { "id": "Chisholm-John", "name": { "family": "Chisholm", "given": "John" }, "orcid": "0000-0002-0302-2577" }, { "id": "James-Bethan-L", "name": { "family": "James", "given": "Bethan L." }, "orcid": "0000-0003-4372-2006" }, { "id": "Martin-Crystal-L", "name": { "family": "Martin", "given": "Crystal L." }, "orcid": "0000-0001-9189-7818" }, { "id": "Stark-Daniel-P", "name": { "family": "Stark", "given": "Daniel P." }, "orcid": "0000-0001-6106-5172" }, { "id": "Aloisi-Alessandra", "name": { "family": "Aloisi", "given": "Alessandra" }, "orcid": "0000-0003-4137-882X" }, { "id": "Amor\u00edn-Ricardo-O", "name": { "family": "Amor\u00edn", "given": "Ricardo O." }, "orcid": "0000-0001-5758-1000" }, { "id": "Arellano-C\u00f3rdova-Karla-Z", "name": { "family": "Arellano-C\u00f3rdova", "given": "Karla Z." }, "orcid": "0000-0003-2589-762X" }, { "id": "Bordoloi-Rongmon", "name": { "family": "Bordoloi", "given": "Rongmon" }, "orcid": "0000-0002-3120-7173" }, { "id": "Chrlot-St\u00e9phane", "name": { "family": "Charlot", "given": "St\u00e9phane" }, "orcid": "0000-0003-3458-2275" }, { "id": "Chen-Zuyi", "name": { "family": "Chen", "given": "Zuyi" }, "orcid": "0000-0002-2178-5471" }, { "id": "Hayes-Matthew", "name": { "family": "Hayes", "given": "Matthew" }, "orcid": "0000-0001-8587-218X" }, { "id": "Mingozzi-Matilde", "name": { "family": "Mingozzi", "given": "Matilde" }, "orcid": "0000-0003-2589-762X" }, { "id": "Sugahara-Yuma", "name": { "family": "Sugahara", "given": "Yuma" }, "orcid": "0000-0001-6958-7856" }, { "id": "Kewley-Lisa-J", "name": { "family": "Kewley", "given": "Lisa J." }, "orcid": "0000-0001-8152-3943" }, { "id": "Ouchi-Masami", "name": { "family": "Ouchi", "given": "Masami" }, "orcid": "0000-0002-1049-6658" }, { "id": "Scarlata-Claudia-M", "name": { "family": "Scarlata", "given": "Claudia" }, "orcid": "0000-0002-9136-8876" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "CLASSY III. The Properties of Starburst-driven Warm Ionized Outflows", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxy evolution; Galaxy kinematics; Galaxy dynamics; Starburst galaxies; Ultraviolet astronomy; Galaxy spectroscopy; Galactic winds; Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2022 February 7; revised 2022 April 19; accepted 2022 May 4; published 2022 July 15. \n\nBased on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc.,\nunder NASA contract NAS 5-26555.\n\nThe CLASSY team is grateful for the support of this program, HST-GO-15840, provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. B.L.J. thanks the European Space Agency (ESA) for its support. The CLASSY Collaboration extends special gratitude to the Lorentz Center for useful discussions during the \"Characterizing Galaxies with Spectroscopy with a view for JWST\" 2017 workshop that led to the formation of the CLASSY Collaboration and survey. \n\nFunding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/. \n\nSDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration, including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. \n\nThis research has made use of the HSLA database, developed and maintained at STScI, Baltimore, MD, USA. \n\nWe also thank the anonymous referee for the insightful comments on the paper. \n\nFacilities: HST (COS) - , LBT (MODS) - , APO (SDSS) - , KECK (ESI) - , VLT (MUSE - , VIMOS) - . \n\nSoftware: astropy (Astropy Collaboration et al. 2018) BEAGLE (Chevallard & Charlot 2016), CalCOS (STScI), dustmaps (Green 2018), jupyter (Kluyver et al. 2016), MPFIT (Markwardt 2009), Photutils (Bradley et al. 2021), python (Van Rossum & Drake 2009), pysynphot (STScI Development Team 2013).\n\nPublished - Xu_2022_ApJ_933_222.pdf
Accepted Version - 2204.09181.pdf
", "abstract": "We report the results of analyses of galactic outflows in a sample of 45 low-redshift starburst galaxies in the COS Legacy Archive Spectroscopic SurveY (CLASSY), augmented by five additional similar starbursts with Cosmic Origins Spectrograph (COS) data. The outflows are traced by blueshifted absorption lines of metals spanning a wide range of ionization potential. The high quality and broad spectral coverage of CLASSY data enable us to disentangle the absorption due to the static interstellar medium (ISM) from that due to outflows. We further use different line multiplets and doublets to determine the covering fraction, column density, and ionization state as a function of velocity for each outflow. We measure the outflow's mean velocity and velocity width, and find that both correlate in a highly significant way with the star formation rate, galaxy mass, and circular velocity over ranges of four orders of magnitude for the first two properties. We also estimate outflow rates of metals, mass, momentum, and kinetic energy. We find that, at most, only about 20% of silicon created and ejected by supernovae in the starburst is carried out in the warm phase we observe. The outflows' mass-loading factor increases steeply and inversely with both circular and outflow velocity (log\u2013log slope \u223c\u22121.6), and reaches \u223c10 for dwarf galaxies. We find that the outflows typically carry about 10%\u2013100% of the momentum injected by massive stars and about 1%\u201320% of the kinetic energy. We show that these results place interesting constraints on, and new insights into, models and simulations of galactic winds.", "date": "2022-07-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "933", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 222", "id_number": "CaltechAUTHORS:20220727-38096000", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220727-38096000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-15840" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ac6d56", "primary_object": { "basename": "2204.09181.pdf", "url": "https://authors.library.caltech.edu/records/2wdj2-v8v82/files/2204.09181.pdf" }, "related_objects": [ { "basename": "Xu_2022_ApJ_933_222.pdf", "url": "https://authors.library.caltech.edu/records/2wdj2-v8v82/files/Xu_2022_ApJ_933_222.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Xu, Xinfeng; Heckman, Timothy; et el." }, { "id": "https://authors.library.caltech.edu/records/4pn50-77y72", "eprint_id": 116017, "eprint_status": "archive", "datestamp": "2023-08-22 16:41:25", "lastmod": "2023-10-24 20:57:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Runco-Jordan-N", "name": { "family": "Runco", "given": "Jordan N." }, "orcid": "0000-0003-4852-8958" }, { "id": "Reddy-Naveen-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Shapley-Alice-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Sanders-Ryan-L", "name": { "family": "Sanders", "given": "Ryan L." }, "orcid": "0000-0003-4792-9119" }, { "id": "Strom-Allison-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Coil-Alison-L", "name": { "family": "Coil", "given": "Alison L." }, "orcid": "0000-0002-2583-5894" }, { "id": "Kriek-Mariska", "name": { "family": "Kriek", "given": "Mariska" }, "orcid": "0000-0002-7613-9872" }, { "id": "Mobasher-Bahram", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Pettini-Max", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Rudie-Gwen-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Siana-Brian-D", "name": { "family": "Siana", "given": "Brian" }, "orcid": "0000-0002-4935-9511" }, { "id": "Topping-Michael-W", "name": { "family": "Topping", "given": "Michael W." }, "orcid": "0000-0001-8426-1141" }, { "id": "Trainor-Ryan-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Freeman-William-R", "name": { "family": "Freeman", "given": "William R." }, "orcid": "0000-0003-3559-5270" }, { "id": "Shivaei-Irene", "name": { "family": "Shivaei", "given": "Irene" }, "orcid": "0000-0003-4702-7561" }, { "id": "Azadi-Mojegan", "name": { "family": "Azadi", "given": "Mojegan" }, "orcid": "0000-0001-6004-9728" }, { "id": "Price-Sedona-H", "name": { "family": "Price", "given": "Sedona H." }, "orcid": "0000-0002-0108-4176" }, { "id": "Leung-Gene-C-K", "name": { "family": "Leung", "given": "Gene C. K." }, "orcid": "0000-0002-9393-6507" }, { "id": "Fetherolf-Tara", "name": { "family": "Fetherolf", "given": "Tara" }, "orcid": "0000-0002-3551-279X" }, { "id": "de-Groot-Laura", "name": { "family": "de\u00a0Groot", "given": "Laura" } }, { "id": "Zick-Tom", "name": { "family": "Zick", "given": "Tom" } }, { "id": "Fornasini-Francesca-M", "name": { "family": "Fornasini", "given": "Francesca M." }, "orcid": "0000-0002-9286-9963" }, { "id": "Barro-Guillermo", "name": { "family": "Barro", "given": "Guillermo" }, "orcid": "0000-0001-6813-875X" } ] }, "title": "Reconciling the results of the z \u223c 2 MOSDEF and KBSS-MOSFIRE Surveys", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: high-redshift, galaxies: ISM; Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model).\n\nReceived: 17 December 2021. Revision received: 12 April 2022. Accepted: 13 April 2022. Published: 29 April 2022. \n\nWe acknowledge support from NSF AAG grants AST1312780, 1312547, 1312764, 1313171, 1313472, 2009313, 2009085, and 2009278; grant AR-13907 from the Space Telescope Science Institute; and grant NNX16AF54G from the NASA ADAP program. We also acknowledge a NASA contract supporting the 'WFIRST Extragalactic Potential Observations (EXPO) Science Investigation Team' (15-WFIRST15-0004), administered by GSFC. Support for this work was also provided through the NASA Hubble Fellowship grant #HST-HF2-51469.001-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. We thank the 3D-HST collaboration, who provided spectroscopic and photometric catalogues used to select MOSDEF targets and to derive stellar population parameters. We acknowledge the First Carnegie Symposium in Honor of Leonard Searle for useful information and discussions that benefited this work. This research made use of ASTROPY,3 a community-developed core PYTHON package for Astronomy (Astropy Collaboration 2013, 2018). Finally, we wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Based on data obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration, and was made possible by the generous financial support of the W.M. Keck Foundation. \n\nFacilities: Keck/MOSFIRE, Keck/LRIS, SDSS \n\nSoftware: Astropy (Astropy Collaboration 2013, 2018), Corner (Foreman-Mackey 2016), IPYTHON (Perez & Granger 2007), IRAF (Tody 1986, 1993), MATPLOTLIB (Hunter 2007), NUMPY (van der Walt, Colbert & Varoquaux 2011; Harris et al. 2020), PANDAS (pandas development team 2020), SciPy (Oliphant 2007; Millman & Aivazis 2011; Virtanen et al. 2020). Based on data obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration, and was made possible by the generous financial support of the W.M. Keck Foundation. \n\nDATA AVAILABILITY. The data underlying this article will be shared on reasonable request to the corresponding author.\n\nPublished - stac1115.pdf
Accepted Version - 2112.09715.pdf
", "abstract": "The combination of the MOSDEF and KBSS-MOSFIRE surveys represents the largest joint investment of Keck/MOSFIRE time to date, with \u223c3000 galaxies at 1.4 \u2272 z \u2272 3.8, roughly half of which are at z \u223c 2. MOSDEF is photometric- and spectroscopic-redshift selected with a rest-optical magnitude limit, while KBSS-MOSFIRE is primarily selected based on rest-UV colours and a rest-UV magnitude limit. Analysing both surveys in a uniform manner with consistent spectral-energy-distribution (SED) models, we find that the MOSDEF z \u223c 2 targeted sample has higher median M* and redder rest U\u2212V colour than the KBSS-MOSFIRE z \u223c 2 targeted sample, and smaller median SED-based SFR and sSFR (SFR(SED) and sSFR(SED)). Specifically, MOSDEF targeted a larger population of red galaxies with U\u2212V and V\u2212J \u22651.25, while KBSS-MOSFIRE contains more young galaxies with intense star formation. Despite these differences in the z \u223c 2 targeted samples, the subsets of the surveys with multiple emission lines detected and analysed in previous work are much more similar. All median host-galaxy properties with the exception of stellar population age \u2013 i.e. M*, SFR(SED), sSFR(SED), AV, and UVJ colours \u2013 agree within the uncertainties. Additionally, when uniform emission-line fitting and stellar Balmer absorption correction techniques are applied, there is no significant offset between both samples in the [O\u2009iii]\u03bb5008/H\u2009\u03b2 versus [N\u2009ii]\u03bb6585/H\u2009\u03b1 diagnostic diagram, in contrast to previously reported discrepancies. We can now combine the MOSDEF and KBSS-MOSFIRE surveys to form the largest z \u223c 2 sample with moderate-resolution rest-optical spectra and construct the fundamental scaling relations of star-forming galaxies during this important epoch.", "date": "2022-07", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "513", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "3871-3892", "id_number": "CaltechAUTHORS:20220802-742857000", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220802-742857000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1312780" }, { "agency": "NSF", "grant_number": "AST-1312547" }, { "agency": "NSF", "grant_number": "AST-1312764" }, { "agency": "NSF", "grant_number": "AST-1313171" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "NSF", "grant_number": "AST-2009313" }, { "agency": "NSF", "grant_number": "AST-2009085" }, { "agency": "NSF", "grant_number": "AST-2009278" }, { "agency": "NSF", "grant_number": "AR-13907" }, { "agency": "NASA", "grant_number": "NNX16AF54G" }, { "agency": "NASA", "grant_number": "15-WFIRST15-0004" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF2-51469.001" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/stac1115", "primary_object": { "basename": "2112.09715.pdf", "url": "https://authors.library.caltech.edu/records/4pn50-77y72/files/2112.09715.pdf" }, "related_objects": [ { "basename": "stac1115.pdf", "url": "https://authors.library.caltech.edu/records/4pn50-77y72/files/stac1115.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Runco, Jordan N.; Reddy, Naveen A.; et el." }, { "id": "https://authors.library.caltech.edu/records/9dmga-rhb38", "eprint_id": 110565, "eprint_status": "archive", "datestamp": "2023-08-20 08:06:44", "lastmod": "2023-10-23 19:43:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Li-Zhihui", "name": { "family": "Li", "given": "Zhihui" }, "orcid": "0000-0001-5113-7558" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Gronke-Max", "name": { "family": "Gronke", "given": "Max" }, "orcid": "0000-0003-2491-060X" }, { "id": "Chen-Yuguang", "name": { "family": "Chen", "given": "Yuguang" }, "orcid": "0000-0003-4520-5395" }, { "id": "Matsuda-Yuichi", "name": { "family": "Matsuda", "given": "Yuichi" }, "orcid": "0000-0003-1747-2891" } ] }, "title": "Where outflows meet inflows: gas kinematics in SSA22 Ly \u03b1 blob 2 decoded by advanced radiative transfer modelling", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: e volution \u2013galaxies: high-redshift \u2013intergalactic medium \u2013galaxies: kinematics and dynamics", "note": "\u00a9 2022 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2022 March 28. Received 2022 February 24; in original form 2021 April 21. Published: 08 April 2022. \n\nWe thank the anonymous referee for carefully reading our manuscript and providing constructive feedback, which significantly improved the quality of this paper. We thank Phil Hopkins for providing computational resources. ZL, CCS, and YC acknowledge financial support by NSF grant AST-2009278. YM acknowledges support from JSPS KAKENHI Grant (17H04831, 17KK0098, 19H00697, and 20H01953). The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We are also grateful to the dedicated staff of the W.M. Keck Observatory who keep the instruments and telescopes running effectively. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409 awarded 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. Numerical calculations were run on the Caltech compute cluster 'Wheeler,' allocations from XSEDE TG-AST130039 and PRAC NSF.1713353 supported by the NSF and NASA HEC SMD-16-7592. This research made use of Montage. It is funded by the National Science Foundation under Grant Number ACI-1440620, and was previously funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology. We also acknowledge the use of the following software packages: ASTROPY (Astropy Collaboration et al. 2018), the SCIPY and NUMPY system (Virtanen et al. 2020; Harris et al. 2020), seaborn (Waskom 2021) and QFitsView.24 \n\nData Availability: The data underlying this article will be shared on reasonable request to the corresponding author.\n\nPublished - stac958.pdf
Submitted - 2104.10682.pdf
", "abstract": "We present new spectroscopic observations of Ly \u03b1 (Ly \u03b1) Blob 2 (z \u223c 3.1). We observed extended Ly \u03b1 emission in three distinct regions, where the highest Ly \u03b1 surface brightness (SB) centre is far away from the known continuum sources. We searched through the MOSFIRE slits that cover the high Ly \u03b1 SB regions, but were unable to detect any significant nebular emission near the highest SB centre. We further mapped the flux ratio of the blue peak to the red peak and found it is anticorrelated with Ly \u03b1 SB with a power-law index of \u223c \u20130.4. We used radiative transfer models with both multiphase, clumpy, and shell geometries and successfully reproduced the diverse Ly \u03b1 morphologies. We found that most spectra suggest outflow-dominated kinematics, while 4/15 spectra imply inflows. A significant correlation exists between parameter pairs, and the multiphase, clumpy model may alleviate previously reported discrepancies. We also modelled Ly \u03b1 spectra at different positions simultaneously and found that the variation of the inferred clump outflow velocities can be approximately explained by line-of-sight projection effects. Our results support the 'central powering + scattering' scenario, i.e. the Ly \u03b1 photons are generated by a central powering source and then scatter with outflowing, multiphase H\u2009 I gas while propagating outwards. The infalling of cool gas near the blob outskirts shapes the observed blue-dominated Ly \u03b1 profiles, but its energy contribution to the total Ly \u03b1 luminosity is less than 10 per\u2009cent, i.e. minor compared to the photoionization by star-forming galaxies and/or AGNs.", "date": "2022-07", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "513", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "3414-3428", "id_number": "CaltechAUTHORS:20210825-184654591", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210825-184654591", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-2009278" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17H04831" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17KK0098" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19H00697" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20H01953" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF2-51409" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NSF", "grant_number": "TG-AST130039" }, { "agency": "NSF", "grant_number": "OAC-1713353" }, { "agency": "NASA", "grant_number": "SMD-16-7592" }, { "agency": "NSF", "grant_number": "ACI-1440620" }, { "agency": "NASA/Caltech", "grant_number": "NCC5-626" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/stac958", "primary_object": { "basename": "2104.10682.pdf", "url": "https://authors.library.caltech.edu/records/9dmga-rhb38/files/2104.10682.pdf" }, "related_objects": [ { "basename": "stac958.pdf", "url": "https://authors.library.caltech.edu/records/9dmga-rhb38/files/stac958.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Li, Zhihui; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/e6nbf-yb608", "eprint_id": 113773, "eprint_status": "archive", "datestamp": "2023-10-09 20:58:49", "lastmod": "2023-10-24 16:29:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nu\u00f1ez-Evan-H", "name": { "family": "Nu\u00f1ez", "given": "Evan H." }, "orcid": "0000-0001-5595-757X" }, { "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "orcid": "0000-0001-6196-5162" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Empirical Constraints on Core-collapse Supernova Yields Using Very Metal-poor Damped Ly\u03b1 Absorbers", "ispublished": "pub", "full_text_status": "public", "keywords": "Core-collapse supernovae; Damped Lyman-alpha systems; Quasar absorption line spectroscopy; Population III stars; Nucleosynthesis; Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 August 1; revised 2021 November 29; accepted 2021 December 7; published 2022 March 4. \n\nWe thank Tuguldur Sukhbold for in-depth comments and correspondence that significantly improved this work. We thank Ryan Cooke, Louise Welsh, Donatella Romano, Carl Fields, Lynne Hillenbrand, and Sanjana Curtis for thoughtful conversations and for sharing information and data that improved the quality of this work. We thank our referee for helpful comments that improved this paper. E.H.N. acknowledges the support of the NSF Graduate Research Fellowship Program. This material is based upon work supported by the National Science Foundation under grant No. AST-1847909. E.N.K. gratefully acknowledges support from a Cottrell Scholar award administered by the Research Corporation for Science Advancement. \n\nSoftware: Astropy (Astropy Collaboration et al. 2013, 2018).\n\nPublished - Nunez_2022_ApJ_927_64.pdf
Submitted - 2108-00659.pdf
", "abstract": "We place empirical constraints on the yields from zero- and low-metallicity core-collapse supernovae (CCSNe) using abundances measured in very metal-poor (VMP; [Fe/H] \u2264 \u22122) damped Ly\u03b1 absorbers (DLAs). For some abundance ratios ([N,Al,S/Fe]), VMP DLAs constrain the metal yields of the first SNe more reliably than VMP stars. We compile a large sample of high-S/N VMP DLAs from over 30 yr of literature, most with high-resolution spectral measurements. We infer the initial-mass-function-averaged CCSNe yield from the median values from the DLA abundance ratios of C, N, O, Al, Si, S, and Fe (over Fe and O). We assume that the DLAs are metal-poor enough that they represent galaxies in their earliest stages of evolution, when CCSNe are the only nucleosynthetic sources of the metals we analyze. We compare five sets of zero- and low-metallicity theoretical yields to the empirical yields derived in this work. We find that the five models agree with the DLA yields for ratios containing Si and S. Only one model (Heger & Woosley 2010, hereafter HW10) reproduced the DLA values for N, and one other model (Limongi & Chieffi 2018, hereafter LC18) reproduced [N/O]. We found little change in the theoretical yields with the adoption of an SN explosion landscape (where certain progenitor masses collapse into black holes, contributing no yields) onto HW10, but fixing explosion energy to progenitor mass results in wide disagreements between the predictions and DLA abundances. We investigate the adoption of a simple, observationally motivated initial distribution of rotational velocities for LC18 and find a slight improvement.", "date": "2022-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "927", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 64", "id_number": "CaltechAUTHORS:20220307-189105000", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220307-189105000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NSF", "grant_number": "AST-1847909" }, { "agency": "Cottrell Scholar of Research Corporation" } ] }, "doi": "10.3847/1538-4357/ac470e", "primary_object": { "basename": "2108-00659.pdf", "url": "https://authors.library.caltech.edu/records/e6nbf-yb608/files/2108-00659.pdf" }, "related_objects": [ { "basename": "Nunez_2022_ApJ_927_64.pdf", "url": "https://authors.library.caltech.edu/records/e6nbf-yb608/files/Nunez_2022_ApJ_927_64.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Nu\u00f1ez, Evan H.; Kirby, Evan N.; et el." }, { "id": "https://authors.library.caltech.edu/records/ybnrp-k4s60", "eprint_id": 113350, "eprint_status": "archive", "datestamp": "2023-08-22 13:56:30", "lastmod": "2023-10-23 23:03:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Reddy-Naveen-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Topping-Michael-W", "name": { "family": "Topping", "given": "Michael W." } }, { "id": "Shapley-Alice-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Sanders-Ryan-L", "name": { "family": "Sanders", "given": "Ryan L." }, "orcid": "0000-0003-4792-9119" }, { "id": "Du-Xinnan", "name": { "family": "Du", "given": "Xinnan" }, "orcid": "0000-0001-5554-5444" }, { "id": "Coil-Alison-L", "name": { "family": "Coil", "given": "Alison L." }, "orcid": "0000-0002-2583-5894" }, { "id": "Mobasher-Bahram", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Price-Sedona-H", "name": { "family": "Price", "given": "Sedona H." }, "orcid": "0000-0002-0108-4176" }, { "id": "Shivaei-Irene", "name": { "family": "Shivaei", "given": "Irene" }, "orcid": "0000-0003-4702-7561" } ] }, "title": "The Effects of Stellar Population and Gas Covering Fraction on the Emergent Ly\u03b1 Emission of High-redshift Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "Stellar abundances; Interstellar abundances; H II regions; High-redshift galaxies; Interstellar medium; Star formation; Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 August 11; revised 2021 November 17; accepted 2021 November 17; published 2022 February 9. \n\nWe acknowledge support from NSF AAG grants AST1312780, 1312547, 1312764, and 1313171; grant AR13907 from the Space Telescope Science Institute; and grant NNX16AF54G from the NASA ADAP program. This work made use of v2.2.1 of the Binary Population and Spectral Synthesis (BPASS) models, as described in Eldridge et al. (2017) and Stanway & Eldridge (2018), and v17.02 of the Cloudy radiative transfer code (Ferland et al. 2017). We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible.\n\nPublished - Reddy_2022_ApJ_926_31.pdf
Accepted Version - 2108.05363.pdf
", "abstract": "We perform joint modeling of the composite rest-frame far-UV and optical spectra of redshift 1.85 \u2264 z \u2264 3.49 star-forming galaxies to deduce key properties of the massive stars, ionized interstellar medium (ISM), and neutral ISM, with the aim of investigating the principal factors affecting the production and escape of Ly\u03b1 photons. Our sample consists of 136 galaxies with deep Keck/LRIS and MOSFIRE spectra covering, respectively, Ly\u03b2 through C iii] \u03bb\u03bb1907, 1909 and [O ii], [Ne iii], H\u03b2, [O iii], H\u03b1, [N ii], and [S ii]. Spectral and photoionization modeling indicates that the galaxies are uniformly consistent with stellar population synthesis models that include the effects of stellar binarity. Over the dynamic range of our sample, there is little variation in stellar and nebular abundance with Ly\u03b1 equivalent width, W_\u03bb(Ly\u03b1), and only a marginal anticorrelation between age and W_\u03bb(Ly\u03b1). The inferred range of ionizing spectral shapes is insufficient to solely account for the variation in W_\u03bb(Ly\u03b1); rather, the covering fraction of optically thick H i appears to be the principal factor modulating the escape of Ly\u03b1, with most of the Ly\u03b1 photons in down-the-barrel observations of galaxies escaping through low column density or ionized channels in the ISM. Our analysis shows that a high star-formation-rate surface density, \u03a3_(SFR), particularly when coupled with a low galaxy potential (i.e., low stellar mass), can aid in reducing the covering fraction and ease the escape of Ly\u03b1 photons. We conclude with a discussion of the implications of our results for the escape of ionizing radiation at high redshift.", "date": "2022-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "926", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 31", "id_number": "CaltechAUTHORS:20220209-266204000", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220209-266204000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1312780" }, { "agency": "NSF", "grant_number": "AST-1312547" }, { "agency": "NSF", "grant_number": "AST-1312764" }, { "agency": "NSF", "grant_number": "AST-1313171" }, { "agency": "NASA", "grant_number": "AR13907" }, { "agency": "NASA", "grant_number": "NNX16AF54G" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ac3b4c", "primary_object": { "basename": "2108.05363.pdf", "url": "https://authors.library.caltech.edu/records/ybnrp-k4s60/files/2108.05363.pdf" }, "related_objects": [ { "basename": "Reddy_2022_ApJ_926_31.pdf", "url": "https://authors.library.caltech.edu/records/ybnrp-k4s60/files/Reddy_2022_ApJ_926_31.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Reddy, Naveen A.; Topping, Michael W.; et el." }, { "id": "https://authors.library.caltech.edu/records/7rgwn-p8n07", "eprint_id": 113259, "eprint_status": "archive", "datestamp": "2023-08-22 13:51:29", "lastmod": "2023-10-23 23:00:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Strom-Allison-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Rudie-Gwen-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Trainor-Ryan-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" } ] }, "title": "Chemical Abundance Scaling Relations for Multiple Elements in z \u2243 2\u20133 Star-forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxy abundances; High-redshift galaxies; Scaling relations; Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 September 18; revised 2021 November 7; accepted 2021 November 9; published 2022 January 31. \n\nThe data presented in this paper were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership between the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. This work has also been supported in part by the US National Science Foundation (NSF) through grants AST-0908805 and AST-1313472 (ALS and CCS). The authors wish to recognize and acknowledge the significant cultural role and reverence that the summit of Maunakea has within the indigenous Hawaiian community. We are privileged to have had the opportunity to conduct observations from this mountain. \n\nFacilities: Keck:I (LRIS - , MOSFIRE) - , Magellan:Baade (FourStar) - , Hale (WIRC) - , Spitzer (IRAC), HST (WFC3). - \n\nSoftware: GalDNA, LINMIX_ERR (Kelly 2007), BPASSv2 (Eldridge & Stanway 2016; Stanway et al. 2016), Cloudy (Ferland et al. 2013), BC03 (Bruzual & Charlot 2003).\n\nPublished - Allison_L._Strom_et_al_2022_ApJ_925_116.pdf
Accepted Version - 2111.06410.pdf
", "abstract": "The chemical abundance patterns of gas and stars in galaxies are powerful probes of galaxies' star formation histories and the astrophysics of galaxy assembly but are challenging to measure with confidence in distant galaxies. In this paper, we report the first measurements of the correlation between stellar mass (M_*) and multiple tracers of chemical enrichment (including O, N, and Fe) in individual z \u223c 2\u20133 galaxies, using a sample of 195 star-forming galaxies from the Keck Baryonic Structure Survey. The galaxies' chemical abundances are inferred using photoionization models capable of reconciling high-redshift galaxies' observed extreme rest-UV and rest-optical spectroscopic properties. We find that the M_*\u2013O/H relation for our sample is relatively shallow, with moderately large scatter, and is offset \u223c0.35 dex higher than the corresponding M_*\u2013Fe/H relation. The two relations have very similar slopes, indicating a high level of \u03b1-enhancement\u2014O/Fe \u2248 2.2 \u00d7 (O/Fe)_\u2299\u2014across two decades in M_*. The M_*\u2013N/H relation has the steepest slope and largest intrinsic scatter, which likely results from the fact that many z \u223c 2 galaxies are observed near or past the transition from \"primary\" to \"secondary\" N production, and may reflect uncertainties in the astrophysical origin of N. Together, these results suggest that z \u223c 2 galaxies are old enough to have seen substantial enrichment from intermediate-mass stars, but are still young enough that Type Ia supernovae have not had time to contribute significantly to their enrichment.", "date": "2022-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "925", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 116", "id_number": "CaltechAUTHORS:20220203-318352000", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220203-318352000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ac38a3", "primary_object": { "basename": "2111.06410.pdf", "url": "https://authors.library.caltech.edu/records/7rgwn-p8n07/files/2111.06410.pdf" }, "related_objects": [ { "basename": "Allison_L._Strom_et_al_2022_ApJ_925_116.pdf", "url": "https://authors.library.caltech.edu/records/7rgwn-p8n07/files/Allison_L._Strom_et_al_2022_ApJ_925_116.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Strom, Allison L.; Rudie, Gwen C.; et el." }, { "id": "https://authors.library.caltech.edu/records/9ctyx-2jw96", "eprint_id": 110564, "eprint_status": "archive", "datestamp": "2023-08-20 05:47:23", "lastmod": "2023-10-23 19:43:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chen-Yuguang", "name": { "family": "Chen", "given": "Yuguang" }, "orcid": "0000-0003-4520-5395" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Erb-Dawn-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Law-David-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" }, { "id": "Trainor-Ryan-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Reddy-Naveen-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Shapley-Alice-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Pahl-Anthony-J", "name": { "family": "Pahl", "given": "Anthony J." }, "orcid": "0000-0003-4464-4505" }, { "id": "Strom-Allison-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Lamb-Noah-R", "name": { "family": "Lamb", "given": "Noah R." }, "orcid": "0000-0002-2052-822X" }, { "id": "Li-Zhihui", "name": { "family": "Li", "given": "Zhihui" }, "orcid": "0000-0001-5113-7558" }, { "id": "Rudie-Gwen-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" } ] }, "title": "The KBSS\u2013KCWI survey: the connection between extended Ly\u2009\u03b1 haloes and galaxy azimuthal angle at z \u223c 2\u20133", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: ISM, galaxies: high-redshift", "note": "\u00a9 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. \n\nReceived: 19 April 2021; Revision received: 14 August 2021; Accepted: 14 August 2021; Published: 19 August 2021. \n\nThis work has included data from Keck/KCWI (Morrissey et al. 2018), Keck/OSIRIS (Larkin et al. 2006), Keck/MOSFIRE (McLean et al. 2012), Keck/LRIS-B (Steidel et al. 2004), HST/WFC3-IR, and HST/ACS. We appreciate the contribution from the staff of the W. M. Keck Observatory and the Space Telescope Science Institute. \n\nThe following software packages have been crucial to the results presented: Astropy (Astropy Collaboration 2018), the SciPy and NumPy system (Harris et al. 2020; Virtanen et al. 2020), QFitsView,9 CWITools (O'Sullivan & Chen 2020), Montage,10GALFIT (Peng et al. 2002, 2010), and DrizzlePac. \n\nThis work has been supported in part by grant AST-2009278 from the US NSF, by NASA through grant HST-GO15287.001, and the JPL/Caltech President's and Director's Program (YC, CS). \n\nThe authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We would like to thank the anonymous referee for providing constructive feedback. We would like to acknowledge Kurt Adelberger, Milan Bogosavljevi\u0107, Max Pettini, and Rachel Theios for their contribution to the KBSS survey. It is a great pleasure for us to thank Don Neill, Mateusz Matuszewski, Luca Rizzi, Donal O'Sullivan, and Sebastiano Cantalupo for their help in handling the KCWI data, and Cameron Hummels and Max Gronke for insightful discussions. YC would like to acknowledge his grandfather, Chen Yizong, who passed away during the preparation of this manuscript. \n\nBased on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. \n\nData Availability: The composite CP2D spectra and the PYTHON program used to generate figures in this article are available upon reasonable request.\n\nPublished - stab2383.pdf
Accepted Version - 2104.10173.pdf
", "abstract": "We present the first statistical analysis of kinematically resolved, spatially extended Ly\u03b1 emission around z = 2\u20133 galaxies in the Keck Baryonic Structure Survey (KBSS) using the Keck Cosmic Web Imager (KCWI). Our sample of 59 star-forming galaxies (z_(med) = 2.29) comprises the subset with typical KCWI integration times of \u223c5 h and with existing imaging data from the Hubble Space Telescope and/or adaptive optics-assisted integral field spectroscopy. The high-resolution images were used to evaluate the azimuthal dependence of the diffuse Ly\u03b1 emission with respect to the stellar continuum within projected galactocentric distances of \u227230 proper kpc. We introduce cylindrically projected 2D spectra (CP2D) that map the averaged Ly\u03b1 spectral profile over a specified range of azimuthal angle, as a function of impact parameter around galaxies. The averaged CP2D spectrum of all galaxies shows clear signatures of Ly\u03b1 resonant scattering by outflowing gas. We stacked the CP2D spectra of individual galaxies over ranges of azimuthal angle with respect to their major axes. The extended Ly\u03b1 emission along the galaxy principal axes is statistically indistinguishable, with residual asymmetry of \u22642 per\u2009cent (\u223c2\u03c3) of the integrated Ly\u03b1 emission. The symmetry implies that the Ly\u03b1 scattering medium is dominated by outflows in all directions within 30 kpc. Meanwhile, we find that the blueshifted component of Ly\u03b1 emission is marginally stronger along galaxy minor axes for galaxies with relatively weak Ly\u03b1 emission. We speculate that this weak directional dependence of Ly\u03b1 emission becomes discernible only when the Ly\u03b1 escape fraction is low. These discoveries highlight the need for similar analyses in simulations with Ly\u03b1 radiative transfer modelling.", "date": "2021-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "508", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "19-43", "id_number": "CaltechAUTHORS:20210825-184651133", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210825-184651133", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NSF", "grant_number": "AST-2009278" }, { "agency": "NASA", "grant_number": "HST-GO15287.001" }, { "agency": "JPL President and Director's Fund" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/stab2383", "primary_object": { "basename": "stab2383.pdf", "url": "https://authors.library.caltech.edu/records/9ctyx-2jw96/files/stab2383.pdf" }, "related_objects": [ { "basename": "2104.10173.pdf", "url": "https://authors.library.caltech.edu/records/9ctyx-2jw96/files/2104.10173.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Chen, Yuguang; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/0m2tq-aec75", "eprint_id": 111357, "eprint_status": "archive", "datestamp": "2023-08-22 11:16:05", "lastmod": "2023-10-23 20:32:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kubo-Mariko", "name": { "family": "Kubo", "given": "Mariko" }, "orcid": "0000-0002-7598-5292" }, { "id": "Umehata-Hideki", "name": { "family": "Umehata", "given": "Hideki" }, "orcid": "0000-0003-1937-0573" }, { "id": "Matsuda-Yuichi", "name": { "family": "Matsuda", "given": "Yuichi" }, "orcid": "0000-0003-1747-2891" }, { "id": "Kajisawa-Masaru", "name": { "family": "Kajisawa", "given": "Masaru" }, "orcid": "0000-0002-1732-6387" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Yamada-Toru", "name": { "family": "Yamada", "given": "Toru" } }, { "id": "Tanaka-Ichi", "name": { "family": "Tanaka", "given": "Ichi" }, "orcid": "0000-0002-4937-4738" }, { "id": "Hatsukade-Bunyo", "name": { "family": "Hatsukade", "given": "Bunyo" }, "orcid": "0000-0001-6469-8725" }, { "id": "Tamura-Yoichi", "name": { "family": "Tamura", "given": "Yoichi" }, "orcid": "0000-0003-4807-8117" }, { "id": "Nakanishi-Kouichiro", "name": { "family": "Nakanishi", "given": "Kouichiro" }, "orcid": "0000-0002-6939-0372" }, { "id": "Kohno-Kotaro", "name": { "family": "Kohno", "given": "Kotaro" }, "orcid": "0000-0002-4052-2394" }, { "id": "Lee-Kianhong", "name": { "family": "Lee", "given": "Kianhong" }, "orcid": "0000-0003-4814-0101" }, { "id": "Matsuda-Keiichi", "name": { "family": "Matsuda", "given": "Keiichi" } } ] }, "title": "A Massive Quiescent Galaxy Confirmed in a Protocluster at z = 3.09", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxy evolution; Galaxy environments; Giant elliptical galaxies; Protoclusters", "note": "\u00a9 2021. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 January 9; revised 2021 June 17; accepted 2021 June 18; published 2021 September 16. \n\nWe thank the anonymous referee for a number of useful suggestions. This work is supported by JSPS KAKENHI grant Numbers 20K14530 (MK), 17K14252, 20H01953 (HU), 17KK0098 (YM), 19K0397 (KN), and 17H06130 (KK). The spectroscopic data were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The observations were carried out within the framework of Subaru-Keck/Subaru-Gemini time exchange program, which is operated by the National Astronomical Observatory of Japan. The K_s-band image was collected with nuMOIRCS at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. We are honored and grateful for the opportunity of observing the universe from Maunakea, which has cultural, historical, and natural significance in Hawaii. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00162.S, ADS/JAO.ALMA#2017.1.01332.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The F814W-band image is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555.\n\nPublished - Kubo_2021_ApJ_919_6.pdf
Accepted Version - 2106.10798.pdf
", "abstract": "We report a massive quiescent galaxy at z_(spec) = 3.0922^(+0.008)_(\u22120.004) spectroscopically confirmed at a protocluster in the SSA22 field by detecting the Balmer and Ca II absorption features with the multi-object spectrometer for infrared exploration on the Keck I telescope. This is the most distant quiescent galaxy confirmed in a protocluster to date. We fit the optical to mid-infrared photometry and spectrum simultaneously with spectral energy distribution (SED) models of parametric and nonparametric star formation histories (SFHs). Both models fit the observed SED well and confirm that this object is a massive quiescent galaxy with a stellar mass of log(M\u22c6/M_\u2299) = 11.26^(+0.03)_(\u22120.04) and 11.54^(+0.03)_(\u22120.00), and a star formation rate of SFR/M_\u2299 yr\u207b\u00b9 < 0.3 and = 0.01^(+0.03)_(\u22120.01) for parametric and nonparametric models, respectively. The SFH from the former modeling is described as an instantaneous starburst whereas that of the latter modeling is longer-lived, but both models agree with a sudden quenching of the star formation at \u223c0.6 Gyr ago. This massive quiescent galaxy is confirmed in an extremely dense group of galaxies predicted as a progenitor of a brightest cluster galaxy formed via multiple mergers in cosmological numerical simulations. We discover three new plausible [O III]\u03bb5007 emitters at 3.0791 \u2264 z_(spec) \u2264 3.0833 serendipitously detected around the target. Two of them just between the target and its nearest massive galaxy are possible evidence of their interactions. They suggest the future great size and stellar mass evolution of this massive quiescent galaxy via mergers.", "date": "2021-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "919", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 6", "id_number": "CaltechAUTHORS:20211011-195252309", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211011-195252309", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20K14530" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17K14252" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20H01953" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17KK0098" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19K0397" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17H06130" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ac0cf8", "primary_object": { "basename": "Kubo_2021_ApJ_919_6.pdf", "url": "https://authors.library.caltech.edu/records/0m2tq-aec75/files/Kubo_2021_ApJ_919_6.pdf" }, "related_objects": [ { "basename": "2106.10798.pdf", "url": "https://authors.library.caltech.edu/records/0m2tq-aec75/files/2106.10798.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Kubo, Mariko; Umehata, Hideki; et el." }, { "id": "https://authors.library.caltech.edu/records/eth6n-fq102", "eprint_id": 110903, "eprint_status": "archive", "datestamp": "2023-08-22 11:12:34", "lastmod": "2023-10-23 19:55:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Umehata-Hideki", "name": { "family": "Umehata", "given": "Hideki" }, "orcid": "0000-0003-1937-0573" }, { "id": "Smail-Ian-R", "name": { "family": "Smail", "given": "Ian" }, "orcid": "0000-0003-3037-257X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Hayes-Matthew", "name": { "family": "Hayes", "given": "Matthew" }, "orcid": "0000-0001-8587-218X" }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "Swinbank-A-Mark", "name": { "family": "Swinbank", "given": "A. M." }, "orcid": "0000-0003-1192-5837" }, { "id": "Ivison-Rob-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Nagao-Toru", "name": { "family": "Nagao", "given": "Toru" } }, { "id": "Kubo-Mariko", "name": { "family": "Kubo", "given": "Mariko" }, "orcid": "0000-0002-7598-5292" }, { "id": "Nakanishi-Kouichiro", "name": { "family": "Nakanishi", "given": "Kouichiro" }, "orcid": "0000-0002-6939-0372" }, { "id": "Matsuda-Yuichi", "name": { "family": "Matsuda", "given": "Yuichi" }, "orcid": "0000-0003-1747-2891" }, { "id": "Ikarashi-Soh", "name": { "family": "Ikarashi", "given": "Soh" } }, { "id": "Tamura-Yoichi", "name": { "family": "Tamura", "given": "Yoichi" }, "orcid": "0000-0003-4807-8117" }, { "id": "Geach-James-E", "name": { "family": "Geach", "given": "J. E." }, "orcid": "0000-0003-4964-4635" } ] }, "title": "ALMA Observations of Ly\u03b1 Blob 1: Multiple Major Mergers and Widely Distributed Interstellar Media", "ispublished": "pub", "full_text_status": "public", "keywords": "Interstellar medium; Intergalactic medium; Starburst galaxies; High-redshift galaxy clusters; Circumgalactic medium", "note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2021 April 12; revised 2021 June 22; accepted 2021 July 1; published 2021 September 9. \n\nWe wish to thank the anonymous referee for constructive comments that improved this paper. We acknowledges valuable discussion with Hidenobu Yajima. We thank Scott Chapman and Ken Mawatari for sharing calibrated optical-to-near-infrared images with us. H.U., Y.M. and K.N. acknowledge support from JSPS KAKENHI grant (17KK0098, 20H01953, 19K03937). I.R.S. acknowledges STFC through grant number ST/T000244/1. R.J.I. is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany's Excellence Strategy\u2014EXC-2094 \u2013390783311. This paper makes use of the following ALMA data: ADS/JAO.ALMA #2013.1.00704.S, #2013.1.00922.S, #2016.1.00485.S, #2016.1.01134.S, #2017.1.01209.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Our data are based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere. This research is based on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. We are honored and grateful for the opportunity of observing the universe from Maunakea, which is cultural, historical, and natural significance in Hawaii. This research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5\u201326555. \n\nFacilities: ALMA - Atacama Large Millimeter Array, Subaru - , VLT(MUSE) - , HST(STIS). - \n\nSoftware: astropy (Astropy Collaboration et al. 2013); casa (McMullin et al. 2007); MUSE pipeline (Weilbacher et al. 2016); mpdaf (Piqueras et al. 2017); (Bacon et al. 2016).\n\nPublished - Umehata_2021_ApJ_918_69.pdf
Accepted Version - 2107.01162.pdf
", "abstract": "We present observations of a giant Ly\u03b1 blob (LAB) in the SSA22 protocluster at z = 3.1, SSA22-LAB1, taken with the Atacama Large Millimeter/submillimeter Array. Dust continuum, along with [C ii] 158 \u03bcm and CO(4\u20133) line emission have been detected in LAB1, showing complex morphology and kinematics across a \u223c100 kpc central region. Seven galaxies at z = 3.0987\u20133.1016 in the surroundings are identified in [C ii] and dust continuum emission, with two of them potential companions or tidal structures associated with the most massive galaxies. Spatially resolved [C ii] and infrared luminosity ratios for the widely distributed media (L_[C\u026a\u026a]/L_(IR) \u2248 10\u207b\u00b2\u221210\u207b\u00b3) suggest that the observed extended interstellar media are likely to have originated from star formation activity and the contribution from shocked gas is probably not dominant. LAB1 is found to harbor a total molecular gas mass M_(mol) = (8.7 \u00b1 2.0) \u00d7 10\u00b9\u2070 M_\u2299, concentrated in the core region of the Ly\u03b1-emitting area. While (primarily obscured) star formation activity in the LAB1 core is one of the most plausible power sources for the Ly\u03b1 emission, multiple major mergers found in the core may also play a role in making LAB1 exceptionally bright and extended in Ly\u03b1 as a result of cooling radiation induced by gravitational interactions.", "date": "2021-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "918", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 69", "id_number": "CaltechAUTHORS:20210914-225410693", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210914-225410693", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17KK0098" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20H01953" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19K03937" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/T000244/1" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "EXC-2094 -390783311" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ac1106", "primary_object": { "basename": "2107.01162.pdf", "url": "https://authors.library.caltech.edu/records/eth6n-fq102/files/2107.01162.pdf" }, "related_objects": [ { "basename": "Umehata_2021_ApJ_918_69.pdf", "url": "https://authors.library.caltech.edu/records/eth6n-fq102/files/Umehata_2021_ApJ_918_69.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Umehata, Hideki; Smail, Ian; et el." }, { "id": "https://authors.library.caltech.edu/records/2n4cj-13937", "eprint_id": 110372, "eprint_status": "archive", "datestamp": "2023-08-20 04:29:00", "lastmod": "2023-10-23 19:37:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pahl-Anthony-J", "name": { "family": "Pahl", "given": "Anthony J." }, "orcid": "0000-0003-4464-4505" }, { "id": "Shapley-Alice-E", "name": { "family": "Shapley", "given": "Alice" }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Chen-Yuguang", "name": { "family": "Chen", "given": "Yuguang" }, "orcid": "0000-0003-4520-5395" }, { "id": "Reddy-Naveen-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" } ] }, "title": "An uncontaminated measurement of the escaping Lyman continuum at z \u223c 3", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift \u2013 dark ages, reionization, first stars \u2013 cosmology: observations", "note": "\u00a9 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2021 May 6. Received 2021 May 5; in original form 2021 April 5. Published: 22 May 2021. \n\nSupport for program HST-GO-15287.001 was provided by the National Aeronautics and Space Administration (NASA) through a grant from the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. CS and YC were supported in part by the Caltech/Jet Propulsion Laboratory President's and Director's program. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible. \n\nData Availability Statement: The HST data presented in this article are publicly available from the Mikulski Archive for Space Telescopes. The ground-based data presented here will be shared on reasonable request to the corresponding author.\n\nPublished - stab1374.pdf
Accepted Version - 2104.02081.pdf
", "abstract": "Observations of reionization-era analogues at z \u223c 3 are a powerful tool for constraining reionization. Rest-ultraviolet observations are particularly useful, in which both direct and indirect tracers of ionizing-photon production and escape can be observed. We analyse a sample of 124 z \u223c 3 galaxies from the Keck Lyman Continuum Spectroscopic Survey, with sensitive spectroscopic measurements of the Lyman continuum region. We present a method of removing foreground contamination from our sample using high-resolution, multiband Hubble Space Telescope imaging. We re-measure the global properties of the cleaned sample of 13 individually detected Lyman continuum sources and 107 individually undetected sources, including a sample-averaged absolute escape fraction of f_(esc, abs) = 0.06 \u00b1 0.01 and a sample-averaged ratio of ionizing to non-ionizing ultraviolet flux density of \u3008f\u2089\u2080\u2080/f\u2081\u2085\u2080\u2080\u3009_(out) = 0.040 \u00b1 0.006, corrected for attenuation from the intergalactic and circumgalactic media. Based on composite spectra, we also recover a strong positive correlation between \u3008f\u2089\u2080\u2080/f\u2081\u2085\u2080\u2080\u3009_(out) and Ly\u03b1 equivalent width (W_\u03bb(Ly\u03b1\u2060)) and a negative correlation between \u3008f\u2089\u2080\u2080/f\u2081\u2085\u2080\u2080\u3009_(out) and UV luminosity. As in previous work, we interpret the relationship between \u3008f\u2089\u2080\u2080/f\u2081\u2085\u2080\u2080\u3009_(out) and W_\u03bb(Ly\u03b1\u2060) in terms of the modulation of the escape of ionizing radiation from star-forming galaxies based on the covering fraction of neutral gas. We also use a W_\u03bb(Ly\u03b1\u2060)-weighted \u3008f\u2089\u2080\u2080/f\u2081\u2085\u2080\u2080\u3009_(out) to estimate an ionizing emissivity from star-forming galaxies at z \u223c 3 as \u03f5_(LyC) \u2243 5.5 \u00d7 10\u00b2\u2074 erg\u2009s\u207b\u00b9\u2009Hz\u207b\u00b9\u2009Mpc\u207b\u00b3. This estimate, evaluated using the uncontaminated sample of this work, affirms that the contribution of galaxies to the ionizing background at z \u223c 3 is comparable to that of active galactic nuclei.", "date": "2021-08", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "505", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "2447-2467", "id_number": "CaltechAUTHORS:20210821-170423382", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210821-170423382", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "JPL President and Director's Fund" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/stab1374", "primary_object": { "basename": "2104.02081.pdf", "url": "https://authors.library.caltech.edu/records/2n4cj-13937/files/2104.02081.pdf" }, "related_objects": [ { "basename": "stab1374.pdf", "url": "https://authors.library.caltech.edu/records/2n4cj-13937/files/stab1374.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Pahl, Anthony J.; Shapley, Alice; et el." }, { "id": "https://authors.library.caltech.edu/records/pzcpm-wq594", "eprint_id": 105263, "eprint_status": "archive", "datestamp": "2023-08-20 02:28:00", "lastmod": "2023-10-20 21:45:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Li-Zhihui", "name": { "family": "Li", "given": "Zhihui" }, "orcid": "0000-0001-5113-7558" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Gronke-Max", "name": { "family": "Gronke", "given": "Max" }, "orcid": "0000-0003-2491-060X" }, { "id": "Chen-Yuguang", "name": { "family": "Chen", "given": "Yuguang" }, "orcid": "0000-0003-4520-5395" } ] }, "title": "Revisiting the gas kinematics in SSA22 Lyman-\u03b1 Blob 1 with radiative transfer modelling in a multiphase, clumpy medium", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: high-redshift, intergalactic medium, galaxies: kinematics and dynamics", "note": "\u00a9 2020 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model) \n\nAccepted 2020 December 16. Received 2020 November 17; in original form 2020 August 24. \n\nWe thank the referee for insightful comments that have significantly improved the paper. We also thank Phil Hopkins for providing us with adequate computational resources. ZL acknowledges Michael Zhang, for his professional guidance and kind company during the excruciating debugging process. The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We are also grateful to the dedicated staff of the W.M. Keck Observatory who keep the instruments and telescopes running effectively. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409 awarded 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. Numerical calculations were run on the Caltech compute cluster 'Wheeler,' allocations from XSEDE TG-AST130039 and PRAC NSF.1713353 supported by the NSF, and NASA HEC SMD-16-7592. This research made use of Montage. It is funded by the National Science Foundation under grant number ACI-1440620, and was previously funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project, under cooperative agreement number NCC5-626 between NASA and the California Institute of Technology. \n\nDATA AVAILABILITY. The data underlying this article will be shared on reasonable request to the corresponding author.\n\nPublished - staa3951.pdf
Accepted Version - 2008.09130.pdf
Supplemental Material - staa3951_online_appendix.pdf
", "abstract": "We present new observations of Lyman-\u03b1 (Ly\u03b1) Blob 1 (LAB1) in the SSA22 protocluster region (z = 3.09) using the Keck Cosmic Web Imager and Keck Multi-object Spectrometer for Infrared Exploration. We have created a narrow-band Ly\u03b1 image and identified several prominent features. By comparing the spatial distributions and intensities of Ly\u03b1 and H\u03b2, we find that recombination of photo-ionized H\u2009I gas followed by resonant scattering is sufficient to explain all the observed Ly\u03b1/H\u03b2 ratios. We further decode the spatially resolved Ly\u03b1 profiles using both moment maps and radiative transfer modelling. By fitting a set of multiphase, 'clumpy' models to the observed Ly\u03b1 profiles, we manage to reasonably constrain many parameters, namely the H\u2009I number density in the interclump medium (ICM), the cloud volume filling factor, the random velocity and outflow velocity of the clumps, the H\u2009I outflow velocity of the ICM, and the local systemic redshift. Our model has successfully reproduced the diverse Ly\u03b1 morphologies, and the main results are: (1) the observed Ly\u03b1 spectra require relatively few clumps per line of sight as they have significant fluxes at the line centre; (2) the velocity dispersion of the clumps yields a significant broadening of the spectra as observed; (3) the clump bulk outflow can also cause additional broadening if the H\u2009I in the ICM is optically thick; (4) and the H\u2009I in the ICM is responsible for the absorption feature close to the Ly\u03b1 line centre.", "date": "2021-04", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "502", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "2389-2408", "id_number": "CaltechAUTHORS:20200908-075612693", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200908-075612693", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF2-51409" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NSF", "grant_number": "TG-AST130039" }, { "agency": "NSF", "grant_number": "OAC-1713353" }, { "agency": "NASA", "grant_number": "SMD-16-7592" }, { "agency": "NSF", "grant_number": "ACI-1440620" }, { "agency": "NASA", "grant_number": "NCC5-626" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/staa3951", "primary_object": { "basename": "2008.09130.pdf", "url": "https://authors.library.caltech.edu/records/pzcpm-wq594/files/2008.09130.pdf" }, "related_objects": [ { "basename": "staa3951.pdf", "url": "https://authors.library.caltech.edu/records/pzcpm-wq594/files/staa3951.pdf" }, { "basename": "staa3951_online_appendix.pdf", "url": "https://authors.library.caltech.edu/records/pzcpm-wq594/files/staa3951_online_appendix.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Li, Zhihui; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/bwww3-z8y74", "eprint_id": 104099, "eprint_status": "archive", "datestamp": "2023-08-20 00:32:03", "lastmod": "2023-10-20 23:00:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chen-Yuguang", "name": { "family": "Chen", "given": "Yuguang" }, "orcid": "0000-0003-4520-5395" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Hummels-Cameron-B", "name": { "family": "Hummels", "given": "Cameron B." }, "orcid": "0000-0002-3817-8133" }, { "id": "Rudie-Gwen-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Dong-Bill", "name": { "family": "Dong", "given": "Bili" } }, { "id": "Trainor-Ryan-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Bogosavljevi\u0107-Milan", "name": { "family": "Bogosavljevi\u0107", "given": "Milan" }, "orcid": "0000-0002-4710-4814" }, { "id": "Erb-Dawn-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Pettini-Max", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Reddy-Naveen-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Shapley-Alice-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Strom-Allison-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Theios-Rachel-L", "name": { "family": "Theios", "given": "Rachel L." }, "orcid": "0000-0002-4236-1037" }, { "id": "Faucher-Gigu\u00e8re-Claude-Andr\u00e9", "name": { "family": "Faucher-Gigu\u00e8re", "given": "Claude-Andr\u00e9" }, "orcid": "0000-0002-4900-6628" }, { "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684" }, { "id": "Kere\u0161-Du\u0161an", "name": { "family": "Kere\u0161", "given": "Du\u0161an" }, "orcid": "0000-0002-1666-7067" } ] }, "title": "The Keck Baryonic Structure Survey: using foreground/background galaxy pairs to trace the structure and kinematics of circumgalactic neutral hydrogen at z \u223c 2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: high-redshift \u2013 galaxies: ISM\u2013 galaxies: intergalatic medium", "note": "\u00a9 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2020 September 10. Received 2020 August 31; in original form 2020 April 30. Published: 23 September 2020. \n\nBased on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. \n\nThis paper has included data obtained using Keck/LRIS (Oke et al. 1995; Steidel et al. 2004; Rockosi et al. 2010) and Keck/MOSFIRE (McLean et al. 2010, 2012). We thank the W. M. Keck Observatory staff for their assistance with the observations over two decades. \n\nThe following software packages have been crucial to preparing for this paper: the IDL Astronomy User's Library,17 the Coyote IDL library,18ASTROPY (Astropy Collaboration 2018), EMCEE (Foreman-Mackey et al. 2013), THE YT PROJECT (Turk et al. 2011), and TRIDENT (Hummels, Smith & Silvia 2017). \n\nThis work was supported in part by grant AST-1313472 from the US NSF, and by a grant from the Caltech/JPL President's and Director's Program. CAFG was supported by NSF through grants AST-1517491, AST-1715216, and CAREER award AST-1652522, by NASA through grant 17-ATP17-0067, by STScI through grants HST-GO-14681.011, HST-GO-14268.022-A, and HST-AR-14293.001-A, and by a Cottrell Scholar Award from the Research Corporation for Science Advancement. \n\nWe would like to thank the anonymous referee for providing valuable feedback. YC would like to thank Hongjie Zhu, for her continuous encouragements when preparing for this paper. We would like to acknowledge Yiqiu Ma, E. Sterl Phinney, and Mateusz Matuszewski, for their constructive discussions. Finally, we thank collaborators Kurt L. Adelberger, Matthew P. Hunt, David R. Law, Olivera Rakic, and Monica L. Turner for their contributions to the KBSS survey over the course of nearly two decades. \n\nData Availability: The processed data underlying this article are available on the KBSS website (http://ramekin.caltech.edu/KBSS) with DOI: 10.22002/D1.1458.\n\nYuguang Chen, (\u9648\u6631\u5149), Charles C Steidel, Cameron B Hummels, Gwen C Rudie, Bili Dong, (\u8463\u6bd4\u7acb), Ryan F Trainor, Milan Bogosavljevi\u0107, Dawn K Erb, Max Pettini, Naveen A Reddy, Alice E Shapley, Allison L Strom, Rachel L Theios, Claude-Andr\u00e9 Faucher-Gigu\u00e8re, Philip F Hopkins, Du\u0161an Kere\u0161, Erratum: The Keck Baryonic Structure Survey: using foreground/background galaxy pairs to trace the structure and kinematics of circumgalactic neutral hydrogen at z \u223c 2, Monthly Notices of the Royal Astronomical Society, Volume 502, Issue 2, April 2021, Page 1702, https://doi.org/10.1093/mnras/stab023\n\nPublished - staa2808.pdf
Submitted - 2006.13236.pdf
Erratum - stab023.pdf
", "abstract": "We present new measurements of the spatial distribution and kinematics of neutral hydrogen in the circumgalactic and intergalactic medium surrounding star-forming galaxies at z \u223c 2. Using the spectra of \u22433000 galaxies with redshifts \u3008z\u3009 = 2.3 \u00b1 0.4 from the Keck Baryonic Structure Survey, we assemble a sample of more than 200\u2009000 distinct foreground-background pairs with projected angular separations of 3\u2013500 arcsec and spectroscopic redshifts, with \u3008z_(fg)\u3009 = 2.23 and \u3008zbg\u3009 = 2.57 (foreground, background redshifts, respectively.) The ensemble of sightlines and foreground galaxies is used to construct a 2D map of the mean excess HI Ly\u03b1 optical depth relative to the intergalactic mean as a function of projected galactocentric distance (20 \u2272 D_(tran)/pkpc \u2272 4000) and line-of-sight velocity. We obtain accurate galaxy systemic redshifts, providing significant information on the line-of-sight kinematics of HI gas as a function of projected distance D_(tran). We compare the map with cosmological zoom-in simulation, finding qualitative agreement between them. A simple two-component (accretion, outflow) analytical model generally reproduces the observed line-of-sight kinematics and projected spatial distribution of HI. The best-fitting model suggests that galaxy-scale outflows with initial velocity v_(out) \u2243 600 km s\u207b\u00b9 dominate the kinematics of circumgalactic HI out to D_(tran) \u2243 50 kpc, while HI at D_(tran) \u2273 100 kpc is dominated by infall with characteristic v_(in) \u2272 circular velocity. Over the impact parameter range 80 \u2272 D_(tran)/pkpc \u2272 200, the HI line-of-sight velocity range reaches a minimum, with a corresponding flattening in the rest-frame Ly\u03b1 equivalent width. These observations can be naturally explained as the transition between outflow-dominated and accretion-dominated flows. Beyond D_(tran) \u2243 300\u2009pkpc (\u223c1\u2009cMpc), the line-of-sight kinematics are dominated by Hubble expansion.", "date": "2020-12", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "499", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1721-1746", "id_number": "CaltechAUTHORS:20200626-150116926", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200626-150116926", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "JPL President and Director's Fund" }, { "agency": "NSF", "grant_number": "AST-1517491" }, { "agency": "NSF", "grant_number": "AST-1715216" }, { "agency": "NSF", "grant_number": "AST-1652522" }, { "agency": "NASA", "grant_number": "17-ATP17-0067" }, { "agency": "NASA", "grant_number": "HST-GO-14681.011" }, { "agency": "NASA", "grant_number": "HST-GO-14268.022-A" }, { "agency": "NASA", "grant_number": "HST-AR-14293.001-A" }, { "agency": "Cottrell Scholar of Research Corporation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "TAPIR" } ] }, "doi": "10.1093/mnras/staa2808", "primary_object": { "basename": "2006.13236.pdf", "url": "https://authors.library.caltech.edu/records/bwww3-z8y74/files/2006.13236.pdf" }, "related_objects": [ { "basename": "staa2808.pdf", "url": "https://authors.library.caltech.edu/records/bwww3-z8y74/files/staa2808.pdf" }, { "basename": "stab023.pdf", "url": "https://authors.library.caltech.edu/records/bwww3-z8y74/files/stab023.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Chen, Yuguang; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/t11b8-q4p25", "eprint_id": 106196, "eprint_status": "archive", "datestamp": "2023-08-22 07:00:14", "lastmod": "2023-10-20 23:11:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Kriek-M", "name": { "family": "Kriek", "given": "Mariska" }, "orcid": "0000-0002-7613-9872" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Shivaei-Irene", "name": { "family": "Shivaei", "given": "Irene" }, "orcid": "0000-0003-4702-7561" }, { "id": "Sanders-Ryan-L", "name": { "family": "Sanders", "given": "Ryan L." }, "orcid": "0000-0003-4792-9119" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Coil-A-L", "name": { "family": "Coil", "given": "Alison L." }, "orcid": "0000-0002-2583-5894" }, { "id": "Siana-Brian-D", "name": { "family": "Siana", "given": "Brian" }, "orcid": "0000-0002-4935-9511" }, { "id": "Freeman-W-R", "name": { "family": "Freeman", "given": "William R." }, "orcid": "0000-0003-3559-5270" }, { "id": "Azadi-M", "name": { "family": "Azadi", "given": "Mojegan" }, "orcid": "0000-0001-6004-9728" }, { "id": "Fetherolf-T", "name": { "family": "Fetherolf", "given": "Tara" }, "orcid": "0000-0002-3551-279X" }, { "id": "Leung-Gene-C-K", "name": { "family": "Leung", "given": "Gene" }, "orcid": "0000-0002-9393-6507" }, { "id": "Price-S-H", "name": { "family": "Price", "given": "Sedona H." }, "orcid": "0000-0002-0108-4176" }, { "id": "Zick-T", "name": { "family": "Zick", "given": "Tom" } } ] }, "title": "The MOSDEF Survey: The First Direct Measurements of the Nebular Dust Attenuation Curve at High Redshift", "ispublished": "pub", "full_text_status": "public", "keywords": "Interstellar dust extinction; Galaxy evolution; High-redshift galaxies; Interstellar dust; Interstellar reddening; Interstellar extinction; Reddening law", "note": "\u00a9 2020. The American Astronomical Society. \n\nReceived 2020 July 4; revised 2020 August 27; accepted 2020 September 7; published 2020 October 20. \n\nBased on data obtained at the W.M. Keck Observatory, which is operated as\na scientific partnership among the California Institute of Technology, the\nUniversity of California, and NASA and was made possible by the generous\nfinancial support of the W.M. Keck Foundation.\n\nWe acknowledge support from NSF AAG grants AST-1312780, 1312547, 1312764, and 1313171; archival grant AR-13907, provided by NASA through the Space Telescope Science Institute; and grant NNX16AF54G from the NASA ADAP program. We are grateful to the MOSFIRE instrument team for building this powerful instrument and to Marc Kassis at the Keck Observatory for his many valuable contributions to the execution of the MOSDEF survey. We also acknowledge the 3D-HST collaboration, who provided us with spectroscopic and photometric catalogs used to select MOSDEF targets and derive stellar population parameters. We also thank I. McLean, K. Kulas, and G. Mace for taking observations for the MOSDEF survey in 2013 May and June. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, the observations presented herein would not have been possible.\n\nPublished - Reddy_2020_ApJ_902_123.pdf
Accepted Version - 2009.10085.pdf
", "abstract": "We use a sample of 532 star-forming galaxies at redshifts z \u2243 1.4\u20132.6 with deep rest-frame optical spectra from the MOSFIRE Deep Evolution Field (MOSDEF) survey to place the first constraints on the nebular attenuation curve at high redshift. Based on the first five low-order Balmer emission lines detected in the composite spectra of these galaxies (H\u03b1 through H\u03b5), we derive a nebular attenuation curve that is similar in shape to that of the Galactic extinction curve, suggesting that the dust covering fraction and absorption/scattering properties along the lines of sight to massive stars at high redshift are similar to those of the average Milky Way sight line. The curve derived here implies nebular reddening values that are, on average, systematically larger than those derived for the stellar continuum. In the context of stellar population synthesis models that include the effects of stellar multiplicity, the difference in reddening of the nebular lines and stellar continuum may imply molecular cloud crossing timescales that are a factor of \u2273 3x longer than those inferred for local molecular clouds, star formation rates that are constant or increasing with time such that newly formed and dustier OB associations always dominate the ionizing flux, and/or that the dust responsible for reddening the nebular emission may be associated with nonmolecular (i.e., ionized and neutral) phases of the interstellar medium. Our analysis points to a variety of investigations of the nebular attenuation curve that will be enabled with the next generation of ground- and space-based facilities.", "date": "2020-10-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "902", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 123", "id_number": "CaltechAUTHORS:20201021-160146951", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201021-160146951", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1312780" }, { "agency": "NSF", "grant_number": "AST-1312547" }, { "agency": "NSF", "grant_number": "AST-1312764" }, { "agency": "NSF", "grant_number": "AST-1313171" }, { "agency": "NASA", "grant_number": "AR-13907" }, { "agency": "NASA", "grant_number": "NNX16AF54G" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/abb674", "primary_object": { "basename": "Reddy_2020_ApJ_902_123.pdf", "url": "https://authors.library.caltech.edu/records/t11b8-q4p25/files/Reddy_2020_ApJ_902_123.pdf" }, "related_objects": [ { "basename": "2009.10085.pdf", "url": "https://authors.library.caltech.edu/records/t11b8-q4p25/files/2009.10085.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Reddy, Naveen A.; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/j58d0-01206", "eprint_id": 100287, "eprint_status": "archive", "datestamp": "2023-08-22 03:16:53", "lastmod": "2023-10-18 19:49:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Chen-Yuguang", "name": { "family": "Chen", "given": "Yuguang" }, "orcid": "0000-0003-4520-5395" }, { "id": "Theios-R-L", "name": { "family": "Theios", "given": "Rachel L." }, "orcid": "0000-0002-4236-1037" } ] }, "title": "Predicting Ly\u03b1 Emission from Galaxies via Empirical Markers of Production and Escape in the KBSS", "ispublished": "pub", "full_text_status": "public", "keywords": "Ly\u03b1 galaxies; Galaxies; High-redshift galaxies", "note": "\u00a9 2019. The American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2019 August 13; revised 2019 September 24; accepted 2019 September 29; published 2019 December 12. \n\nBased on data obtained at the W. M. Keck Observatory, which is operated as\na scientific partnership among the California Institute of Technology, the\nUniversity of California, and NASA, and was made possible by the generous\nfinancial support of the W. M. Keck Foundation.\n\nWe are indebted to the staff of the W. M. Keck Observatory who keep the instruments and telescopes running effectively. We also wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. This work has been supported in part by the US National Science Foundation through grants AST-0908805 and AST-1313472. We also acknowledge support from the JPL/Caltech President's and Director's Program. \n\nSoftware: Astropy (Astropy Collaboration et al. 2013), Matplotlib (Hunter 2007).\n\nPublished - Trainor_2019_ApJ_887_85.pdf
Accepted Version - 1908.04794.pdf
", "abstract": "Ly\u03b1 emission is widely used to detect and confirm high-redshift galaxies and characterize the evolution of the intergalactic medium (IGM). However, many galaxies do not display Ly\u03b1 emission in typical spectroscopic observations, and intrinsic Ly\u03b1 emitters represent a potentially biased set of high-redshift galaxies. In this work, we analyze a set of 703 galaxies at 2 \u227e z \u227e 3 with both Ly\u03b1 spectroscopy and measurements of other rest-frame ultraviolet and optical properties in order to develop an empirical model for Ly\u03b1 emission from galaxies and understand how the probability of Ly\u03b1 emission depends on other observables. We consider several empirical proxies for the efficiency of Ly\u03b1 photon production, as well as the subsequent escape of these photons through their local interstellar medium. We find that the equivalent width of metal-line absorption and the O3 ratio of rest-frame optical nebular lines are advantageous empirical proxies for Ly\u03b1 escape and production, respectively. We develop a new quantity, X_(LIS)^(O3), that combines these two properties into a single predictor of net Ly\u03b1 emission, which we find describes ~90% of the observed variance in Ly\u03b1 equivalent width when accounting for our observational uncertainties. We also construct conditional probability distributions demonstrating that galaxy selection based on measurements of galaxy properties yield samples of galaxies with widely varying probabilities of net Ly\u03b1 emission. The application of the empirical models and probability distributions described here may be used to infer the selection biases of current galaxy surveys and evaluate the significance of high-redshift Ly\u03b1 (non)detections in studies of reionization and the IGM.", "date": "2019-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "887", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 85", "id_number": "CaltechAUTHORS:20191213-105036789", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191213-105036789", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "JPL President and Director's Fund" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ab4993", "primary_object": { "basename": "Trainor_2019_ApJ_887_85.pdf", "url": "https://authors.library.caltech.edu/records/j58d0-01206/files/Trainor_2019_ApJ_887_85.pdf" }, "related_objects": [ { "basename": "1908.04794.pdf", "url": "https://authors.library.caltech.edu/records/j58d0-01206/files/1908.04794.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Trainor, Ryan F.; Strom, Allison L.; et el." }, { "id": "https://authors.library.caltech.edu/records/9ff3a-y8a36", "eprint_id": 99597, "eprint_status": "archive", "datestamp": "2023-08-22 02:56:29", "lastmod": "2023-10-18 18:35:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Hummels-C-B", "name": { "family": "Hummels", "given": "Cameron B." }, "orcid": "0000-0002-3817-8133" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" } ] }, "title": "Column Density, Kinematics, and Thermal State of Metal-bearing Gas within the Virial Radius of z \u223c 2 Star-forming Galaxies in the Keck Baryonic Structure Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift; intergalactic medium; quasars: absorption lines", "note": "\u00a9 2019. The American Astronomical Society. \n\nReceived 2019 February 26; revised 2019 August 30; accepted 2019 September 5; published 2019 October 31. \n\nWe thank collaborators K. Adelberger, M. Bogosavljevi\u0107 D. Erb, N. Konidaris, D. Law, O. Rakic, and M. Turner for their contributions to the KBSS survey. The authors thank D. Fielding, J. Stern, S. Johnson, A. Benson, A. Piro, A. Newman, M. Rauch, H.-W. Chen, F. Zahedy, E. Schneider, M. Gronke, J. Kollmeier, S. Garrison-Kimmel, and the anonymous referee for useful discussions that shaped the content or direction of this manuscript. We also wish to acknowledge the staff of the W.M. Keck Observatory, whose efforts ensure the telescopes and instruments perform reliably. Further, we extend our gratitude to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Early phases of this work were supported by NSF through grants AST-0908805 and AST-1313472. This research has made use of the Keck Observatory Archive (KOA), which is operated by the W.M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. This work was completed in part at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1607611. \n\nFacility: Keck (LRIS). - \n\nSoftware: VPFIT, Grackle (Smith et al. 2017).\n\nPublished - Rudie_2019_ApJ_885_61.pdf
Submitted - 1903.00004.pdf
", "abstract": "We present results from the Keck Baryonic Structure Survey (KBSS) including the first detailed measurements of the column densities, kinematics, and internal energy of metal-bearing gas within the virial radius (35\u2013100 physical kpc) of eight ~L* galaxies at z ~ 2. From our full sample of 130 metal-bearing absorbers, we infer that halo gas is kinematically complex when viewed in singly, doubly, and triply ionized species. Broad O vi and C iv absorbers are detected at velocities similar to the lower-ionization gas but with a very different kinematic structure, indicating that the circumgalactic medium (CGM) is multiphase. There is a high covering fraction of metal-bearing gas within 100 kpc, including highly ionized gas such as O vi; however, observations of a single galaxy probed by a lensed background QSO suggest the size of metal-bearing clouds is small (<400 pc for all but the O vi-bearing gas). The mass in metals found within the halo is substantial, equivalent to \u227325% of the metal mass within the interstellar medium. The gas kinematics unambiguously show that 70% of galaxies with detected metal absorption have some unbound metal-enriched gas, suggesting galactic winds may commonly eject gas from halos at z ~ 2. When modeled assuming that ions with different ionization potentials can originate within a single gaseous structure, significant thermal broadening is detected in CGM absorbers that dominates the internal energy of the gas. Some 40% of the detected gas has temperatures in the range 10^(4.5-5.5) K where cooling times are short, suggesting the CGM is dynamic, with constant heating or cooling to produce this short-lived thermal phase.", "date": "2019-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "885", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 61", "id_number": "CaltechAUTHORS:20191031-141639995", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191031-141639995", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "PHY-1607611" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ab4255", "primary_object": { "basename": "1903.00004.pdf", "url": "https://authors.library.caltech.edu/records/9ff3a-y8a36/files/1903.00004.pdf" }, "related_objects": [ { "basename": "Rudie_2019_ApJ_885_61.pdf", "url": "https://authors.library.caltech.edu/records/9ff3a-y8a36/files/Rudie_2019_ApJ_885_61.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Rudie, Gwen C.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/0ynak-kmy93", "eprint_id": 99065, "eprint_status": "archive", "datestamp": "2023-08-19 18:13:23", "lastmod": "2023-10-18 17:49:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Umehata-Hideki", "name": { "family": "Umehata", "given": "H." } }, { "id": "Fumagalli-M", "name": { "family": "Fumagalli", "given": "M." }, "orcid": "0000-0001-6676-3842" }, { "id": "Smail-Ian-R", "name": { "family": "Smail", "given": "I." }, "orcid": "0000-0003-3037-257X" }, { "id": "Matsuda-Yuichi", "name": { "family": "Matsuda", "given": "Y." } }, { "id": "Swinbank-A-M", "name": { "family": "Swinbank", "given": "A. M." } }, { "id": "Cantalupo-S", "name": { "family": "Cantalupo", "given": "S." }, "orcid": "0000-0001-5804-1428" }, { "id": "Sykes-C-M", "name": { "family": "Sykes", "given": "C." } }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "A. E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Vernet-Joel", "name": { "family": "Vernet", "given": "J." }, "orcid": "0000-0002-8639-8560" }, { "id": "Yamada-Toru", "name": { "family": "Yamada", "given": "T." } }, { "id": "Tamura-Yoichi", "name": { "family": "Tamura", "given": "Y." } }, { "id": "Kubo-Mariko", "name": { "family": "Kubo", "given": "M." } }, { "id": "Nakanishi-Kouichiro", "name": { "family": "Nakanishi", "given": "K." }, "orcid": "0000-0002-6939-0372" }, { "id": "Kajisawa-Masaru", "name": { "family": "Kajisawa", "given": "M." }, "orcid": "0000-0002-1732-6387" }, { "id": "Hatsukade-Bunyo", "name": { "family": "Hatsukade", "given": "B." } }, { "id": "Kohno-Kotaro", "name": { "family": "Kohno", "given": "K." }, "orcid": "0000-0002-4052-2394" } ] }, "title": "Gas filaments of the cosmic web located around active galaxies in a protocluster", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2019 American Association for the Advancement of Science. This is an article distributed under the terms of the Science Journals Default License. \n\nReceived 25 January 2019; accepted 2 September 2019. \n\nWe thank the reviewers for their constructive comments, which were very helpful in improving this paper. Our data are based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere. We thank all ESO staff who supported us in observation preparation and execution. We thank the JAO and EA-ARC staffs for preparation, observation, and initial data reduction. ALMA is a partnership of ESO (representing its member states), NSF (United States), 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. Some of the data were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. We thank S. Yeh for assistance on the MOSFIRE observations. The observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors recognize and acknowledge the very important cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have had the opportunity to conduct observations from this mountain. Funding: H.U., Y.M., B.H., Y.T., and K.K. are supported by JSPS KAKENHI (grant nos. 17K14252, 25287043/17H04831/17KK0098, 19K03925, 17H06130, and 17H06130, respectively). Y.T. acknowledges support from NAOJ (ALMA Scientific Research grant no. 2018-09B). M.F., I.S., and A.M.S. acknowledge support from the Science and Technology Facilities Council (grant no. ST/P000541/1). This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant no. 757535). C.S. acknowledges an STFC studentship (grant no. ST/R504725/1). S.C. gratefully acknowledges support from the Swiss National Science Foundation (grant no. PP00P2_163824). Author contributions: H.U. led the project and analyzed the data (MUSE, Subaru, ALMA, Keck). M.F., I.S., S.C., and A.M.S. worked on the MUSE data reduction. C.C.S. worked on the Keck data reduction. Y.M. worked on the Subaru data reduction. M.F. and C.S. performed radiative transfer calculations. R.J.I., A.E.S., J.V., T.Y., Y.T., M.Ku., K.N., M.Ka., B.H., and K.K. contributed to interpreting the results. All authors reviewed, discussed, and commented on the results and the manuscript, and met the journal's authorship criteria. Competing interests: The authors declare no competing interests. Data and materials availability: The MUSE data are available in the ESO archive at http://archive.eso.org/cms.html under programs 099.A-0638 and 0101.A-0679; the ALMA data are archived at http://almascience.nrao.edu/aq/ under project codes 2013.1.00162.S, 2015.1.00212.S, and 2016.1.00543.S; and MOSFIRE observations are in the Keck Observatory Archive https://www2.keck.hawaii.edu/koa under semester 2017B, program ID S412. Input parameter files for our CLOUDY simulations are provided in data files S1 and S2.\n\nSupplemental Material - aaw5949-Data_files.zip
Supplemental Material - aaw5949-Umehata-SM.pdf
", "abstract": "Cosmological simulations predict that the Universe contains a network of intergalactic gas filaments, within which galaxies form and evolve. However, the faintness of any emission from these filaments has limited tests of this prediction. We report the detection of rest-frame ultraviolet Lyman-\u03b1 radiation from multiple filaments extending more than one megaparsec between galaxies within the SSA22 protocluster at a redshift of 3.1. Intense star formation and supermassive black-hole activity is occurring within the galaxies embedded in these structures, which are the likely sources of the elevated ionizing radiation powering the observed Lyman-\u03b1 emission. Our observations map the gas in filamentary structures of the type thought to fuel the growth of galaxies and black holes in massive protoclusters.", "date": "2019-10-04", "date_type": "published", "publication": "Science", "volume": "366", "number": "6461", "publisher": "American Association for the Advancement of Science", "pagerange": "97-100", "id_number": "CaltechAUTHORS:20191004-072437663", "issn": "0036-8075", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191004-072437663", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17K14252" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "25287043" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17H04831" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17KK0098" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19K03925" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17H06130" }, { "agency": "National Astronomical Observatory of Japan", "grant_number": "2018-09B" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/P000541/1" }, { "agency": "European Research Council (ERC)", "grant_number": "757535" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/R504725/1" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "PP00P2_163824" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1126/science.aaw5949", "primary_object": { "basename": "aaw5949-Data_files.zip", "url": "https://authors.library.caltech.edu/records/0ynak-kmy93/files/aaw5949-Data_files.zip" }, "related_objects": [ { "basename": "aaw5949-Umehata-SM.pdf", "url": "https://authors.library.caltech.edu/records/0ynak-kmy93/files/aaw5949-Umehata-SM.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Umehata, H.; Fumagalli, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/2kcz7-hqx13", "eprint_id": 94914, "eprint_status": "archive", "datestamp": "2023-08-19 17:32:45", "lastmod": "2023-10-20 18:23:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "O'Sullivan-Donal", "name": { "family": "O'Sullivan", "given": "Donal" }, "orcid": "0000-0002-4959-9179" }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Mateusz" } }, { "id": "Hamden-E-T", "name": { "family": "Hamden", "given": "Erika T." } }, { "id": "Dekel-Avishai", "name": { "family": "Dekel", "given": "Avishai" }, "orcid": "0000-0003-4174-0374" }, { "id": "Lapiner-Sharon", "name": { "family": "Lapiner", "given": "Sharon" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Cantalupo-S", "name": { "family": "Cantalupo", "given": "Sebastiano" }, "orcid": "0000-0001-5804-1428" }, { "id": "Prochaska-J-X", "name": { "family": "Prochaska", "given": "Jason Xavier" }, "orcid": "0000-0002-7738-6875" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles" }, "orcid": "0000-0002-4834-7260" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan" }, "orcid": "0000-0002-6967-7322" }, { "id": "Moore-A-M", "name": { "family": "Moore", "given": "Anna" }, "orcid": "0000-0002-2894-6936" }, { "id": "Ceverino-D", "name": { "family": "Ceverino", "given": "Daniel" }, "orcid": "0000-0002-8680-248X" }, { "id": "Primack-J-R", "name": { "family": "Primack", "given": "Joel" }, "orcid": "0000-0001-5091-5098" }, { "id": "Rizzi-L", "name": { "family": "Rizzi", "given": "Luca" }, "orcid": "0000-0003-0882-2327" } ] }, "title": "Multi-filament gas inflows fuelling young star-forming galaxies", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2019 Springer Nature Publishing AG. \n\nReceived 07 March 2019. Accepted 25 April 2019. Published 01 July 2019. \n\nThis work was supported by the National Science Foundation, the W. M. Keck Observatory and the California Institute of Technology. The VELA simulations were performed at NASA Advanced Supercomputing at NASA Ames Research Center. D.C. is funded by the ERC Advanced Grant, STARLIGHT: Formation of the First Stars (project number 339177). \n\nAuthor Contributions: D.C.M. is the Principal Investigator of KCWI, performed the analysis of the simulated galaxy, data and MFI models, and was principal author on the paper. D.O. and D.C.M. led the observations of UM287 and CSO 38. D.O. and M.M. reduced the data. D.O., M.M. and E.H. contributed to the paper writing. P.M., M.M., D.C.M., J.D.N., D.O. and A.M. designed, constructed and operated KCWI. J.D.N., M.M. and D.C.M. developed the KCWI data pipeline and produced the final data cubes. D.C. developed the VELA simulations. A.D. and S.L. provided the simulated galaxy VELA07 and contributed to the writing of the paper. D.C. and J.P. contributed the cosmological simulation. C.S., R.T., S.C. and J.X.P. contributed to the development of KCWI, to Keck data for the two protogalaxies, and to the editing of the paper. L.R. made major contributions to KCWI commissioning and participated in the observations of CSO 38. \n\nData availability: KCWI data on CSO38 and UM287 is publicly available. Data on UM287 will be available 18 months after the observation in Oct 2017. The data that support the plots within this paper and other findings of this study are available from the corresponding author upon reasonable request. \n\nCode availability: KCWI pipeline code is available on the W. M. Keck Observatory website. The authors declare no competing interests.\n\nAccepted Version - 1904.11465.pdf
Supplemental Material - 41550_2019_791_MOESM1_ESM.pdf
", "abstract": "Theory suggests that there are two primary modes of accretion through which dark-matter halos acquire the gas to form and fuel galaxies: hot- and cold-flow accretion. In cold-flow accretion, gas streams along cosmic web filaments to the centre of the halo, allowing for the efficient delivery of star-forming fuel. Recently, two quasar-illuminated H\u2009I Lyman \u0251 (Ly\u03b1)-emitting objects were reported to have properties of cold, rotating structures. However, the spatial and spectral resolution available was insufficient to constrain the radial flows associated with connecting filaments. With the Keck Cosmic Web Imager (KCWI), we now have eight times the spatial resolution, permitting the detection of these inspiralling flows. To detect these inflows, we introduce a suite of models that incorporate zonal radial flows, demonstrate their performance on a numerical simulation that exhibits cold-flow accretion, and show that they are an excellent match to KCWI velocity maps of two Ly\u03b1 emitters observed around high-redshift quasars. These multi-filament inflow models kinematically isolate zones of radial inflow that correspond to extended filamentary emission. The derived gas flux and inflow path is sufficient to fuel the inferred central galaxy star-formation rate and angular momentum. Thus, our kinematic emission maps provide strong evidence that the inflow of gas from the cosmic web is building galaxies at the peak of star formation.", "date": "2019-09", "date_type": "published", "publication": "Nature Astronomy", "volume": "3", "number": "9", "publisher": "Nature Publishing Group", "pagerange": "822-831", "id_number": "CaltechAUTHORS:20190424-101356136", "issn": "2397-3366", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190424-101356136", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "W. M. Keck Observatory" }, { "agency": "Caltech" }, { "agency": "European Research Council (ERC)", "grant_number": "339177" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1038/s41550-019-0791-2", "primary_object": { "basename": "1904.11465.pdf", "url": "https://authors.library.caltech.edu/records/2kcz7-hqx13/files/1904.11465.pdf" }, "related_objects": [ { "basename": "41550_2019_791_MOESM1_ESM.pdf", "url": "https://authors.library.caltech.edu/records/2kcz7-hqx13/files/41550_2019_791_MOESM1_ESM.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Martin, D. Christopher; O'Sullivan, Donal; et el." }, { "id": "https://authors.library.caltech.edu/records/gt4jr-22n21", "eprint_id": 98599, "eprint_status": "archive", "datestamp": "2023-08-19 17:37:22", "lastmod": "2023-10-18 17:29:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lacaille-Kevin-M", "name": { "family": "Lacaille", "given": "Kevin M." }, "orcid": "0000-0001-9870-5663" }, { "id": "Chapman-Scott-C", "name": { "family": "Chapman", "given": "Scott C." } }, { "id": "Smail-Ian-R", "name": { "family": "Smail", "given": "Ian" }, "orcid": "0000-0003-3037-257X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Blain-Andrew-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Geach-James-E", "name": { "family": "Geach", "given": "J." }, "orcid": "0000-0003-4964-4635" }, { "id": "Golob-Anneya", "name": { "family": "Golob", "given": "A." } }, { "id": "Gurwell-Mark-A", "name": { "family": "Gurwell", "given": "M." }, "orcid": "0000-0003-0685-3621" }, { "id": "Ivison-Rob-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Reddy-Naveen-A", "name": { "family": "Reddy", "given": "N." }, "orcid": "0000-0001-9687-4973" }, { "id": "Sawicki-Marcin", "name": { "family": "Sawicki", "given": "M." }, "orcid": "0000-0002-7712-7857" } ] }, "title": "Two sub-millimetre bright protoclusters bounding the epoch of peak star-formation activity", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general, galaxies: high-redshift, cosmology: observations, sub-millimetre: galaxies", "note": "\u00a9 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2019 June 12. Received 2019 May 3; in original form 2018 September 18. Published: 26 June 2019. \n\nKL acknowledges NSGS and OGS for support. SCC acknowledges NSERC and CFI for support. IRS acknowleges support from the ERC advanced Grant DUSTYGAL (321334), STFC (ST/P000541/1), and a Royal Society/Wolfson Merit Award. This work is based on observations carried out with the the James Clerk Maxwell Telescope. The James Clerk Maxwell Telescope is operated by the East Asian Observatory on behalf of The National Astronomical Observatory of Japan, Academia Sinica Institute of Astronomy and Astrophysics, the Korea Astronomy and Space Science Institute, the National Astronomical Observatories of China and the Chinese Academy of Sciences (Grant No. XDB09000000), with additional funding support from the Science and Technology Facilities Council of the United Kingdom and participating universities in the United Kingdom and Canada. The 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. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina), and Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil). \n\nFacilities: James Clerk Maxwell Telescope (JCMT) (Holland et al. 2013), Submillimeter Array (SMA), and Gemini. \n\nSoftware: STARLINK (Currie et al. 2014), SMURF (Chapin et al. 2013; Jenness et al. 2013), PYTHON version 2.7, MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration 2013), and APLPY (Robitaille & Bressert 2012).\n\nPublished - stz1742.pdf
Accepted Version - 1809.06882.pdf
", "abstract": "We present James Clerk Maxwell Telescope Submillimetre Common-User Bolometer Array 2 (SCUBA-2) 850 and 450 \u03bcm observations (\u03c3_(850) \u223c 0.5 mJy, \u03c3_(450) \u223c 5 mJy) of the HS1549+19 and HS1700+64 survey fields containing two of the largest known galaxy overdensities at z = 2.85 and 2.30, respectively. We detect 56 sub-millimetre galaxies (SMGs) with SNR > 4 over \u223c50 arcmin^2 at 850 \u03bcm with flux densities of 3\u201317 mJy. The number counts indicate overdensities in the 3-arcmin diameter core region (\u223c1.5 Mpc at z = 2.5) of 6^(+4)_(\u22122)\u00d7 (HS1549) and 4^(+6)_(\u22122)\u00d7 (HS1700) compared to blank field surveys. Within these core regions, we spectroscopically confirm that approximately one-third of the SMGs lie at the protocluster redshifts for both HS1549 and HS1700. We use statistical identifications of other SMGs in the wider fields to constrain an additional four candidate protocluster members in each system. We combine multiwavelength estimates of the star-formation rates (SFRs) from Lyman-break dropout- and narrow-band-selected galaxies, and the SCUBA-2 SMGs, to estimate total SFRs of 12\u2009500 \u00b1 2800 M\u2299 yr^(\u22121) (4900 \u00b1 1200 M\u2299 yr^(\u22121)) in HS1549 (HS1700), and SFR densities (SFRDs) within the central 1.5-Mpc diameter of each protocluster to be 3000 \u00b1 900 M\u2299\u2009yr^(\u22121) Mpc^(\u22123) (1300 \u00b1 400 M\u2299 yr^(\u22121) Mpc^(\u22123)) in the HS1549 (HS1700) protocluster, \u223c10^4 \u00d7 larger than the global SFRDs found at their respective epochs, due to the concentration of star-forming galaxies in the small volume of the dense cluster cores. Our results suggest centrally concentrated starbursts within protoclusters may be a relatively common scenario for the build-up of mass in rich clusters assembling at z \u2273 2.", "date": "2019-09", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "488", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1790-1812", "id_number": "CaltechAUTHORS:20190912-081725307", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190912-081725307", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Nova Scotia Graduate Scholarship" }, { "agency": "Ontario Graduate Scholarship" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "European Research Council (ERC)", "grant_number": "321334" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/P000541/1" }, { "agency": "Royal Society" }, { "agency": "Chinese Academy of Sciences", "grant_number": "XDB09000000" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/stz1742", "primary_object": { "basename": "1809.06882.pdf", "url": "https://authors.library.caltech.edu/records/gt4jr-22n21/files/1809.06882.pdf" }, "related_objects": [ { "basename": "stz1742.pdf", "url": "https://authors.library.caltech.edu/records/gt4jr-22n21/files/stz1742.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Lacaille, Kevin M.; Chapman, Scott C.; et el." }, { "id": "https://authors.library.caltech.edu/records/y6a34-1ey90", "eprint_id": 99469, "eprint_status": "archive", "datestamp": "2023-08-19 16:08:14", "lastmod": "2023-10-18 18:20:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kikuta-Satoshi", "name": { "family": "Kikuta", "given": "Satoshi" } }, { "id": "Matsuda-Yuichi", "name": { "family": "Matsuda", "given": "Yuichi" } }, { "id": "Cen-Renyue", "name": { "family": "Cen", "given": "Renyue" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Yagi-Masafumi", "name": { "family": "Yagi", "given": "Masafumi" } }, { "id": "Hahashino-Tomoki", "name": { "family": "Hayashino", "given": "Tomoki" } }, { "id": "Imanishi-Masatoshi", "name": { "family": "Imanishi", "given": "Masatoshi" }, "orcid": "0000-0001-6186-8792" }, { "id": "Komiyama-Yutaka", "name": { "family": "Komiyama", "given": "Yutaka" } }, { "id": "Momose-Rieko", "name": { "family": "Momose", "given": "Rieko" } }, { "id": "Saito-Tomoki", "name": { "family": "Saito", "given": "Tomoki" } } ] }, "title": "Ly\u03b1 view around a z = 2.84 hyperluminous QSO at a node of the cosmic web", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation (galaxies:) intergalactic medium galaxies: high-redshift (galaxies:) quasars: individual", "note": "\u00a9 The Author(s) 2019. Published by Oxford University Press on behalf of the Astronomical Society of Japan. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nReceived 2019 March 25; Accepted 2019 April 19. Published: 05 June 2019. \n\nBased on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. \n\nWe thank Yukie Oishi and the HSC pipeline team for their helpful comments on HSC data analyses, the anonymous referee for his/her thoughtful comments, and Pimpunyawat Tummuangpak for reading the manuscript. We would like to acknowledge all who supported our observations with the Subaru Telescope, including the staffs of the National Astronomical Observatory of Japan, Mauna Kea Observatories, and the local Hawaiian people who have been making efforts to preserve and share the beautiful dark sky of Mauna Kea with us. \n\nData analysis was carried out on the Multi-wavelength Data Analysis System operated by the Astronomy Data Center (ADC), National Astronomical Observatory of Japan. \n\nSK acknowledges supports from the Japan Society for the Promotion of Science (JSPS) KAKENHI grant No. 18J11477 and the Course-by-Course Education Program of SOKENDAI. YM acknowledges supports from the JSPS KAKENHI grant Nos. 25287043, 17H04831, 17KK0098. MI acknowledges supports from the JSPS KAKENHI grant No. 15K05030.\n\nSubmitted - 1904.07747.pdf
", "abstract": "We report on the results of deep and wide-field (1.1\u2009deg\u00b2) narrow-band observations with Subaru/Hyper Suprime-Cam (HSC) of a field around a hyperluminous QSO (HLQSO), HS1549+1549+1919, residing in a protocluster at z = 2.84, to map the large-scale structure of Ly\u03b1 emitters (LAEs). One HSC pointing enables us to detect 3490 LAEs and 76 extended Ly\u03b1 blobs (LABs), probing diverse environments from voids to protoclusters. The HLQSO is found to be near the center of the protocluster, which corresponds to the intersection of \u223c100 comoving Mpc-scale structures of LAEs. LABs are basically distributed along the large-scale structure, with larger ones particularly clustering around the HLQSO, confirming a previously noted tendency of LABs to prefer denser environments. Moreover, the shapes of LABs near the HLQSO appear to be aligned with the large-scale structure. Finally, a deep Ly\u03b1 image reveals a diffuse Ly\u03b1 nebula along a filamentary structure with no luminous UV/sub-mm counterpart. We suggest that the diffuse nebula is due to a cold filament with high clumping factor illuminated by the QSO, with the required high clumpiness provided by unresolved residing halos of mass \u226410\u2079\u207b\u00b9\u2070 M_\u2299\u2060.", "date": "2019-06", "date_type": "published", "publication": "Publications of the Astronomical Society of Japan", "volume": "71", "number": "3", "publisher": "Astronomical Society of Japan", "pagerange": "Art. No. L2", "id_number": "CaltechAUTHORS:20191025-154919609", "issn": "0004-6264", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191025-154919609", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "18J11477" }, { "agency": "Graduate University for Advanced Studies (Japan)" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "25287043" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17H04831" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17KK0098" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15K05030" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1093/pasj/psz055", "primary_object": { "basename": "1904.07747.pdf", "url": "https://authors.library.caltech.edu/records/y6a34-1ey90/files/1904.07747.pdf" }, "resource_type": "article", "pub_year": "2019", "author_list": "Kikuta, Satoshi; Matsuda, Yuichi; et el." }, { "id": "https://authors.library.caltech.edu/records/fdnhb-wtz64", "eprint_id": 95736, "eprint_status": "archive", "datestamp": "2023-08-19 15:38:43", "lastmod": "2023-10-20 22:01:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hill-Ryley", "name": { "family": "Hill", "given": "Ryley" } }, { "id": "Chapman-Scott-C", "name": { "family": "Chapman", "given": "Scott C." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "Smail-Ian-R", "name": { "family": "Smail", "given": "Ian" }, "orcid": "0000-0003-3037-257X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Krips-Melanie", "name": { "family": "Krips", "given": "Melanie" } }, { "id": "Babul-Arif", "name": { "family": "Babul", "given": "Arif" }, "orcid": "0000-0003-1746-9529" }, { "id": "Berg-Trystyn", "name": { "family": "Berg", "given": "Trystyn" }, "orcid": "0000-0002-2606-5078" }, { "id": "Bertoldi-Frank", "name": { "family": "Bertoldi", "given": "Frank" }, "orcid": "0000-0002-1707-1775" }, { "id": "Gao-Yu", "name": { "family": "Gao", "given": "Yu" }, "orcid": "0000-0003-0007-2197" }, { "id": "Lacaille-Kevin-M", "name": { "family": "Lacaille", "given": "Kevin" }, "orcid": "0000-0001-9870-5663" }, { "id": "Matsuda-Yuichi", "name": { "family": "Matsuda", "given": "Yuichi" } }, { "id": "Ross-Colin", "name": { "family": "Ross", "given": "Colin" } }, { "id": "Rudie-Gwen-C", "name": { "family": "Rudie", "given": "Gwen" }, "orcid": "0000-0002-8459-5413" }, { "id": "Trainor-Ryan-F", "name": { "family": "Trainor", "given": "Ryan" }, "orcid": "0000-0002-6967-7322" } ] }, "title": "SCUBA-2 web survey: I. Observations of CO(3\u20132) in hyper-luminous QSO fields", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active \u2013 quasars: emission lines \u2013 submillimetre: galaxies", "note": "\u00a9 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2019 February 5. Received 2018 December 31; in original form 2018 October 24. Published: 13 February 2019. \n\nThe authors would like to thank Christine Done, Stuart McAlpine, and Chris Willott for their helpful discussions. This work is based on observations carried out under project number S17BS with the Institut de Radioastronomie Millim\u00e9trique (IRAM) NOEMA Interferometer. IRAM is supported by the Institut National des Sciences de l'Univers/Centre National de la Recherche Scientifique (INSU/CNRS, France), the Max Planck Gesellschaft (MPG, Germany), and the Instituto Geogr\u00e1fico Nacional (IGN, Spain). The James Clerk Maxwell Telescope is operated by the East Asian Observatory on behalf of The National Astronomical Observatory of Japan; Academia Sinica Institute of Astronomy and Astrophysics; the Korea Astronomy and Space Science Institute; the Operation, Maintenance and Upgrading Fund for Astronomical Telescopes and Facility Instruments, budgeted from the Ministry of Finance (MOF) of China and administrated by the Chinese Academy of Sciences (CAS), as well as the National Key R&D Program of China (No. 2017YFA0402700). Additional funding support is provided by the Science and Technology Facilities Council of the United Kingdom and participating universities in the United Kingdom and Canada. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. This work was supported by the Natural Sciences and Engineering Research Council of Canada. Ian Smail acknowledges the European Research Council Advanced Investigator programme DUSTYGAL 321334 and the Science and Technology Facilities Council grant ST/P000541/1. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration (NASA). Yuichi Matsuda acknowledges Japan Society for the Promotion of Science (JSPS) KAKENHI grants 17H04831 and 17KK0098. This paper includes data gathered with the 6.5\u2009m Magellan Telescopes located at Las Campanas Observatory, Chile.\n\nThe version originally published online and in print contained an error in the title. In the online version the term 'field' has been corrected to 'fields'. The publisher apologises for this error.\n\nPublished - stz429.pdf
Accepted Version - 1810.10655.pdf
Erratum - stz1075_er.pdf
", "abstract": "A primary goal of the Submillimetre Common User Bolometer Array-2 web survey is to perform tomography of the early intergalactic medium by studying systems containing some of the brightest quasi-stellar objects (QSOs; 2.5 < z < 3.0) and nearby submillimetre galaxies (SMGs). As a first step, this paper aims to characterize the galaxies that host the QSOs. To achieve this, a sample of 13 hyper-luminous (\u2060L_(AGN) > 10^(14) L\u2299) QSOs with previous submillimetre continuum detections were followed up with CO(3\u20132) observations using the NOrthern Extended Millimeter Array interferometer. All but two of the QSOs are detected in CO(3\u20132); for one non-detection, our observations show a tentative 2\u03c3 line at the expected position and redshift, and for the other non-detection we find only continuum flux density an order of magnitude brighter than the other sources. In three of the fields, a companion potentially suitable for tomography is detected in CO line emission within 25\u2009arcsec of the QSO. We derive gas masses, dynamical masses, and far-infrared luminosities, and show that the QSOs in our sample have similar properties compared to less luminous QSOs and SMGs in the literature, despite the fact that their black hole masses (which are proportional to L_(AGN)) are 1\u20132 orders of magnitude larger. We discuss two interpretations of these observations: this is due to selection effects, such as preferential face-on viewing angles and picking out objects in the tail ends of the scatter in host-galaxy mass and black hole mass relationships; or the black hole masses have been overestimated because the accretion rates are super-Eddington.", "date": "2019-05", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "485", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "753-769", "id_number": "CaltechAUTHORS:20190523-111840539", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190523-111840539", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Institut de Radioastronomie Millim\u00e9trique (IRAM)", "grant_number": "S17BS" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Max Planck Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" }, { "agency": "National Key Research and Development Program of China", "grant_number": "2017YFA0402700" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/P000541/1" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "European Research Council (ERC)", "grant_number": "321334" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17H04831" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17KK0098" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/stz429", "primary_object": { "basename": "1810.10655.pdf", "url": "https://authors.library.caltech.edu/records/fdnhb-wtz64/files/1810.10655.pdf" }, "related_objects": [ { "basename": "stz1075_er.pdf", "url": "https://authors.library.caltech.edu/records/fdnhb-wtz64/files/stz1075_er.pdf" }, { "basename": "stz429.pdf", "url": "https://authors.library.caltech.edu/records/fdnhb-wtz64/files/stz429.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Hill, Ryley; Chapman, Scott C.; et el." }, { "id": "https://authors.library.caltech.edu/records/stdpm-0na72", "eprint_id": 91335, "eprint_status": "archive", "datestamp": "2023-08-19 13:56:51", "lastmod": "2023-10-19 22:25:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Theios-R-L", "name": { "family": "Theios", "given": "Rachel L." }, "orcid": "0000-0002-4236-1037" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" } ] }, "title": "Dust Attenuation, Star Formation, and Metallicity in z ~ 2-3 Galaxies \n from KBSS-MOSFIRE", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction \u2013 galaxies: evolution \u2013 galaxies: high-redshift \u2013 galaxies: star formation \u2013 HII regions \u2013\nISM: abundances", "note": "\u00a9 2019 The American Astronomical Society.\n\nReceived 2018 April 30; revised 2018 November 8; accepted 2018 November 21; published 2019 January 25.\n\nThe authors thank Max Pettini and the anonymous referee for helpful comments. This work has been supported in part by the NSF through grants AST-0908805 and AST-1313472 (CCS, RLT, ALS), by the JPL President-Director Fund (CCS, RLT), by the Professor Wallace L. W. Sargent Graduate Fellowship (RLT) and the Troesh Family Distinguished Scholars Fund (also RLT), and by an Alfred P. Sloan Research Fellowship (NAR). Finally, the authors wish to recognize and acknowledge the significant cultural role and reverence that the summit of Maunakea has within the indigenous Hawaiian community. We are privileged to have the opportunity to conduct observations from this mountain.\n\nPublished - Theios_2019_ApJ_871_128.pdf
Submitted - 1805.00016.pdf
", "abstract": "We present a detailed analysis of 317 2.0 \u2264 z \u2264 2.7 star-forming galaxies from the Keck Baryonic Structure Survey. Using complementary spectroscopic observations with Keck/LRIS and Keck/MOSFIRE, as well as spectral energy distribution (SED) fits to broadband photometry, we examine the joint rest-UV and rest-optical properties of the same galaxies, including stellar and nebular dust attenuation, metallicity, and star formation rate (SFR). The inferred parameters of the stellar population (reddening, age, SFR, and stellar mass) are strongly dependent on the details of the assumed stellar population model and the shape of the attenuation curve. Nebular reddening is generally larger than continuum reddening, but with large scatter. Compared to local galaxies, high-redshift galaxies have lower gas-phase metallicities (and/or higher nebular excitation) at fixed nebular reddening, and higher nebular reddening at fixed stellar mass, consistent with gas fractions that increase with redshift. We find that continuum reddening is correlated with 12 + log(O/H)_(O3N2) at 3.0\u03c3 significance, whereas nebular reddening is correlated with only 1.1\u03c3 significance. This may reflect the dependence of both continuum reddening and O3N2 on the shape of the ionizing radiation field produced by the massive stars. Finally, we show that H\u03b1-based and SED-based estimates of SFR exhibit significant scatter relative to one another, and on average agree only for particular combinations of spectral synthesis models and attenuation curves. We find that the SMC extinction curve predicts consistent SFRs if we assume the subsolar (0.14 Z\u2299) binary star models that are favored for high-redshift galaxies.", "date": "2019-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "871", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 128", "id_number": "CaltechAUTHORS:20181129-135233204", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181129-135233204", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "JPL President and Director's Fund" }, { "agency": "Wallace L. W. Sargent Graduate Fellowship" }, { "agency": "Troesh Family Distinguished Scholars Fund" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aaf386", "primary_object": { "basename": "1805.00016.pdf", "url": "https://authors.library.caltech.edu/records/stdpm-0na72/files/1805.00016.pdf" }, "related_objects": [ { "basename": "Theios_2019_ApJ_871_128.pdf", "url": "https://authors.library.caltech.edu/records/stdpm-0na72/files/Theios_2019_ApJ_871_128.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Theios, Rachel L.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/t59zs-kmb59", "eprint_id": 91336, "eprint_status": "archive", "datestamp": "2023-08-19 13:24:24", "lastmod": "2023-10-19 22:25:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Bogosavljevi\u0107-M", "name": { "family": "Bogosavljevi\u0107", "given": "Milan" } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" } ] }, "title": "The Keck Lyman Continuum Spectroscopic Survey (KLCS): The Emergent Ionizing Spectrum of Galaxies at z \u223c 3", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 galaxies: evolution \u2013 galaxies: high-redshift \u2013 intergalactic medium \u2013 ultraviolet: galaxies", "note": "\u00a9 2018 The American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2018 May 16; revised 2018 October 18; accepted 2018 October 27; published 2018 December 18. \n\nBased on data obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W.M. Keck Foundation. \n\nThis work has been supported in part by the US National Science Foundation through grants AST-0606912, AST-0908805, and AST-1313472 (M.B., C.C.S., G.C.R., R.F.T., A.L.S.). C.C.S. acknowledges additional support from the John D. and Catherine T. MacArthur Foundation, the David and Lucile Packard Foundation, and the JPL/Caltech President's and Director's program. We thank J. J. Eldridge and Elizabeth Stanway for their continued work developing the BPASS SPS models and for many illuminating conversations. We are grateful to the dedicated staff of the W.M. Keck Observatory who keep the instruments and telescopes running effectively. We wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests.\n\nPublished - Steidel_2018_ApJ_869_123.pdf
Submitted - 1805.06071.pdf
", "abstract": "We present results of a deep spectroscopic survey quantifying the statistics of the escape of ionizing radiation from star-forming galaxies at z ~ 3. We measure the ratio of ionizing to non-ionizing UV flux density \u3008f_(900)/f_(1500) \u3009_(obs), where f_(900) is the mean flux density evaluated over the range [880, 910] \u00c5. We quantify the emergent ratio of ionizing to non-ionizing UV flux density by analyzing high signal-to-noise ratio composite spectra formed from subsamples with common observed properties and numbers sufficient to reduce the statistical uncertainty in the modeled IGM+CGM correction to obtain precise values of \u3008f_(900)/f_(1500) \u3009_(out), including a full-sample average \u3008f_(900)/f_(1500) \u3009_(out) = 0.057 \u00b1 0.006. We show that \u3008f_(900)/f_(1500) \u3009_(out) increases monotonically with W_ \u03bb(Ly\u03b1), inducing an inverse correlation with UV luminosity as a by-product. We fit the composite spectra using stellar spectral synthesis together with models of the ISM in which a fraction f c of the stellar continuum is covered by gas with column density N_(H1). We show that the composite spectra simultaneously constrain the intrinsic properties of the stars (L_(900)/L_(1500))_(int) along with f_c , N_(H1), E(B - V), and f_(esc,abs), the absolute escape fraction of ionizing photons. We find a sample-averaged f-(esc,abs) = 0.09 \u00b1 0.01, with subsamples falling along a linear relation \u3008f_(esc,abs) \u3009 \u2243\n0.75[W_ \u03bb(Ly\u03b1)/110 \u00c5]. Using the far-UV luminosity function, the distribution function n(W(Ly\u03b1)), and the relationship between W_ \u03bb(Ly\u03b1) and f_(900)/f_(1500) \u3009_(out), we estimate the total ionizing emissivity of z ~ 3 star-forming galaxies with M_(uv) \u2264 \u221219.5, which exceeds the contribution of quasi-stellar objects by a factor of ~3, and accounts for ~50% of the total \u03f5_(LyC) at z ~ 3 estimated using indirect methods.", "date": "2018-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "869", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 123", "id_number": "CaltechAUTHORS:20181129-135236660", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181129-135236660", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "JPL President and Director's Fund" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aaed28", "primary_object": { "basename": "1805.06071.pdf", "url": "https://authors.library.caltech.edu/records/t59zs-kmb59/files/1805.06071.pdf" }, "related_objects": [ { "basename": "Steidel_2018_ApJ_869_123.pdf", "url": "https://authors.library.caltech.edu/records/t59zs-kmb59/files/Steidel_2018_ApJ_869_123.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Steidel, Charles C.; Bogosavljevi\u0107, Milan; et el." }, { "id": "https://authors.library.caltech.edu/records/6xg2f-w4a38", "eprint_id": 91329, "eprint_status": "archive", "datestamp": "2023-08-22 00:26:55", "lastmod": "2023-10-19 22:25:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" } ] }, "title": "Measuring the Physical Conditions in High-redshift Star-forming Galaxies: Insights from KBSS-MOSFIRE", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: ISM; galaxies: high-redshift; H ii regions; ISM: abundances", "note": "\u00a9 2018. The American Astronomical Society. \n\nReceived 2017 November 20; revised 2018 September 3; accepted 2018 September 12; published 2018 November 29. \n\nThe data presented in this paper were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. This work has been supported in part by a US National Science Foundation (NSF) Graduate Research Fellowship (A.L.S.), by the NSF through grants AST-0908805 and AST-1313472 (C.C.S. and A.L.S.). Finally, the authors wish to recognize and acknowledge the significant cultural role and reverence that the summit of Maunakea has within the indigenous Hawaiian community. We are privileged to have the opportunity to conduct observations from this mountain.\n\nPublished - Strom_2018_ApJ_868_117.pdf
Accepted Version - 1711.08820
", "abstract": "We use photoionization models that are designed to reconcile the joint rest-UV-optical spectra of high-z star-forming galaxies to self-consistently infer the gas chemistry and nebular ionization and excitation conditions for ~150 galaxies from the Keck Baryonic Structure Survey (KBSS), using only observations of their rest-optical nebular spectra. We find that the majority of z ~ 2\u20133 KBSS galaxies are moderately O-rich, with an interquartile range in 12 + log(O/H) = 8.29\u20138.56, and have significantly sub-solar Fe enrichment, with an interquartile range of [Fe/H] = [\u22120.79, \u22120.53], which contributes additional evidence in favor of super-solar O/Fe in high-z galaxies. The model-inferred ionization parameters and N/O are strongly correlated with common strong-line indices (such as O32 and N2O2), with the latter exhibiting similar behavior to local extragalactic H ii regions. In contrast, diagnostics commonly used for measuring gas-phase O/H (such as N2 and O3N2) show relatively large scatter with the overall amount of oxygen present in the gas and behave differently than observed at z ~ 0. We provide a new calibration for using R23 to measure O/H in typical high-z galaxies, although it is most useful for relatively O-rich galaxies; combining O32 and R23 does not yield a more effective calibration. Finally, we consider the implications for the intrinsic correlations between physical conditions across the galaxy sample and find that N/O varies with O/H in high-z galaxies in a manner that is almost identical to local H ii regions. However, we do not find a strong anti-correlation between ionization parameter and metallicity (O/H or Fe/H) in high-z galaxies, which is one of the principal bases for using strong-line ratios to infer oxygen abundance.", "date": "2018-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "868", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 117", "id_number": "CaltechAUTHORS:20181129-110052473", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181129-110052473", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aae1a5", "primary_object": { "basename": "1711.08820", "url": "https://authors.library.caltech.edu/records/6xg2f-w4a38/files/1711.08820" }, "related_objects": [ { "basename": "Strom_2018_ApJ_868_117.pdf", "url": "https://authors.library.caltech.edu/records/6xg2f-w4a38/files/Strom_2018_ApJ_868_117.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Strom, Allison L.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/kk3q3-vy571", "eprint_id": 90344, "eprint_status": "archive", "datestamp": "2023-08-19 12:02:36", "lastmod": "2023-10-18 23:23:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Chen-Yuguang", "name": { "family": "Chen", "given": "Yuguang" }, "orcid": "0000-0003-4520-5395" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" } ] }, "title": "Imaging Spectroscopy of Ionized Gaseous Nebulae around Optically Faint AGNs at Redshift z \u223c 2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active \u2013 galaxies: fundamental parameters \u2013 galaxies: high-redshift \u2013 galaxies: structure", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 July 26; revised 2018 September 7; accepted 2018 September 11; published 2018 October 19. \n\nThe authors thank Alice Shapley, Dawn Erb, Naveen Reddy, and Max Pettini for their participation in early KBSS observations, particularly the near-IR and Spitzer mid-IR photometry and the Keck/LRIS spectroscopic campaign. D.R.L. also thanks Alice Shapley for assistance with early OSIRIS observations and Jay Anderson for assistance with PSF subtraction of the Q2343-BX415 HST imaging and appreciates productive conversations with Tim Heckman, Nadia Zakamska, and the STScI AGN Reading Group. This work includes observations taken by the CANDELS Multi-Cycle Treasury Program and 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. Finally, we wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests.\n\nPublished - Law_2018_ApJ_866_119.pdf
Accepted Version - 1809.04089.pdf
", "abstract": "We present Keck/OSIRIS laser guide-star assisted adaptive optics (LGSAO) integral-field spectroscopy of [O III] \u03bb5007 nebular emission from 12 galaxies hosting optically faint (R = 20\u201325; \u03bd L_\u03bd ~ 10^(44) \u2013 10^(46) erg s^(\u22121)) active galactic nuclei (AGNs) at redshift z ~ 2\u20133. In combination with deep Hubble Space Telescope Wide Field Camera 3 (HST/WFC3) rest-frame optical imaging, Keck/MOSFIRE rest-optical spectroscopy, and Keck/KCWI rest-UV integral-field spectroscopy, we demonstrate that both the continuum and emission-line structures of these sources exhibit a wide range of morphologies, from compact, isolated point sources to double-AGN merging systems with extensive ~50 kpc tidal tails. One of the 12 galaxies previously known to exhibit a proximate damped Ly\u03b1 system coincident in redshift with the galaxy shows evidence for both an extended [O III] narrow-line emission region and spatially offset Ly\u03b1 emission (with morphologically distinct blueshifted and redshifted components) indicative of large-scale gas flows photoionized by the central AGN. We do not find widespread evidence of star formation in the host galaxies surrounding these AGNs; the [O III] velocity dispersions tend to be high (\u03c3 = 100\u2013500 km s^(-1)), the continuum morphologies are much more compact than a mass-matched star-forming comparison sample, and the diagnostic nebular emission-line ratios are dominated by an AGN-like ionizing spectrum. The sample is most consistent with a population of AGNs that radiate at approximately their Eddington limit and photoionize extended [O III] nebulae whose characteristic sizes scale approximately as the square root of the AGN luminosity.", "date": "2018-10-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "866", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 119", "id_number": "CaltechAUTHORS:20181023-082855040", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181023-082855040", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO 12177" }, { "agency": "NASA", "grant_number": "GO 12328" }, { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aae156", "primary_object": { "basename": "1809.04089.pdf", "url": "https://authors.library.caltech.edu/records/kk3q3-vy571/files/1809.04089.pdf" }, "related_objects": [ { "basename": "Law_2018_ApJ_866_119.pdf", "url": "https://authors.library.caltech.edu/records/kk3q3-vy571/files/Law_2018_ApJ_866_119.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Law, David R.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/egwej-8z636", "eprint_id": 88670, "eprint_status": "archive", "datestamp": "2023-08-19 10:32:01", "lastmod": "2023-10-18 22:13:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Chen-Yuguang", "name": { "family": "Chen", "given": "Yuguang" }, "orcid": "0000-0003-4520-5395" } ] }, "title": "The Kinematics of Extended Ly\u03b1 Emission in a Low-mass, Low-metallicity Galaxy at z = 2.3", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 galaxies: evolution \u2013 galaxies: high-redshift", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 May 21; revised 2018 June 19; accepted 2018 June 28; published 2018 July 24. \n\nThe data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. \n\nThe authors thank the referee for a thoughtful and constructive report, Max Gronke, David Kaplan, Aaron Smith, and Anne Verhamme for useful discussions and suggestions, KCWI team members Don Neill and Matt Matuszewski for their continued development of the KCWI DRP and for very useful conversations, and the organizers and participants of the \"Sakura Cosmic Ly\u03b1 Workshop\" at the University of Tokyo in 2018 March. D.K.E. is supported by the US National Science Foundation through the Faculty Early Career Development (CAREER) Program, grant AST-1255591. C.C.S. and Y.C. acknowledge support from the Caltech/JPL President's and Director's Fund. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. \n\nFacility: Keck:II (KCWI). - \n\nSoftware: KCWI DRP,4 astropy (Astropy Collaboration et al. 2013), spectral_cube (Ginsburg et al. 2015), QFitsView,5 seaborn (Waskom et al. 2017).\n\nPublished - Erb_2018_ApJL_862_L10.pdf
Accepted Version - 1807.00065.pdf
", "abstract": "Ly\u03b1 photons are resonantly scattered by neutral hydrogen, and may therefore trace both the spatial extent and the kinematics of the gas surrounding galaxies. We present new observations of the extended Ly\u03b1 halo of Q2343-BX418, a low-mass (M\u22c6 = 5 x 10^8 M\u2299), low-metallicity (Z \u2248 0.25 Z\u2299) star-forming galaxy at z = 2.3. Using the Keck Cosmic Web Imager (KCWI), the blue-sensitive optical integral field spectrograph recently installed on the Keck II telescope, we detect Ly\u03b1 in emission to a radius of 23 kpc, and measure an exponential scale length of 6 kpc in the outer region of the extended halo. We study the double-peaked spectroscopic Ly\u03b1 profile in individual spectral pixels (\"spaxels\") over a ~25 \u00d7 30 kpc region, finding significant variations in the peak ratio and peak separation. The profile is dominated by the red peak in the central regions, while in the outskirts of the extended halo the red and blue peak strengths are roughly equal; these observations are consistent with a model in which the peak ratio is largely determined by the radial component of the outflow velocity. We find a gradient of 300 km s^(-1) in the Ly\u03b1 peak separation across the extended halo, indicating variations in the column density, covering fraction, or velocity range of the gas. These new observations emphasize the need for realistic, spatially resolved models of Ly\u03b1 radiative transfer in the halos of galaxies.", "date": "2018-07-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "862", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L10", "id_number": "CaltechAUTHORS:20180808-145514148", "issn": "2041-8213", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180808-145514148", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NSF", "grant_number": "AST-1255591" }, { "agency": "Caltech/JPL President and Director Fund" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/2041-8213/aacff6", "primary_object": { "basename": "1807.00065.pdf", "url": "https://authors.library.caltech.edu/records/egwej-8z636/files/1807.00065.pdf" }, "related_objects": [ { "basename": "Erb_2018_ApJL_862_L10.pdf", "url": "https://authors.library.caltech.edu/records/egwej-8z636/files/Erb_2018_ApJL_862_L10.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Erb, Dawn K.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/vak9j-gtx16", "eprint_id": 88485, "eprint_status": "archive", "datestamp": "2023-08-21 23:36:54", "lastmod": "2023-10-18 22:05:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P. A." }, "orcid": "0000-0001-5851-6649" }, { "id": "Montes-M", "name": { "family": "Montes", "given": "M." }, "orcid": "0000-0001-7847-0393" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "N." }, "orcid": "0000-0001-9687-4973" }, { "id": "Bouwens-R-J", "name": { "family": "Bouwens", "given": "R. J." }, "orcid": "0000-0002-4989-2471" }, { "id": "Illingworth-G-D", "name": { "family": "Illingworth", "given": "G. D." }, "orcid": "0000-0002-8096-2837" }, { "id": "Magee-D-K", "name": { "family": "Magee", "given": "D." } }, { "id": "Atek-H", "name": { "family": "Atek", "given": "H." }, "orcid": "0000-0002-7570-0824" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Cibinel-A", "name": { "family": "Cibinel", "given": "A." }, "orcid": "0000-0003-4578-514X" }, { "id": "Franx-M", "name": { "family": "Franx", "given": "M." }, "orcid": "0000-0002-8871-3026" }, { "id": "Holden-B-P", "name": { "family": "Holden", "given": "B." }, "orcid": "0000-0002-6153-3076" }, { "id": "Labb\u00e9-I", "name": { "family": "Labb\u00e9", "given": "I." }, "orcid": "0000-0002-2057-5376" }, { "id": "Nelson-E-J", "name": { "family": "Nelson", "given": "E. J." }, "orcid": "0000-0002-7524-374X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "van-Dokkum-P-G", "name": { "family": "van Dokkum", "given": "P. G." }, "orcid": "0000-0002-8282-9888" }, { "id": "Morselli-L", "name": { "family": "Morselli", "given": "L." } }, { "id": "Naidu-R-P", "name": { "family": "Naidu", "given": "R. P." }, "orcid": "0000-0003-3997-5705" }, { "id": "Wilkins-S", "name": { "family": "Wilkins", "given": "S." } } ] }, "title": "HDUV: The Hubble Deep UV Legacy Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: abundances; galaxies: evolution; techniques: image processing", "note": "\u00a9 2018. The American Astronomical Society. \n\nReceived 2016 September 1; revised 2018 May 17; accepted 2018 June 5; published 2018 July 13. \n\n\nBased on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in\nAstronomy, Inc. under NASA contract NAS 5-26555. The data are available from the Mikulski Archive for Space Telescopes (MAST) at doi:10.17909/T90T2N.\n\nThe authors thank the anonymous referee who helped improve this manuscript and encouraged the release of the initial catalogs. The authors thank Marc Rafelski, Brian Siana, and Harry Teplitz for several very helpful discussions regarding the WFC3/UVIS data acquisition and reduction. The authors also thank Tomer Tal for help during the proposal stage, and Ros Skelton for help with the 3D-HST detection images and SExtractor settings. Support for this work was provided by NASA through grant HST-GO-13872 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. P.O. further acknowledges support by the Swiss National Science Foundation. The data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). \n\nFacility: HST(ACS/WFC3). -\n\nPublished - Oesch_2018_ApJS_237_12.pdf
Accepted Version - 1806.01853
", "abstract": "We present the Hubble Deep UV Legacy Survey (HDUV), a 132-orbit imaging program with the WFC3/UVIS camera on board the Hubble Space Telescope (HST). The HDUV extends and builds on the few previous UV imaging surveys in the two GOODS/CANDELS-Deep fields to provide deep images over a total area of ~100 arcmin2 in the two filters F275W and F336W. Our release also includes all the F275W imaging data taken by the CANDELS survey, which were aligned using a novel approach and combined with the HDUV survey data. By reaching depths of 27.5\u201328.0 mag (5\u03c3 in 0farcs4 apertures), these are the deepest high-resolution UV data over such a large area taken to date. Such unique UV imaging enables a wide range of science by the community. A few of the main goals of the HDUV survey are as follows: (1) to provide a complete sample of faint star-forming galaxies at z ~ 1\u20133; (2) to constrain the ionizing photon escape fraction from galaxies at z ~ 2\u20133; and (3) to track the build-up of bulges and the disappearance of clumpy disk galaxies through reliable internal stellar population properties at sub-kiloparsec resolution out to z ~ 3. The addition of the HDUV data further enhances the legacy value of the two GOODS/CANDELS-Deep fields, which now include deep 11-band HST imaging, as well as very deep ancillary data from X-ray to radio, enabling unique multi-wavelength studies. Here, we provide an overview of the survey design, describe the data reduction, and highlight a few basic analyses of the images that are available to the community as high-level science products, via the Mikulski Archive for Space Telescopes.", "date": "2018-07", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "237", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 12", "id_number": "CaltechAUTHORS:20180801-164036045", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180801-164036045", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-13872" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4365/aacb30", "primary_object": { "basename": "1806.01853", "url": "https://authors.library.caltech.edu/records/vak9j-gtx16/files/1806.01853" }, "related_objects": [ { "basename": "Oesch_2018_ApJS_237_12.pdf", "url": "https://authors.library.caltech.edu/records/vak9j-gtx16/files/Oesch_2018_ApJS_237_12.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Oesch, P. A.; Montes, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/2q37d-d1838", "eprint_id": 87053, "eprint_status": "archive", "datestamp": "2023-08-19 09:45:42", "lastmod": "2023-10-18 20:49:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Du-Xinnan", "name": { "family": "Du", "given": "Xinnan" } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Jones-T", "name": { "family": "Jones", "given": "Tucker" }, "orcid": "0000-0001-5860-3419" }, { "id": "Stark-D-P", "name": { "family": "Stark", "given": "Daniel P." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" } ] }, "title": "The Redshift Evolution of Rest-UV Spectroscopic Properties in Lyman-break Galaxies at z ~ 2\u20134", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: high-redshift \u2013 galaxies: ISM", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 March 15; revised 2018 April 18; accepted 2018 April 19; published 2018 June 13. \n\nWe acknowledge support from the David & Lucile Packard Foundation (A.E.S). We are grateful to the 3D-HST team for providing ancillary data on galaxy properties. This paper also includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible.\n\nPublished - Du_2018_ApJ_860_75.pdf
Accepted Version - 1803.05912.pdf
", "abstract": "We present the first comprehensive evolutionary analysis of the rest-frame UV spectroscopic properties of star-forming galaxies at z ~ 2\u20134. We match samples at different redshifts in UV luminosity and stellar mass, and perform systematic measurements of spectral features and stellar population modeling. By creating composite spectra grouped according to Ly\u03b1 equivalent width (EW) and various galaxy properties, we study the evolutionary trends among Ly\u03b1, low- and high-ionization interstellar (LIS and HIS) absorption features, and integrated galaxy properties. We also examine the redshift evolution of Ly\u03b1 and LIS absorption kinematics, and fine-structure emission EWs. The connections among the strengths of Ly\u03b1, LIS lines, and dust extinction are redshift independent, as is the decoupling of the Ly\u03b1 and HIS line strengths, and the bulk outflow kinematics as traced by the LIS lines. Stronger Ly\u03b1 emission is observed at higher redshift at fixed UV luminosity, stellar mass, SFR, and age. Much of this variation in the average Ly\u03b1 strength with redshift, and the variation in Ly\u03b1 strength at fixed redshift, can be explained in terms of variations in the neutral gas covering fraction and/or dust content in the ISM and CGM. However, based on the connection between Ly\u03b1 and C iii] emission strengths, we additionally find evidence for variations in the intrinsic production rate of Ly\u03b1 photons at the highest Ly\u03b1 EWs. The challenge now is to understand the observed evolution of the neutral gas covering fraction and dust extinction within a coherent model for galaxy formation, and make robust predictions for the escape of ionizing radiation at z > 6.", "date": "2018-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "860", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 75", "id_number": "CaltechAUTHORS:20180613-094038182", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180613-094038182", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "David and Lucile Packard Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aabfcf", "primary_object": { "basename": "1803.05912.pdf", "url": "https://authors.library.caltech.edu/records/2q37d-d1838/files/1803.05912.pdf" }, "related_objects": [ { "basename": "Du_2018_ApJ_860_75.pdf", "url": "https://authors.library.caltech.edu/records/2q37d-d1838/files/Du_2018_ApJ_860_75.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Du, Xinnan; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/arbz6-cbp56", "eprint_id": 86323, "eprint_status": "archive", "datestamp": "2023-08-19 09:12:22", "lastmod": "2023-10-18 19:28:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hayward-C-C", "name": { "family": "Hayward", "given": "Christopher C." }, "orcid": "0000-0003-4073-3236" }, { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "Scott C." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Golob-A", "name": { "family": "Golob", "given": "Anneya" } }, { "id": "Casey-C-M", "name": { "family": "Casey", "given": "Caitlin M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Smith-D-J-B", "name": { "family": "Smith", "given": "Daniel J. B." } }, { "id": "Zitrin-Adi", "name": { "family": "Zitrin", "given": "Adi" }, "orcid": "0000-0002-0350-4488" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bremer-M-N", "name": { "family": "Bremer", "given": "Malcolm N." } }, { "id": "Chen-Chian-Chou", "name": { "family": "Chen", "given": "Chian-Chou" }, "orcid": "0000-0002-3805-0789" }, { "id": "Coppin-K-E-K", "name": { "family": "Coppin", "given": "Kristen E. K." } }, { "id": "Farrah-D", "name": { "family": "Farrah", "given": "Duncan" }, "orcid": "0000-0003-1748-2010" }, { "id": "Ibar-E", "name": { "family": "Ibar", "given": "Eduardo" } }, { "id": "Micha\u0142owski-M-J", "name": { "family": "Micha\u0142owski", "given": "Micha\u0142 J." }, "orcid": "0000-0001-9033-4140" }, { "id": "Sawicki-M", "name": { "family": "Sawicki", "given": "Marcin" }, "orcid": "0000-0002-7712-7857" }, { "id": "Scott-D", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "van-der-Werf-P-P", "name": { "family": "van der Werf", "given": "Paul" }, "orcid": "0000-0001-5434-5942" }, { "id": "Fazio-G-G", "name": { "family": "Fazio", "given": "Giovanni G." }, "orcid": "0000-0002-0670-0708" }, { "id": "Geach-J-E", "name": { "family": "Geach", "given": "James E." }, "orcid": "0000-0003-4964-4635" }, { "id": "Gurwell-M-A", "name": { "family": "Gurwell", "given": "Mark" }, "orcid": "0000-0003-0685-3621" }, { "id": "Petitpas-G-R", "name": { "family": "Petitpas", "given": "Glen" } }, { "id": "Wilner-D-J", "name": { "family": "Wilner", "given": "David J." }, "orcid": "0000-0003-1526-7587" } ] }, "title": "Observational constraints on the physical nature of submillimetre source multiplicity: chance projections are common", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift \u2013 galaxies: starburst \u2013 infrared: galaxies \u2013 submillimetre: galaxies", "note": "\u00a9 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2018 February 1. Received 2018 January 29; in original form 2017 August 25. Published: 09 February 2018. \n\nCCH thanks Nick Scoville for encouragement to try his hand at observing, Ian Smail for inspiration via his Fifth Rule of Observational Cosmology (If you see an observational paper with a theorist as lead author be very afraid), and Allison Strom for advice when planning the observations. We also thank James Simpson and Ian Smail for comments on an earlier version of the manuscript, Mark Swinbank for useful discussion, and the anonymous referee for useful comments that led us to improve the manuscript. The Flatiron Institute is supported by the Simons Foundation. Some of this work was supported by a National Aeronautics and Space Administration (NASA) Keck PI Data Award, administered by the NASA Exoplanet Science Institute. EI acknowledges partial support from Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT) through grant no. \u20091171710. MJM acknowledges the support of the National Science Centre, Poland through POLONEZ grant 2015/19/P/ST9/04010. This project has received funding from the European Union's Horizon 2020 research and innovation programme under Marie Sk\u0142odowska-Curie grant agreement no. \u2009665778. \n\nSome of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Partially based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the National Science Foundation (NSF) on behalf of the Gemini partnership: the NSF (United States), the National Research Council (Canada), Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT) (Chile), Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina), and Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil). \n\nThis research has made use of the NASA/Infrared Processing and Analysis Center (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, the VizieR data base of astronomical catalogues (Ochsenbein, Bauer & Marcout 2000), NASA's Astrophysics Data System Bibliographic Services, the arXiv.org preprint server, and ASTROPY, a community-developed core PYTHON package for astronomy (Astropy Collaboration 2013).\n\nPublished - sty304.pdf
Accepted Version - 1802.00452.pdf
", "abstract": "Interferometric observations have demonstrated that a significant fraction of single-dish submillimetre (submm) sources are blends of multiple submm galaxies (SMGs), but the nature of this multiplicity, i.e. whether the galaxies are physically associated or chance projections, has not been determined. We performed spectroscopy of 11 SMGs in six multicomponent submm sources, obtaining spectroscopic redshifts for nine of them. For an additional two component SMGs, we detected continuum emission but no obvious features. We supplement our observed sources with four single-dish submm sources from the literature. This sample allows us to statistically constrain the physical nature of single-dish submm source multiplicity for the first time. In three (3/7, or 43^(+39__(\u221233) per cent at 95 percent confidence) of the single-dish sources for which the nature of the blending is unambiguous, the components for which spectroscopic redshifts are available are physically associated, whereas 4/7 (57^(+33)_(\u221239) per cent) have at least one unassociated component. When components whose spectra exhibit continuum but no features and for which the photometric redshift is significantly different from the spectroscopic redshift of the other component are also considered, 6/9 (67^(+26)_(\u221237) per cent) of the single-dish sources are comprised of at least one unassociated component SMG. The nature of the multiplicity of one single-dish source is ambiguous. We conclude that physically associated systems and chance projections both contribute to the multicomponent single-dish submm source population. This result contradicts the conventional wisdom that bright submm sources are solely a result of merger-induced starbursts, as blending of unassociated galaxies is also important.", "date": "2018-05-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "476", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "2278-2287", "id_number": "CaltechAUTHORS:20180509-152638878", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180509-152638878", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Simons Foundation" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1171710" }, { "agency": "National Science Centre (Poland)", "grant_number": "2015/19/P/ST9/04010" }, { "agency": "Marie Curie Fellowship", "grant_number": "665778" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/sty304", "primary_object": { "basename": "1802.00452.pdf", "url": "https://authors.library.caltech.edu/records/arbz6-cbp56/files/1802.00452.pdf" }, "related_objects": [ { "basename": "sty304.pdf", "url": "https://authors.library.caltech.edu/records/arbz6-cbp56/files/sty304.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Hayward, Christopher C.; Chapman, Scott C.; et el." }, { "id": "https://authors.library.caltech.edu/records/9ag5t-p7362", "eprint_id": 85244, "eprint_status": "archive", "datestamp": "2023-08-19 08:17:51", "lastmod": "2023-10-18 18:00:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cooke-R-J", "name": { "family": "Cooke", "given": "Ryan J." }, "orcid": "0000-0001-7653-5827" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "One Percent Determination of the Primordial Deuterium Abundance", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 cosmology: theory \u2013 primordial nucleosynthesis \u2013 quasars: absorption lines \u2013 quasars: individual (Q1243+307)", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2017 July 26; revised 2018 January 26; accepted 2018 January 27; published 2018 March 12. \n\nBased on observations collected at the W.M. Keck Observatory which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. \n\nWe are grateful to the staff astronomers at Keck Observatory for their assistance with the observations, and to Jason X. Prochaska, Tom Barlow, and Michael T. Murphy for providing some of the software that was used to reduce the data. We also thank an anonymous referee who provided helpful suggestions that improved the presentation of this work, following a referee who was unable to respond in a timely manner. During this work, R.J.C. was supported by a Royal Society University Research Fellowship. R.J.C. acknowledges support from STFC (ST/L00075X/1, ST/P000541/1). C.C.S. has been supported by grant AST-1313472 from the U.S. NSF. This research was also supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time partially allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We thank the Hawaiian people for the opportunity to observe from MaunaKea; without their hospitality, this work would not have been possible. This work used the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (http://www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, and STFC DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure. This research has made use of NASA's Astrophysics Data System. R.J.C. thanks S.O.C. for her impeccable timing and invaluable insight. \n\nFacility: Keck(HIRES) - . \n\nSoftware: Astropy (Astropy Collaboration et al. 2013), Matplotlib (Hunter 2007), NumPy (van der Walt et al. 2011).\n\nPublished - Cooke_2018_ApJ_855_102.pdf
Accepted Version - 1710.11129.pdf
", "abstract": "We report a reanalysis of a near-pristine absorption system, located at a redshift z_(abs) = 2.52564 toward the quasar Q1243+307, based on the combination of archival and new data obtained with the HIRES echelle spectrograph on the Keck telescope. This absorption system, which has an oxygen abundance [O/H] = \u22122.769 \u00b1 0.028 ( 1/600 of the solar abundance), is among the lowest metallicity systems currently known where a precise measurement of the deuterium abundance is afforded. Our detailed analysis of this system concludes, on the basis of eight D I absorption lines, that the deuterium abundance of this gas cloud is log_(10)(D/H) = -4.622 \u00b1 0.015, which is in very good agreement with the results previously reported by Kirkman et al., but with an improvement on the precision of this single measurement by a factor of ~3.5. Combining this new estimate with our previous sample of six high precision and homogeneously analyzed D/H measurements, we deduce that the primordial deuterium abundance is log_(10)(D/H)_P = -4.5974 \u00b1 0.0052 or, expressed as a linear quantity, 10^5(D/H)_P = 2.527 \u00b1 0.030; this value corresponds to a one percent determination of the primordial deuterium abundance. Combining our result with a big bang nucleosynthesis (BBN) calculation that uses the latest nuclear physics input, we find that the baryon density derived from BBN agrees to within 2\u03c3 of the latest results from the Planck cosmic microwave background data.", "date": "2018-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "855", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 102", "id_number": "CaltechAUTHORS:20180312-102710851", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180312-102710851", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L00075X/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/P000541/1" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "NASA" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/K00042X/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/H008519/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/K003267/1" }, { "agency": "Durham University" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aaab53", "primary_object": { "basename": "1710.11129.pdf", "url": "https://authors.library.caltech.edu/records/9ag5t-p7362/files/1710.11129.pdf" }, "related_objects": [ { "basename": "Cooke_2018_ApJ_855_102.pdf", "url": "https://authors.library.caltech.edu/records/9ag5t-p7362/files/Cooke_2018_ApJ_855_102.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Cooke, Ryan J.; Pettini, Max; et el." }, { "id": "https://authors.library.caltech.edu/records/0zej3-aam34", "eprint_id": 84618, "eprint_status": "archive", "datestamp": "2023-09-28 19:53:39", "lastmod": "2023-10-24 15:26:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "Pascal A." }, "orcid": "0000-0001-5851-6649" }, { "id": "Bouwens-R-J", "name": { "family": "Bouwens", "given": "Rychard J." }, "orcid": "0000-0002-4989-2471" }, { "id": "Montes-M", "name": { "family": "Montes", "given": "Mireia" }, "orcid": "0000-0001-7847-0393" }, { "id": "Illingworth-G-D", "name": { "family": "Illingworth", "given": "Garth D." }, "orcid": "0000-0002-6668-2011" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "van-Dokkum-P-G", "name": { "family": "van Dokkum", "given": "Pieter G." }, "orcid": "0000-0002-8282-9888" }, { "id": "Atek-H", "name": { "family": "Atek", "given": "Hakim" }, "orcid": "0000-0002-7570-0824" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "Marcella C." }, "orcid": "0000-0003-1624-7609" }, { "id": "Cibinel-A", "name": { "family": "Cibinel", "given": "Anna" }, "orcid": "0000-0003-4578-514X" }, { "id": "Holden-B", "name": { "family": "Holden", "given": "Brad" }, "orcid": "0000-0002-6153-3076" }, { "id": "Labb\u00e9-I", "name": { "family": "Labb\u00e9", "given": "Ivo" }, "orcid": "0000-0002-2057-5376" }, { "id": "Magee-D-K", "name": { "family": "Magee", "given": "Dan" } }, { "id": "Morselli-", "name": { "family": "Morselli", "given": "Laura" } }, { "id": "Nelson-E-J", "name": { "family": "Nelson", "given": "Erica J." }, "orcid": "0000-0002-7524-374X" }, { "id": "Wilkins-S", "name": { "family": "Wilkins", "given": "Steve" } } ] }, "title": "The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "dark ages, reionization, first stars dust, extinction galaxies: evolution galaxies: formation galaxies: high-redshift galaxies: ISM", "note": "\u00a9 2018 American Astronomical Society. \n\nReceived 2017 May 24. Accepted 2017 December 18. Published 2018 January 23. \n\nThis work was supported by NASA through grant HST-GO-13871 and from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. K. Penner kindly provided data from his published work in electronic format. N.A.R. is supported by an Alfred P. Sloan Research Fellowship.\n\nPublished - Reddy_2018_ApJ_853_56.pdf
Submitted - 1705_09302.pdf
", "abstract": "We use a newly assembled sample of 3545 star-forming galaxies with secure spectroscopic, grism, and photometric redshifts at z = 1.5\u20132.5 to constrain the relationship between UV slope (\u03b2) and dust attenuation (L_(IR)/L_(UV) \u2261 IRX). Our sample significantly extends the range of L_(UV) and \u03b2 probed in previous UV-selected samples, including those as faint as M_(1600) = \u221217.4 (\u22430.05L_(UV)^*) and \u22122.6 \u227e \u03b2 \u227e 0.0. IRX is measured using stacks of deep Herschel data, and the results are compared with predictions of the IRX\u2212\u03b2 relation for different assumptions of the stellar population model and obscuration curve. We find that z = 1.5\u20132.5 galaxies have an IRX\u2212\u03b2 relation that is consistent with the predictions for an SMC curve if we invoke subsolar-metallicity models currently favored for high-redshift galaxies, while the commonly assumed starburst curve overpredicts the IRX at a given \u03b2 by a factor of \u22733. IRX is roughly constant with L_(UV) for L_(UV) \u2273 3 \u00d7 10^9 L_\u2299. Thus, the commonly observed trend of fainter galaxies having bluer \u03b2 may simply reflect bluer intrinsic slopes for such galaxies, rather than lower obscurations. The IRX\u2212\u03b2 relation for young/low-mass galaxies at z \u2273 2 implies a dust curve that is steeper than the SMC. The lower attenuations and higher ionizing photon output for low-metallicity stellar populations point to Lyman continuum production efficiencies, \u03be_(ion), that may be elevated by a factor of \u22482 relative to the canonical value for L^* galaxies, aiding in their ability to keep the universe ionized at z ~ 2.", "date": "2018-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "853", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 56", "id_number": "CaltechAUTHORS:20180201-082359298", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180201-082359298", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-13871" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aaa3e7", "primary_object": { "basename": "1705.09302.pdf", "url": "https://authors.library.caltech.edu/records/0zej3-aam34/files/1705.09302.pdf" }, "related_objects": [ { "basename": "Reddy_2018_ApJ_853_56.pdf", "url": "https://authors.library.caltech.edu/records/0zej3-aam34/files/Reddy_2018_ApJ_853_56.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Reddy, Naveen A.; Oesch, Pascal A.; et el." }, { "id": "https://authors.library.caltech.edu/records/k90je-bxd26", "eprint_id": 84392, "eprint_status": "archive", "datestamp": "2023-08-21 22:35:47", "lastmod": "2023-10-18 16:10:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Topping-M-W", "name": { "family": "Topping", "given": "Michael W." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Naoz-S", "name": { "family": "Naoz", "given": "Smadar" }, "orcid": "0000-0002-9802-9279" }, { "id": "Primack-J-R", "name": { "family": "Primack", "given": "Joel R." }, "orcid": "0000-0001-5091-5098" } ] }, "title": "Understanding Large-scale Structure in the SSA22 Protocluster Region Using Cosmological Simulations", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: individual (SSA22); galaxies: formation; galaxies: high-redshift; galaxies: starburst; large-scale structure of universe", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2017 September 18. Accepted 2017 December 2. Published 2018 January 16. \n\nThe authors gratefully acknowledge the Gauss Centre for Supercomputing e.V. (www.Gauss-centre.eu) and the Partnership for Advanced Supercomputing in Europe (PRACE, www.prace-ri.eu) for funding the MultiDark simulation project by providing computing time on the GCS Supercomputer SuperMUC at Leibniz Supercomputing Centre (LRZ, www.lrz.de). The Bolshoi simulations have been performed within the Bolshoi project of the University of California High-Performance AstroComputing Center (UC-HiPACC) and were run at the NASA Ames Research Center. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible. S.N. acknowledges partial support from a Sloan Foundation Fellowship. C.C.S. acknowledges support from NSF grants AST-0908805 and AST-1313472.\n\nPublished - Topping_2018_ApJ_852_134.pdf
Accepted Version - 1709.06572.pdf
", "abstract": "We investigate the nature and evolution of large-scale structure within the SSA22 protocluster region at z = 3.09 using cosmological simulations. A redshift histogram constructed from current spectroscopic observations of the SSA22 protocluster reveals two separate peaks at z = 3.065 (blue) and z = 3.095 (red). Based on these data, we report updated overdensity and mass calculations for the SSA22 protocluster. We find \u03b4_(b.gal) = 4.8 \u00b1 1.8 and \u03b4_(r.gal) = 9.5 \u00b1 2.0 for the blue and red peaks, respectively, and \u03b4_(r.gal) = 7.6 \u00b1 1.4 for the entire region. These overdensities correspond to masses of M_b = (0.76 \u00b1 0.17) x 10^(15)h^(-1) M_\u2299 M_r = (2.15 \u00b1 0.32) x 10^(15)h^(-1) M_\u2299, and M_t = (3.19 \u00b1 0.40) x 10^(15)h^(-1),M_\u2299 for the red, blue, and total peaks, respectively. We use the Small MultiDark Planck (SMDPL) simulation to identify comparably massive z ~ 3 protoclusters, and uncover the underlying structure and ultimate fate of the SSA22 protocluster. For this analysis, we construct mock redshift histograms for each simulated z ~ 3 protocluster, quantitatively comparing them with the observed SSA22 data. We find that the observed double-peaked structure in the SSA22 redshift histogram corresponds not to a single coalescing cluster, but rather the proximity of a ~ 10^(15)h^(-1) M_\u2299 protocluster and at least one \u3009 10^(14)h^(-1) M_\u2299 cluster progenitor. Such associations in the SMDPL simulation are easily understood within the framework of hierarchical clustering of dark matter halos. We finally find that the opportunity to observe such a phenomenon is incredibly rare, with an occurrence rate of 7.4h^3 Gpc^(-3).", "date": "2018-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "852", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 134", "id_number": "CaltechAUTHORS:20180118-133854987", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180118-133854987", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aa9f0f", "primary_object": { "basename": "1709.06572.pdf", "url": "https://authors.library.caltech.edu/records/k90je-bxd26/files/1709.06572.pdf" }, "related_objects": [ { "basename": "Topping_2018_ApJ_852_134.pdf", "url": "https://authors.library.caltech.edu/records/k90je-bxd26/files/Topping_2018_ApJ_852_134.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Topping, Michael W.; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/9m469-m6z49", "eprint_id": 81294, "eprint_status": "archive", "datestamp": "2023-08-19 05:18:18", "lastmod": "2023-10-17 19:43:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Turner-M-L", "name": { "family": "Turner", "given": "Monica L." } }, { "id": "Schaye-J", "name": { "family": "Schaye", "given": "Joop" } }, { "id": "Crain-R-A", "name": { "family": "Crain", "given": "Robert A." } }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen" }, "orcid": "0000-0002-8459-5413" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison" }, "orcid": "0000-0001-6369-1636" }, { "id": "Theuns-T", "name": { "family": "Theuns", "given": "Tom" } } ] }, "title": "A comparison of observed and simulated absorption from H I, C IV, and Si IV around z \u2248 2 star-forming galaxies suggests redshift\u2013space distortions are due to inflows", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation \u2013 intergalactic medium \u2013 quasars: absorption lines", "note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2017 June 23. Received 2017 May 17; in original form 2017 February 28. Published: 30 June 2017.\n\nWe would like to thank the anonymous referee for a constructive report that improved this article. This work used the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grants ST/H008519/1 and ST/K00087X/1, STFC DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure. This work was supported by the Netherlands Organisation for Scientific Research (NWO), through VICI grant 639.043.409 and by the European Research Council under the European Union's Seventh Framework Programme (FP7/2007- 2013)/ERC Grant agreement 278594-GasAroundGalaxies. RAC is a Royal Society University Research Fellow.\n\nPublished - Turner_2017p690.pdf
Submitted - 1703.00086.pdf
", "abstract": "We study H\u2009I and metal-line absorption around z \u2248 2 star-forming galaxies by comparing an analysis of data from the Keck Baryonic Structure Survey to mock spectra generated from the Evolution and Assembly of Galaxies and their Environments (EAGLE) cosmological, hydrodynamical simulations. We extract sightlines from the simulations and compare the properties of the absorption by H\u2009I, C IV, and Si IV around simulated and observed galaxies using pixel optical depths. We mimic the resolution, pixel size, and signal-to-noise ratio of the observations, as well as the distributions of impact parameters and galaxy redshift errors. We find that the EAGLE reference model is in excellent agreement with the observations. In particular, the simulation reproduces the high metal-line optical depths found at small galactocentric distances, the optical depth enhancements out to impact parameters of 2 proper Mpc, and the prominent redshift\u2013space distortions which we find are due to peculiar velocities rather than redshift errors. The agreement is best for halo masses \u223c10^(12.0) M\u2299, for which the observed and simulated stellar masses also agree most closely. We examine the median ion mass-weighted radial gas velocities around the galaxies, and find that most of the gas is infalling, with the infall velocity depending on halo rather than stellar mass. From this, we conclude that the observed redshift\u2013space distortions are predominantly caused by infall rather than outflows.", "date": "2017-10", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "471", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "690-705", "id_number": "CaltechAUTHORS:20170911-124424108", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170911-124424108", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/K00042X/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/H008519/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/K00087X/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/K003267/1" }, { "agency": "Durham University" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "639.043.409" }, { "agency": "European Research Council (ERC)", "grant_number": "278594" }, { "agency": "Royal Society" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/stx1616", "primary_object": { "basename": "1703.00086.pdf", "url": "https://authors.library.caltech.edu/records/9m469-m6z49/files/1703.00086.pdf" }, "related_objects": [ { "basename": "Turner_2017p690.pdf", "url": "https://authors.library.caltech.edu/records/9m469-m6z49/files/Turner_2017p690.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Turner, Monica L.; Schaye, Joop; et el." }, { "id": "https://authors.library.caltech.edu/records/s0bh9-zem78", "eprint_id": 81465, "eprint_status": "archive", "datestamp": "2023-08-19 05:10:28", "lastmod": "2023-10-17 19:52:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Naidu-R-P", "name": { "family": "Naidu", "given": "R. P." }, "orcid": "0000-0003-3997-5705" }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P. A." }, "orcid": "0000-0001-5851-6649" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "N." }, "orcid": "0000-0001-9687-4973" }, { "id": "Holden-B", "name": { "family": "Holden", "given": "B." }, "orcid": "0000-0002-6153-3076" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Montes-M", "name": { "family": "Montes", "given": "M." }, "orcid": "0000-0001-7847-0393" }, { "id": "Atek-H", "name": { "family": "Atek", "given": "H." }, "orcid": "0000-0002-7570-0824" }, { "id": "Bouwens-R-J", "name": { "family": "Bouwens", "given": "R. J." }, "orcid": "0000-0002-4989-2471" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Cibinel-A", "name": { "family": "Cibinel", "given": "A." }, "orcid": "0000-0003-4578-514X" }, { "id": "Illingworth-G-D", "name": { "family": "Illingworth", "given": "G. D." }, "orcid": "0000-0002-8096-2837" }, { "id": "Labb\u00e9-I", "name": { "family": "Labb\u00e9", "given": "I." }, "orcid": "0000-0002-2057-5376" }, { "id": "Magee-D-K", "name": { "family": "Magee", "given": "D." } }, { "id": "Morselli-L", "name": { "family": "Morselli", "given": "L." } }, { "id": "Nelson-E-J", "name": { "family": "Nelson", "given": "E. J." }, "orcid": "0000-0002-7524-374X" }, { "id": "van-Dokkum-P-G", "name": { "family": "van Dokkum", "given": "P. G." }, "orcid": "0000-0002-8282-9888" }, { "id": "Wilkins-S", "name": { "family": "Wilkins", "given": "S." } } ] }, "title": "The HDUV Survey: Six Lyman Continuum Emitter Candidates at z \u223c 2 Revealed by HST UV Imaging", "ispublished": "pub", "full_text_status": "public", "keywords": "dark ages, reionization, first stars \u2013 galaxies: evolution \u2013 galaxies: high-redshift", "note": "\u00a9 2017 American Astronomical Society. \n\nReceived 2016 November 22; revised 2017 July 27; accepted 2017 August 22; published 2017 September 14. \n\nWe thank the referee for a critical appraisal of this paper. R.N. was supported by Yale Astronomy's Dorrit Hoffleit Undergraduate Research Scholarship, Alice & Peter Tan, and Yale-NUS College's Summer Independent Research Program (SIRP) while working on this research. P.O. acknowledges support by the Swiss National Science Foundation through the SNSF Professorship grant 157567 \"Galaxy Build-up at Cosmic Dawn.\" \n\nWe are grateful to Akio Inoue for providing Monte Carlo realizations of the IGM transmission at high redshift. The primary data for this work were obtained with the Hubble Space Telescope operated by AURA, Inc., for NASA under contract NAS 5-26555. Support for this work was provided by NASA through grant HST-GO-13871 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). \n\nFacilities: HST (ACS - , WFC3) - .\n\nPublished - Naidu_2017_ApJ_847_12.pdf
Submitted - 1611.07038.pdf
", "abstract": "We present six galaxies at z ~ 2 that show evidence of Lyman continuum (LyC) emission based on the newly acquired UV imaging of the Hubble Deep UV legacy survey (HDUV) conducted with the WFC3/UVIS camera on the Hubble Space Telescope (HST). At the redshift of these sources, the HDUV F275W images partially probe the ionizing continuum. By exploiting the HST multiwavelength data available in the HDUV/GOODS fields, models of the UV spectral energy distributions, and detailed Monte Carlo simulations of the intergalactic medium absorption, we estimate the absolute ionizing photon escape fractions of these galaxies to be very high\u2014typically >60% (>13% for all sources at 90% likelihood). Our findings are in broad agreement with previous studies that found only a small fraction of galaxies with high escape fraction. These six galaxies compose the largest sample yet of LyC leaking candidates at z ~ 2 whose inferred LyC flux has been observed at HST resolution. While three of our six candidates show evidence of hosting an active galactic nucleus, two of these are heavily obscured and their LyC emission appears to originate from star-forming regions rather than the central nucleus. Extensive multiwavelength data in the GOODS fields, especially the near-IR grism spectra from the 3D-HST survey, enable us to study the candidates in detail and tentatively test some recently proposed indirect methods to probe LyC leakage. High-resolution spectroscopic follow-up of our candidates will help constrain such indirect methods, which are our only hope of studying f_(esc) at z ~ 5 - 9 in the JWST era.", "date": "2017-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "847", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 12", "id_number": "CaltechAUTHORS:20170914-155935445", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170914-155935445", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Yale University" }, { "agency": "Alice and Peter Tan" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "157567" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NASA", "grant_number": "HST-GO-13871" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aa8863", "primary_object": { "basename": "1611.07038.pdf", "url": "https://authors.library.caltech.edu/records/s0bh9-zem78/files/1611.07038.pdf" }, "related_objects": [ { "basename": "Naidu_2017_ApJ_847_12.pdf", "url": "https://authors.library.caltech.edu/records/s0bh9-zem78/files/Naidu_2017_ApJ_847_12.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Naidu, R. P.; Oesch, P. A.; et el." }, { "id": "https://authors.library.caltech.edu/records/e3x5h-tj078", "eprint_id": 77200, "eprint_status": "archive", "datestamp": "2023-08-19 02:52:34", "lastmod": "2023-10-25 21:58:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cooke-R-J", "name": { "family": "Cooke", "given": "Ryan J." }, "orcid": "0000-0001-7653-5827" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Discovery of the most metal-poor damped Lyman-\u03b1 system", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: Population III, ISM: abundances, galaxies: dwarf, quasars: absorption lines", "note": "\u00a9 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2017 January 5. Received 2016 December 15; in original form 2016 November 21. \n\nWe are grateful to the staff astronomers at Keck Observatory for their assistance with the observations. We thank the anonymous referee for their prompt review, and for offering several helpful suggestions that improved the presentation of this paper. During this work, RJC was supported by a Royal Society University Research Fellowship, and by NASA through Hubble Fellowship grant HST-HF-51338.001-A, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. RJC acknowledges support from STFC (ST/L00075X/1). CCS has been supported by grant AST-1313472 from the US NSF. This research was also supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time partially allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. Our work made use of the matplotlib (Hunter 2007), emcee (Foreman-Mackey et al. 2013) and corner (Foreman-Mackey et al. 2016) python packages, which we gratefully acknowledge. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We thank the Hawaiian people for the opportunity to observe from Mauna Kea; without their hospitality, this work would not have been possible.\n\nPublished - stx037.pdf
Submitted - 1701.03103.pdf
", "abstract": "We report the discovery and analysis of the most metal-poor damped Lyman \u03b1 (DLA) system currently known, based on observations made with the Keck HIRES spectrograph. The metal paucity of this system has only permitted the determination of three element abundances: [C/H] = \u22123.43 \u00b1 0.06, [O/H] = \u22123.05 \u00b1 0.05 and [Si/H] = \u22123.21 \u00b1 0.05, as well as an upper limit on the abundance of iron: [Fe/H] \u2264 \u22122.81. This DLA is among the most carbon-poor environment currently known with detectable metals. By comparing the abundance pattern of this DLA to detailed models of metal-free nucleosynthesis, we find that the chemistry of the gas is consistent with the yields of a 20.5\u2009M_\u2299 metal-free star that ended its life as a core-collapse supernova; the abundances we measure are inconsistent with the yields of pair-instability supernovae. Such a tight constraint on the mass of the progenitor Population III star is afforded by the well-determined C/O ratio, which we show depends almost monotonically on the progenitor mass when the kinetic energy of the supernova explosion is Eexp \u2273 1.5 \u00d7 10^(51)\u2009erg. We find that the DLA presented here has just crossed the critical 'transition discriminant' threshold, rendering the DLA gas now suitable for low mass star formation. We also discuss the chemistry of this system in the context of recent models that suggest some of the most metal-poor DLAs are the precursors of the 'first galaxies', and are the antecedents of the ultrafaint dwarf galaxies.", "date": "2017-05", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "467", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "802-811", "id_number": "CaltechAUTHORS:20170505-064608864", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170505-064608864", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51338.001-A" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L00075X/1" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/stx037", "primary_object": { "basename": "1701.03103.pdf", "url": "https://authors.library.caltech.edu/records/e3x5h-tj078/files/1701.03103.pdf" }, "related_objects": [ { "basename": "stx037.pdf", "url": "https://authors.library.caltech.edu/records/e3x5h-tj078/files/stx037.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Cooke, Ryan J.; Pettini, Max; et el." }, { "id": "https://authors.library.caltech.edu/records/q98a4-0x079", "eprint_id": 76786, "eprint_status": "archive", "datestamp": "2023-08-19 02:41:55", "lastmod": "2023-10-25 16:51:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Goobar-A", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Amanullah-R", "name": { "family": "Amanullah", "given": "R." }, "orcid": "0000-0002-5559-9351" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Johansson-J", "name": { "family": "Johansson", "given": "J." }, "orcid": "0000-0001-5975-290X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Lawrence-D-J", "name": { "family": "Lawrence", "given": "D." } }, { "id": "M\u00f6rtsell-E", "name": { "family": "M\u00f6rtsell", "given": "E." } }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R." }, "orcid": "0000-0001-9171-5236" }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Brandeker-A", "name": { "family": "Brandeker", "given": "A." } }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Ferretti-R", "name": { "family": "Ferretti", "given": "R." }, "orcid": "0000-0001-7814-5814" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Hangard-L", "name": { "family": "Hangard", "given": "L." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "T." }, "orcid": "0000-0002-6540-1484" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "A. A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Nayyeri-H", "name": { "family": "Nayyeri", "given": "H." }, "orcid": "0000-0001-8242-9983" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Papadogiannakis-S", "name": { "family": "Papadogiannakis", "given": "S." }, "orcid": "0000-0003-0783-3323" }, { "id": "Petrushevska-T", "name": { "family": "Petrushevska", "given": "T." }, "orcid": "0000-0003-4743-1679" }, { "id": "Ravi-Vikram", "name": { "family": "Ravi", "given": "V." }, "orcid": "0000-0002-7252-5485" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Walters-R", "name": { "family": "Walters", "given": "R." }, "orcid": "0000-0002-1835-6078" }, { "id": "Wilson-D-M", "name": { "family": "Wilson", "given": "D. M." }, "orcid": "0000-0001-6002-423X" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" } ] }, "title": "iPTF16geu: A multiply imaged, gravitationally lensed type Ia supernova", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2017 American Association for the Advancement of Science. \n\nReceived for publication 25 October 2016; accepted for publication 24 March 2017. \n\nSupported by the Swedish National Science Council and the Swedish National Space Board (A.G., R.A., and E.M.); U.S. Department of Energy (DOE) grant DE-AC02-05CH11231 (P.E.N.); European Research Council grant 615929 (M.S.); NASA (S.R.K.); and NSF grant 1545949. The iPTF Swedish collaboration is funded through a grant from the Knut and Alice Wallenberg foundation. This research used resources of the National Energy Research Scientific Computing Center, supported by DOE contract DE-AC02-05CH11231. Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA grant HST-GO-14862.002. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Some of the data presented here were obtained with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. The Space Telescope Science Data Analysis System (STSDAS) and the command language PyRAF are products of the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy (AURA) for NASA. Part of the processing was carried out off-line using the commercial software package MATLAB and Statistics Toolbox Release 2013a, The MathWorks Inc., Natick, MA. Photometric data used in this paper are available in tables S1, S2, and S5, spectroscopic data are available at public repository WISeREP (33) (http://wiserep.weizmann.ac.il) under the ID \"SN 2016geu\"; the positions of the SN images used in the lensing model are provided in table S4.\n\nSubmitted - 1611.00014.pdf
Supplemental Material - aal2729_Goobar_SM.pdf
", "abstract": "We report the discovery of a multiply imaged, gravitationally lensed type Ia supernova, iPTF16geu (SN 2016geu), at redshift z = 0.409. This phenomenon was identified because the light from the stellar explosion was magnified more than 50 times by the curvature of space around matter in an intervening galaxy. We used high-spatial-resolution observations to resolve four images of the lensed supernova, approximately 0.3 arc seconds from the center of the foreground galaxy. The observations probe a physical scale of ~1 kiloparsec, smaller than is typical in other studies of extragalactic gravitational lensing. The large magnification and symmetric image configuration imply close alignment between the lines of sight to the supernova and to the lens. The relative magnifications of the four images provide evidence for substructures in the lensing galaxy.", "date": "2017-04-21", "date_type": "published", "publication": "Science", "volume": "356", "number": "6335", "publisher": "American Association for the Advancement of Science", "pagerange": "291-295", "id_number": "CaltechAUTHORS:20170420-143345464", "issn": "0036-8075", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170420-143345464", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swedish National Science Council" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "NASA", "grant_number": "HST-GO-14862.002" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1126/science.aal2729", "primary_object": { "basename": "1611.00014.pdf", "url": "https://authors.library.caltech.edu/records/q98a4-0x079/files/1611.00014.pdf" }, "related_objects": [ { "basename": "aal2729_Goobar_SM.pdf", "url": "https://authors.library.caltech.edu/records/q98a4-0x079/files/aal2729_Goobar_SM.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Goobar, A.; Amanullah, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/1jyw6-vm494", "eprint_id": 76819, "eprint_status": "archive", "datestamp": "2023-08-21 20:51:39", "lastmod": "2023-10-25 16:53:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Stern-D", "name": { "family": "Stern", "given": "Daniel" }, "orcid": "0000-0003-2686-9241" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Arav-N", "name": { "family": "Arav", "given": "Nahum" } }, { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "S. G." }, "orcid": "0000-0002-0603-3087" }, { "id": "Chamberlain-C", "name": { "family": "Chamberlain", "given": "Carter" } }, { "id": "Barth-A-J", "name": { "family": "Barth", "given": "Aaron J." }, "orcid": "0000-0002-3026-0562" }, { "id": "Donalek-C", "name": { "family": "Donalek", "given": "Ciro" } }, { "id": "Drake-A-J", "name": { "family": "Drake", "given": "Andrew J." } }, { "id": "Glikman-E", "name": { "family": "Glikman", "given": "Eilat" }, "orcid": "0000-0003-0489-3750" }, { "id": "Jun-Hyunsung-David", "name": { "family": "Jun", "given": "Hyunsung D." }, "orcid": "0000-0003-1470-5901" }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "Ashish A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Extreme Variability in a Broad Absorption Line Quasar", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; quasars: individual (CRTS J084133.15+200525.8)", "note": "\u00a9 2017 American Astronomical Society. \n\nReceived 2017 January 13. Accepted 2017 February 15. Published 2017 April 21. \n\nWe thank the anonymous referee for a prompt and helpful referee report. CRTS was supported by the NSF grants AST-1313422, AST-1413600, and AST-1518308. The work of D.S. and H.J. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. D.S. also acknowledges support from NASA through ADAP award 12-ADAP12-0109. N.A. and C.C. acknowledge support from NSF through grant AST 1413319, and from NASA through STScI grants GO 11686 and GO 12022. Research by A.J.B. was supported by NSF grant AST-1412693. E.G. acknowledges the generous support of the Cottrell College Award through the Research Corporation for Science Advancement. H.J. is supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Universities Space Research Association under contract with NASA. The authors are grateful to the staff at the Palomar and Keck observatories, where some of the data presented here were obtained. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. \n\nFacilities: CRTS - , Keck (MOSFIRE) - , NEOWISE - , Palomar (DBSP) - , SDSS - , WISE - Wide-field Infrared Survey Explorer.\n\nPublished - Stern_2017_ApJ_839_106.pdf
Submitted - 1704.03923.pdf
", "abstract": "CRTS J084133.15+200525.8 is an optically bright quasar at z = 2.345 that has shown extreme spectral variability over the past decade. Photometrically, the source had a visual magnitude of V ~ 17.3 between 2002 and 2008. Then, over the following five years, the source slowly brightened by approximately one magnitude, to V ~ 16.2. Only ~1 in 10,000 quasars show such extreme variability, as quantified by the extreme parameters derived for this quasar assuming a damped random walk model. A combination of archival and newly acquired spectra reveal the source to be an iron low-ionization broad absorption line quasar with extreme changes in its absorption spectrum. Some absorption features completely disappear over the 9 years of optical spectra, while other features remain essentially unchanged. We report the first definitive redshift for this source, based on the detection of broad H\u03b1 in a Keck/MOSFIRE spectrum. Absorption systems separated by several 1000 km s^(\u22121) in velocity show coordinated weakening in the depths of their troughs as the continuum flux increases. We interpret the broad absorption line variability to be due to changes in photoionization, rather than due to motion of material along our line of sight. This source highlights one sort of rare transition object that astronomy will now be finding through dedicated time-domain surveys.", "date": "2017-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "839", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 106", "id_number": "CaltechAUTHORS:20170421-131659519", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170421-131659519", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1313422" }, { "agency": "NSF", "grant_number": "AST-1413600" }, { "agency": "NSF", "grant_number": "AST-1518308" }, { "agency": "NASA", "grant_number": "12-ADAP12-0109" }, { "agency": "NSF", "grant_number": "AST-1413319" }, { "agency": "NASA", "grant_number": "GO 11686" }, { "agency": "NASA", "grant_number": "GO 12022" }, { "agency": "NSF", "grant_number": "AST-1412693" }, { "agency": "Cottrell Scholar of Research Corporation" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aa683c", "primary_object": { "basename": "1704.03923.pdf", "url": "https://authors.library.caltech.edu/records/1jyw6-vm494/files/1704.03923.pdf" }, "related_objects": [ { "basename": "Stern_2017_ApJ_839_106.pdf", "url": "https://authors.library.caltech.edu/records/1jyw6-vm494/files/Stern_2017_ApJ_839_106.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Stern, Daniel; Graham, Matthew J.; et el." }, { "id": "https://authors.library.caltech.edu/records/pj0zz-egp71", "eprint_id": 74443, "eprint_status": "archive", "datestamp": "2023-08-22 19:43:18", "lastmod": "2023-10-24 22:38:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" } ] }, "title": "Nebular Emission Line Ratios in z \u2243 2\u20133 Star-forming Galaxies with KBSS-MOSFIRE: Exploring the Impact of Ionization, Excitation, and Nitrogen-to-Oxygen Ratio", "ispublished": "pub", "full_text_status": "public", "keywords": "Cosmology: observations; galaxies: evolution; galaxies: high-redshift; galaxies: ISM; H ii regions; ISM: abundances", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 August 2; accepted 2017 January 16; published 2017 February 17. \n\nWe are grateful to the referee for the thoughtful and constructive feedback provided during the review process. We also thank the organizers and attendees of the Carnegie Symposium in honor of Leonard Searle, \"Understanding Nebular Emission in High-redshift Galaxies,\" held at the Carnegie Observatories in Pasadena, for many interesting conversations that contributed to the work presented here. This work has been supported in part by a US National Science Foundation (NSF) Graduate Research Fellowship (ALS), by the NSF through grants AST-0908805 and AST-1313472 (CCS, ALS, RFT, GCR), and by an Alfred P. Sloan Research Fellowship (NAR). Finally, the authors wish to recognize and acknowledge the significant cultural role and reverence that the summit of Maunakea has within the indigenous Hawaiian community. We are privileged to have the opportunity to conduct observations from this mountain.\n\nPublished - Strom_2017_ApJ_836_164.pdf
Submitted - 1608.02587.pdf
", "abstract": "We present a detailed study of the rest-optical (3600\u20137000 \u00c5) nebular spectra of ~380 star-forming galaxies at z \u2243 2\u20133, obtained with Keck/Multi-object Spectrometer for Infrared Exploration (MOSFIRE) as part of the Keck Baryonic Structure Survey (KBSS). The KBSS-MOSFIRE sample is representative of star-forming galaxies at these redshifts, with stellar masses M_* = M^9 \u2013 M^(11.5) M_\u2299 and star formation rates SFR = 3\u20131000 M_\u2299 yr^(-1). We focus on robust measurements of many strong diagnostic emission lines for individual galaxies: [O II]\u03bb\u03bb3727, 3729, [Ne III]\u03bb3869, H\u03b2, [O III]\u03bb\u03bb 4960, 5008, [N II]\u03bb\u03bb 6549, 6585, H\u03b1, and [S II]\u03bb\u03bb6718, 6732. Comparisons with observations of typical local galaxies from the Sloan Digital Sky Survey and between subsamples of KBSS-MOSFIRE show that high-redshift galaxies exhibit a number of significant differences in addition to the well-known offset in log([O III]\u03bb5008/H\u03b2) and log([N II]\u03bb6585/H\u03b1). We argue that the primary difference between H II regions in z ~ 2.3 galaxies and those at z ~ 0 is an enhancement in the degree of nebular excitation, as measured by [O III]/H\u03b2 and R23 \u2261 log [([O III]\u03bb\u03bb4960, 5008+[O II]\u03bb\u03bb3727, 3729)/H\u03b2]. At the same time, KBSS-MOSFIRE galaxies are ~10 times more massive than z ~ 0 galaxies with similar ionizing spectra and have higher N/O (likely accompanied by higher O/H) at fixed excitation. These results indicate the presence of harder ionizing radiation fields at fixed N/O and O/H relative to typical z ~ 0 galaxies, consistent with Fe-poor stellar population models that include massive binaries, and highlight a population of massive, high-specific star formation rate galaxies at high redshift with systematically different star formation histories than galaxies of similar stellar mass today.", "date": "2017-02-17", "date_type": "published", "publication": "Astrophysical Journal", "volume": "836", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 164", "id_number": "CaltechAUTHORS:20170221-162631848", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170221-162631848", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/836/2/164", "primary_object": { "basename": "1608.02587.pdf", "url": "https://authors.library.caltech.edu/records/pj0zz-egp71/files/1608.02587.pdf" }, "related_objects": [ { "basename": "Strom_2017_ApJ_836_164.pdf", "url": "https://authors.library.caltech.edu/records/pj0zz-egp71/files/Strom_2017_ApJ_836_164.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Strom, Allison L.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/mpsdx-2xf13", "eprint_id": 73788, "eprint_status": "archive", "datestamp": "2023-08-22 19:40:15", "lastmod": "2023-10-24 16:27:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "van-Roestel-J", "name": { "family": "van Roestel", "given": "Jan" }, "orcid": "0000-0002-2626-2872" }, { "id": "Brooks-J", "name": { "family": "Brooks", "given": "Jared" } }, { "id": "Geier-S", "name": { "family": "Geier", "given": "Stephan" }, "orcid": "0000-0002-3948-9339" }, { "id": "Marsh-T-R", "name": { "family": "Marsh", "given": "Tom R." }, "orcid": "0000-0002-2498-7589" }, { "id": "Groot-P-J", "name": { "family": "Groot", "given": "Paul J." }, "orcid": "0000-0002-4488-726X" }, { "id": "Bloemen-S", "name": { "family": "Bloemen", "given": "Steven" } }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric" }, "orcid": "0000-0001-8018-5348" }, { "id": "Heber-U", "name": { "family": "Heber", "given": "Ulrich" }, "orcid": "0000-0001-7798-6769" }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "Lars" } }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Dyer-M-J", "name": { "family": "Dyer", "given": "Martin J." } }, { "id": "Dhillon-V-S", "name": { "family": "Dhillon", "given": "Vik S." } }, { "id": "Green-M", "name": { "family": "Green", "given": "Matthew" } }, { "id": "Irawati-P", "name": { "family": "Irawati", "given": "Puji" } }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Littlefair-S-P", "name": { "family": "Littlefair", "given": "Stuart P." }, "orcid": "0000-0001-7221-855X" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "David L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Rattansoon-S", "name": { "family": "Rattansoon", "given": "Somsawat" } }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" } ] }, "title": "PTF1 J082340.04+081936.5: A Hot Subdwarf B Star with a Low-mass White Dwarf Companion in an 87-minute Orbit", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: close; stars: individual (PTF1 J082340.04+081936.5); subdwarfs; white dwarfs", "note": "\u00a9 2017. The American Astronomical Society. \n\nReceived 2016 November 14; revised 2016 December 5; accepted 2016 December 6; published 2017 January 23. \n\nThis work was supported by the GROWTH project funded by the National Science Foundation under Grant No 1545949. J.v.R. acknowledges support by the Netherlands Research School of Astronomy (NOVA) and the foundation for Fundamental Research on Matter (FOM). T.R.M. acknowledges the support from the Science and Technology Facilities Council (STFC), ST/L00733. This research was partially funded by the Gordon and Betty Moore Foundation through Grant GBMF5076 to Lars Bildsten. This work was supported by the National Science Foundation under grants PHY 11-25915, AST 11-09174, and AST 12-05574. 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 where parts of this paper was written. We thank the referee for helpful and timely comments. \n\nObservations were obtained with the Samuel Oschin Telescope at the Palomar Observatory as part of the PTF project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Some results presented in this paper are based on observations made with the WHT operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Institutio de Astrofisica de Canarias. \n\nSoftware: PyRAF (Bellm & Sesar 2016), MAKEE (http://www.astro.caltech.edu/tb/ipac staff/tab/makee/), Gatspy (VanderPlas & Ivezi\u0107 2015), LCURVE (Copperwheat et al. 2010), emcee (Foreman-Mackey et al. 2013), MESA (Paxton et al. 2011, 2013, 2015), FITSB2 (Napiwotzki et al. 2004).\n\nPublished - Kupfer_2017_ApJ_835_131.pdf
Accepted Version - 1612.02019.pdf
", "abstract": "We present the discovery of the hot subdwarf B star (sdB) binary PTF1 J082340.04+081936.5. The system has an orbital period of P_(orb) = 87.49668(1) minutes (0.060761584(10) days), making it the second-most compact sdB binary known. The light curve shows ellipsoidal variations. Under the assumption that the sdB primary is synchronized with the orbit, we find a mass of M_(sdB) = 0.45_(-0.07)^(+0.09) M_\u2299, a companion white dwarf mass of M_(WD) = 0.46_(-0.09)^(+0.12) M_\u2299, and a mass ratio of q = M_(WD)/M_(sdB) = 1.03_(-0.08)^(+0.10). The future evolution was calculated using the MESA stellar evolution code. Adopting a canonical sdB mass of M_(sdB) = 0.47 M_\u2299, we find that the sdB still burns helium at the time it will fill its Roche lobe if the orbital period was less than 106 minutes at the exit from the last common envelope (CE) phase. For longer CE exit periods, the sdB will have stopped burning helium and turned into a C/O white dwarf at the time of contact. Comparing the spectroscopically derived log g and T_(eff) with our MESA models, we find that an sdB model with a hydrogen envelope mass of 5 x 10^(-4) M_\u2299 matches the measurements at a post-CE age of 94 Myr, corresponding to a post-CE orbital period of 109 minutes, which is close to the limit to start accretion while the sdB is still burning helium.", "date": "2017-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "835", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 131", "id_number": "CaltechAUTHORS:20170127-143159985", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170127-143159985", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "Nederlandse Onderzoekschool voor de Astronomie (NOVA)" }, { "agency": "Stichting voor Fundamenteel Onderzoek der Materie (FOM)" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L00733" }, { "agency": "Gordon and Betty Moore Foundation", "grant_number": "GBMF5076" }, { "agency": "NSF", "grant_number": "PHY 11-25915" }, { "agency": "NSF", "grant_number": "AST 11-09174" }, { "agency": "NSF", "grant_number": "AST 12-05574" }, { "agency": "NSF", "grant_number": "PHYS-1066293" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/835/2/131", "primary_object": { "basename": "1612.02019.pdf", "url": "https://authors.library.caltech.edu/records/mpsdx-2xf13/files/1612.02019.pdf" }, "related_objects": [ { "basename": "Kupfer_2017_ApJ_835_131.pdf", "url": "https://authors.library.caltech.edu/records/mpsdx-2xf13/files/Kupfer_2017_ApJ_835_131.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Kupfer, Thomas; van Roestel, Jan; et el." }, { "id": "https://authors.library.caltech.edu/records/ypbf9-2gq76", "eprint_id": 73725, "eprint_status": "archive", "datestamp": "2023-08-22 19:33:41", "lastmod": "2023-10-24 16:23:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Umehata-Hideki", "name": { "family": "Umehata", "given": "Hideki" }, "orcid": "0000-0003-1937-0573" }, { "id": "Tamura-Yoichi", "name": { "family": "Tamura", "given": "Yoichi" }, "orcid": "0000-0003-4807-8117" }, { "id": "Kohno-Kotaro", "name": { "family": "Kohno", "given": "Kotaro" }, "orcid": "0000-0002-4052-2394" }, { "id": "Ivison-Rob-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Smail-Ian-R", "name": { "family": "Smail", "given": "Ian" }, "orcid": "0000-0003-3037-257X" }, { "id": "Hatsukade-Bunyo", "name": { "family": "Hatsukade", "given": "Bunyo" }, "orcid": "0000-0001-6469-8725" }, { "id": "Nakanishi-Kouichiro", "name": { "family": "Nakanishi", "given": "Kouichiro" }, "orcid": "0000-0002-6939-0372" }, { "id": "Kato-Yuta", "name": { "family": "Kato", "given": "Yuta" } }, { "id": "Ikarashi-Soh", "name": { "family": "Ikarashi", "given": "Soh" } }, { "id": "Matsuda-Yuichi", "name": { "family": "Matsuda", "given": "Yuichi" }, "orcid": "0000-0003-1747-2891" }, { "id": "Fujimoto-Seiji", "name": { "family": "Fujimoto", "given": "Seiji" }, "orcid": "0000-0001-7201-5066" }, { "id": "Iono-Daisuke", "name": { "family": "Iono", "given": "Daisuke" }, "orcid": "0000-0002-2364-0823" }, { "id": "Lee-Minju", "name": { "family": "Lee", "given": "Minju" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Saito-Tomoki", "name": { "family": "Saito", "given": "Tomoki" } }, { "id": "Alexander-David-M", "name": { "family": "Alexander", "given": "D. M." }, "orcid": "0000-0002-5896-6313" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "Min S." }, "orcid": "0000-0001-7095-7543" }, { "id": "Kubo-Mariko", "name": { "family": "Kubo", "given": "Mariko" }, "orcid": "0000-0002-7598-5292" } ] }, "title": "ALMA Deep Field in SSA22: Source Catalog and Number Counts", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: high-redshift; galaxies: star formation; galaxies: starburst; galaxies: structure", "note": "\u00a9 2017 American Astronomical Society. \n\nReceived 2016 July 15. Accepted 2016 November 28. Published 2017 January 20. \n\nWe deeply appreciate the anonymous referee for a significant number of valuable comments. We are thankful for Ken Mawatari for helping us to compile redshift catalogs of z = 3.09 LAEs and LBGs in the literature. H.U. is supported by the ALMA Japan Research Grant of NAOJ Chile Observatory, NAOJ-ALMA-0071, 0131, 140, and 0152. H.U. is also supported by JSPS Grant-in-Aid for Research Activity Start-up (16H06713). Y.T. is supported by JSPS KAKENHI No. 15H02073. R.J.I. acknowledges support from ERC in the form of the Advanced Investigator Programme, 321302, COSMICISM. I.R.S. and D.M.A. acknowledge support from STFC (ST/L00075X/1). I.R.S. acknowledges support from the ERC Advanced Investigator program DUSTYGAL 321334, and a Royal Society/Wolfson Merit Award. S.I. acknowledges the support of the Netherlands Organization for Scientific Research (NWO) through the Top Grant Project 614.001.403. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00162.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), along with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. \n\nFacility: ALMA - Atacama Large Millimeter Array.\n\nPublished - Umehata_2017_ApJ_835_98.pdf
Submitted - 1611.09857v1.pdf
", "abstract": "We present results from a deep 2' \u00d7 3' (comoving scale of 3.7 Mpc \u00d7 5.5 Mpc at z = 3) survey at 1.1 mm, taken with the Atacama Large Millimeter/submillimeter Array (ALMA) in the SSA22 field. We observe the core region of a z = 3.09 protocluster, achieving a typical rms sensitivity of 60 \u03bcJy beam^(\u22121) at a spatial resolution of 0\"7. We detect 18 robust ALMA sources at a signal-to-noise ratio (S/N) > 5. Comparison between the ALMA map and a 1.1 mm map, taken with the AzTEC camera on the Atacama Submillimeter Telescope Experiment (ASTE), indicates that three submillimeter sources discovered by the AzTEC/ASTE survey are resolved into eight individual submillimeter galaxies (SMGs) by ALMA. At least 10 of our 18 ALMA SMGs have spectroscopic redshifts of z sime 3.09, placing them in the protocluster. This shows that a number of dusty starburst galaxies are forming simultaneously in the core of the protocluster. The nine brightest ALMA SMGs with S/N > 10 have a median intrinsic angular size of 0.\"32_(-0.06)^(+0.13)(2.4_(-0.4^(+1.0 physical kpc at z = 3.09), which is consistent with previous size measurements of SMGs in other fields. As expected, the source counts show a possible excess compared to the counts in the general fields at S_(1.1mm) \u2265 1.0 mJy, due to the protocluster. Our contiguous mm mapping highlights the importance of large-scale structures on the formation of dusty starburst galaxies.", "date": "2017-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "835", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 98", "id_number": "CaltechAUTHORS:20170125-134707645", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170125-134707645", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Astronomical Observatory of Japan", "grant_number": "NAOJ-ALMA-0071" }, { "agency": "National Astronomical Observatory of Japan", "grant_number": "NAOJ-ALMA-0131" }, { "agency": "National Astronomical Observatory of Japan", "grant_number": "NAOJ-ALMA-140" }, { "agency": "National Astronomical Observatory of Japan", "grant_number": "NAOJ-ALMA-152" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "16H06713" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15H02073" }, { "agency": "European Research Council (ERC)", "grant_number": "321302" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L00075X/1" }, { "agency": "European Research Council (ERC)", "grant_number": "DUSTYGAL 321334" }, { "agency": "Royal Society" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "614.001.403" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/835/1/98", "primary_object": { "basename": "1611.09857v1.pdf", "url": "https://authors.library.caltech.edu/records/ypbf9-2gq76/files/1611.09857v1.pdf" }, "related_objects": [ { "basename": "Umehata_2017_ApJ_835_98.pdf", "url": "https://authors.library.caltech.edu/records/ypbf9-2gq76/files/Umehata_2017_ApJ_835_98.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Umehata, Hideki; Tamura, Yoichi; et el." }, { "id": "https://authors.library.caltech.edu/records/nbj1s-gbp47", "eprint_id": 73590, "eprint_status": "archive", "datestamp": "2023-08-22 19:31:01", "lastmod": "2023-10-24 15:30:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Umehata-Hideki", "name": { "family": "Umehata", "given": "Hideki" }, "orcid": "0000-0003-1937-0573" }, { "id": "Matsuda-Yuichi", "name": { "family": "Matsuda", "given": "Yuichi" }, "orcid": "0000-0003-1747-2891" }, { "id": "Tamura-Yoichi", "name": { "family": "Tamura", "given": "Yoichi" }, "orcid": "0000-0003-4807-8117" }, { "id": "Kohno-Kotaro", "name": { "family": "Kohno", "given": "Kotaro" }, "orcid": "0000-0002-4052-2394" }, { "id": "Smail-Ian-R", "name": { "family": "Smail", "given": "Ian" }, "orcid": "0000-0003-3037-257X" }, { "id": "Ivison-Rob-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Chapman-Scott-C", "name": { "family": "Chapman", "given": "Scott C." }, "orcid": "0000-0002-8487-3153" }, { "id": "Geach-James-E", "name": { "family": "Geach", "given": "James E." }, "orcid": "0000-0003-4964-4635" }, { "id": "Hayes-Matthew", "name": { "family": "Hayes", "given": "Matthew" }, "orcid": "0000-0001-8587-218X" }, { "id": "Nagao-Tohru", "name": { "family": "Nagao", "given": "Tohru" }, "orcid": "0000-0002-7402-5441" }, { "id": "Ao-Yiping", "name": { "family": "Ao", "given": "Yiping" }, "orcid": "0000-0003-3139-2724" }, { "id": "Kawabe-Ryohei", "name": { "family": "Kawabe", "given": "Ryohei" }, "orcid": "0000-0002-8049-7525" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "Min S." }, "orcid": "0000-0001-7095-7543" }, { "id": "Hatsukade-Bunyo", "name": { "family": "Hatsukade", "given": "Bunyo" }, "orcid": "0000-0001-6469-8725" }, { "id": "Kubo-Mariko", "name": { "family": "Kubo", "given": "Mariko" }, "orcid": "0000-0002-7598-5292" }, { "id": "Kato-Yuta", "name": { "family": "Kato", "given": "Yuta" } }, { "id": "Saito-Tomoki", "name": { "family": "Saito", "given": "Tomoki" } }, { "id": "Ikarashi-Soh", "name": { "family": "Ikarashi", "given": "Soh" } }, { "id": "Nakanishi-Kouichiro", "name": { "family": "Nakanishi", "given": "Kouichiro" }, "orcid": "0000-0002-6939-0372" }, { "id": "Lee-Minju", "name": { "family": "Lee", "given": "Minju" } }, { "id": "Izumi-Takuma", "name": { "family": "Izumi", "given": "Takuma" } }, { "id": "Mori-Masao", "name": { "family": "Mori", "given": "Masao" } }, { "id": "Ouchi-Masami", "name": { "family": "Ouchi", "given": "Masami" }, "orcid": "0000-0002-1049-6658" } ] }, "title": "ALMA Reveals Strong [C II] Emission in a Galaxy Embedded in a Giant Ly\u03b1 Blob at z = 3.1", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: halos; galaxies: high-redshift; galaxies: ISM; submillimeter: galaxies", "note": "\u00a9 2017. The American Astronomical Society. \n\nReceived 2016 December 2. Accepted 2016 December 27. Published 2017 January 12. \n\nWe greatly appreciate the anonymous referee for a helpful report. H.U. is supported by the ALMA Japan Research Grant of NAOJ Chile Observatory, NAOJ-ALMA-0071, 0131, 140, and 0152. H.U. is supported by JSPS Grant-in-Aid for Research Activity Start-up (16H06713). H.U. is thankful for the support from JSPS KAKENHI No. 16H02166 (PI: Y. Taniguchi). Y.T. is supported by JSPS KAKENHI No. 25102073. R.J.I. acknowledges support from ERC in the form of the Advanced Investigator Programme, 321302, COSMICISM. I.R.S. acknowledges support from STFC (ST/L00075X/1). I.R.S. acknowledges support from the ERC Advanced Investigator program DUSTYGAL 321334, and a Royal Society/Wolfson Merit Award. M.H. acknowledges the support of the Swedish Research Council, Vetenskapsr\u00e5det and the Swedish National Space Board (SNSB), and is Fellow of the Knut and Alice Wallenberg Foundation. This Letter makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00159.S, ADS/JAO.ALMA#2013.1.00704.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. \n\nFacility: ALMA.\n\nPublished - Umehata_2017_ApJL_834_L16.pdf
Submitted - 1701.00043v1.pdf
", "abstract": "We report the result from observations conducted with the Atacama Large Millimeter/submillimeter Array (ALMA) to detect [C ii] 158 \u03bcm fine structure line emission from galaxies embedded in one of the most spectacular Ly\u03b1 blobs (LABs) at z = 3.1, SSA22-LAB1. Of three dusty star-forming galaxies previously discovered by ALMA 860 \u03bcm dust continuum survey toward SSA22-LAB1, we detected the [C ii] line from one, LAB1-ALMA3 at z = 3.0993 \u00b1 0.0004. No line emission was detected, associated with the other ALMA continuum sources or from three rest-frame UV/optical selected z_(spec) \u2243 3.1 galaxies within the field of view. For LAB1-ALMA3, we find relatively bright [C ii] emission compared to the infrared luminosity (L_([C ii])/L_(IR) \u2248 0.01) and an extremely high [C ii] 158 \u03bcm and [N ii] 205 \u03bcm emission line ratio (L_([C ii])/L_([N ii]) > 55). The relatively strong [C ii] emission may be caused by abundant photodissociation regions and sub-solar metallicity, or by shock heating. The origin of the unusually strong [C ii] emission could be causally related to the location within the giant LAB, although the relationship between extended Ly\u03b1 emission and interstellar medium conditions of associated galaxies is yet to be understand.", "date": "2017-01-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "834", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L16", "id_number": "CaltechAUTHORS:20170120-133954598", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170120-133954598", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Astronomical Observatory of Japan", "grant_number": "NAOJ-ALMA-0071" }, { "agency": "National Astronomical Observatory of Japan", "grant_number": "NAOJ-ALMA-0131" }, { "agency": "National Astronomical Observatory of Japan", "grant_number": "NAOJ-ALMA-140" }, { "agency": "National Astronomical Observatory of Japan", "grant_number": "NAOJ-ALMA-0152" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "16H06713" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "16H02166" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "25102073" }, { "agency": "European Research Council (ERC)", "grant_number": "321302" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L00075X/1" }, { "agency": "European Research Council (ERC)", "grant_number": "DUSTYGAL 321334" }, { "agency": "Royal Society" }, { "agency": "Swedish Research Council" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Knut and Alice Wallenberg Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/2041-8213/834/2/L16", "primary_object": { "basename": "1701.00043v1.pdf", "url": "https://authors.library.caltech.edu/records/nbj1s-gbp47/files/1701.00043v1.pdf" }, "related_objects": [ { "basename": "Umehata_2017_ApJL_834_L16.pdf", "url": "https://authors.library.caltech.edu/records/nbj1s-gbp47/files/Umehata_2017_ApJL_834_L16.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Umehata, Hideki; Matsuda, Yuichi; et el." }, { "id": "https://authors.library.caltech.edu/records/f7j21-mm492", "eprint_id": 72448, "eprint_status": "archive", "datestamp": "2023-08-22 19:16:05", "lastmod": "2023-10-23 22:35:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" } ] }, "title": "The Rest-frame Optical Spectroscopic Properties of Ly\u03b1-emitters at z~2.5: The Physical Origins of Strong Ly\u03b1 Emission", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: dwarf; galaxies: formation; galaxies: high-redshift", "note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2016 August 17; revised 2016 September 15; accepted 2016 September 21; published 2016 November 30. \n\nWe thank Eliot Quataert, Mariska Kriek, and Dawn Erb for extremely useful discussions. In addition, we thank the organizers of the Escape of Lyman radiation from galactic labyrinths conference at the Orthodox Academy of Crete in 2016 April; this paper was much improved by the talks and discussion that took place at that meeting. This paper uses data collected through Keck program 2015B_U42M, and we are indebted to the staff of the W.M. Keck Observatory who keep the instruments and telescopes running effectively. We also wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. This work has been supported in part by the US National Science Foundation through grants AST-0908805 and AST-1313472. RFT is grateful for support from the Miller Institute for Basic Research in Science at the University of California, Berkeley. \n\nBased on data obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W.M. Keck Foundation.\n\nPublished - Trainor_2016_ApJ_832_171.pdf
Accepted Version - 1608.07280.pdf
", "abstract": "We present the rest-frame optical spectroscopic properties of 60 faint (R_(AB) ~ 27; L ~ 0.1 L_*) Ly\u03b1-selected galaxies (LAEs) at z \u2248 2.56. These LAEs also have rest-UV spectra of their Ly\u03b1 emission line morphologies, which trace the effects of interstellar and circumgalactic gas on the escape of Ly\u03b1 photons. We find that the LAEs have diverse rest-optical spectra, but their average spectroscopic properties are broadly consistent with the extreme low-metallicity end of the populations of continuum-selected galaxies selected at z \u2248 2\u20133. In particular, the LAEs have extremely high [O iii] \u03bb5008/H\u03b2 ratios (log([O iii]/H\u03b2) ~ 0.8) and low [N ii] \u03bb6585/H\u03b1 ratios (log([N ii]/H\u03b1) < 1.15). Coupled with a detection of the [O iii] \u03bb4364 auroral line, these measurements indicate that the star-forming regions in faint LAEs are characterized by high electron temperatures (T_e \u2248 1.8 \u00d7 10^4 K), low oxygen abundances (12 + log(O/H) \u2248 8.04, Z_(neb) \u2248 0.22Z_\u2299), and high excitations with respect to their more luminous continuum-selected analogs. Several of our faintest LAEs have line ratios consistent with even lower metallicities, including six with 12 + log(O/H) \u2248 6.9\u20137.4 (Z_(neb) \u2248 0.02\u20130.05Z_\u2299). We interpret these observations in light of new models of stellar evolution (including binary interactions) that have been shown to produce long-lived populations of hot, massive stars at low metallicities. We find that strong, hard ionizing continua are required to reproduce our observed line ratios, suggesting that faint galaxies are efficient producers of ionizing photons and important analogs of reionization-era galaxies. Furthermore, we investigate the physical trends accompanying Ly\u03b1 emission across the largest current sample of combined Ly\u03b1 and rest-optical galaxy spectroscopy, including both the 60 KBSS-Ly\u03b1 LAEs and 368 more luminous galaxies at similar redshifts. We find that the net Ly\u03b1 emissivity (parameterized by the Ly\u03b1 equivalent width) is strongly correlated with nebular excitation and ionization properties and weakly correlated with dust attenuation, suggesting that metallicity plays a strong role in determining the observed properties of these galaxies by modulating their stellar spectra, nebular excitation, and dust content.", "date": "2016-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "832", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 171", "id_number": "CaltechAUTHORS:20161130-114300659", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161130-114300659", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "Miller Institute for Basic Research in Science" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.3847/0004-637X/832/2/171", "primary_object": { "basename": "1608.07280.pdf", "url": "https://authors.library.caltech.edu/records/f7j21-mm492/files/1608.07280.pdf" }, "related_objects": [ { "basename": "Trainor_2016_ApJ_832_171.pdf", "url": "https://authors.library.caltech.edu/records/f7j21-mm492/files/Trainor_2016_ApJ_832_171.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Trainor, Ryan F.; Strom, Allison L.; et el." }, { "id": "https://authors.library.caltech.edu/records/r49qx-3rp08", "eprint_id": 72058, "eprint_status": "archive", "datestamp": "2023-08-19 00:05:58", "lastmod": "2023-10-23 17:49:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Geach-J-E", "name": { "family": "Geach", "given": "J. E." }, "orcid": "0000-0003-4964-4635" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "ALMA Observations of Ly\u03b1 Blob 1: Halo Substructure Illuminated from Within", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: halos \u2013 galaxies: high-redshift", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 June 10; revised 2016 July 21; accepted 2016 August 8; published 2016 November 14. \n\nWe thank the referee for a constructive report that has improved this work. J.E.G. is supported by a Royal Society University Research Fellowship. Partial support for D.N. was provided by NSF AST-1442650, NASA HST AR-13906.001, and a Cottrell College Science Award. M.H. acknowledges the support of the Swedish Research Council, Vetenskapsr\u00e5det and the Swedish National Space Board (SNSB), and is a Fellow of the Knut and Alice Wallenberg Foundation. H.D. acknowledges financial support from the Spanish Ministry of Economy and Competitiveness (MINECO) under the 2014 Ram\u00f3n y Cajal program MINECO RYC-2014-15686. A.V. is supported by a Research Fellowship from the Leverhulme Trust. The authors acknowledge excellent support of the UK ALMA Regional Centre Node. This letter makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00704S, ADS/JAO.ALMA#2013.1.00922.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This work was supported by the ALMA Japan Research Grant of NAOJ Chile Observatory, NAOJ-ALMA-0086.\n\nPublished - Geach_2016_ApJ_832_37.pdf
Submitted - 1608.02941v1.pdf
", "abstract": "We present new Atacama Large Millimeter/Submillimeter Array (ALMA) 850 \u03bcm continuum observations of the original Ly\u03b1 Blob (LAB) in the SSA22 field at z = 3.1 (SSA22-LAB01). The ALMA map resolves the previously identified submillimeter source into three components with a total flux density of S_(850) = 1.68 \u00b1 0.06 mJy, corresponding to a star-formation rate of ~150 M \u2299 yr^(\u22121). The submillimeter sources are associated with several faint (m \u2248 27 mag) rest-frame ultraviolet sources identified in Hubble Space Telescope Imaging Spectrograph (STIS) clear filter imaging (\u03bb \u2248 5850 \u00c5). One of these companions is spectroscopically confirmed with the Keck Multi-Object Spectrometer For Infra-Red Exploration to lie within 20 projected kpc and 250 km s^(\u22121) of one of the ALMA components. We postulate that some of these STIS sources represent a population of low-mass star-forming satellites surrounding the central submillimeter sources, potentially contributing to their growth and activity through accretion. Using a high-resolution cosmological zoom simulation of a 10^(13) M\u2299 halo at z = 3, including stellar, dust, and Ly\u03b1 radiative transfer, we can model the ALMA+STIS observations and demonstrate that Ly\u03b1 photons escaping from the central submillimeter sources are expected to resonantly scatter in neutral hydrogen, the majority of which is predicted to be associated with halo substructure. We show how this process gives rise to extended Ly\u03b1 emission with similar surface brightness and morphology to observed giant LABs.", "date": "2016-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "832", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 37", "id_number": "CaltechAUTHORS:20161116-125343348", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161116-125343348", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" }, { "agency": "NSF", "grant_number": "AST-1442650" }, { "agency": "NASA", "grant_number": "HST AR-13906.001" }, { "agency": "Cottrell College Science Award" }, { "agency": "Swedish Research Council" }, { "agency": "Vetenskapsr\u00e5det" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)", "grant_number": "RYC-2014-15686" }, { "agency": "Leverhulme Trust" }, { "agency": "National Astronomical Observatory of Japan", "grant_number": "NAOJ-ALMA-0086" } ] }, "doi": "10.3847/0004-637X/832/1/37", "primary_object": { "basename": "1608.02941v1.pdf", "url": "https://authors.library.caltech.edu/records/r49qx-3rp08/files/1608.02941v1.pdf" }, "related_objects": [ { "basename": "Geach_2016_ApJ_832_37.pdf", "url": "https://authors.library.caltech.edu/records/r49qx-3rp08/files/Geach_2016_ApJ_832_37.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Geach, J. E. and Steidel, C. C." }, { "id": "https://authors.library.caltech.edu/records/16ggw-cw493", "eprint_id": 72171, "eprint_status": "archive", "datestamp": "2023-08-22 19:05:10", "lastmod": "2023-10-23 18:00:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kelly-P-L", "name": { "family": "Kelly", "given": "P. L." }, "orcid": "0000-0003-3142-997X" }, { "id": "Brammer-G", "name": { "family": "Brammer", "given": "G." } }, { "id": "Selsing-J", "name": { "family": "Selsing", "given": "J." } }, { "id": "Foley-R-J", "name": { "family": "Foley", "given": "R. J." } }, { "id": "Hjorth-J", "name": { "family": "Hjorth", "given": "J." }, "orcid": "0000-0002-4571-2306" }, { "id": "Rodney-S-A", "name": { "family": "Rodney", "given": "S. A." }, "orcid": "0000-0003-1947-687X" }, { "id": "Christensen-L-E", "name": { "family": "Christensen", "given": "L." } }, { "id": "Strolger-L-G", "name": { "family": "Strolger", "given": "L.-G." } }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Treu-Tommaso", "name": { "family": "Treu", "given": "T." }, "orcid": "0000-0002-8460-0390" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "A." }, "orcid": "0000-0001-6369-1636" }, { "id": "Riess-A-G", "name": { "family": "Riess", "given": "A. G." } }, { "id": "Zitrin-Adi", "name": { "family": "Zitrin", "given": "A." }, "orcid": "0000-0002-0350-4488" }, { "id": "Schmidt-K-B", "name": { "family": "Schmidt", "given": "K. B." } }, { "id": "Brada\u010d-M", "name": { "family": "Brada\u010d", "given": "M." } }, { "id": "Jha-S-W", "name": { "family": "Jha", "given": "S. W." }, "orcid": "0000-0001-8738-6011" }, { "id": "Graham-M-L", "name": { "family": "Graham", "given": "M. L." }, "orcid": "0000-0002-9154-3136" }, { "id": "McCully-C", "name": { "family": "McCully", "given": "C." }, "orcid": "0000-0001-5807-7893" }, { "id": "Graur-O", "name": { "family": "Graur", "given": "O." } }, { "id": "Weiner-B-J", "name": { "family": "Weiner", "given": "B. J." } }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "J. M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" } ] }, "title": "SN Refsdal: Classification as a Luminous and Blue SN 1987A-like Type II Supernova", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general; galaxies: clusters: individual (MACS J1149+2223); gravitational lensing: strong; supernovae: general; supernovae: individual (SN Refsdal)", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2015 December 31. Accepted 2016 August 9. Published 2016 November 9. \n\nWe would like to thank Space Telescope Science Institute (STScI) director Matt Mountain for making it possible to obtain the HST WFC3 grism spectra of SN Refsdal. We express our appreciation for the efforts of HST Program Coordinator Beth Periello and Contact Scientist Norbert Pirzkal, as well as Claus Leitherer, Andrew Fox, Ken Sembach, and Miranda Link for scheduling the grism observations. Based in part on observations made with ESO telescopes at the La Silla Paranal Observatory under program ID 295.D-5014. We thank Ori Fox for helpful discussions about the Type IIn SN 2005cp, and Nathan Smith for useful comments about CSM interaction and SN 1987A-like SNe. \n\nSupport for the preparation of the paper is from HST grants GO-14041 and GO-14199. The GLASS program was supported by GO-13459, and the FrontierSN photometric follow-up program has funding through GO-13386. A.Z. is supported by a Hubble Fellowship (HF2-51334.001-A) awarded by STScI, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. R.J.F. gratefully acknowledges support from National Science Foundation (NSF) grant AST-1518052 and the Alfred P. Sloan Foundation. Supernova research at Rutgers University (S.W.J.) is supported by NSF CAREER award AST-0847157, and NASA/Keck JPL RSA 1508337 and 1520634. C.M. is supported through NSF grant AST-1313484. The DNRF provided funding for the Dark Cosmology Centre. JMS is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. A.V.F.'s group at UC Berkeley has received generous financial assistance from the Christopher R. Redlich Fund, the TABASGO Foundation, Gary & Cynthia Bengier, and NSF grant AST-1211916. The work of A.V.F. was completed at the Aspen Center for Physics, which is supported by NSF grant PHY-1066293; he thanks the Center for its hospitality during the black holes workshop in 2016 June and July. \n\nThis research uses services or data provided by the NOAO Science Archive. NOAO is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under a cooperative agreement with the NSF. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. We recognize the Hawaiian community for the opportunity to conduct these observations from the summit of Mauna Kea.\n\nPublished - Kelly_2016_ApJ_831_205.pdf
Submitted - 1512.09093v1.pdf
", "abstract": "We have acquired Hubble Space Telescope (HST) and Very Large Telescope near-infrared spectra and images of supernova (SN) Refsdal after its discovery as an Einstein cross in fall 2014. The HST light curve of SN Refsdal has a shape consistent with the distinctive, slowly rising light curves of SN 1987A-like SNe, and we find strong evidence for a broad H\u03b1 P-Cygni profile and Na I D absorption in the HST grism spectrum at the redshift (z = 1.49) of the spiral host galaxy. SNe IIn, largely powered by circumstellar interaction, could provide a good match to the light curve of SN Refsdal, but the spectrum of a SN IIn would not show broad and strong H\u03b1 and Na I D absorption. From the grism spectrum, we measure an H\u03b1 expansion velocity consistent with those of SN 1987A-like SNe at a similar phase. The luminosity, evolution, and Gaussian profile of the H\u03b1 emission of the WFC3 and X-shooter spectra, separated by ~2.5 months in the rest frame, provide additional evidence that supports the SN 1987A-like classification. In comparison with other examples of SN 1987A-like SNe, photometry of SN Refsdal favors bluer B \u2212 V and V \u2212 R colors and one of the largest luminosities for the assumed range of potential magnifications. The evolution of the light curve at late times will provide additional evidence about the potential existence of any substantial circumstellar material. Using MOSFIRE and X-shooter spectra, we estimate a subsolar host-galaxy metallicity (8.3 \u00b1 0.1 dex and <8.4 dex, respectively) near the explosion site.", "date": "2016-11-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "831", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 205", "id_number": "CaltechAUTHORS:20161118-133421969", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161118-133421969", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO-14041" }, { "agency": "NASA", "grant_number": "GO-14199" }, { "agency": "NASA", "grant_number": "GO-13459" }, { "agency": "NASA", "grant_number": "GO-13386" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HF2-51334.001-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF", "grant_number": "AST-1518052" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF", "grant_number": "AST-0847157" }, { "agency": "NASA/Keck JPL RSA", "grant_number": "1508337" }, { "agency": "NASA/Keck JPL RSA", "grant_number": "1520634" }, { "agency": "NSF", "grant_number": "AST-1313484" }, { "agency": "Danish National Research Foundation" }, { "agency": "NSF Astronomy and Astrophysics Fellowship", "grant_number": "AST-1302771" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.3847/0004-637X/831/2/205", "primary_object": { "basename": "Kelly_2016_ApJ_831_205.pdf", "url": "https://authors.library.caltech.edu/records/16ggw-cw493/files/Kelly_2016_ApJ_831_205.pdf" }, "related_objects": [ { "basename": "1512.09093v1.pdf", "url": "https://authors.library.caltech.edu/records/16ggw-cw493/files/1512.09093v1.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Kelly, P. L.; Brammer, G.; et el." }, { "id": "https://authors.library.caltech.edu/records/5f12m-5ze74", "eprint_id": 71558, "eprint_status": "archive", "datestamp": "2023-08-22 19:03:00", "lastmod": "2023-10-23 15:54:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Vasei-Kaveh", "name": { "family": "Vasei", "given": "Kaveh" } }, { "id": "Siana-Brian-D", "name": { "family": "Siana", "given": "Brian" }, "orcid": "0000-0002-4935-9511" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Quider-A-M", "name": { "family": "Quider", "given": "Anna M." } }, { "id": "Alavi-A", "name": { "family": "Alavi", "given": "Anahita" }, "orcid": "0000-0002-8630-6435" }, { "id": "Rafelski-M", "name": { "family": "Rafelski", "given": "Marc" }, "orcid": "0000-0002-9946-4731" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Lewis-G-F", "name": { "family": "Lewis", "given": "Geraint F." } } ] }, "title": "The Lyman Continuum Escape Fraction of the Cosmic Horseshoe: A Test of Indirect Estimates", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (Cosmic Horseshoe); galaxies: starburst; gravitational lensing: strong; intergalactic medium; ultraviolet: galaxies", "note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2016 March 8; revised 2016 July 26; accepted 2016 August 6; published 2016 October 26. \n\nThe 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. We also thank the referee for comments that helped clarify specific points. \n\nFacilities: HST (WFC3 - , UVIS) - , Keck (ESI).\n\nPublished - Vasei_2016_ApJ_831_38.pdf
", "abstract": "High-redshift star-forming galaxies are likely responsible for the reionization of the universe, yet direct detection of their escaping ionizing (Lyman continuum [LyC]) photons has proven to be extremely challenging. In this study, we search for escaping LyC of the Cosmic Horseshoe, a gravitationally lensed, star-forming galaxy at z = 2.38 with a large magnification of ~24. Transmission at wavelengths of low-ionization interstellar absorption lines in the rest-frame ultraviolet suggests a patchy, partially transparent interstellar medium. This makes it an ideal candidate for direct detection of the LyC. We obtained a 10-orbit Hubble near-UV image using the Wide Field Camera 3 (WFC3)/UVIS F275W filter that probes wavelengths just below the Lyman limit at the redshift of the Horseshoe in an attempt to detect escaping LyC radiation. After fully accounting for the uncertainties in the opacity of the intergalactic medium (IGM) and accounting for the charge transfer inefficiency in the WFC3 CCDs, we find a 3 \u03c3 upper limit for the relative escape fraction of f_(esc,rel) < 0.08. This value is a factor of five lower than the value (0.4) predicted by the 40% transmission in the low-ion absorption lines. Though possible, it is unlikely that the nondetection is due to a high-opacity line of sight through the IGM < 20% chance). We discuss several possible causes for the discrepancy between the escape fraction and the covering fraction and consider the implications for future attempts at both direct LyC detection and indirect estimates of the escape fraction.", "date": "2016-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "831", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 38", "id_number": "CaltechAUTHORS:20161027-140937011", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161027-140937011", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Postdoctoral Program" } ] }, "doi": "10.3847/0004-637X/831/1/38", "primary_object": { "basename": "Vasei_2016_ApJ_831_38.pdf", "url": "https://authors.library.caltech.edu/records/5f12m-5ze74/files/Vasei_2016_ApJ_831_38.pdf" }, "resource_type": "article", "pub_year": "2016", "author_list": "Vasei, Kaveh; Siana, Brian; et el." }, { "id": "https://authors.library.caltech.edu/records/a2t40-09w45", "eprint_id": 71031, "eprint_status": "archive", "datestamp": "2023-08-22 18:53:03", "lastmod": "2023-10-23 15:17:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" } ] }, "title": "A High Fraction of Ly\u03b1-Emitters Among Galaxies with Extreme Emission Line Ratios at z ~ 2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 March 8; revised 2016 May 16; accepted 2016 June 4; published 2016 October 10. \n\nWe would like to thank the anonymous referee for a helpful and constructive report. D.K.E. is supported by the U.S. National Science Foundation through the Faculty Early Career Development (CAREER) Program, grant AST-1255591. Additional support comes from the NSF through grants AST-0908805 (C.C.S.) and AST-1313472 (C.C.S., A.L.S.), and an NSF Graduate Student Research Fellowship (A.L.S.). We are grateful to Alaina Henry for providing flux measurements for the Green Pea galaxies, and to the organizers and participants of the First Carnegie Symposium in Honor of Leonard Searle, \"Understanding Nebular Emission in High-Redshift Galaxies,\" held at the Carnegie Observatories in 2015 July, for many useful discussions. Finally, we wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests.\n\nPublished - Erb_2016_ApJ_830_52.pdf
Submitted - 1605.04919v2.pdf
", "abstract": "Star-forming galaxies form a sequence in the [O III] \u03bb5007/H\u03b2 versus [N II] \u03bb6584/H\u0251 diagnostic diagram, with low-metallicity, highly ionized galaxies falling in the upper left corner. Drawing from a large sample of UV-selected star-forming galaxies at z ~ 2 with rest-frame optical nebular emission line measurements from Keck-MOSFIRE, we select the extreme ~5% of the galaxies lying in this upper left corner, requiring log([NII]/H\u03b2) \u2a7d -1.1 and log([O III]/H\u03b2) \u2a7e/0.75. These cuts identify galaxies with 12 + log(O/H \u227e 8.0, when oxygen abundances are measured via the O3N2 diagnostic. We study the Ly\u03b1 properties of the resulting sample of 14 galaxies. The mean (median) rest-frame Ly\u03b1 equivalent width is 39 (36) \u00c5, and 11 of the 14 objects (79%) are Ly\u03b1 emitters (LAEs) with W_(Ly\u03b1) > 20 \u00c5. We compare the equivalent width distribution of a sample of 522 UV-selected galaxies at 2.0 < z < 2.6 identified without regard to their optical line ratios; this sample has mean (median) Ly\u03b1 equivalent width \u22121 (\u22124) \u00c5, and only 9% of these galaxies qualify as LAEs. The extreme galaxies typically have lower attenuation at Ly\u03b1 than those in the comparison sample and have ~50% lower median oxygen abundances. Both factors are likely to facilitate the escape of Ly\u03b1: in less dusty galaxies Ly\u03b1 photons are less likely to be absorbed during multiple scatterings, while the harder ionizing spectrum and higher ionization parameter associated with strong, low-metallicity star formation may reduce the covering fraction or column density of neutral hydrogen, further easing Ly\u03b1 escape. The use of nebular emission line ratios may prove useful in the identification of galaxies with low opacity to Ly\u03b1 photons across a range of redshifts.", "date": "2016-10-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "830", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 52", "id_number": "CaltechAUTHORS:20161012-142337724", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161012-142337724", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1255591" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "NSF Graduate Research Fellowship" } ] }, "doi": "10.3847/0004-637X/830/1/52", "primary_object": { "basename": "1605.04919v2.pdf", "url": "https://authors.library.caltech.edu/records/a2t40-09w45/files/1605.04919v2.pdf" }, "related_objects": [ { "basename": "Erb_2016_ApJ_830_52.pdf", "url": "https://authors.library.caltech.edu/records/a2t40-09w45/files/Erb_2016_ApJ_830_52.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Erb, Dawn K.; Pettini, Max; et el." }, { "id": "https://authors.library.caltech.edu/records/ndgt1-ssz15", "eprint_id": 70282, "eprint_status": "archive", "datestamp": "2023-08-22 18:40:46", "lastmod": "2023-10-20 22:06:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Bogosavljevi\u0107-M", "name": { "family": "Bogosavljevi\u0107", "given": "Milan" } } ] }, "title": "Spectroscopic Measurements of the Far-Ultraviolet Dust Attenuation Curve at z~3", "ispublished": "pub", "full_text_status": "public", "keywords": "dark ages, reionization, first stars; dust, extinction; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: ISM", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2015 December 7; revised 2016 May 10; accepted 2016 May 23; published 2016 September 8. \n\nN.A.R. is supported by an Alfred P. Sloan Research Fellowship, and acknowledges the visitors program at the Institute of Astronomy in Cambridge, UK, where part of this research was conducted. C.C.S. acknowledges NSF grants AST-0908805 and AST-1313472. M.B. acknowledges support of the Serbian MESTD through grant ON176021. We thank Allison Strom for providing the photometry for the KBSS galaxies. We are grateful to the anonymous referee whose comments led to significant improvements in the presentation of the analysis. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, the observations presented herein would not have been possible.\n\nPublished - apj_828_2_107.pdf
Submitted - 1606.00434v1.pdf
", "abstract": "We present the first spectroscopic measurements of the shape of the far-ultraviolet (far-UV; \u03bb = 950-1500 \u00c5) dust attenuation curve at high redshift (z ~ 3). Our analysis employs rest-frame UV spectra of 933 galaxies at z ~ 3, 121 of which have very deep spectroscopic observations (\u22737hr) at \u03bb = 850 - 1300 \u00c5, with the Low Resolution Imaging Spectrograph on the Keck Telescope. By using an iterative approach in which we calculate the ratios of composite spectra in different bins of continuum color excess, E(B-V), we derive a dust curve that implies a lower attenuation in the far-UV for a given E(B-V) than those obtained with standard attenuation curves. We demonstrate that the UV composite spectra of z ~ 3 galaxies can be modeled well by assuming our new attenuation curve, a high covering fraction of Hi, and absorption from the Lyman\u2013Werner bands of H_2 with a small (\u227e20%) covering fraction. The low covering fraction of H_2 relative to that of the H_I and dust suggests that most of the dust in the ISM of typical galaxies at z ~ 3 is unrelated to the catalysis of H_2, and is associated with other phases of the ISM (i.e., the ionized and neutral gas). The far-UV dust curve implies a factor of \u2248 2 lower dust attenuation of Lyman continuum (ionizing) photons relative to those inferred from the most commonly assumed attenuation curves for L^* galaxies at z ~ 3. Our results may be utilized to assess the degree to which ionizing photons are attenuated in H ii regions or, more generally, in the ionized or low column density N(HI) \u227e 10^(17.2) cm^(\u22122) neutral ISM of high-redshift galaxies.", "date": "2016-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "828", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 107", "id_number": "CaltechAUTHORS:20160912-133213600", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160912-133213600", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "Ministry of Education, Science and Technological Development (Serbia)", "grant_number": "ON176021" } ] }, "doi": "10.3847/0004-637X/828/2/107", "primary_object": { "basename": "1606.00434v1.pdf", "url": "https://authors.library.caltech.edu/records/ndgt1-ssz15/files/1606.00434v1.pdf" }, "related_objects": [ { "basename": "apj_828_2_107.pdf", "url": "https://authors.library.caltech.edu/records/ndgt1-ssz15/files/apj_828_2_107.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Reddy, Naveen A.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/pkhb8-e1y26", "eprint_id": 70273, "eprint_status": "archive", "datestamp": "2023-08-22 18:40:39", "lastmod": "2023-10-20 22:05:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Bogosavljevi\u0107-M", "name": { "family": "Bogosavljevi\u0107", "given": "Milan" } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" } ] }, "title": "The Connection Between Reddening, Gas Covering Fraction, and the Escape of Ionizing Radiation at High Redshift", "ispublished": "pub", "full_text_status": "public", "keywords": "dark ages, reionization, first stars; dust, extinction; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: ISM", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 May 10; revised 2016 June 8; accepted 2016 June 8; published 2016 September 8. \n\nN.A.R. is supported by an Alfred P. Sloan Research Fellowship, and acknowledges the visitors program at the Institute of Astronomy in Cambridge, UK, where part of this research was conducted. C.C.S. acknowledges NSF grants AST-0908805 and AST-1313472. MB acknowledges support of the Serbian MESTD through grant ON176021. NAR acknowledges Gwen Rudie for useful discussions. We are grateful to the anonymous referee whose comments led to significant improvements in the clarity, content, and presentation of the analysis and results. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, the observations presented herein would not have been possible.\n\nPublished - apj_828_2_108.pdf
Submitted - 1606.03452v1.pdf
", "abstract": "Using a large sample of spectroscopically confirmed z ~ 3 galaxies, we establish an empirical relationship between reddening (E(B-V), neutral gas covering fraction (f_(cov)HI), and the escape of ionizing (Lyman continuum, LyC) photons. Our sample includes 933 galaxies at z ~ 3,121 of which have deep spectroscopic observations (\u22737 hr) at 850 \u227e \u03bb_(rest) \u227e 1300 \u00c5 with the Low Resolution Imaging Spectrograph on Keck. The high covering fraction of outflowing optically thick HI indicated by the composite pectra of these galaxies implies that photoelectric absorption, rather than dust attenuation, dominates the depletion of LyC photons. By modeling the composite spectra as the combination of an unattenuated stellar spectrum including nebular continuum emission with one that is absorbed by HI and reddened by a line-of-sight extinction, we derive an empirical relationship between E(B-V) and f_(cov) HI. Galaxies with redder UV continua have larger covering fractions of HI characterized by higher line-of-sight extinctions. We develop a model which connects the ionizing escape fraction with E(B-V), and which may be used to estimate the ionizing escape fraction for an ensemble of galaxies. Alternatively, direct measurements of the escape fraction for our sample allow us to constrain the intrinsic LyC-to-UV flux density ratio to be \u3008900 \u00c5)/S(1500 \u00c5\u3009_(int) \u2273 0.20, a value that favors stellar population models that include weaker stellar winds, a flatter initial mass function, and/or binary evolution. Last, we demonstrate how the framework discussed here may be used to assess the pathways by which ionizing radiation escapes from high-redshift galaxies.", "date": "2016-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "828", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 108", "id_number": "CaltechAUTHORS:20160912-091542652", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160912-091542652", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "Ministry of Education, Science and Technological Development (Serbia)", "grant_number": "ON176021" } ] }, "doi": "10.3847/0004-637X/828/2/108", "primary_object": { "basename": "1606.03452v1.pdf", "url": "https://authors.library.caltech.edu/records/pkhb8-e1y26/files/1606.03452v1.pdf" }, "related_objects": [ { "basename": "apj_828_2_108.pdf", "url": "https://authors.library.caltech.edu/records/pkhb8-e1y26/files/apj_828_2_108.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Reddy, Naveen A.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/bzybh-hg986", "eprint_id": 70852, "eprint_status": "archive", "datestamp": "2023-08-20 13:28:20", "lastmod": "2023-10-20 23:35:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kato-Y", "name": { "family": "Kato", "given": "Y." } }, { "id": "Matsuda-Yuichi", "name": { "family": "Matsuda", "given": "Y." } }, { "id": "Smail-Ian-R", "name": { "family": "Smail", "given": "Ian" }, "orcid": "0000-0003-3037-257X" }, { "id": "Swinbank-A-M", "name": { "family": "Swinbank", "given": "A. M." } }, { "id": "Hatsukade-B", "name": { "family": "Hatsukade", "given": "B." } }, { "id": "Umehata-Hideki", "name": { "family": "Umehata", "given": "H." } }, { "id": "Tanaka-I", "name": { "family": "Tanaka", "given": "I." } }, { "id": "Saito-T", "name": { "family": "Saito", "given": "T." } }, { "id": "Iono-Daisuke", "name": { "family": "Iono", "given": "D." }, "orcid": "0000-0002-2364-0823" }, { "id": "Tamura-Yoichi", "name": { "family": "Tamura", "given": "Y." } }, { "id": "Kohno-Kotaro", "name": { "family": "Kohno", "given": "K." }, "orcid": "0000-0002-4052-2394" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "D. K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Lehmer-B-D", "name": { "family": "Lehmer", "given": "B. D." }, "orcid": "0000-0003-2192-3296" }, { "id": "Geach-J-E", "name": { "family": "Geach", "given": "J. E." }, "orcid": "0000-0003-4964-4635" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Alexander-D-M", "name": { "family": "Alexander", "given": "D. M." }, "orcid": "0000-0002-5896-6313" }, { "id": "Yamada-Toru", "name": { "family": "Yamada", "given": "T." } }, { "id": "Hayashino-T", "name": { "family": "Hayashino", "given": "T." } } ] }, "title": "Herschel protocluster survey: a search for dusty star-forming galaxies in protoclusters at z = 2\u20133", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation galaxies: high-redshift infrared: galaxies submillimetre: galaxies", "note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 May 19. Received 2016 May 16. In original form 2016 March 18. First published online May 23, 2016. \n\nWe thank the anonymous referee for helpful comments which significantly improved the clarity of this paper. We thank Scott Chapman, James Colbert, Emanuele Daddi, Koichiro Nakanishi, and Kazuhiro Shimasaku for useful discussions and supports. Rhythm Shimakawa and Mariko Kubo made enormous contribution to analyses. We acknowledge Masaru Kajisawa for our use of his MOIRCS fringe-removal software (Kajisawa et al. 2015) during the data reduction. \n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK). Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. UKIRT is funded by the STFC (UK). The W.M. Keck Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. \n\nThis research was supported in part by a grant from the Hayakawa Satio Fund awarded by the Astronomical Society of Japan. YM acknowledges support from JSPS KAKENHI Grant Number 20647268. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Grant DUSTYGAL (321334), and a Royal Society/Wolfson Merit Award. BH acknowledges support from JSPS KAKENHI Grant Number 15K17616. HU acknowledges support from Grant-in-Aid for JSPS Fellows, 26.11481.\n\nPublished - MNRAS-2016-Kato-3861-72.pdf
Submitted - 1605.07370v1.pdf
Supplemental Material - Supplement.zip
", "abstract": "We present a Herschel/SPIRE survey of three protoclusters at z = 2 \u2212 3 (2QZCluster, HS1700, SSA22). Based on the SPIRE colours (S_(350)/S_(250) and S_(500)/S_(350)) of 250 \u03bcm sources, we selected high redshift dusty star-forming galaxies potentially associated with the protoclusters. In the 2QZCluster field, we found a 4\u03c3 overdensity of six SPIRE sources around 4.5\u2032 (\u223c 2.2 Mpc) from a density peak of H\u03b1 emitters at z = 2.2. In the HS1700 field, we found a 5\u03c3 overdensity of eight SPIRE sources around 2.1\u2032 (\u223c 1.0 Mpc) from a density peak of LBGs at z = 2.3. We did not find any significant overdensities in SSA22 field, but we found three 500 \u03bcm sources are concentrated 3\u2032 (\u223c1.4 Mpc) east to the LAEs overdensity. If all the SPIRE sources in these three overdensities are associated with protoclusters, the inferred star-formation rate densities are 10^3 \u2212 10^4 times higher than the average value at the same redshifts. This suggests that dusty star-formation activity could be very strongly enhanced in z \u223c 2 \u2212 3 protoclusters. Further observations are needed to confirm the redshifts of the SPIRE sources and to investigate what processes enhance the dusty star-formation activity in z \u223c 2 \u2212 3 protoclusters.", "date": "2016-08-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "460", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3861-3872", "id_number": "CaltechAUTHORS:20161005-073437352", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161005-073437352", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "Astronomical Society of Japan" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20647268" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L00075X/1" }, { "agency": "European Research Council (ERC)", "grant_number": "DUSTYGAL 321334" }, { "agency": "Royal Society" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15K17616" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "26.11481" } ] }, "doi": "10.1093/mnras/stw1237", "primary_object": { "basename": "Supplement.zip", "url": "https://authors.library.caltech.edu/records/bzybh-hg986/files/Supplement.zip" }, "related_objects": [ { "basename": "1605.07370v1.pdf", "url": "https://authors.library.caltech.edu/records/bzybh-hg986/files/1605.07370v1.pdf" }, { "basename": "MNRAS-2016-Kato-3861-72.pdf", "url": "https://authors.library.caltech.edu/records/bzybh-hg986/files/MNRAS-2016-Kato-3861-72.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Kato, Y.; Matsuda, Y.; et el." }, { "id": "https://authors.library.caltech.edu/records/j5d4c-w5z10", "eprint_id": 69366, "eprint_status": "archive", "datestamp": "2023-08-22 18:25:53", "lastmod": "2023-10-20 16:50:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Bogosavljevi\u0107-M", "name": { "family": "Bogosavljevi\u0107", "given": "Milan" } }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Siana-Brian-D", "name": { "family": "Siana", "given": "Brian" }, "orcid": "0000-0002-4935-9511" }, { "id": "Mostardi-Robin-E", "name": { "family": "Mostardi", "given": "Robin E." } }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" } ] }, "title": "Q1549-C25: A Clean Source of Lyman-Continuum Emission at z = 3.15", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; diffuse radiation; galaxies: high-redshift; intergalactic medium", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 June 1; revised 2016 June 30; accepted 2016 July 13; published 2016 July 26. \n\nWe thank the anonymous referee for a constructive report. C.C.S. acknowledges support from NSF grants AST-0908805 and AST-1313472. A.E.S. acknowledges support from the David & Lucile Packard Foundation. N.A.R. is supported by an Alfred P. Sloan Research Fellowship. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible. \n\nBased on data obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration, and was made possible by the generous financial support of the W.M. Keck Foundation.\n\nPublished - apjl_826_2_L24.pdf
Submitted - 1606.00443v2.pdf
", "abstract": "We present observations of Q1549-C25, an ~L^* star-forming galaxy at z = 3.15 for which Lyman-continuum (LyC) radiation is significantly detected in deep Keck/LRIS spectroscopy. We find no evidence of contamination from a lower-redshift interloper close to the line of sight in the high signal-to-noise spectrum of Q1549-C25. Furthermore, the morphology of Q1549-C25 in V 606, J 125, and H 160 Hubble Space Telescope (HST) imaging reveals that the object consists of a single, isolated component within 1\". In combination, these data indicate Q1549-C25 as a clean spectroscopic detection of LyC radiation, only the second such object discovered to date at z ~ 3. We model the spectral energy distribution of Q1549-C25, finding evidence of negligible dust extinction, an age (assuming continuous star formation) of ~1 Gyr, and a stellar mass of M_* =7.9 x 10^9,M_\u2609. Although it is not possible to derive strong constraints on the absolute escape fraction of LyC emission, f _(esc)(LyC), from a single object, we use simulations of intergalactic and circumgalactic absorption to infer f_(esc)(LyC)\u2a7e 0.51 at 95% confidence. The combination of deep Keck/LRIS spectroscopy and Hubble Space Telescope imaging is required to assemble a larger sample of objects like Q1549-C25, and obtain robust constraints on the average f _(esc)(LyC) at z ~ 3 and beyond.", "date": "2016-08-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "826", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L24", "id_number": "CaltechAUTHORS:20160801-154642815", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160801-154642815", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.3847/2041-8205/826/2/L24", "primary_object": { "basename": "1606.00443v2.pdf", "url": "https://authors.library.caltech.edu/records/j5d4c-w5z10/files/1606.00443v2.pdf" }, "related_objects": [ { "basename": "apjl_826_2_L24.pdf", "url": "https://authors.library.caltech.edu/records/j5d4c-w5z10/files/apjl_826_2_L24.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Shapley, Alice E.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/wwx1c-get84", "eprint_id": 70791, "eprint_status": "archive", "datestamp": "2023-08-22 18:26:51", "lastmod": "2023-10-20 23:30:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" } ] }, "title": "Reconciling the Stellar and Nebular Spectra of High-redshift Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: high-redshift; H ii regions; ISM: abundances; stars: massive", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 March 28; revised 2016 May 3; accepted 2016 May 19; published 2016 July 28. \n\nWe thank Jarle Brinchmann, J. J. Eldridge, Elizabeth Stanway, Eric Pellegrini, Selma de Mink, Evan Kirby, Jim Fuller, Phil Hopkins, and Maryam Shirazi for very informative conversations. We benefited significantly from talks, discussions, and conversations during the First Carnegie Symposium in Honor of Leonard Searle, \"Understanding Nebular Emission in High-Redshift Galaxies,\" held at the Carnegie Observatories in Pasadena, 2015 July 13\u201317. T. Bensby, C. Esteban, and D. Erb kindly provided machine-readable data from their published work. This work has been supported in part by the US National Science Foundation through grants AST-0908805 and AST-1313472 (C.C.S., A.L.S., R.F.T.), as well as by an NSF Graduate Student Research Fellowship (A.L.S.). Finally, we wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests.\n\nPublished - apj_826_2_159.pdf
Submitted - 1605.07186v1.pdf
", "abstract": "We present a combined analysis of rest-frame far-UV (FUV; 1000\u20132000 \u00c5) and rest-frame optical (3600\u20137000 \u00c5) composite spectra formed from very deep Keck/LRIS and Keck/MOSFIRE observations of a sample of 30 star-forming galaxies with z = 2.40 \u00b1 0.11, selected to be broadly representative of the full KBSS-MOSFIRE spectroscopic survey. Since the same massive stars are responsible for the observed FUV continuum and for the excitation of the observed nebular emission, a self-consistent stellar population synthesis model should simultaneously match the details of the FUV stellar+nebular continuum and\u2014when inserted as the excitation source in photoionization models\u2014predict all observed nebular emission line ratios. We find that only models including massive star binaries, having low stellar metallicity (Z_*/Z_\u2299 \u2243 0.1) but relatively high nebular (ionized gas-phase) abundances Z_(neb)/Z_\u2299 \u2243 0.5), can successfully match all of the observational constraints. We show that this apparent discrepancy is naturally explained by highly super-solar O/Fe (\u22434-5(O/Fe_\u2299), expected for a gas whose enrichment is dominated by the products of core-collapse supernovae. While O dominates the physics of the ionized gas (and thus the nebular emission lines), Fe dominates the extreme-UV (EUV) and FUV opacity and controls the mass-loss rate from massive stars, resulting in particularly dramatic effects for massive stars in binary systems. This high nebular excitation\u2014caused by the hard EUV spectra of Fe-poor massive stars\u2014is much more common at high redshift (z \u2273 2) than low redshift due to systematic differences in the star formation history of typical galaxies.", "date": "2016-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "826", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 159", "id_number": "CaltechAUTHORS:20161004-083721878", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161004-083721878", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "NSF Graduate Research Fellowship" } ] }, "doi": "10.3847/0004-637X/826/2/159", "primary_object": { "basename": "1605.07186v1.pdf", "url": "https://authors.library.caltech.edu/records/wwx1c-get84/files/1605.07186v1.pdf" }, "related_objects": [ { "basename": "apj_826_2_159.pdf", "url": "https://authors.library.caltech.edu/records/wwx1c-get84/files/apj_826_2_159.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Steidel, Charles C.; Strom, Allison L.; et el." }, { "id": "https://authors.library.caltech.edu/records/raavv-3gb41", "eprint_id": 68880, "eprint_status": "archive", "datestamp": "2023-09-15 05:29:20", "lastmod": "2023-10-23 21:18:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Mateusz" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Moore-A-M", "name": { "family": "Moore", "given": "Anna" }, "orcid": "0000-0002-2894-6936" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan" }, "orcid": "0000-0002-6967-7322" } ] }, "title": "A Newly Forming Cold Flow Protogalactic Disk, a Signature of Cold Accretion from the Cosmic Web", "ispublished": "pub", "full_text_status": "public", "keywords": "dark matter; galaxies: evolution; galaxies: formation; galaxies: high-redshift; intergalactic medium; quasars: general", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 February 23; revised 2016 April 11; accepted 2016 April 13; published 2016 June 3. \n\nThis work was supported by the National Science Foundation and the California Institute of Technology. R.F.T. receives financial support from the UC Berkeley Miller Institute for Basic Research in Science.\n\nPublished - apjl_824_1_L5.pdf
", "abstract": "How galaxies form from, and are fueled by, gas from the intergalactic medium (IGM) remains one of the major unsolved problems in galaxy formation. While the classical Cold Dark Matter paradigm posits galaxies forming from cooling virialized gas, recent theory and numerical simulations have highlighted the importance of cold accretion flows\u2014relatively cool (T ~ few \u00d7 104 K) unshocked gas streaming along filaments into dark matter halos, including hot, massive, high-redshift halos. These flows are thought to deposit gas and angular momentum into the circumgalactic medium resulting in disk- or ring-like structures, eventually coalescing into galaxies forming at filamentary intersections. We earlier reported a bright, Ly\u03b1 emitting filament near the QSO HS1549+19 at redshift z = 2.843 discovered with the Palomar Cosmic Web Imager. We now report that the bright part of this filament is an enormous (R > 100 kpc) rotating structure of hydrogen gas with a disk-like velocity profile consistent with a 4 \u00d7 10^(12) M_\u2299 halo. The orbital time of the outer part of the what we term a \"protodisk\" is comparable to the virialization time and the age of the universe at this redshift. We propose that this protodisk can only have recently formed from cold gas flowing directly from the cosmic web.", "date": "2016-06-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "824", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L5", "id_number": "CaltechAUTHORS:20160707-085528559", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160707-085528559", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Caltech" }, { "agency": "Miller Institute for Basic Research in Science" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.3847/2041-8205/824/1/L5", "primary_object": { "basename": "apjl_824_1_L5.pdf", "url": "https://authors.library.caltech.edu/records/raavv-3gb41/files/apjl_824_1_L5.pdf" }, "resource_type": "article", "pub_year": "2016", "author_list": "Martin, D. Christopher; Matuszewski, Mateusz; et el." }, { "id": "https://authors.library.caltech.edu/records/w5jz4-gq343", "eprint_id": 68886, "eprint_status": "archive", "datestamp": "2023-09-15 05:29:28", "lastmod": "2023-10-23 21:18:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Topping-M-W", "name": { "family": "Topping", "given": "Michael W." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Substructure within the SSA22 protocluster at z \u2248 3.09", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: individual (SSA22); galaxies: formation; galaxies: high-redshift; galaxies: starburst; large-scale structure of universe", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 May 5; revised 2016 May 20; accepted 2016 May 20; published 2016 June 8. \n\nWe thank Abhimat Gautam and Tommaso Treu for useful comments. C.C.S. acknowledges support from NSF grants AST-0908805 and AST-1313472. A.E.S. acknowledges support from the David & Lucile Packard Foundation. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible.\n\nPublished - apjl_824_1_L11.pdf
Submitted - 1605.02079v2.pdf
", "abstract": "We present the results of a densely sampled spectroscopic survey of the SSA22 protocluster at z \u2248 3.09. Our sample with Keck/LRIS spectroscopy includes 106 Ly\u03b1 emitters (LAEs) and 40 Lyman break galaxies (LBGs) at z = 3.05\u20133.12. These galaxies are contained within the 9' \u00d7 9' region in which the protocluster was discovered, which also hosts the maximum galaxy overdensity in the SSA22 region. The redshift histogram of our spectroscopic sample reveals two distinct peaks, at z = 3.069 (blue; 43 galaxies) and z = 3.095 (red; 103 galaxies). Furthermore, objects in the blue and red peaks are segregated on the sky, with galaxies in the blue peak concentrating toward the western half of the field. These results suggest that the blue and red redshift peaks represent two distinct structures in physical space. Although the double-peaked redshift histogram is traced in the same manner by LBGs and LAEs, and brighter and fainter galaxies, we find that 9 out of 10 X-ray AGNs in SSA22, and all 7 spectroscopically confirmed giant Ly\u03b1 \"blobs,\" reside in the red peak. We combine our data set with sparsely sampled spectroscopy from the literature over a significantly wider area, finding preliminary evidence that the double-peaked structure in redshift space extends beyond the region of our dense spectroscopic sampling. In order to fully characterize the three-dimensional structure, dynamics, and evolution of large-scale structure in the SSA22 overdensity, we require the measurement of large samples of LAE and LBG redshifts over a significantly wider area, as well as detailed comparisons with cosmological simulations of massive cluster formation.", "date": "2016-06-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "824", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L11", "id_number": "CaltechAUTHORS:20160707-102219945", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160707-102219945", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "David and Lucile Packard Foundation" } ] }, "doi": "10.3847/2041-8205/824/1/L11", "primary_object": { "basename": "1605.02079v2.pdf", "url": "https://authors.library.caltech.edu/records/w5jz4-gq343/files/1605.02079v2.pdf" }, "related_objects": [ { "basename": "apjl_824_1_L11.pdf", "url": "https://authors.library.caltech.edu/records/w5jz4-gq343/files/apjl_824_1_L11.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Topping, Michael W.; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/tz4vr-4q521", "eprint_id": 63410, "eprint_status": "archive", "datestamp": "2023-08-20 08:37:34", "lastmod": "2023-10-25 23:47:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S. C." } }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Smail-Ian-R", "name": { "family": "Smail", "given": "Ian" }, "orcid": "0000-0003-3037-257X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Geach-J-E", "name": { "family": "Geach", "given": "J. E." }, "orcid": "0000-0003-4964-4635" }, { "id": "Gurwell-M-A", "name": { "family": "Gurwell", "given": "M." }, "orcid": "0000-0003-0685-3621" }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Petitpas-G-R", "name": { "family": "Petitpas", "given": "G. R." } }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "N." }, "orcid": "0000-0001-9687-4973" } ] }, "title": "A millimetre-wave redshift search for the unlensed HyLIRG, HS1700.850.1", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: abundances \u2013 galaxies: high-redshift \u2013 submillimetre: galaxies", "note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 July 15. Received 2015 July 14; in original form 2015 March 5. First published online August 22, 2015. \n\nWe thank an anonymous referee for constructive comments on the manuscript. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). The submillimetre array (SMA) is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. We thank summer students K. Lacaille and R. Perry for their work on the KBSS-SCUBA2 survey project. SCC acknowledges NSERC and CFI for support. FB acknowledges support through the Collaborative Research Centre 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). IRS acknowledges support from STFC, a Leverhulme Fellowship, the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson Merit Award. JEG acknowledges support from the Royal Society.\n\nPublished - MNRAS-2015-Chapman-951-9.pdf
Submitted - 1503.02195v2.pdf
", "abstract": "We report the redshift of an unlensed, highly obscured submillimetre galaxy (SMG), HS1700.850.1, the brightest SMG (S_(850\u2009\u03bcm) = 19.1 mJy) detected in the James Clerk Maxwell Telescope/Submillimetre Common-user Bolometer Array-2 (JCMT/SCUBA-2) Baryonic Structure Survey, based on the detection of its ^(12)CO line emission. Using the Institute Radio Astronomie Millimetrique Plateau de Bure Interferometer with 3.6 GHz band width, we serendipitously detect an emission line at 150.6 GHz. From a search over 14.5 GHz in the 3- and 2-mm atmospheric windows, we confirm the identification of this line as ^(12)CO(5\u20134) at z = 2.816, meaning that it does not reside in the z \u223c 2.30 proto-cluster in this field. Measurement of the 870 \u03bcm source size (<0.85 arcsec) from the Sub-Millimetre Array (SMA) confirms a compact emission in a S_(870\u2009\u03bcm) = 14.5 mJy, L_(IR) \u223c 10^(13) L\u2299 component, suggesting an Eddington-limited starburst. We use the double-peaked 12CO line profile measurements along with the SMA size constraints to study the gas dynamics of a HyLIRG, estimating the gas and dynamical masses of HS1700.850.1. While HS1700.850.1 is one of the most extreme galaxies known in the Universe, we find that it occupies a relative void in the Lyman-Break Galaxy distribution in this field. Comparison with other extreme objects at similar epochs (HyLIRG Quasars), and cosmological simulations, suggests such an anti-bias of bright SMGs could be relatively common, with the brightest SMGs rarely occupying the most overdense regions at z = 2\u20134.", "date": "2015-10-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "453", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "951-959", "id_number": "CaltechAUTHORS:20160106-084019133", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160106-084019133", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" }, { "agency": "Smithsonian Institution" }, { "agency": "Academia Sinica" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Leverhulme Trust" }, { "agency": "European Research Council (ERC)", "grant_number": "DUSTYGAL 321334" }, { "agency": "Royal Society" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "doi": "10.1093/mnras/stv1618", "primary_object": { "basename": "1503.02195v2.pdf", "url": "https://authors.library.caltech.edu/records/tz4vr-4q521/files/1503.02195v2.pdf" }, "related_objects": [ { "basename": "MNRAS-2015-Chapman-951-9.pdf", "url": "https://authors.library.caltech.edu/records/tz4vr-4q521/files/MNRAS-2015-Chapman-951-9.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Chapman, S. C.; Bertoldi, F.; et el." }, { "id": "https://authors.library.caltech.edu/records/v68jb-mcw20", "eprint_id": 61568, "eprint_status": "archive", "datestamp": "2023-08-20 08:11:06", "lastmod": "2023-10-25 15:00:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mostardi-R-E", "name": { "family": "Mostardi", "given": "R. E." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "A. E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "R. F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "N. A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Siana-Brian-D", "name": { "family": "Siana", "given": "B." }, "orcid": "0000-0002-4935-9511" } ] }, "title": "A High-Resolution Hubble Space Telescope Study of Apparent Lyman Continuum Leakers at z~3", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 diffuse radiation \u2013 galaxies: high-redshift \u2013 intergalactic medium", "note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 June 24; accepted 2015 July 31; published 2015 September 3. \n\nWe thank Anahita Alavi and Eros Vanzella for helpful discussions about the HST imaging reduction and photometry. Support for program GO-12959 was provided by NASA through a grant from the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. A. E. S. acknowledges additional support from the David and Lucile Packard and Sloan Foundations, C.C.S. acknowledges support from the NSF grants AST-0908805 and AST-1313472, as well as STScI grants GO-11638.01 and GO-11694.02, and R.E.M. and A.E.S. acknowledge the generous support of Mr. Richard Kaplan. R.F.T. receives funding from the Miller Institute for Basic Research in Science at U.C. Berkeley. N.A.R. acknowledges support from the Sloan Foundation. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible.\n\nPublished - Mostardi_2015.pdf
Accepted Version - 1506.08201v2.pdf
", "abstract": "We present U_(336)V_(606)J_(125)H_(160) follow-up Hubble Space Telescope (HST) observations of 16 z ~ 3 candidate Lyman continuum (LyC) emitters in the HS1549+1919 field. With these data, we obtain high spatial-resolution photometric redshifts of all sub-arcsecond components of the LyC candidates in order to eliminate foreground contamination and identify robust candidates for leaking LyC emission. Of the 16 candidates, we find one object with a robust LyC detection that is not due to foreground contamination. This object (MD5) resolves into two components; we refer to the LyC-emitting component as MD5b. MD5b has an observed 1500 \u00c5 to 900 \u00c5 flux-density ratio of (F_(UV)/F_(LyC)_(obs) = 4.0 \u00b1 2.0, compatible with predictions from stellar population synthesis models. Assuming minimal IGM absorption, this ratio corresponds to a relative (absolute) escape fraction of f_(esc,rel)^(MD5b) = 75%\u2013100% f_(esc,abs)^(MD5b) = 14%\u201319%). The stellar population fit to MD5b indicates an age of \u227e50 Myr, which is in the youngest 10% of the HST sample and the youngest third of typical z ~ 3 Lyman break galaxies, and may be a contributing factor to its LyC detection. We obtain a revised, contamination-free estimate for the comoving specific ionizing emissivity at z = 2.85, indicating (with large uncertainties) that star-forming galaxies provide roughly the same contribution as QSOs to the ionizing background at this redshift. Our results show that foreground contamination prevents ground-based LyC studies from obtaining a full understanding of LyC emission from z ~ 3 star-forming galaxies. Future progress in direct LyC searches is contingent upon the elimination of foreground contaminants through high spatial-resolution observations, and upon acquisition of sufficiently deep LyC imaging to probe ionizing radiation in high-redshift galaxies.", "date": "2015-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "810", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 107", "id_number": "CaltechAUTHORS:20151027-125431249", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151027-125431249", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO-12959" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "NASA", "grant_number": "GO-11638.01" }, { "agency": "NASA", "grant_number": "GO-11694.02" }, { "agency": "Richard Kaplan" }, { "agency": "Miller Institute for Basic Research in Science" } ] }, "doi": "10.1088/0004-637X/810/2/107", "primary_object": { "basename": "1506.08201v2.pdf", "url": "https://authors.library.caltech.edu/records/v68jb-mcw20/files/1506.08201v2.pdf" }, "related_objects": [ { "basename": "Mostardi_2015.pdf", "url": "https://authors.library.caltech.edu/records/v68jb-mcw20/files/Mostardi_2015.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Mostardi, R. E.; Shapley, A. E.; et el." }, { "id": "https://authors.library.caltech.edu/records/c1m4b-a5j47", "eprint_id": 61319, "eprint_status": "archive", "datestamp": "2023-08-20 07:44:13", "lastmod": "2023-10-25 14:44:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" } ] }, "title": "The Spectroscopic Properties of Ly\u03b1-Emitters at z ~2.7: Escaping Gas and Photons from Faint Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation \u2013 galaxies: high-redshift \u2013 intergalactic medium", "note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 March 25; accepted 2015 July 6; published 2015 August 12. \n\nWe are indebted to the staff of the W.M. Keck Observatory who keep the instruments and telescopes running effectively. We also wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. This work has been supported in part by the US National Science Foundation through grants AST-0908805 and AST-1313472. We thank Mariska Kriek and Eliot Quataert for many useful discussions as well as the anonymous referee for comments and suggestions that significantly improved this work. R.F.T. also acknowledges support from Dennis and Carol Troesh and from the Miller Institute for Basic Research in Science at the University of California, Berkeley. \n\nBased on data obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W.M. Keck Foundation.\n\nPublished - Trainor_2015.pdf
Submitted - 1506.08205v1.pdf
", "abstract": "We present a spectroscopic survey of 318 faint (R ~ 27, L ~ 0.1 L*), Ly\u03b1-emission-selected galaxies (LAEs) in regions centered on the positions of hyperluminous QSOs (HLQSOs) at 2.5 < z < 3. A sample of 32 LAEs with rest-frame optical emission line spectra from Keck/Multi-Object Spectrometer For InfraRed Exploration (MOSFIRE) are used to interpret the LAE spectra in the context of their systemic redshifts. The fields are part of the Keck Baryonic Structure Survey, which includes substantial ancillary multi-wavelength imaging from both the ground and space. From a quantitative analysis of the diverse Ly\u03b1 spectral morphologies, including line widths, asymmetries, and multi-peaked profiles, we find that peak widths and separations are typically smaller than among samples of more luminous continuum-selected galaxies (Lyman-break galaxies and their analogs; LBGs) at similar redshifts. We find tentative evidence for an association between Ly\u03b1 spectral morphology and external illumination by the nearby HLQSO. Using the MOSFIRE subsample, we find that the peak of the resolved (R \u2248 1300) Ly\u03b1 line is shifted by +200 km s^(\u22121) with respect to systemic across a diverse set of galaxies including both LAEs and LBGs. We also find a small number of objects with significantly blueshifted Ly\u03b1 emission, a potential indicator of accreting gas. The Ly\u03b1-to-H\u03b1 line ratios measured for the MOSFIRE subset suggest that the LAEs in this sample have Ly\u03b1 escape fractions f_(esc,Ly\u03b1) \u2248 30%, significantly higher than typical LBG samples. Using redshifts calibrated by our MOSFIRE sample, we construct composite LAE spectra, finding the first evidence for metal-enriched outflows in such intrinsically faint high-redshift galaxies. These outflows have smaller continuum covering fractions (f_c \u2248 0.3) and velocities (\u03bd_(ave) \u2248 100\u2013200 km s^(\u22121), \u03bd_(max) \u2248 500 km s^(\u22121)) than those associated with typical LBGs, suggesting that the gas covering fraction is a likely driver of the high Ly\u03b1 and Ly-continuum escape fractions of LAEs with respect to LBGs. Our results suggest a similar scaling of outflow velocity with star formation rate (SFR) as is observed at lower redshifts (\u03bd_(outflow) ~ SFR^(0.25)) and indicate that a substantial fraction of gas is ejected with \u03bd > \u03bd_(sec). Further observations, including deep spectroscopy in the observed near-IR, will further probe the evolution and enrichment of these galaxies in the context of their gaseous environments.", "date": "2015-08-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "809", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 89", "id_number": "CaltechAUTHORS:20151020-100556005", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151020-100556005", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "Dennis and Carol Troesh" }, { "agency": "Miller Institute for Basic Research in Science" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA" } ] }, "doi": "10.1088/0004-637X/809/1/89", "primary_object": { "basename": "1506.08205v1.pdf", "url": "https://authors.library.caltech.edu/records/c1m4b-a5j47/files/1506.08205v1.pdf" }, "related_objects": [ { "basename": "Trainor_2015.pdf", "url": "https://authors.library.caltech.edu/records/c1m4b-a5j47/files/Trainor_2015.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Trainor, Ryan F.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/nc4dq-zkn31", "eprint_id": 60729, "eprint_status": "archive", "datestamp": "2023-08-22 16:09:20", "lastmod": "2023-10-24 21:08:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shimakawa-Rhythm", "name": { "family": "Shimakawa", "given": "Rhythm" } }, { "id": "Kodama-Tadayuki", "name": { "family": "Kodama", "given": "Tadayuki" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Tadaki-Ken-ichi", "name": { "family": "Tadaki", "given": "Ken-ichi" } }, { "id": "Tanaka-Ichi", "name": { "family": "Tanaka", "given": "Ichi" } }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Hayashi-Masao", "name": { "family": "Hayashi", "given": "Masao" } }, { "id": "Koyama-Yusei", "name": { "family": "Koyama", "given": "Yusei" } }, { "id": "Suzuki-Tomoko-L", "name": { "family": "Suzuki", "given": "Tomoko L." } }, { "id": "Yamamoto-Moegi", "name": { "family": "Yamamoto", "given": "Moegi" } } ] }, "title": "Correlation between star formation activity and electron density of ionized gas at z = 2.5", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation; galaxies: high-redshift; galaxies: ISM", "note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 April 22. Received 2015 March 25. In original form 2014 November 5. First published online June 5, 2015. \n\nWe are grateful to the anonymous referee for useful comments. The data presented in this paper were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Data analyses were in part carried out on common use data analysis computer system at the Astronomy Data Center, ADC, of the National Astronomical Observatory of Japan.\n\nPublished - MNRAS-2015-Shimakawa-1284-9.pdf
Submitted - 1411.1408v3.pdf
", "abstract": "In the redshift interval of 2 < z < 3, the physical conditions of the interstellar medium (ISM) in star-forming galaxies are likely to be different from those in the local Universe because of lower gaseous metallicities, higher gas fractions, and higher star formation activities. In fact, observations suggest that higher electron densities, higher ionization parameters, and harder UV radiation fields are common. In this paper, based on the spectra of H \u03b1-selected star-forming galaxies at z = 2.5 taken with Multi-Object Spectrometer for InfraRed Exploration on Keck-1 telescope, we measure electron densities (n_e) using the oxygen line ratio ([O\u2009II] \u03bb\u03bb3726,3729), and investigate the relationships between the electron density of ionized gas and other physical properties. As a result, we find that the specific star formation rate (sSFR) and the surface density of SFR (\u03a3_(SFR)) are correlated with the electron density at z = 2.5 for the first time. The \u03a3_(SFR)\u2013n_e relation is likely to be linked to the star formation law in H\u2009II regions (where star formation activity is regulated by interstellar pressure). Moreover, we discuss the mode of star formation in those galaxies. The correlation between sSFR and \u03a3_(SFR) suggests that highly star-forming galaxies (with high sSFR) tend to be characterized by higher surface densities of star formation (\u03a3_(SFR)) and thus higher n_e values as well.", "date": "2015-08-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "451", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1284-1289", "id_number": "CaltechAUTHORS:20151002-150103207", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151002-150103207", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1093/mnras/stv915", "primary_object": { "basename": "1411.1408v3.pdf", "url": "https://authors.library.caltech.edu/records/nc4dq-zkn31/files/1411.1408v3.pdf" }, "related_objects": [ { "basename": "MNRAS-2015-Shimakawa-1284-9.pdf", "url": "https://authors.library.caltech.edu/records/nc4dq-zkn31/files/MNRAS-2015-Shimakawa-1284-9.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Shimakawa, Rhythm; Kodama, Tadayuki; et el." }, { "id": "https://authors.library.caltech.edu/records/05zv6-1fh11", "eprint_id": 65433, "eprint_status": "archive", "datestamp": "2023-08-22 16:08:01", "lastmod": "2023-10-18 16:00:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Chaclair-J", "name": { "family": "Checlair", "given": "Jade" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Physical Properties of a Pilot Sample of Spectroscopic Close Pair Galaxies at z ~ 2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: fundamental parameters; galaxies: high-redshift; galaxies: structure", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 January 30; accepted 2015 June 25; published 2015 July 30. \n\nThese results are based in part on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. D.R.L. and C.C.S. have been supported by grant GO-11694 from 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. C.C.S. has been supported by the U.S. National Science Foundation through grants AST-0606912 and AST-0908805. A.E.S. acknowledges support from the David and Lucile Packard Foundation. D.R.L. thanks Kristen Kulas for assistance obtaining the Keck/NIRSPEC spectroscopy, Dawn Erb for making available previous NIRSPEC observations of Q2343-BX429, and George Becker for sharing a copy of his IDL-based NIRSPEC data reduction code. Finally, we extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests.\n\nPublished - Law_2016p160.pdf
Submitted - 1507.00721v1.pdf
", "abstract": "We use Hubble Space Telescope Wide-field Camera 3 rest-frame optical imaging to select a pilot sample of star-forming galaxies in the redshift range z = 2.00\u20132.65 whose multi-component morphologies are consistent with expectations for major mergers. We follow up this sample of major merger candidates with Keck/NIRSPEC long-slit spectroscopy obtained in excellent seeing conditions (FWHM ~0.5 arcsec) to obtain H\u03b1-based redshifts of each of the morphological components in order to distinguish spectroscopic pairs from false pairs created by projection along the line of sight. Of the six candidate pairs observed, companions (estimated mass ratios 5:1 and 7:1) are detected for two galaxies down to a 3\u03c3 limiting emission-line flux of ~ 10^(-17) erg s^(\u22121) cm^(\u22122). This detection rate is consistent with a ~50% false-pair fraction at such angular separations (1\u20132 arcsec) and with recent claims that the star formation rate (SFR) can differ by an order of magnitude between the components in such mergers. The two spectroscopic pairs identified have a total SFR, SFR surface densities, and stellar masses consistent on average with the overall z ~ 2 star-forming galaxy population.", "date": "2015-08", "date_type": "published", "publication": "Astrophysical Journal", "volume": "808", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 60", "id_number": "CaltechAUTHORS:20160317-113846199", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160317-113846199", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NASA", "grant_number": "GO-11694" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "David and Lucile Packard Foundation" } ] }, "doi": "10.1088/0004-637X/808/2/160", "primary_object": { "basename": "1507.00721v1.pdf", "url": "https://authors.library.caltech.edu/records/05zv6-1fh11/files/1507.00721v1.pdf" }, "related_objects": [ { "basename": "Law_2016p160.pdf", "url": "https://authors.library.caltech.edu/records/05zv6-1fh11/files/Law_2016p160.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Law, David R.; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/csece-dhm83", "eprint_id": 52486, "eprint_status": "archive", "datestamp": "2023-08-20 06:58:27", "lastmod": "2023-10-18 19:55:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Turner-M-L", "name": { "family": "Turner", "given": "Monica L." } }, { "id": "Schaye-J", "name": { "family": "Schaye", "given": "Joop" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" } ] }, "title": "Detection of hot, metal-enriched outflowing gas around z \u2248 2.3 star-forming galaxies in the Keck Baryonic Structure Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation, intergalactic medium, quasars: absorption lines", "note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 April 2. Received 2015 April 2. In original form 2014. October 30. First published online April 30, 2015. \n\nWe are very grateful to Milan Bogosavljevic, Alice Shapley, Dawn Erb, Naveen Reddy, Max Pettini, Ryan Trainor, and David Law for their invaluable contributions to the Keck Baryonic Structure Survey, without which the results presented here would not have been possible. We also thank Ryan Cooke for his help with the continuum fitting of QSO spectra. We gratefully acknowledge support from Marie Curie Training Network CosmoComp (PITN-GA-2009-238356) and the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement 278594-GasAroundGalaxies. CCS, GCR, ALS acknowledge support from grants AST-0908805 and AST-13131472 from the US National Science Foundation. We thank the W. M. Keck Observatory staff for their assistance with the observations. We also thank the Hawaiian people, as without their hospitality the observations presented here would not have been possible.\n\nPublished - MNRAS-2015-Turner-2067-82.pdf
Submitted - 1410.8214v1.pdf
", "abstract": "We use quasar absorption lines to study the physical conditions in the circumgalactic medium of redshift z \u2248 2.3 star-forming galaxies taken from the Keck Baryonic\nStructure Survey (KBSS). In Turner et al. (2014) we used the pixel optical depth technique to show that absorption by Hi and the metal ions OvI, Nv, CIv, CIII and SiIv is strongly enhanced within \u2502\u0394v\u2502\u227e. 170 km s^(-1) and projected distances \u2502d\u2502\u227e. 180 proper kpc from sightlines to the background quasars. Here we demonstrate that the OvI absorption is also strongly enhanced at fixed HI, CIv, and SiIv optical depths, and that this enhancement extends out to ~ 350 km s^(-1). At fixed HI the increase in the median OvI optical depth near galaxies is 0.3-0.7 dex and is detected at 2-3-\u03c3 confidence for all seven HI bins that have log_(10) T_(HI) \u2265 -1.5. We use ionisation models to show that the observed strength of OvI as a function of HI is consistent with enriched, photoionised gas for pixels with T_(HI) \u2273 10. However, for pixels with T_(HI) \u227e 1 this would lead to implausibly high metallicities at low densities if the gas were photoionised by the background radiation. This indicates that the galaxies are surrounded by gas that is sufficiently hot to be collisionally ionised (T > 10^5 K) and that a substantial fraction of the hot gas has a metallicity \u2273 10^(-1) of solar. Given the high metallicity and large velocity extent (out to ~ 1.5 x v_(circ)) of this gas, we conclude that we have detected hot, metal enriched outflows arising from star-forming\ngalaxies.", "date": "2015-06-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "450", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "2067-2082", "id_number": "CaltechAUTHORS:20141209-081520548", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141209-081520548", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Marie Curie Fellowship", "grant_number": "PITN-GA-2009-238356" }, { "agency": "European Research Council (ERC)", "grant_number": "278594" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-13131472" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1093/mnras/stv750", "primary_object": { "basename": "1410.8214v1.pdf", "url": "https://authors.library.caltech.edu/records/csece-dhm83/files/1410.8214v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2015-Turner-2067-82.pdf", "url": "https://authors.library.caltech.edu/records/csece-dhm83/files/MNRAS-2015-Turner-2067-82.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Turner, Monica L.; Schaye, Joop; et el." }, { "id": "https://authors.library.caltech.edu/records/x5hcn-7jd37", "eprint_id": 58376, "eprint_status": "archive", "datestamp": "2023-08-22 15:33:40", "lastmod": "2023-10-23 19:17:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shivaei-Irene", "name": { "family": "Shivaei", "given": "Irene" } }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" } ] }, "title": "Investigating H\u03b1, UV, and IR Star-formation Rate Diagnostics for a Large Sample of z ~ 2 Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: star formation", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2014 August 26; accepted 2015 March 12; published 2015 May 12. \n\nI.S. thanks Valentino Gonz\u00e1lez for useful discussions. Support for I.S. is provided through the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1326120. N.A.R. is supported by an Alfred P. Sloan Research Fellowship.\n\nPublished - 0004-637X_804_2_149.pdf
Submitted - 1503.03929v1.pdf
", "abstract": "We use a sample of 262 spectroscopically confirmed star-forming galaxies at redshifts 2.08 \u2264 z \u2264 2.51 to compare H\u03b1, ultraviolet (UV), and IR star formation rate (SFR) diagnostics and to investigate the dust properties of the galaxies. At these redshifts, the H\u03b1 line shifts to the K_s band. By comparing K_s-band photometry to underlying stellar population model fits to other UV, optical, and near-infrared data, we infer the H\u03b1 flux for each galaxy. We obtain the best agreement between H\u03b1- and UV-based SFRs if we assume that the ionized gas and stellar continuum are reddened by the same value and that the Calzetti attenuation curve is applied to both. Aided with MIPS 24 \u03bcm data, we find that an attenuation curve steeper than the Calzetti curve is needed to reproduce the observed IR/UV ratios of galaxies younger than 100 Myr. Furthermore, using the bolometric SFR inferred from the UV and mid-IR data (SFR_(IR)+SFR_(UV), we calculated the conversion between the H\u03b1 luminosity and SFR to be (7.5 \u00b1 1.3) x 10^(-42) for a Salpeter initial mass function, which is consistent with the Kennicutt conversion. The derived conversion factor is independent of any assumption of the dust correction and is robust to stellar population model uncertainties.", "date": "2015-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "804", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 149", "id_number": "CaltechAUTHORS:20150619-095300192", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150619-095300192", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1326120" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "doi": "10.1088/0004-637X/804/2/149", "primary_object": { "basename": "0004-637X_804_2_149.pdf", "url": "https://authors.library.caltech.edu/records/x5hcn-7jd37/files/0004-637X_804_2_149.pdf" }, "related_objects": [ { "basename": "1503.03929v1.pdf", "url": "https://authors.library.caltech.edu/records/x5hcn-7jd37/files/1503.03929v1.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Shivaei, Irene; Reddy, Naveen A.; et el." }, { "id": "https://authors.library.caltech.edu/records/bdv16-5nt36", "eprint_id": 55716, "eprint_status": "archive", "datestamp": "2023-08-22 15:30:17", "lastmod": "2023-10-20 23:03:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Siana-Brian-D", "name": { "family": "Siana", "given": "Brian" }, "orcid": "0000-0002-4935-9511" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Kulas-K-R", "name": { "family": "Kulas", "given": "Kristin R." } }, { "id": "Nestor-D-B", "name": { "family": "Nestor", "given": "Daniel B." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "Harry I." }, "orcid": "0000-0002-7064-5424" }, { "id": "Alavi-A", "name": { "family": "Alavi", "given": "Anahita" }, "orcid": "0000-0002-8630-6435" }, { "id": "Brown-T-M", "name": { "family": "Brown", "given": "Thomas M." }, "orcid": "0000-0002-1793-9968" }, { "id": "Conselice-C-J", "name": { "family": "Conselice", "given": "Christopher J." }, "orcid": "0000-0003-1949-7638" }, { "id": "Ferguson-H-C", "name": { "family": "Ferguson", "given": "Henry C." }, "orcid": "0000-0001-7113-2738" }, { "id": "Dickinson-Mark-E", "name": { "family": "Dickinson", "given": "Mark" }, "orcid": "0000-0001-5414-5131" }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "Mauro" }, "orcid": "0000-0002-7831-8751" }, { "id": "Colbert-J-W", "name": { "family": "Colbert", "given": "James W." } }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "Carrie R." } }, { "id": "Gardner-J-P", "name": { "family": "Gardner", "given": "Jonathan P." } }, { "id": "de-Mello-D-F", "name": { "family": "de Mello", "given": "Duilia F." } } ] }, "title": "A Deep Hubble Space Telescope and Keck Search for Definitive Identification of Lyman Continuum Emitters at z ~ 3.1", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: starburst; intergalactic medium; ultraviolet: galaxies", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2014 December 19; accepted 2015 February 20; published 2015 April 24. \n\nBased on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs 10405, 11636, and 11735. \n\nSome of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. \n\nSupport for program 11636 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. 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. Facilities: HST (WFC3, ACS), Keck:I (LRIS), Keck:II (NIRSPEC)\n\nPublished - Siana_2015_ApJ_804_17.pdf
Submitted - 1502.06978v1.pdf
", "abstract": "Narrowband imaging of the rest-frame Lyman continuum (LyC) of galaxies at z ~ 3.1 has produced a large number of candidate LyC-emitting galaxies. These samples are contaminated by galaxies at lower redshift. To better understand LyC escape, we need an uncontaminated sample of galaxies that emit strongly in the LyC. Here we present deep Hubble Space Telescope imaging of five bright galaxies at z ~ 3.1 that had previously been identified as candidate LyC emitters with ground-based images. The WFC3 F336W images probe the LyC of galaxies at z > 3.06 and provide an order-of-magnitude increase in spatial resolution over ground-based imaging. The non-ionizing UV images often show multiple galaxies (or components) within ~ 1\" of the candidate LyC emission seen from the ground. In each case, only one of the components is emitting light in the F336W filter, which would indicate LyC escape if that component is at z > 3.06. We use Keck/NIRSPEC near-IR spectroscopy to measure redshifts of these components to distinguish LyC emitters from foreground contamination. We find that two candidates are low-redshift contaminants, one candidate had a previously misidentified redshift, and the other two cannot be confirmed as LyC emitters. The level of contamination is consistent with previous estimates. For the galaxies with z > 3.06, we derive strong l\u03c3 limits on the relative escape fraction between 0.07 and 0.09. We still do not have a sample of definitive LyC emitters, and a much larger study of low-luminosity galaxies is required. The combination of high-resolution imaging and deep spectroscopy is critical for distinguishing LyC emitters from foreground contaminants.", "date": "2015-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "804", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 17", "id_number": "CaltechAUTHORS:20150311-182729941", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150311-182729941", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/804/1/17", "primary_object": { "basename": "1502.06978v1.pdf", "url": "https://authors.library.caltech.edu/records/bdv16-5nt36/files/1502.06978v1.pdf" }, "related_objects": [ { "basename": "Siana_2015_ApJ_804_17.pdf", "url": "https://authors.library.caltech.edu/records/bdv16-5nt36/files/Siana_2015_ApJ_804_17.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Siana, Brian; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/97yhd-e6s75", "eprint_id": 57590, "eprint_status": "archive", "datestamp": "2023-08-22 15:30:29", "lastmod": "2023-10-23 17:33:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S. C." } }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Smail-Ian-R", "name": { "family": "Smail", "given": "Ian" }, "orcid": "0000-0003-3037-257X" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Geach-J-E", "name": { "family": "Geach", "given": "J. E." }, "orcid": "0000-0003-4964-4635" }, { "id": "Gurwell-M-A", "name": { "family": "Gurwell", "given": "M." }, "orcid": "0000-0003-0685-3621" }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Petitpas-G-R", "name": { "family": "Petitpas", "given": "G. R." } }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "N." }, "orcid": "0000-0001-9687-4973" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "A blind CO detection of a distant red galaxy in the HS1700+64 protocluster", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: molecules; galaxies: clusters: general; galaxies: high-redshift; galaxies: starburst", "note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2015 January 19; Received 2015 January 15; In original form 2014 October 23; First published online March 4, 2015.\n\nThis work is based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. SC and IS acknowledge the Aspen Center for Physics where parts of this manuscript were written. SC acknowledges support from NSERC and CFI.\n\nPublished - MNRAS-2015-Chapman-L68-72.pdf
Submitted - 1501.02839v2.pdf
", "abstract": "We report the blind detection of ^(12)CO emission from a distant red galaxy, HS1700.DRG55. We have used the IRAM Plateau de Bure Interferometer WideX, with its 3.6 GHz of instantaneous dual-polarization bandwidth, to target ^(12)CO(3\u20132) from galaxies lying in the protocluster at z = 2.300 in the field HS1700+64. If indeed this line in DRG55 is ^(12)CO(3\u20132), its detection at 104.9 GHz indicates zCO = 2.296. None of the other eight known z \u223c 2.30 protocluster galaxies lying within the primary beam (PB) are detected in ^(12)CO, although the limits are \u223c2 \u00d7 worse towards the edge of the PB where several lie. The optical/near-IR magnitudes of DRG55 (R_AB > 27, KAB = 22.3) mean that optical spectroscopic redshifts are difficult with 10-m-class telescopes, but near-IR redshifts would be feasible. The 24-\u03bcm-implied star formation rate (210\u2009M_\u2299\u2009yr^\u22121), stellar mass (\u223c10^11\u2009M_\u2299) and ^(12)CO line luminosity (3.6 \u00d7 10^10\u2009K\u2009km\u2009s^\u22121\u2009 pc^2) are comparable to other normal ^(12)CO-detected star-forming galaxies in the literature, although the galaxy is some \u223c2 mag (\u223c6 \u00d7) fainter in the rest-frame UV than ^(12)CO-detected galaxies at z > 2. The detection of DRG55 in ^(12)CO complements three other ^(12)CO detected UV-bright galaxies in this protocluster from previous studies, and suggests that many optically faint galaxies in the protocluster may host substantial molecular gas reservoirs, and a full blind census of ^(12)CO in this overdense environment is warranted.", "date": "2015-05-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "449", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "L68-L72", "id_number": "CaltechAUTHORS:20150518-101259875", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150518-101259875", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Smithsonian Institution" }, { "agency": "Academica Sinica" } ] }, "doi": "10.1093/mnrasl/slv010", "primary_object": { "basename": "1501.02839v2.pdf", "url": "https://authors.library.caltech.edu/records/97yhd-e6s75/files/1501.02839v2.pdf" }, "related_objects": [ { "basename": "MNRAS-2015-Chapman-L68-72.pdf", "url": "https://authors.library.caltech.edu/records/97yhd-e6s75/files/MNRAS-2015-Chapman-L68-72.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Chapman, S. C.; Bertoldi, F.; et el." }, { "id": "https://authors.library.caltech.edu/records/csrxc-h7d62", "eprint_id": 52245, "eprint_status": "archive", "datestamp": "2023-08-22 14:15:51", "lastmod": "2023-10-18 19:42:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Turner-M-L", "name": { "family": "Turner", "given": "Monica L." } }, { "id": "Schaye-J", "name": { "family": "Schaye", "given": "Joop" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" } ] }, "title": "Metal-line absorption around z \u2248 2.4 star-forming galaxies in the Keck Baryonic Structure Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation; intergalactic medium; quasars: absorption lines", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2014 September 1. Received 2014 August 29; in original form 2014 March 5. First published online September 30, 2014. \n\nWe are very grateful to Milan Bogosavljevic, Alice Shapley, Dawn\nErb, Naveen Reddy, Max Pettini, Ryan Trainor, and David Law for\ntheir invaluable contributions to the Keck Baryonic Structure Survey,\nwithout which the results presented here would not have been\npossible. We also thank Ryan Cooke for his help with the continuum\nfitting of QSO spectra, and the anonymous referee whose valuable\ncomments greatly improved this work. We gratefully acknowledge\nsupport from Marie Curie Training Network CosmoComp (PITNGA-\n2009- 238356) and the European Research Council under\nthe European Union's Seventh Framework Programme (FP7/2007-\n2013)/ERC Grant agreement 278594-GasAroundGalaxies. CCS,\nGCR, ALS acknowledge support from grants AST-0908805 and\nAST-13131472 from the US National Science Foundation. We thank\nthe W. M. Keck Observatory staff for their assistance with the observations. We also thank the Hawaiian people, as without their\nhospitality the observations presented here would not have been\npossible.\n\nPublished - MNRAS-2014-Turner-794-822.pdf
Supplemental Material - online_tables.pdf
", "abstract": "We study metal absorption around 854 z \u2248 2.4 star-forming galaxies taken from the Keck Baryonic Structure Survey. The galaxies examined in this work lie in the fields of 15 hyperluminous background quasi-stellar objects, with galaxy impact parameters ranging from 35 proper kpc (pkpc) to 2 proper Mpc (pMpc). Using the pixel optical depth technique, we present the first galaxy-centred 2D maps of the median absorption by O\u2009VI, N\u2009V, C\u2009IV, C\u2009III, and Si\u2009IV, as well as updated results for H\u2009I. At small galactocentric radii we detect a strong enhancement of the absorption relative to randomly located regions that extend out to at least 180 pkpc in the transverse direction, and \u00b1240 km\u2009s^(\u22121) along the line of sight (LOS, \u223c1\u2009pMpc in the case of pure Hubble flow) for all ions except N\u2009V. For C\u2009IV (and H\u2009I) we detect a significant enhancement of the absorption signal out to 2\u2009pMpc in the transverse direction, corresponding to the maximum impact parameter in our sample. After normalizing the median absorption profiles to account for variations in line strengths and detection limits, in the transverse direction we find no evidence for a sharp drop-off in metals distinct from that of H\u2009I. We argue instead that non-detection of some metal-line species in the extended circumgalactic medium is consistent with differences in the detection sensitivity. Along the LOS, the normalized profiles reveal that the enhancement in the absorption is more extended for O\u2009VI, C\u2009IV, and Si\u2009IV than for H\u2009I. We also present measurements of the scatter in the pixel optical depths, covering fractions, and equivalent widths as a function of projected galaxy distance. Limiting the sample to the 340 galaxies with redshifts measured from nebular emission lines does not decrease the extent of the enhancement along the LOS compared to that in the transverse direction. This rules out redshift errors as the source of the observed redshift-space anisotropy and thus implies that we have detected the signature of gas peculiar velocities from infall, outflows, or virial motions for H\u2009I, O\u2009VI, C\u2009IV, C\u2009III, and Si\u2009IV.", "date": "2014-11-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "445", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "794-822", "id_number": "CaltechAUTHORS:20141201-150453949", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141201-150453949", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Marie Curie Fellowship", "grant_number": "PITN-GA-2009-238356" }, { "agency": "European Research Council (ERC)", "grant_number": "278594" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-13131472" } ] }, "doi": "10.1093/mnras/stu1801", "primary_object": { "basename": "online_tables.pdf", "url": "https://authors.library.caltech.edu/records/csrxc-h7d62/files/online_tables.pdf" }, "related_objects": [ { "basename": "MNRAS-2014-Turner-794-822.pdf", "url": "https://authors.library.caltech.edu/records/csrxc-h7d62/files/MNRAS-2014-Turner-794-822.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Turner, Monica L.; Schaye, Joop; et el." }, { "id": "https://authors.library.caltech.edu/records/5mkzm-qj837", "eprint_id": 46189, "eprint_status": "archive", "datestamp": "2023-08-22 14:10:20", "lastmod": "2023-10-26 19:34:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Turner-M-L", "name": { "family": "Turner", "given": "Monica L." } }, { "id": "Konidaris-N-P", "name": { "family": "Konidaris", "given": "Nicholas P." }, "orcid": "0000-0003-1905-2815" }, { "id": "Kulas-K-R", "name": { "family": "Kulas", "given": "Kristin R." } }, { "id": "Mace-G-N", "name": { "family": "Mace", "given": "Gregory N." }, "orcid": "0000-0001-7875-6391" }, { "id": "Matthews-Keith-Astronomy", "name": { "family": "Matthews", "given": "Keith" } }, { "id": "McLean-I-S", "name": { "family": "McLean", "given": "Ian S." } } ] }, "title": "Strong Nebular Line Ratios in the Spectra of z ~ 2-3 Star Forming Galaxies: First Results from KBSS-MOSFIRE", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: abundances; galaxies: evolution; galaxies: formation; galaxies: fundamental parameters; galaxies: high-redshift; galaxies: starburst; instrumentation: spectrographs", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2014 May 7; accepted 2014 September 18; published 2014 October 28. \n\nBased on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. \n\nThis work has been supported in part by the US National Science Foundation through grants AST-0908805 and AST-1313472 (CCS), as well as by an NSF Graduate Student Research Fellowship (ALS). The MOSFIRE instrument was made possible by grants to the W. M. Keck Observatory from the NSF Telescope System Instrumentation Program (TSIP) and by a generous donation from Gordon and Betty Moore. We thank our colleagues on the MOSFIRE instrument team, particularly Marcia Brown, Khan Bui, John Cromer, Jason Fucik, Hector Rodriguez, Bob Weber, and Jeff Zolkower at Caltech; Ted Aliado, George Brims, John Canfield, Chris Johnson, Ken Magnone, and Jason Weiss at UCLA; Harland Epps at UCO/Lick Observatory; and Sean Adkins at WMKO. Special thanks to the WMKO staff who helped make MOSFIRE commissioning successful, especially Marc Kassis, Allan Honey, Greg Wirth, Shui Kwok, Liz Chock, and Jim Lyke. We benefited significantly from an illuminating discussion on the subject of massive stars with Selma de Mink. Constructive comments from the anonymous referee, which led to significant improvements in the content and presentation of the results, are gratefully acknowledged. Finally, we wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests.\n\nPublished - 0004-637X_795_2_165.pdf
Submitted - 1405.5473v1.pdf
", "abstract": "We present initial results of a deep near-IR spectroscopic survey covering the 15 fields of the Keck Baryonic Structure Survey using the recently commissioned MOSFIRE spectrometer on the Keck 1 telescope. We focus on a sample of 251 galaxies with redshifts 2.0 < z < 2.6, star formation rates (SFRs) 2 \u227e SFR \u227e 200 M_\u2609 yr^(\u20131), and stellar masses 8.6 < log (M_*/M_\u2609) < 11.4, with high-quality spectra in both H- and K-band atmospheric windows. We show unambiguously that the locus of z ~ 2.3 galaxies in the \"BPT\" nebular diagnostic diagram exhibits an almost entirely disjointed, yet similarly tight, relationship between the line ratios [N II] \u03bb6585/H\u03b1 and [O III]/H\u03b2 as compared to local galaxies. Using photoionization models, we argue that the offset of the z ~ 2.3 BPT locus relative to that at z ~ 0 is caused by a combination of harder stellar ionizing radiation field, higher ionization parameter, and higher N/O at a given O/H compared to most local galaxies, and that the position of a galaxy along the z ~ 2.3 star-forming BPT locus is surprisingly insensitive to gas-phase oxygen abundance. The observed nebular emission line ratios are most easily reproduced by models in which the net stellar ionizing radiation field resembles a blackbody with effective temperature T_(eff) = 50, 000-60, 000 K, the gas-phase oxygen abundances lie in the range 0.2 < Z/Z_\u2609 < 1.0, and the ratio of gas-phase N/O is close to the solar value. We critically assess the applicability at high redshift of commonly used strong line indices for estimating gas-phase metallicity, and consider the implications of the small intrinsic scatter of the empirical relationship between excitation-sensitive line indices and M_* (i.e., the \"mass-metallicity\" relation) at z \u2243 2.3.", "date": "2014-11-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "795", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 165", "id_number": "CaltechAUTHORS:20140610-153701276", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140610-153701276", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/795/2/165", "primary_object": { "basename": "0004-637X_795_2_165.pdf", "url": "https://authors.library.caltech.edu/records/5mkzm-qj837/files/0004-637X_795_2_165.pdf" }, "related_objects": [ { "basename": "1405.5473v1.pdf", "url": "https://authors.library.caltech.edu/records/5mkzm-qj837/files/1405.5473v1.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Steidel, Charles C.; Rudie, Gwen C.; et el." }, { "id": "https://authors.library.caltech.edu/records/7fnq2-n6y28", "eprint_id": 52205, "eprint_status": "archive", "datestamp": "2023-08-22 14:08:37", "lastmod": "2023-10-18 19:39:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Bogosavljevi\u0107-M", "name": { "family": "Bogosavljevi\u0107", "given": "Milan" } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Nestor-D-B", "name": { "family": "Nestor", "given": "Daniel B." } }, { "id": "Kulas-K-R", "name": { "family": "Kulas", "given": "Kristin R." } }, { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" }, { "id": "Strom-A-L", "name": { "family": "Strom", "given": "Allison L." }, "orcid": "0000-0001-6369-1636" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Konidaris-N-P", "name": { "family": "Konidaris", "given": "Nicholas P." }, "orcid": "0000-0003-1905-2815" }, { "id": "Mace-G-N", "name": { "family": "Mace", "given": "Gregory" }, "orcid": "0000-0001-7875-6391" }, { "id": "Matthews-Keith-Astronomy", "name": { "family": "Matthews", "given": "Keith" } }, { "id": "McLean-I-S", "name": { "family": "McLean", "given": "Ian S." } } ] }, "title": "The Ly\u03b1 Properties of Faint Galaxies at z ~ 2-3 with Systemic Redshifts and Velocity Dispersions from Keck-MOSFIRE", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2014 June 24; accepted 2014 September 2; published 2014 October 9. \n\nWe would like to thank the referee for a thoughtful and constructive report. D.K.E. is supported by the US National Science Foundation through the Faculty Early Career Development (CAREER) Program, grant AST-1255591. Additional support comes from the NSF through grants AST-0908805 (C.C.S., G.C.R., M.B.) and AST-1313472 (C.C.S., R.F.T., A.L.S.), and an NSF Graduate Student Research Fellowship (A.L.S.). M.B. acknowledges support of Serbian MESTD through grant ON176021. MOSFIRE was made possible by grants to WMKO from the NSF \"Telescope System Instrumentation Program\" (TSIP) and a generous donation from Gordon and Betty Moore. We thank our colleagues on the MOSFIRE instrument team, particularly Marcia Brown, Khan Bui, John Cromer, Jason Fucik, Hector Rodriguez, Bob Weber, and Jeff Zolkower at Caltech; Ted Aliado, George Brims, John Canfield, Chris Johnson, Ken Magnone, and Jason Weiss at UCLA; Harland Epps at UCO/Lick Observatory; and Sean Adkins at WMKO. Special thanks to all of the WMKO staff who helped make MOSFIRE commissioning successful, especially Marc Kassis, Allan Honey, Greg Wirth, Shui Kwok, Liz Chock, and Jim Lyke. Finally, we wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests.\n\nPublished - 0004-637X_795_1_33.pdf
Submitted - 1408.3638v3.pdf
", "abstract": "We study the Ly\u03b1 profiles of 36 spectroscopically detected Ly\u03b1-emitters (LAEs) at z ~ 2-3, using Keck MOSFIRE to measure systemic redshifts and velocity dispersions from rest-frame optical nebular emission lines. The sample has a median optical magnitude R = 26.0, and ranges from R \u2243 23 to R > 27, corresponding to rest-frame UV absolute magnitudes M _(UV) \u2243 \u201322 to M ^(UV) > \u201318.2. Dynamical masses range from M_(dyn) < 1.3 \u00d7 10^8 M_\u2609 to M_(dyn) = 6.8 \u00d7 10^9 M_\u2609, with a median value of M_(dyn) = 6.3 \u00d7 10^8 M_\u2609. Thirty of the 36 Ly\u03b1 emission lines are redshifted with respect to the systemic velocity with at least 1\u03c3 significance, and the velocity offset with respect to systemic \u0394v_(Ly\u03b1) is correlated with the R-band magnitude, M_(UV), and the velocity dispersion measured from nebular emission lines with >3\u03c3 significance: brighter galaxies with larger velocity dispersions tend to have larger values of \u0394v Ly\u03b1. We also make use of a comparison sample of 122 UV-color-selected R < 25.5 galaxies at z ~ 2, all with Ly\u03b1 emission and systemic redshifts measured from nebular emission lines. Using the combined LAE and comparison samples for a total of 158 individual galaxies, we find that \u0394v_(Ly\u03b1) is anti-correlated with the Ly\u03b1 equivalent width with 7\u03c3 significance. Our results are consistent with a scenario in which the Ly\u03b1 profile is determined primarily by the properties of the gas near the systemic redshift; in such a scenario, the opacity to Ly\u03b1 photons in lower mass galaxies may be reduced if large gaseous disks have not yet developed and if the gas is ionized by the harder spectrum of young, low metallicity stars.", "date": "2014-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "795", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 33", "id_number": "CaltechAUTHORS:20141201-093722795", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141201-093722795", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1255591" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NSF", "grant_number": "AST-1313472" }, { "agency": "Ministry of Education, Science and Technological Development (Serbia)", "grant_number": "ON176021" }, { "agency": "Gordon and Betty Moore Foundation" } ] }, "doi": "10.1088/0004-637X/795/1/33", "primary_object": { "basename": "0004-637X_795_1_33.pdf", "url": "https://authors.library.caltech.edu/records/7fnq2-n6y28/files/0004-637X_795_1_33.pdf" }, "related_objects": [ { "basename": "1408.3638v3.pdf", "url": "https://authors.library.caltech.edu/records/7fnq2-n6y28/files/1408.3638v3.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Erb, Dawn K.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/bdwkr-1zy75", "eprint_id": 44109, "eprint_status": "archive", "datestamp": "2023-08-20 00:54:36", "lastmod": "2023-10-26 00:11:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Chang-Daphne", "name": { "family": "Chang", "given": "Daphne" } }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Matt" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Rahman-S", "name": { "family": "Rahman", "given": "Shahin" } }, { "id": "Moore-A", "name": { "family": "Moore", "given": "Anna" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Intergalactic Medium Emission Observations with the Cosmic Web Imager. I. The Circum-QSO Medium of QSO 1549+19, and Evidence for a Filamentary Gas Inflow", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2014. The American Astronomical Society. \n\nReceived 9 February 2013, accepted for publication 10 February 2014. Published 24 April 2014. \n\nWe thank Tom Tombrello and Shri Kulkarni for their support of PCWI. We thank Marty Crabill, Steve Kaye and the staff of the Palomar Observatory for their constant support. Nicole Lingner participated in the observations. We are deeply grateful to Dean Joe Shepard, to the Caltech Counselling Office, and to the family of Daphne Chang for their strength and support. We acknowledge the detailed and helpful comments from the anonymous referee. This work was supported by the National Science Foundation and the California Institute of Technology.\n\nPublished - 0004-637X_786_2_106.pdf
Submitted - 1402.4816.pdf
", "abstract": "The Palomar Cosmic Web Imager (PCWI), an integral field spectrograph designed to detect and map low surface brightness emission, has obtained imaging spectroscopic maps of Ly\u03b1 from the circum-QSO medium (CQM) of QSO HS1549+19 at redshift z=2.843. Extensive extended emission is detected from the CQM, consistent with fluorescent and pumped Ly\u03b1 produced by the ionizing and Ly\u03b1 continuum of the QSO. Many features present in PCWI spectral images match those detected in narrow-band images. Filamentary structures with narrow line profiles are detected in several cases as long as 250-400 kpc. One of these is centered at a velocity redshifted with respect to the systemic velocity, and displays a spatially collimated and\nkinematically cold line profile increasing in velocity width approaching the QSO. This suggests that the filament gas is infalling onto the QSO, perhaps in a cold accretion flow. Because of the strong ionizing flux, the neutral column density is low, typically N(HI) ~ 10^(12)\u221210^(15) cm^(\u22122), and the line center optical depth is also low (typically \u03c4_0 <10), insufficient to display well-separated\ndouble peak emission characteristic of higher line optical depths. With a simple ionization and cloud model we can very roughly estimate the total gas mass (log M_(gas) = 12.5 \u00b1 0.5) and the total (log M_(tot) = 13.3\u00b1 0.5). We can also calculate a kinematic mass from the total line profile (2\u00d710^(13)M_\u2609), which agrees with the mass estimated from the gas emission. The intensity-binned\nspectrum of the CQM shows a progression in kinematic properties consistent with heirarchical structure formation.", "date": "2014-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "768", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 106", "id_number": "CaltechAUTHORS:20140303-152428640", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140303-152428640", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Caltech" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/786/2/106", "primary_object": { "basename": "0004-637X_786_2_106.pdf", "url": "https://authors.library.caltech.edu/records/bdwkr-1zy75/files/0004-637X_786_2_106.pdf" }, "related_objects": [ { "basename": "1402.4816.pdf", "url": "https://authors.library.caltech.edu/records/bdwkr-1zy75/files/1402.4816.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Martin, D. Christopher; Chang, Daphne; et el." }, { "id": "https://authors.library.caltech.edu/records/mtwgn-gkm57", "eprint_id": 44105, "eprint_status": "archive", "datestamp": "2023-08-20 00:54:29", "lastmod": "2023-10-26 00:11:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Chang-Daphne", "name": { "family": "Chang", "given": "Daphne" } }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Matt" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Rahman-S", "name": { "family": "Rahman", "given": "Shahin" } }, { "id": "Moore-A-M", "name": { "family": "Moore", "given": "Anna" }, "orcid": "0000-0002-2894-6936" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Matsuda-Yuichi", "name": { "family": "Matsuda", "given": "Yuichi" } } ] }, "title": "Intergalactic Medium Emission Observations with the Cosmic Web Imager. II. Discovery of Extended, Kinematically-Linked Emission around SSA22 Ly\u03b1 Blob 2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: formation \u2013 galaxies: high-redshift \u2013 intergalactic medium \u2013\ntechniques: imaging spectroscopy", "note": "\u00a9 2014. The American Astronomical Society. \n\nReceived 2013 May 24; accepted 2013 October 31; published 2014 April 24. \n\nWe thank Tom Tombrello and Shri Kulkarni for their support of CWI. We thank Marty Crabill, Steve Kaye and the staff of the Palomar Observatory for their constant support. Nicole Ligner participated in the observations. We are deeply grateful to Dean Joe Shepard, to the Caltech Counselling Office, and to the family of Daphne Chang for their strength and support. The anonymous referee provided excellent suggestions that significantly improved the paper. This\nwork was supported by the National Science Foundation and the California Institute of Technology.\n\nPublished - 0004-637X_786_2_107.pdf
Submitted - 1402.4809.pdf
", "abstract": "The intergalactic medium (IGM) is the dominant reservoir of baryons, delineates the large scale structure of the universe at low to moderate overdensities, and provides gas from which galaxies form and evolve. Simulations of a Cold Dark Matter (CDM) dominated universe predict that the\nIGM is distributed in a cosmic web of filaments, and that galaxies should form along and at the intersections of these filaments (Bond, Kofman, & Pogosyan 1994; Miralda-Escude et al. 1996). While observations of QSO absorption lines and the large-scale distribution of galaxies have\nconfirmed the CDM paradigm, the cosmic web of IGM has never been confirmed by direct imaging. Here we report our observation of the Ly\u03b1 blob-2 (LAB2) in SSA22, with the Cosmic Web Imager. This is an integral field spectrograph optimized for low surface brightness, extended emission. With 22 hours of total on- and off-source exposure, CWI has revealed that LAB2 has extended Ly\u03b1 emission which is organized into azimuthal zones consistent with filaments. We perform numerous tests with simulations and the data to secure the robustness of this result, which relies on data with modest signal-to-noise ratio. We have developed a\nsmoothing algorithm that permits visualization of data cube slices along image or spectral-image planes. With both raw and smoothed data cubes we demonstrate that the filaments are kinematically associated with LAB2 and display double-peaked profiles characteristic of optically thick Ly\u03b1 emission. The flux is 10-20 times brighter than expected for the average emission from the IGM but is consistent with boosted fluorescence from a buried QSO or gravitation cooling radiation. Using simple emission models we infer a baryon mass in the filaments of at least 1\u22124 \u00d7 10^(11)M_\u2609, and the dark halo mass is at least 2 \u00d7 10^(12)M_\u2609. The spatial-kinematic morphology is more consistent with inflow from the cosmic web than outflow from LAB2, although an outflow feature maybe present at one azimuth. LAB2 and the surrounding gas have significant and coaligned angular momentum, strengthening the case for their association.", "date": "2014-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "786", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 107", "id_number": "CaltechAUTHORS:20140303-145821259", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140303-145821259", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Caltech" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/786/2/107", "primary_object": { "basename": "0004-637X_786_2_107.pdf", "url": "https://authors.library.caltech.edu/records/mtwgn-gkm57/files/0004-637X_786_2_107.pdf" }, "related_objects": [ { "basename": "1402.4809.pdf", "url": "https://authors.library.caltech.edu/records/mtwgn-gkm57/files/1402.4809.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Martin, D. Christopher; Chang, Daphne; et el." }, { "id": "https://authors.library.caltech.edu/records/8qq9j-2r382", "eprint_id": 46012, "eprint_status": "archive", "datestamp": "2023-08-20 00:04:12", "lastmod": "2023-10-26 18:36:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "James-B-L", "name": { "family": "James", "given": "Bethan L." } }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Christensen-L", "name": { "family": "Christensen", "given": "Lise" } }, { "id": "Auger-M-W", "name": { "family": "Auger", "given": "Matthew W." } }, { "id": "Becker-G-D", "name": { "family": "Becker", "given": "George D." } }, { "id": "King-L-J", "name": { "family": "King", "given": "Lindsay J." } }, { "id": "Quider-A-M", "name": { "family": "Quider", "given": "Anna M." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Testing metallicity indicators at z \u223c 1.4 with the gravitationally lensed galaxy CASSOWARY 20", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: strong, galaxies: abundances, galaxies: evolution", "note": "\u00a9 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nFirst published online: March 27, 2014. Accepted 2014 February 10. Received 2014 February 10; in original form 2013 September 20. \n\nWe are grateful to the European Southern Observatory time assignment committee who awarded time to this programme and to the staff astronomers at Paranal who conducted the observations. It is a pleasure to acknowledge the help by Sergey Koposov with various aspects of the data analysis. Vasily Belokurov kindly provided the WHT images of CSWA 20 reproduced in Fig. 1, and Naveen Reddy the composite of BM galaxy spectra used in Fig. 5. We are also grateful to Mike Barlow, Claus Leitherer and Daniela Calzetti for useful discussions, and to the anonymous referee whose comments\nand suggestions improved the paper. LC is supported by the\nEuropean Union under a Marie Curie Intra-European fellowship, contract PIEF-GA-2010-274117.\n\nPublished - MNRAS-2014-James-1794-809.pdf
Submitted - 1311.5092v2.pdf
", "abstract": "We present X-shooter observations of CASSOWARY 20 (CSWA 20), a star-forming (SFR \u223c 6 M_\u2299 yr^(\u22121)) galaxy at z = 1.433, magnified by a factor of 11.5 by the gravitational lensing produced by a massive foreground galaxy at z = 0.741. We analysed the integrated physical properties of the H\u2009ii regions of CSWA 20 using temperature- and density-sensitive emission lines. We find the abundance of oxygen to be \u223c1/7 of solar, while carbon is \u223c50 times less abundant than in the Sun. The unusually low C/O ratio may be an indication of a particularly rapid time-scale of chemical enrichment. The wide wavelength coverage of X-shooter gives us access to five different methods for determining the metallicity of CSWA 20, three based on emission lines from H\u2009ii regions and two on absorption features formed in the atmospheres of massive stars. All five estimates are in agreement, within the factor of \u223c2 uncertainty of each method. The interstellar medium (ISM) of CSWA 20 only partially covers the star-forming region as viewed from our direction; in particular, absorption lines from neutrals and first ions are exceptionally weak. We find evidence for large-scale outflows of the ISM with speeds of up 750\u2009km\u2009s^(\u22121), similar to the values measured in other high-z galaxies sustaining much higher rates of star formation.", "date": "2014-03-27", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "440", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1794-1809", "id_number": "CaltechAUTHORS:20140530-134610304", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140530-134610304", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Marie Curie Fellowship", "grant_number": "PIEF-GA-2010-274117" } ] }, "doi": "10.1093/mnras/stu287", "primary_object": { "basename": "1311.5092v2.pdf", "url": "https://authors.library.caltech.edu/records/8qq9j-2r382/files/1311.5092v2.pdf" }, "related_objects": [ { "basename": "MNRAS-2014-James-1794-809.pdf", "url": "https://authors.library.caltech.edu/records/8qq9j-2r382/files/MNRAS-2014-James-1794-809.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "James, Bethan L.; Pettini, Max; et el." }, { "id": "https://authors.library.caltech.edu/records/rjxr9-e5x90", "eprint_id": 43723, "eprint_status": "archive", "datestamp": "2023-08-22 11:29:57", "lastmod": "2023-10-25 23:48:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cooke-R-J", "name": { "family": "Cooke", "given": "Ryan J." }, "orcid": "0000-0001-7653-5827" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Jorgenson-R-A", "name": { "family": "Jorgenson", "given": "Regina A." } }, { "id": "Murphy-M-T", "name": { "family": "Murphy", "given": "Michael T." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Precision Measures of the Primordial Abundance of Deuterium", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; primordial nucleosynthesis; quasars: absorption lines", "note": "\u00a9 2014 The American Astronomical Society. \n\nReceived 2013 August 14; accepted 2013 November 13; published 2014 January 3. \n\nBased on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile (VLT program IDs: 68.B-0115(A), 70.A-0425(C), 078.A-0185(A), 085.A-0109(A)), and at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. \n\nKeck telescope time was partially granted by NOAO, through the Telescope System Instrumentation Program (TSIP). TSIP is funded by NSF. \n\nWe are grateful to the staff astronomers at the ESO VLT and Keck Observatory for their assistance with the observations. We are indebted to Gary Steigman for kindly communicating ahead of publication the latest fitting formulae used in this work, and for providing valuable comments on the manuscript. We also thank an anonymous referee who provided useful suggestions that improved the presentation of this work. Discussions, advice, and help with various aspects of the work described in this paper were provided by Antony Lewis, Jordi Miralda-Escud\u00e9, Paolo Molaro, Ken Nollett, Pasquier Noterdaeme, John O'Meara, Jason X. Prochaska, Signe Riemer-S\u00f8renson, Donatella Romano, and John Webb. We thank the Hawaiian people for the opportunity to observe from Mauna Kea; without their hospitality, this work would not have been possible. \n\nR.J.C. is partially supported by NSF grant AST-1109447. R.A.J. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1102683. M.T.M. thanks the Australian Research Council for a QEII Research Fellowship (DP0877998) and a Discovery Project grant (DP130100568).\n\nPublished - 0004-637X_781_1_31.pdf
Submitted - 1308.3240v2.pdf
", "abstract": "We report the discovery of deuterium absorption in the very metal-poor ([Fe/H] = \u20132.88) damped Ly\u03b1 system at z_abs = 3.06726 toward the QSO SDSS J1358+6522. On the basis of 13 resolved D I absorption lines and the damping wings of the H I Ly\u03b1 transition, we have obtained a new, precise measure of the primordial abundance of deuterium. Furthermore, to bolster the present statistics of precision D/H measures, we have reanalyzed all of the known deuterium absorption-line systems that satisfy a set of strict criteria. We have adopted a blind analysis strategy (to remove human bias) and developed a software package that is specifically designed for precision D/H abundance measurements. For this reanalyzed sample of systems, we obtain a weighted mean of (D/H)_p = (2.53 \u00b1 0.04) \u00d7 10^\u20135, corresponding to a universal baryon density 100 \u03a9_b, 0 h^2 = 2.202 \u00b1 0.046 for the standard model of big bang nucleosynthesis (BBN). By combining our measure of (D/H)p with observations of the cosmic microwave background (CMB), we derive the effective number of light fermion species, N eff = 3.28 \u00b1 0.28. We therefore rule out the existence of an additional (sterile) neutrino (i.e., N_eff = 4.046) at 99.3% confidence (2.7\u03c3), provided that the values of N eff and of the baryon-to-photon ratio (\u03b7_10) did not change between BBN and recombination. We also place a strong bound on the neutrino degeneracy parameter, independent of the 4He primordial mass fraction, Y P: \u03beD = +0.05 \u00b1 0.13 based only on the CMB+(D/H)_p observations. Combining this value of \u03beD with the current best literature measure of Y P, we find a 2\u03c3 upper bound on the neutrino degeneracy parameter, |\u03be| \u2264 +0.062.", "date": "2014-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "781", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 31", "id_number": "CaltechAUTHORS:20140207-112247242", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140207-112247242", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1109447" }, { "agency": "NSF Astronomy and Astrophysics Fellowship", "grant_number": "AST-1102683" }, { "agency": "Australian Research Council", "grant_number": "DP0877998" }, { "agency": "Australian Research Council", "grant_number": "DP130100568" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/781/1/31", "primary_object": { "basename": "0004-637X_781_1_31.pdf", "url": "https://authors.library.caltech.edu/records/rjxr9-e5x90/files/0004-637X_781_1_31.pdf" }, "related_objects": [ { "basename": "1308.3240v2.pdf", "url": "https://authors.library.caltech.edu/records/rjxr9-e5x90/files/1308.3240v2.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Cooke, Ryan J.; Pettini, Max; et el." }, { "id": "https://authors.library.caltech.edu/records/r2crt-zvb06", "eprint_id": 43439, "eprint_status": "archive", "datestamp": "2023-08-22 11:06:06", "lastmod": "2023-10-25 23:32:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mostardi-R-E", "name": { "family": "Mostardi", "given": "R. E." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "A. E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Nestor-D-B", "name": { "family": "Nestor", "given": "D. B." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "N. A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "R. F." }, "orcid": "0000-0002-6967-7322" } ] }, "title": "Narrowband Lyman-continuum Imaging of Galaxies at z ~ 2.85", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; diffuse radiation; galaxies: high-redshift; intergalactic medium", "note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 May 24; accepted 2013 September 28; published 2013 November 26. \n\nWe thank Kevin Hainline for his helpful discussions regarding our photometric simulations, Katherine Kornei for advice on the spectroscopic data reduction, and the anonymous referee for constructive suggestions. R.E.M., A.E.S., and D.B.N. acknowledge support from the David and Lucile Packard Foundation. C.C.S. acknowledges additional support from NSF grant AST-0908805 and GO-11638.01 from the Space Telescope Science Institute. We extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible.\n\nPublished - 0004-637X_779_1_65.pdf
Submitted - 1306.1535v2.pdf
", "abstract": "We present results from a survey for z ~ 2.85 Lyman-continuum (LyC) emission in the HS1549+1933 field and place constraints on the amount of ionizing radiation escaping from star-forming galaxies. Using a custom narrowband filter (NB3420) tuned to wavelengths just below the Lyman limit at z \u2265 2.82, we probe the LyC spectral region of 49 Lyman break galaxies (LBGs) and 91 Ly\u03b1 emitters (LAEs) spectroscopically confirmed at z \u2265 2.82. Four LBGs and seven LAEs are detected in NB3420. Using V-band data probing the rest-frame nonionizing UV, we observe that many NB3420-detected galaxies exhibit spatial offsets between their LyC and nonionizing UV emission and are characterized by extremely blue NB3420\u2013V colors, corresponding to low ratios of nonionizing to ionizing radiation (F_(UV)/F_(LyC)) that are in tension with current stellar population synthesis models. We measure average values of (F_(UV)/F_(LyC)) for our LBG and LAE samples, correcting for foreground galaxy contamination and H I absorption in the intergalactic medium. We find (F_(UV)/F_(LyC)_(corr)^(LBG)= 82 \u00b1 45 and (F_(UV)/F_(LyC)_(corr)^(LAE)= 7.4 \u00b1 3.6. These flux density ratios correspond, respectively, to relative LyC escape fractions of f_(esc,rel)^(LBG) = 5%-8% and f_(esc,rel)^(LAE)=18%-49%, absolute LyC escape fractions of f_(esc)^(LBG)=1%-2% and f_(esc)^(LAE)=5%-15%, and a comoving LyC emissivity from star-forming galaxies of 8.8-15.0 \u00d7 10^(24) erg s^(\u20131) Hz^(\u20131) Mpc^(\u20133). In order to study the differential properties of galaxies with and without LyC detections, we analyze narrowband Ly\u03b1 imaging and rest-frame near-infrared imaging, finding that while LAEs with LyC detections have lower Ly\u03b1 equivalent widths on average, there is no substantial difference in the rest-frame near-infrared colors of LBGs or LAEs with and without LyC detections. These preliminary results are consistent with an orientation-dependent model where LyC emission escapes through cleared paths in a patchy interstellar medium.", "date": "2013-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "779", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 65", "id_number": "CaltechAUTHORS:20140117-143100184", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140117-143100184", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "David and Lucile Packard Foundation" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "NASA", "grant_number": "GO-11638.01" } ] }, "doi": "10.1088/0004-637X/779/1/65", "primary_object": { "basename": "1306.1535v2.pdf", "url": "https://authors.library.caltech.edu/records/r2crt-zvb06/files/1306.1535v2.pdf" }, "related_objects": [ { "basename": "0004-637X_779_1_65.pdf", "url": "https://authors.library.caltech.edu/records/r2crt-zvb06/files/0004-637X_779_1_65.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Mostardi, R. E.; Shapley, A. E.; et el." }, { "id": "https://authors.library.caltech.edu/records/a1sr0-bnm69", "eprint_id": 41974, "eprint_status": "archive", "datestamp": "2023-08-22 10:22:20", "lastmod": "2023-10-25 14:59:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan" }, "orcid": "0000-0002-6967-7322" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Constraints on Hyperluminous QSO Lifetimes via Fluorescent Ly\u03b1 Emitters at Z \u2243 2.7", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation; galaxies: high-redshift; quasars: general", "note": "\u00a9 2013. The American Astronomical Society. \n\nReceived 19 July 2013, accepted for publication 6 August 2013. Published 29 August 2013. \n\nWe are indebted to the staff of the W.M. Keck Observatory who keep the instruments and telescopes running effectively. We also extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. This work has been supported in part by the U.S. National Science Foundation through grant AST-0908805.\n\nPublished - 2041-8205_775_1_L3.pdf
Submitted - 1308.1678.pdf
", "abstract": "We present observations of a population of Ly\u03b1 emitters (LAEs) exhibiting fluorescent emission via the reprocessing of ionizing radiation from nearby hyperluminous QSOs. These LAEs are part of a survey at redshifts 2.5 < z < 2.9 combining narrow-band photometric selection and spectroscopic follow-up to characterize the emission mechanisms, physical properties, and three-dimensional locations of the emitters with respect to their nearby hyperluminous QSOs. These data allow us to probe the radiation field, and thus the radiative history, of the QSOs, and we determine that most of the eight QSOs in our sample have been active and of comparable luminosity for a time 1 Myr \u2272 t_Q \u2272 20 Myr. Furthermore, we find that the ionizing QSO emission must have an opening angle \u03b8 ~ 30\u00b0 or larger relative to the line of sight.", "date": "2013-09-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "775", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L3", "id_number": "CaltechAUTHORS:20131017-133655029", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131017-133655029", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0908805" } ] }, "doi": "10.1088/2041-8205/775/1/L3", "primary_object": { "basename": "2041-8205_775_1_L3.pdf", "url": "https://authors.library.caltech.edu/records/a1sr0-bnm69/files/2041-8205_775_1_L3.pdf" }, "related_objects": [ { "basename": "1308.1678.pdf", "url": "https://authors.library.caltech.edu/records/a1sr0-bnm69/files/1308.1678.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Trainor, Ryan and Steidel, Charles C." }, { "id": "https://authors.library.caltech.edu/records/z54pq-69f03", "eprint_id": 41605, "eprint_status": "archive", "datestamp": "2023-08-19 21:26:17", "lastmod": "2023-10-24 23:53:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kulas-K-R", "name": { "family": "Kulas", "given": "Kristin R." } }, { "id": "McLean-I-S", "name": { "family": "McLean", "given": "Ian S." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Konidaris-N-P", "name": { "family": "Konidaris", "given": "Nicholas P." }, "orcid": "0000-0003-1905-2815" }, { "id": "Matthews-K-D", "name": { "family": "Matthews", "given": "Keith D." } }, { "id": "Mace-G-N", "name": { "family": "Mace", "given": "Gregory N." }, "orcid": "0000-0001-7875-6391" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" } ] }, "title": "The Mass-Metallicity Relation of a z ~ 2 Protocluster with MOSFIRE", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: abundances \u2013 galaxies: clusters: general \u2013 galaxies: evolution \u2013 galaxies: formation \u2013 galaxies: high-redshift", "note": "\u00a9 2013 The American Astronomical Society. \n\nReceived 2013 June 21; accepted 2013 August 2; published 2013 August 23. \n\nMOSFIRE was developed by the consortium of the University of California, Los Angeles, the California Institute of Technology, the University of California, Santa Cruz and the W. M. Keck Observatory. Funding was provided by a grant from the National Science Foundation's Telescope System Instrumentation Program and by a generous donation from Gordon and Betty Moore to the Keck Observatory. We thank the entire MOSFIRE team, whose dedication and hard work made this project possible. We also gratefully acknowledge the outstanding support of the entire Keck Observatory staff during commissioning, especially Marc Kassis, Greg Wirth and Al Honey. A.E.S. acknowledges support from the David and Lucile Packard Foundation. N.P.K. acknowledges support from the NSF grant 1106171. Additionally, we acknowledge Romeel Dav\u00e9 for insightful conversations. Finally, we wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible.\n\nPublished - Kulas_2013p130.pdf
Submitted - 1306.6334v2.pdf
", "abstract": "We present Keck/MOSFIRE observations of the role of environment in the formation of galaxies at z ~ 2. Using K-band spectroscopy of H\u03b1 and [N\u2009ii] emission lines, we have analyzed the metallicities of galaxies within and around a z = 2.3 protocluster discovered in the HS1700+643 field. Our main sample consists of 23 protocluster and 20 field galaxies with estimates of stellar masses and gas-phase metallicities based on the N2 strong-line metallicity indicator. With these data we have examined the mass\u2013metallicity relation with respect to environment at z ~ 2. We find that field galaxies follow the well-established trend between stellar mass and metallicity, such that more massive galaxies have larger metallicities. The protocluster galaxies, however, do not exhibit a dependence of metallicity on mass, with the low-mass protocluster galaxies showing an enhancement in metallicity compared to field galaxies spanning the same mass range. A comparison with galaxy formation models suggests that the mass-dependent environmental trend we observed can be qualitatively explained in the context of the recycling of \"momentum-driven\" galaxy wind material. Accordingly, winds are recycled on a shorter timescale in denser environments, leading to an enhancement in metallicity at fixed mass for all but the most massive galaxies. Future hydrodynamical simulations of z ~ 2 overdensities matching the one in the HS1700 field will be crucial for understanding the origin of the observed environmental trend in detail.", "date": "2013-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "774", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 130", "id_number": "CaltechAUTHORS:20131002-100802038", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131002-100802038", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "NSF", "grant_number": "AST-1106171" } ] }, "doi": "10.1088/0004-637X/774/2/130", "primary_object": { "basename": "1306.6334v2.pdf", "url": "https://authors.library.caltech.edu/records/z54pq-69f03/files/1306.6334v2.pdf" }, "related_objects": [ { "basename": "Kulas_2013p130.pdf", "url": "https://authors.library.caltech.edu/records/z54pq-69f03/files/Kulas_2013p130.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Kulas, Kristin R.; McLean, Ian S.; et el." }, { "id": "https://authors.library.caltech.edu/records/m4x1p-n1j94", "eprint_id": 41169, "eprint_status": "archive", "datestamp": "2023-08-19 20:55:40", "lastmod": "2023-10-24 23:30:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rakic-O", "name": { "family": "Rakic", "given": "Olivera" } }, { "id": "Schaye-J", "name": { "family": "Schaye", "given": "Joop" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Booth-C-M", "name": { "family": "Booth", "given": "C. M." } }, { "id": "Dalla-Vecchia-C", "name": { "family": "Dalla Vecchia", "given": "Claudio" } }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" } ] }, "title": "A measurement of galaxy halo mass from the surrounding H i Ly\u03b1 absorption", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift \u2013 intergalactic medium \u2013 quasars: absorption lines", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2013 May 30. Received 2013 May 29; in original form 2012 October 5. First published online: June 29, 2013. \n\nThe authors would like to thank all the members of the OWLS\nteam for useful discussions and the anonymous referee whose suggestions have improved the clarity of the paper. The simulations\npresented here were run on Stella, the LOFAR BlueGene/L system\nin Groningen, on the Cosmology Machine at the Institute for\nComputational Cosmology in Durham (which is part of the DiRAC\nFacility jointly funded by STFC, the Large Facilities Capital Fund\nof BIS and Durham University) as part of the Virgo Consortium\nresearch programme and on Darwin in Cambridge. This work\nwas sponsored by the National Computing Facilities Foundation\n(NCF) for the use of supercomputer facilities, with financial support\nfrom the Netherlands Organization for Scientific Research (NWO),\nalso through a VIDI grant. The research leading to these results\nhas received funding from the European Research Council under\nthe European Union's Seventh Framework Programme (FP7/2007-\n2013)/ERC Grant agreement 278594-GasAroundGalaxies and from\nthe Marie Curie Training Network CosmoComp (PITN-GA-2009-\n238356).\n\nPublished - MNRAS-2013-Rakic-3103-14.pdf
Submitted - 1306.1563v1.pdf
", "abstract": "We measure the dark matter halo masses of \u3008z\u3009 \u2248 2.36 UV colour-selected star-forming galaxies by matching the observed median H I Ly\u03b1 absorption around them, as observed in the spectra of background QSOs, to the absorption around haloes above a given mass in cosmological simulations. Focusing on transverse separations 0\u20132 proper Mpc (pMpc) and line-of-sight separations 154\u2013616\u2009km\u2009s^(\u22121), we find a minimum halo mass of log_(10)M_(min)/M\u2299 = 11.6 \u00b1 0.2, which is in good agreement with published halo mass estimates from clustering analyses. We verified that the measured halo mass is insensitive to a change in the cosmological parameters (Wilkinson Microwave Anisotropy Probe 1 versus Wilkinson Microwave Anisotropy Probe 3) and to the inclusion of strong AGN feedback. One unique strength of this method is that it can be used in narrow field galaxy\u2013QSO surveys, i.e. \u224830 \u00d7 30\u2009arcsec. In addition, we find that the observed anisotropy in the 2D H I Ly\u03b1 absorption distribution on scales of 1.5\u20132\u2009pMpc is consistent with being a consequence of large-scale gas infall into the potential wells occupied by galaxies.", "date": "2013-08", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "433", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3103-3114", "id_number": "CaltechAUTHORS:20130909-104553617", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130909-104553617", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Computing Facilities Foundation" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "European Research Council (ERC)", "grant_number": "278594" }, { "agency": "Marie Curie Fellowship", "grant_number": "PITN-GA-2009-238356" } ] }, "doi": "10.1093/mnras/stt950", "primary_object": { "basename": "1306.1563v1.pdf", "url": "https://authors.library.caltech.edu/records/m4x1p-n1j94/files/1306.1563v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2013-Rakic-3103-14.pdf", "url": "https://authors.library.caltech.edu/records/m4x1p-n1j94/files/MNRAS-2013-Rakic-3103-14.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Rakic, Olivera; Schaye, Joop; et el." }, { "id": "https://authors.library.caltech.edu/records/fpx9v-zt321", "eprint_id": 38531, "eprint_status": "archive", "datestamp": "2023-08-19 20:20:52", "lastmod": "2023-10-23 20:15:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" } ] }, "title": "The Column Density Distribution and Continuum Opacity of the Intergalactic and Circumgalactic Medium at RedshiftPublished - 0004-637X_769_2_146.pdf
Submitted - 1304.6719v1.pdf
", "abstract": "We present new high-precision measurements of the opacity of the intergalactic and circumgalactic medium (IGM, CGM) at =2.4. Using Voigt profile fits to the full Lyman alpha and Lyman beta forests in 15 high-resolution high-S/N spectra of hyperluminous QSOs, we make the first statistically robust measurement of the frequency of absorbers with HI column densities 14\u227elog(N_(HI))\u227e 17.2. We also present the first measurements of the frequency distribution of HI absorbers in the volume surrounding high-z galaxies (the CGM, 300 pkpc), finding that the incidence of absorbers in the CGM is much higher than in the IGM. In agreement with Rudie et al. (2012), we find that there are fractionally more high-N_(HI) absorbers than low-N_(HI) absorbers in the CGM compared to the IGM, leading to a shallower power law fit to the CGM frequency distribution. We use these new measurements to calculate the total opacity of the IGM and CGM to hydrogen-ionizing photons, finding significantly higher opacity than most previous studies, especially from absorbers with log(N_(HI))< 17.2. Reproducing the opacity measured in our data as well as the incidence of absorbers with log(N_(HI)/cm^(-2)) > 17.2 requires a broken power law parameterization of the frequency distribution with a break near log(N^(HI))\u224810^(15)cm^(-2). We compute new estimates of the mean free path \u03bb_(mfp) to hydrogen-ionizing photons at Z_(em)=2.4, finding \u03bb_(mfp) = 147 + 15 Mpc when considering only IGM opacity. If instead, we consider photons emanating from a high-z star-forming galaxy and account for the local excess opacity due to the surrounding CGM of the galaxy itself, the mean free path is reduced to \u03bb_(mfp) = 121 + 15 Mpc. These \u03bb_(mfp) measurements are smaller than recent estimates and should inform future studies of the metagalactic UV background and of ionizing sources at z\u22482-3.", "date": "2013-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "769", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 146", "id_number": "CaltechAUTHORS:20130516-074741446", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130516-074741446", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "NASA" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/769/2/146", "primary_object": { "basename": "0004-637X_769_2_146.pdf", "url": "https://authors.library.caltech.edu/records/fpx9v-zt321/files/0004-637X_769_2_146.pdf" }, "related_objects": [ { "basename": "1304.6719v1.pdf", "url": "https://authors.library.caltech.edu/records/fpx9v-zt321/files/1304.6719v1.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Rudie, Gwen C.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/mwz40-sac38", "eprint_id": 38938, "eprint_status": "archive", "datestamp": "2023-08-19 19:40:51", "lastmod": "2023-10-24 14:52:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cooke-R-J", "name": { "family": "Cooke", "given": "Ryan" }, "orcid": "0000-0001-7653-5827" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Jorgenson-R-A", "name": { "family": "Jorgenson", "given": "Regina A." } }, { "id": "Murphy-M-T", "name": { "family": "Murphy", "given": "Michael T." } }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "The explosion energy of early stellar populations: the Fe-peak element ratios in low-metallicity damped Ly\u03b1 systems", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general\n galaxies: abundances\n galaxies: evolution\n quasars: absorption lines", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2013 February 12. Received 2013 February 12; in original form 2012 October 10. First published online: March 19, 2013. \n\nBased on observations collected at the European Organization for Astronomical Research in the Southern hemisphere, Chile [Proposals 67.A-0078(A), 69.A-0613(A), 083.A-0042(A) and 085.A-0109(A)], and at the W.M. Keck Observatory which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. \n\nKeck telescope time was partially granted by NOAO, through the Telescope System Instrumentation Program (TSIP). TSIP is funded by NSF. \n\nWe are grateful to the staff astronomers at the VLT and Keck Observatories for their assistance with the observations, and to the telescope time assignment committees for their support of the VMP DLA survey. We thank the referee, Paolo Molaro, for a prompt and helpful report that improved the paper, and Piercarlo Bonifacio for communicating his measurements of Cr/Fe in very metal poor stars. It is also a pleasure to acknowledge valuable discussions with Poul\nNissen and Stan Woosley, regarding the stellar abundance measurements and nucleosynthesis calculations. We thank the Hawaiian people for the opportunity to observe from Mauna Kea; without their hospitality, this work would not have been possible. RC acknowledges the support of a Morrison Fellowship provided by the University of California, Santa Cruz. RAJ is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1102683. MTM thanks the Australian Research Council for a QEII Research Fellowship (DP0877998).\n\nPublished - MNRAS-2013-Cooke-1625-37.pdf
", "abstract": "The relative abundances of the Fe-peak elements (Ti\u2013Zn) at the lowest metallicities are intimately linked to the physics of core-collapse supernova explosions. With a sample of 25 very metal poor damped Ly\u03b1 systems (DLAs), we investigate the trends of the Fe-peak element ratios with metallicity. For nine of the 25 DLAs, a direct measurement (or useful upper limit) of one or more of the Ti, Cr, Co, Ni, Zn/Fe abundance ratios could be determined from detected absorption lines. For the remaining systems (without detections), we devised a new form of spectral stacking to estimate the typical Fe-peak element ratios of the DLA population in this metallicity regime. We compare these data to analogous measurements in metal-poor stars of the Galactic halo and to detailed calculations of explosive nucleosynthesis in metal-free stars. We conclude that most of the DLAs in our sample were enriched by stars that released an energy of \u22721.2 \u00d7 10^(51) erg when they exploded as core-collapse supernovae. Finally, we discuss the exciting prospect of measuring Fe-peak element ratios in DLAs with Fe/H < 1/1000 of solar when 30-m class telescopes become available. Only then will we be able to pin down the energy that was released by the supernovae of the first stars.", "date": "2013-05", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "431", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1625-1637", "id_number": "CaltechAUTHORS:20130613-092507120", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130613-092507120", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "University of California, Santa Cruz" }, { "agency": "NSF Astronomy and Astrophysics Fellowship", "grant_number": "AST-1102683" }, { "agency": "Australian Research Council", "grant_number": "DP0877998" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1093/mnras/stt282", "primary_object": { "basename": "MNRAS-2013-Cooke-1625-37.pdf", "url": "https://authors.library.caltech.edu/records/mwz40-sac38/files/MNRAS-2013-Cooke-1625-37.pdf" }, "resource_type": "article", "pub_year": "2013", "author_list": "Cooke, Ryan; Pettini, Max; et el." }, { "id": "https://authors.library.caltech.edu/records/n8rpc-eb272", "eprint_id": 37718, "eprint_status": "archive", "datestamp": "2023-08-22 08:51:55", "lastmod": "2023-10-23 17:59:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nestor-D-B", "name": { "family": "Nestor", "given": "Daniel B." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Kornei-K-A", "name": { "family": "Kornei", "given": "Katherine A." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Siana-Brian-D", "name": { "family": "Siana", "given": "Brian" }, "orcid": "0000-0002-4935-9511" } ] }, "title": "A Refined Estimate of the Ionizing Emissivity from Galaxies at z \u2243 3: Spectroscopic Follow-up in the SSA22a Field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; diffuse radiation; galaxies: high-redshift; intergalactic medium", "note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2012 October 3; accepted 2012 December 28; published 2013 February 14. \n\nBased, in part, on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. \n\nWe thank Gwen Rudie for providing us with updated measurements of the z \u223c 2\u20133 IGM opacity, and Gwen Rudie and Milan Bogosavljevi\u0107 for their assistance in the collection of some of the data used in this paper. D.B.N., A.E.S., and K.A.K acknowledge support from the David and Lucile Packard Foundation. C.C.S. acknowledges additional support from the John D. and Catherine T. MacArthur Foundation, the Peter and Patricia Gruber Foundation, and NSF grants AST-0606912 and AST-0908805. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible.\n\nPublished - 0004-637X_765_1_47.pdf
", "abstract": "We investigate the contribution of star-forming galaxies to the ionizing background at z ~ 3, building on previous work based on narrowband (NB3640) imaging in the SSA22a field. We use new Keck/LRIS spectra of Lyman break galaxies (LBGs) and narrowband-selected Ly\u03b1 emitters (LAEs) to measure redshifts for 16 LBGs and 87 LAEs at z > 3.055, such that our NB3640 imaging probes the Lyman-continuum (LyC) region. When we include the existing set of spectroscopically confirmed LBGs, our total sample with z > 3.055 consists of 41 LBGs and 91 LAEs, of which 9 LBGs and 20 LAEs are detected in our NB3640 image. With our combined imaging and spectroscopic data sets, we critically investigate the origin of NB3640 emission for detected LBGs and LAEs. We remove from our samples three LBGs and three LAEs with spectroscopic evidence of contamination of their NB3640 flux by foreground galaxies and statistically model the effects of additional, unidentified foreground contaminants. The resulting contamination and LyC-detection rates, respectively, are 62% \u00b1 13% and 8% \u00b1 3% for our LBG sample, and 47% \u00b1 10% and 12% \u00b1 2% for our LAE sample. The corresponding ratios of non-ionizing UV to LyC flux density, corrected for intergalactic medium (IGM) attenuation, are 18.0^(+34.8)_(\u20137.4) for LBGs and 3.7^(+2.5)_(\u20131.1) for LAEs. We use these ratios to estimate the total contribution of star-forming galaxies to the ionizing background and the hydrogen photoionization rate in the IGM, finding values larger than, but consistent with, those measured in the Ly\u03b1 forest. Finally, the measured UV to LyC flux-density ratios imply model-dependent LyC escape fractions of f^(LyC)_(esc) ~ 5%-7% for our LBG sample and f^(LyC)_(esc) ~ 10%-30% for our fainter LAE sample.", "date": "2013-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "765", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 47", "id_number": "CaltechAUTHORS:20130402-103239789", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130402-103239789", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "David and Lucile Packard Foundation" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/765/1/47", "primary_object": { "basename": "0004-637X_765_1_47.pdf", "url": "https://authors.library.caltech.edu/records/n8rpc-eb272/files/0004-637X_765_1_47.pdf" }, "resource_type": "article", "pub_year": "2013", "author_list": "Nestor, Daniel B.; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/h3jx5-r6604", "eprint_id": 38391, "eprint_status": "archive", "datestamp": "2023-08-19 18:52:16", "lastmod": "2023-10-23 20:07:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Wallace L. W. Sargent (1935\u20132012)", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2013 The Astronomical Society of the Pacific. \n\nReceived 2013 January 10; accepted 2013 January 14; published 2013 February 12.\n\nPublished - 669931.pdf
", "abstract": "By any measure, Professor Wallace L. W. Sargent (known to colleagues and friends as \"Wal\") was one of the most influential and consistently productive astronomers of the last 50 years; he authored or coauthored more than 320 refereed journal articles, which have received more than 25,000 citations. He never rested on past laurels\u201465 of his papers (with >5000 citations) have appeared since the year 2000. Wal remained active as a teacher and researcher until just weeks before the end of his life (he officially retired from the Caltech faculty on 2012 October 1). His impact on the field of astrophysics was remarkably broad as well as seminal; among many other awards, he was elected in 1981 as a Fellow of the Royal Society (U.K.) and as a member of the National Academy of Sciences in 2005, his first year of eligibility after becoming a naturalized U.S. citizen.", "date": "2013-03", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "125", "number": "925", "publisher": "Astronomical Society of the Pacific", "pagerange": "225-226", "id_number": "CaltechAUTHORS:20130509-112648069", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130509-112648069", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1086/669931", "primary_object": { "basename": "669931.pdf", "url": "https://authors.library.caltech.edu/records/h3jx5-r6604/files/669931.pdf" }, "resource_type": "article", "pub_year": "2013", "author_list": "Steidel, Charles C." }, { "id": "https://authors.library.caltech.edu/records/xg01k-7fd97", "eprint_id": 36236, "eprint_status": "archive", "datestamp": "2023-08-22 07:58:49", "lastmod": "2023-10-20 22:54:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kacprzak-G-G", "name": { "family": "Kacprzak", "given": "Glenn G." } }, { "id": "Churchill-C-W", "name": { "family": "Churchill", "given": "Christopher W." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Spitler-L-R", "name": { "family": "Spitler", "given": "Lee R." } }, { "id": "Holtzman-J-A", "name": { "family": "Holtzman", "given": "Jon A." } } ] }, "title": "Discovery of multiphase cold accretion in a massive galaxy at z = 0.7", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM; quasars: absorption lines", "note": "\u00a9 2012 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2012 RAS. \n\nAccepted 2012 August 15. Received 2012 August 15; in original form 2012 February 28. Article first published online: 7 Dec. 2012. \n\nWe thank Nicolas Bouch\u00b4e for his useful comments, models and for carefully reading this paper. We also thank the anonymous referee for carefully reading the paper and for providing insightful comments. CWC was partially supported through grant HST-GO-11667.01-A provided by NASA via the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. CWC thanks GGK, and Michael T. Murphy, and Swinburne Faculty Research Grants for providing funding for a visit to Swinburne University of Technology. This work is based on observations made with the NASA/ESA Hubble Space Telescope (PID 11667) and those obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This work is also based on observations obtained with the Apache Point Observatory 3.5-m telescope, which is owned and operated by the Astrophysical Research Consortium. Observations were also made with the NASA/ESA Hubble Space Telescope or obtained from the data archive at the Space Telescope Institute.\n\nPublished - mnr21945.pdf
", "abstract": "We present detailed photo+collisional ionization models and kinematic models of the multiphase absorbing gas, detected within the Hubble Space Telescope(HST)/COS, HST/STIS and Keck/HIRES spectra of the background quasar TON 153 at 104\u2009kpc along the projected minor axis of a star-forming spiral galaxy (z = 0.6610). Complementary g\u2032r\u2032i\u2032Ks photometry and stellar population models indicate that the host galaxy is dominated by an \u223c4 Gyr stellar population with slightly greater than solar metallicity and has an estimated log\u2009M* = 11 and a log\u2009M_vir = 13. Photoionization models of the low-ionization absorption (Mg\u2009i, Si\u2009ii, Mg\u2009ii and C\u2009iii), which trace the bulk of hydrogen, constrain the multicomponent gas to be cold (log T = 3.8\u20135.2) and metal poor (inline image). A lagging halo model reproduces the low-ionization absorption kinematics, suggesting gas coupled to the disc angular momentum, consistent with cold accretion mode material in simulations. The C\u2009iv and O\u2009vi absorption is best modelled in a separate collisionally ionized metal-poor (\u22122.50 \u2264 [X/H] \u2264 \u22121.93) warm phase with log T = 5.3. Although their kinematics are consistent with a wind model, given the 2\u20132.5 dex difference between the galaxy stellar metallicity and the absorption metallicity we indicate that the gas cannot arise from galactic winds. We discuss and conclude that although the quasar sightline passes along the galaxy minor axis at a projected distance of 0.3 virial radii, well inside its virial shock radius, the combination of the relative kinematics, temperatures and relative metallicities indicates that the multiphase absorbing gas arises from cold accretion around this massive galaxy. Our results appear to contradict recent interpretations that absorption probing the projected minor axis of a galaxy is sampling winds.", "date": "2012-12-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "427", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3029-3043", "id_number": "CaltechAUTHORS:20130108-115006064", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130108-115006064", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-11667.01-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "W. M. Keck Foundation" } ] }, "primary_object": { "basename": "mnr21945.pdf", "url": "https://authors.library.caltech.edu/records/xg01k-7fd97/files/mnr21945.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Kacprzak, Glenn G.; Churchill, Christopher W.; et el." }, { "id": "https://authors.library.caltech.edu/records/g4tp2-r4773", "eprint_id": 36029, "eprint_status": "archive", "datestamp": "2023-08-22 07:46:00", "lastmod": "2023-10-20 22:09:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Churchill-C-W", "name": { "family": "Churchill", "given": "Christopher W." } }, { "id": "Kacprzak-G-G", "name": { "family": "Kacprzak", "given": "Glenn G." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Spitler-L-R", "name": { "family": "Spitler", "given": "Lee R." } }, { "id": "Holtzman-J-A", "name": { "family": "Holtzman", "given": "Jon" } }, { "id": "Nielsen-N-M", "name": { "family": "Nielsen", "given": "Nikole M." }, "orcid": "0000-0003-2377-8352" }, { "id": "Trujillo-Gomez-S", "name": { "family": "Trujillo-Gomez", "given": "Sebastian" } } ] }, "title": "Quenched Cold Accretion of a Large-scale Metal-poor Filament due to Virial Shocking in the Halo of a Massive z = 0.7 Galaxy", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: halos; quasars: absorption lines", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2012 April 17; accepted 2012 August 16; published 2012 November 6. \n\nThe anonymous referee is gratefully acknowledged for helpful comments to clarify points, and for carefully reading this manuscript. We thank Daniel Ceverino for several stimulating and informative discussions during his visit to New Mexico State University and for helpful comments on an early draft of this paper, Kyle Stewart for several informative email exchanges with regard to halo abundance matching methods, and Avishai Dekel for helpful comments on cold streams penetrating the virialized shock-heated medium in massive halos. This research was primarily support through grant HST-GO-11667.01-A provided by NASA via the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy (AURA) under NASA contract NAS 5-26555. C.W.C. thanks G.G.K., and Michael T. Murphy, and Swinburne Faculty Research Grants for providing funding for a visit to Swinburne University of Technology. Some observations are obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium (ARC). Additional data were obtained at Kitt Peak National Optical Astronomy Observatory, which is operated by AURA under cooperative agreement with the National Science Foundation. Some data presented herein were obtained at the W. M. Keck observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. 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. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This research has also made use of the SIMBAD database, operated at Centre de Donn\u00e9es, Strasbourg, France. \n\nFacilities: HST (WFPC2, STIS, COS), Keck:I (HIRES, LRIS), ARC (3.5-m Telescope), Mayall (IRIM)\n\nPublished - 0004-637X_760_1_68.pdf
", "abstract": "Using HST/COS/STIS and HIRES/Keck high-resolution spectra, we have studied a remarkable H I absorbing complex at z = 0.672 toward the quasar Q1317+277. The H I absorption has a velocity spread of \u0394v = 1600 km s^(\u20131), comprises 21 Voigt profile components, and resides at an impact parameter of D = 58 kpc from a bright, high-mass (log M_(vir)/M_\u2609 \u2243 13.7) elliptical galaxy that is deduced to have a 6 Gyr old, solar metallicity stellar population. Ionization models suggest the majority of the structure is cold gas surrounding a shock-heated cloud that is kinematically adjacent to a multi-phase group of clouds with detected C III, C IV, and O VI absorption, suggestive of a conductive interface near the shock. The deduced metallicities are consistent with the moderate in situ enrichment relative to the levels observed in the z ~ 3 Ly\u03b1 forest. We interpret the H I complex as a metal-poor filamentary structure being shock heated as it accretes into the halo of the galaxy. The data support the scenario of an early formation period (z > 4) in which the galaxy was presumably fed by cold-mode gas accretion that was later quenched via virial shocking by the hot halo such that, by intermediate redshift, the cold filamentary accreting gas is continuing to be disrupted by shock heating. Thus, continued filamentary accretion is being mixed into the hot halo, indicating that the star formation of the galaxy will likely remain quenched. To date, the galaxy and the H I absorption complex provide some of the most compelling observational data supporting the theoretical picture in which accretion is virial shocked in the hot coronal halos of high-mass galaxies.", "date": "2012-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "760", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 68", "id_number": "CaltechAUTHORS:20121218-102207465", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121218-102207465", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-11667.01-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Swinburne University of Technology" }, { "agency": "NSF" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/760/1/68", "primary_object": { "basename": "0004-637X_760_1_68.pdf", "url": "https://authors.library.caltech.edu/records/g4tp2-r4773/files/0004-637X_760_1_68.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Churchill, Christopher W.; Kacprzak, Glenn G.; et el." }, { "id": "https://authors.library.caltech.edu/records/4mb1e-3ev53", "eprint_id": 36044, "eprint_status": "archive", "datestamp": "2023-08-22 07:46:04", "lastmod": "2023-10-20 22:10:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hainline-K-N", "name": { "family": "Hainline", "given": "Kevin N." }, "orcid": "0000-0003-4565-8239" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Greene-J-E", "name": { "family": "Greene", "given": "Jenny E." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" } ] }, "title": "Stellar Populations of Ultraviolet-selected Active Galactic Nuclei Host Galaxies at z ~ 2\u20133", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: evolution; galaxies: high-redshift; galaxies: nuclei", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2012 June 14; accepted 2012 September 24; published 2012 November 6. \n\nBased, in part, on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. \n\nThe authors wish to thank Roberto Assef, James Aird, and Alison Coil for helpful discussions. A.E.S. acknowledges support from the David and Lucile Packard Foundation. C.C.S. acknowledges support from the John D. and Catherine T. MacArthur Foundation and the Peter and Patricia Gruber Foundation. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible.\n\nPublished - 0004-637X_760_1_74.pdf
", "abstract": "We use stellar population synthesis modeling to analyze the host-galaxy properties of a sample of 33 UV-selected, narrow-lined active galactic nuclei (AGNs) at z ~ 2-3. In order to quantify the contribution of AGN emission to host galaxy broadband spectral energy distributions (SEDs), we use the subsample of 11 AGNs with photometric coverage spanning from rest-frame UV through near-IR wavelengths. Modeling the SEDs of these objects with a linear combination of stellar population and AGN templates, we infer the effect of the AGN on derived stellar population parameters. We also estimate the typical bias in derived stellar populations for AGNs lacking rest-frame near-IR wavelength coverage, and develop a method for inferring the true host-galaxy properties. We compare AGN host-galaxy properties to those of a sample of UV-selected, star-forming non-AGNs in the same redshift range, including a subsample carefully matched in stellar mass. Although the AGNs have higher masses and star-formation rates than the full non-active sample, their stellar population properties are consistent with those of the mass-selected sample, suggesting that the presence of an AGN is not connected with the cessation of star formation activity in star-forming galaxies at z ~ 2-3. We suggest that a correlation between M_(BH) and galaxy stellar mass is already in place at this epoch. Assuming a roughly constant Eddington ratio for AGNs at all stellar masses, we are unable to detect the AGNs in low-mass galaxies because they are simply too faint.", "date": "2012-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "760", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 74", "id_number": "CaltechAUTHORS:20121219-095633258", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121219-095633258", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "David and Lucile Packard Foundation" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/760/1/74", "primary_object": { "basename": "0004-637X_760_1_74.pdf", "url": "https://authors.library.caltech.edu/records/4mb1e-3ev53/files/0004-637X_760_1_74.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Hainline, Kevin N.; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/15y0z-r9n70", "eprint_id": 36011, "eprint_status": "archive", "datestamp": "2023-08-22 07:42:25", "lastmod": "2023-10-20 22:07:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Nagy-S-R", "name": { "family": "Nagy", "given": "Sarah R." } }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" } ] }, "title": "A HST/WFC3-IR Morphological Survey of Galaxies at z = 1.5-3.6. II. The Relation between Morphology and Gas-phase Kinematics", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: fundamental parameters; galaxies: high-redshift; galaxies: structure", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2012 June 28; accepted 2012 September 11; published 2012 October 15. \n\nBased in part on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. \n\nD.R.L., C.C.S., and S.R.N. have been supported by grant GO-11694 from 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. C.C.S. has been supported by the US National Science Foundation through grants AST-0606912 and AST-0908805. A.E.S. acknowledges support from the David and Lucile Packard Foundation. Finally, we extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests.\n\nPublished - 0004-637X_759_1_29.pdf
", "abstract": "We analyze rest-frame optical morphologies and gas-phase kinematics as traced by rest-frame far-UV and optical spectra for a sample of 204 star-forming galaxies in the redshift range z ~ 2-3 drawn from the Keck Baryonic Structure Survey. We find that spectroscopic properties and gas-phase kinematics are closely linked to morphology: compact galaxies with semimajor axis radii r \u227e 2 kpc are substantially more likely than their larger counterparts to exhibit Ly\u03b1 in emission. Although Ly\u03b1 emission strength varies widely within galaxies of a given morphological type, all but one of 19 galaxies with Ly\u03b1 equivalent width W_(Ly\u03b1) > 20 \u00c5 have compact and/or multiple-component morphologies with r \u2264 2.5 kpc. The velocity structure of absorption lines in the galactic continuum spectra also varies as a function of morphology. Galaxies of all morphological types drive similarly strong outflows (as traced by the blue wing of interstellar absorption line features), but the outflows of larger galaxies are less highly ionized and exhibit larger optical depth at the systemic redshift that may correspond to a decreasing efficiency of feedback in evacuating gas from the galaxy. This v ~ 0 km s^(\u20131) gas is responsible both for shifting the mean absorption line redshift and attenuating W_(Ly\u03b1) (via a longer resonant scattering path) in galaxies with larger rest-optical half-light radii. In contrast to galaxies at lower redshifts, there is no evidence for a correlation between outflow velocity and inclination, suggesting that outflows from these puffy and irregular systems may be poorly collimated. Our observations are broadly consistent with theoretical models of inside-out growth of galaxies in the young universe, in which typical z ~ 2-3 star-forming galaxies are predominantly unstable, dispersion-dominated, systems fueled by rapid gas accretion that later form extended rotationally supported disks when stabilized by a sufficiently massive stellar component.", "date": "2012-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "759", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 29", "id_number": "CaltechAUTHORS:20121217-112707609", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121217-112707609", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO-11694" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/759/1/29", "primary_object": { "basename": "0004-637X_759_1_29.pdf", "url": "https://authors.library.caltech.edu/records/15y0z-r9n70/files/0004-637X_759_1_29.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Law, David R.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/1t6vt-kve74", "eprint_id": 34187, "eprint_status": "archive", "datestamp": "2023-08-22 07:06:09", "lastmod": "2023-10-19 14:43:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" } ] }, "title": "The Temperature-Density Relation in the Intergalactic Medium at RedshiftPublished - 2041-8205_757_2_L30.pdf
Submitted - 1209.0005v1.pdf
", "abstract": "We present new measurements of the temperature-density (T-\u03c1) relation for neutral hydrogen in the 2.0 < z < 2.8 intergalactic medium (IGM) using a sample of ~6000 individual H I absorbers fitted with Voigt profiles constrained in all cases by multiple Lyman series transitions. We find model-independent evidence for a positive correlation between the column density of H I (N_(HI)) and the minimum observed velocity width of absorbers (b_(min)). With minimal interpretation, this implies that the T-\u03c1 relation in the IGM is not \"inverted,\" contrary to many recent studies. Fitting b_(min) as a function of N_(HI) results in line-width-column-density dependence of the form b_(min) = b_0(N_(HI)/N_(HI,0))^(\u0393\u20131) with a minimum line width at mean density (\u03c1/\u03c1 = 1, N_(HI,0) = 10^(13.6) cm^(\u20132)) of b_0 = 17.9 \u00b1 0.2 km s^(\u20131) and a power-law index of (\u0393 \u2013 1) = 0.15 \u00b1 0.02. Using analytic arguments, these measurements imply an \"equation of state\" for the IGM at (z) = 2.4 of the form T=T_0 (\u03c1/\u03c1)^(y-1) with a temperature at mean density of T_0 = [1.94 \u00b1 0.05] \u00d7 10^4 K and a power-law index (\u03b3 \u2013 1) = 0.46 \u00b1 0.05.", "date": "2012-10-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "757", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L30-L35", "id_number": "CaltechAUTHORS:20120918-142739382", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120918-142739382", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Peter and Patricia Gruber Foundation" } ] }, "doi": "10.1088/2041-8205/757/2/L30", "primary_object": { "basename": "1209.0005v1.pdf", "url": "https://authors.library.caltech.edu/records/1t6vt-kve74/files/1209.0005v1.pdf" }, "related_objects": [ { "basename": "2041-8205_757_2_L30.pdf", "url": "https://authors.library.caltech.edu/records/1t6vt-kve74/files/2041-8205_757_2_L30.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Rudie, Gwen C.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/gcz6e-3cf44", "eprint_id": 32991, "eprint_status": "archive", "datestamp": "2023-08-22 06:12:46", "lastmod": "2023-10-18 17:59:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" } ] }, "title": "The Characteristic Star Formation Histories of Galaxies at Redshifts z ~ 2-7", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: star formation", "note": "\u00a9 2012 The American Astronomical Society. \n\nReceived 2012 February 12; accepted 2012 April 27; published 2012 July 2. \n\nN.A.R. thanks Rychard Bouwens, Romeel Dav\u00e9, Claude-Andr\u00e9 Faucher-Gigu\u00e8re, and Kristian Finlator for useful discussions and comments. We acknowledge the referee for useful suggestions that improved the clarity of the manuscript. We thank the staff of the Keck and Palomar Observatories for their help in obtaining the data presented here. Support for N.A.R. was provided by NASA through Hubble Fellowship Grant HST-HF-01223.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Additional support has been provided by research funding for the Spitzer Space Telescope Legacy Science Program, provided by NASA through contracts 1224666 and 1287778, issued by the Jet Propulsion Laboratory, California Institute of Technology. N.A.R. also acknowledges the Beatrice Tinsley Visiting Scholar program administered by the Astronomy Department at the University of Texas at Austin, where part of this research was conducted as well as the visitors program at the Institute of Astronomy in Cambridge, UK. C.C.S. has been supported by NSF Grants AST-0606912 and AST-0908805, with additional support from the John D. and Catherine T. MacArthur Foundation and the Peter and Patricia Gruber Foundation. Based, in part, on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and made possible by the generous financial support of the W. M. Keck Foundation.\n\nPublished - Reddy2012p19053Astrophys_J.pdf
", "abstract": "A large sample of spectroscopically confirmed star-forming galaxies at redshifts 1.4 \u2264 z_(spec) \u2264 3.7, with\ncomplementary imaging in the near- and mid-IR from the ground and from the Hubble Space Telescope and\nSpitzer Space Telescope, is used to infer the average star formation histories (SFHs) of typical galaxies from z \u223c 2\nto 7. For a subset of 302 galaxies at 1.5 \u2264 z_(spec) < 2.6, we perform a detailed comparison of star formation rates\n(SFRs) determined from spectral energy distribution (SED) modeling (SFRs[SED]) and those calculated from deep\nKeck UV and Spitzer/MIPS 24\u03bcm imaging (SFRs[IR+UV]). Exponentially declining SFHs yield SFRs[SED]\nthat are 5\u201310 times lower on average than SFRs[IR+UV], indicating that declining SFHs may not be accurate for\ntypical galaxies at z \u2273 2. The SFRs of z \u223c 2\u20133 galaxies are directly proportional to their stellar masses (M_*),\nwith unity slope\u2014a result that is confirmed with Spitzer/IRAC stacks of 1179 UV-faint (R > 25.5) galaxies\u2014for\nM_* \u2273 5 \u00d7 10^8M_\u2299 and SFRs \u2273 2M_\u2299 yr^(\u22121). We interpret this result in the context of several systematic biases that\ncan affect determinations of the SFR\u2013M_* relation. The average specific SFRs at z \u223c 2\u20133 are remarkably similar\nwithin a factor of two to those measured at z \u2273 4, implying that the average SFH is one where SFRs increase with\ntime. A consequence of these rising SFHs is that (1) a substantial fraction of UV-bright z \u223c 2\u20133 galaxies had faint\nsub-L* progenitors at z \u2273 4; and (2) gas masses must increase with time from z = 2 to 7, over which time the\nnet cold gas accretion rate\u2014as inferred from the specific SFR and the Kennicutt\u2013Schmidt relation\u2014is \u223c2\u20133 times\nlarger than the SFR. However, if we evolve to higher redshift the SFHs and masses of the halos that are expected\nto host L* galaxies at z \u223c 2, then we find that \u227e10% of the baryons accreted onto typical halos at z \u2273 4 actually\ncontribute to star formation at those epochs. These results highlight the relative inefficiency of star formation even\nat early cosmic times when galaxies were first assembling.", "date": "2012-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "754", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 25", "id_number": "CaltechAUTHORS:20120807-145459722", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120807-145459722", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-01223.01" }, { "agency": "NASA", "grant_number": "1224666" }, { "agency": "NASA", "grant_number": "1287778" }, { "agency": "University of Texas at Austin" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/754/1/25", "primary_object": { "basename": "Reddy2012p19053Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/gcz6e-3cf44/files/Reddy2012p19053Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Reddy, Naveen A.; Pettini, Max; et el." }, { "id": "https://authors.library.caltech.edu/records/90qry-bx065", "eprint_id": 33106, "eprint_status": "archive", "datestamp": "2023-08-19 11:44:28", "lastmod": "2023-10-18 18:48:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Christensen-C-R", "name": { "family": "Christensen", "given": "Charlotte R." } }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" } ] }, "title": "High velocity dispersion in a rare grand-design spiral galaxy at redshift z = 2.18", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2012 Macmillan Publishers Limited. \n\nReceived 02 January 2012. Accepted 22 May 2012. Published online 18 July 2012. \n\nD.R.L and C.C.S have been supported by grant GO-11694 from 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. A.E.S acknowledges support from the David and Lucile Packard Foundation. C.R.C acknowledges support from the US National Science Foundation through grant AST-1009452. D.R.L appreciates discussions with J. Taylor, R. Abraham, J. Dubinski, F. Governato and A. Brooks, and thanks M. Peeples for help in obtaining the Keck/OSIRIS data. \n\nAuthor Contributions: D.R.L. performed the morphological analysis of the Hubble Space Telescope data and wrote the main manuscript text. The Keck/OSIRIS data were obtained by D.R.L. and A.E.S., and analysed by D.R.L. with extensive input from A.E.S. and C.C.S.. N.A.R. provided the Keck/LRIS spectra, Spitzer/MIPS photometry and stellar population modelling code, C.R.C. contributed the hydrodynamic galaxy simulations, and D.K.E. provided the Keck/NIRSPEC spectra. All authors reviewed, discussed and commented on the manuscript. \n\nThe authors declare no competing financial interests.\n\nSupplemental Material - nature11256-s1.pdf
", "abstract": "Although grand-design spiral galaxies are relatively common in the local Universe, only one has been spectroscopically confirmed to lie at redshift z\u2009>\u20092 (HDFX 28; z = 2.011); and it may prove to be a major merger that simply resembles a spiral in projection. The rarity of spirals has been explained as a result of disks being dynamically 'hot' at z\u2009>\u20092 (refs 2-5), which may instead favour the formation of commonly observed clumpy structures. Alternatively, current instrumentation may simply not be sensitive enough to detect spiral structures comparable to those in the modern Universe. At z\u2009<\u20092, the velocity dispersion of disks decreases, and spiral galaxies are more numerous by z\u2009\u2248\u20091 (refs 7, 13-15). Here we report observations of the grand-design spiral galaxy Q2343-BX442 at z = 2.18. Spectroscopy of ionized gas shows that the disk is dynamically hot, implying an uncertain origin for the spiral structure. The kinematics of the galaxy are consistent with a thick disk undergoing a minor merger, which can drive the formation of short-lived spiral structure. A duty cycle of <100\u2009Myr for such tidally induced spiral structure in a hot massive disk is consistent with its rarity.", "date": "2012-07-19", "date_type": "published", "publication": "Nature", "volume": "487", "number": "7407", "publisher": "Nature Publishing Group", "pagerange": "338-340", "id_number": "CaltechAUTHORS:20120810-145208297", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120810-145208297", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO-11694" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "NSF", "grant_number": "AST-1009452" } ] }, "doi": "10.1038/nature11256", "primary_object": { "basename": "nature11256-s1.pdf", "url": "https://authors.library.caltech.edu/records/90qry-bx065/files/nature11256-s1.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Law, David R.; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/gmfpk-prr22", "eprint_id": 32462, "eprint_status": "archive", "datestamp": "2023-08-22 05:54:32", "lastmod": "2023-10-18 14:26:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "The Halo Masses and Galaxy Environments of Hyperluminous QSOs at z \u2243 2.7 in the Keck Baryonic Structure Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; large-scale structure of universe; quasars: general", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2011 October 14; accepted 2012 April 8; published 2012 May 23. \n\nWe thank our collaborators for their important contributions to the Keck Baryonic Structure Survey over the course of many years: M. Bogosavljevic, D. Erb, D. R. Law, M. Pettini, O. Rakic, N. Reddy, G. Rudie, and A. Shapley. We also thank C. Bilinski for his help reducing some of the TripleSpec QSO spectra. R.F.T. also thanks B. Siana, N. Konidaris, A. Benson, C. Hirata, R. Quadri, and J. R. Gauthier for many useful discussions. We are grateful for the many useful comments we received from an anonymous referee, particularly in regard to the estimation of uncertainties in the correlation function parameters. The MultiDark Database used in this paper and the web application providing online access to it were constructed as part of the activities of the German Astrophysical Virtual Observatory as result of a collaboration between the Leibniz-Institute for Astrophysics Potsdam (AIP) and the Spanish MultiDark Consolider Project CSD2009-00064. The MultiDark simulation was run on NASA's Pleiades supercomputer at the NASA Ames Research Center. The Millennium Simulation databases used in this paper and the web application providing online access to them were constructed as part of the activities of the German Astrophysical Virtual Observatory. We are indebted to the staff of the W.M. Keck Observatory who keep the instruments and telescopes running effectively. We also wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. This work has been supported by the US National Science Foundation through grants AST-0606912 and AST-0908805. C.C.S. acknowledges additional support from the John D. and Catherine T. MacArthur Foundation and the Peter and Patricia Gruber Foundation. \n\nBased on data obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W.M. Keck Foundation.\n\nPublished - Trainor2012p18833Astrophys_J.pdf
", "abstract": "We present an analysis of the galaxy distribution surrounding 15 of the most luminous (\u227310^(14) L_\u2609; M_1450 \u2243 \u201330) QSOs in the sky with z \u2243 2.7. Our data are drawn from the Keck Baryonic Structure Survey, which has been optimized to examine the small-scale interplay between galaxies and the intergalactic medium during the peak of the galaxy formation era at z ~ 2-3. In this work, we use the positions and spectroscopic redshifts of 1558 galaxies that lie within ~3' (4.2 h^(\u20131) comoving Mpc; cMpc) of the hyperluminous QSO (HLQSO) sight line in 1 of 15 independent survey fields, together with new measurements of the HLQSO systemic redshifts. By combining the spatial and redshift distributions, we measure the galaxy-HLQSO cross-correlation function, the galaxy-galaxy autocorrelation function, and the characteristic scale of galaxy overdensities surrounding the sites of exceedingly rare, extremely rapid, black hole accretion. On average, the HLQSOs lie within significant galaxy overdensities, characterized by a velocity dispersion \u03c3_v \u2243 200 km s^(\u20131) and a transverse angular scale of ~25\" (~200 physical kpc). We argue that such scales are expected for small groups with log (M _(h_/M_\u2609) \u2243 13. The galaxy-HLQSO cross-correlation function has a best-fit correlation length r^(GQ)_0 = (7.3 \u00b1 1.3) h^(\u20131) cMpc, while the galaxy autocorrelation measured from the spectroscopic galaxy sample in the same fields has r^(GG)_0 = (6.0 \u00b1 0.5) h^(\u20131) cMpc. Based on a comparison with simulations evaluated at z ~ 2.6, these values imply that a typical galaxy lives in a host halo with log (M_(h)/M_\u2609) = 11.9 \u00b1 0.1, while HLQSOs inhabit host halos of log (M_(h)/M_\u2609) = 12.3 \u00b1 0.5. In spite of the extremely large black hole masses implied by their observed luminosities [log (M_(BH)/M_\u2609) \u2273 9.7], it appears that HLQSOs do not require environments very different from their much less luminous QSO counterparts. Evidently, the exceedingly low space density of HLQSOs (\u2272 10^(\u20139) cMpc^(\u20133)) results from a one-in-a-million event on scales \u226a1 Mpc, and not from being hosted by rare dark matter halos.", "date": "2012-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "752", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 39", "id_number": "CaltechAUTHORS:20120716-102035050", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120716-102035050", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/752/1/39", "primary_object": { "basename": "Trainor2012p18833Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/gmfpk-prr22/files/Trainor2012p18833Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Trainor, Ryan F. and Steidel, Charles C." }, { "id": "https://authors.library.caltech.edu/records/a4n9w-fzz83", "eprint_id": 31992, "eprint_status": "archive", "datestamp": "2023-08-22 05:53:03", "lastmod": "2023-10-17 21:45:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rakic-O", "name": { "family": "Rakic", "given": "Olivera" } }, { "id": "Schaye-J", "name": { "family": "Schaye", "given": "Joop" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" } ] }, "title": "Neutral Hydrogen Optical Depth near Star-forming Galaxies at z \u2248 2.4 in the Keck Baryonic Structure Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation; galaxies: halos; galaxies: high-redshift; intergalactic medium; quasars: absorption lines", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2011 September 20; accepted 2012 March 22; published 2012 May 9. \n\nBased on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. We are very grateful to Milan Bogosavljevi\u0107 , Alice Shapley, Dawn Erb, Naveen Reddy,Max Pettini, Ryan Trainor, and David Law for their invaluable contributions to the Keck Baryonic Structure Survey, without which the results presented here would not have been possible. We also thank Ryan Cooke for his help with the continuum fitting of QSO spectra, and we thank the anonymous referee for a careful reading of the manuscript and for valuable suggestions. This work was supported by an NWO VIDI grant (O.R., J.S.), by the U.S. National Science Foundation through grants AST-0606912 and AST-0908805, and by the David and Lucile Packard Foundation (C.C.S.). C.C.S. acknowledges additional support from the John D. and Catherine T. MacArthur Foundation and the Peter and Patricia Gruber Foundation. We thank the W.M. Keck Observatory staff for their assistance with the observations. We also thank the Hawaiian people, as without their hospitality the observations presented here would not have been possible.\n\nPublished - Rakic2012p18530Astrophys_J.pdf
", "abstract": "We study the interface between galaxies and the intergalactic medium by measuring the absorption by neutral hydrogen in the vicinity of star-forming galaxies at z \u2248 2.4. Our sample consists of 679 rest-frame UV-selected galaxies with spectroscopic redshifts that have impact parameters <2 (proper) Mpc to the line of sight of one of the 15 bright, background QSOs and that fall within the redshift range of its Ly\u03b1 forest. We present the first two-dimensional maps of the absorption around galaxies, plotting the median Ly\u03b1 pixel optical depth as a function of transverse and line-of-sight separation from galaxies. The Ly\u03b1 optical depths are measured using an automatic algorithm that takes advantage of all available Lyman series lines. The median optical depth, and hence the median density of atomic hydrogen, drops by more than an order of magnitude around 100 kpc, which is similar to the virial radius of the halos thought to host the galaxies. The median remains enhanced, at the >3\u03c3 level, out to at least 2.8 Mpc (i.e., >9 comoving Mpc), but the scatter at a given distance is large compared with the median excess optical depth, suggesting that the gas is clumpy. Within 100 (200) kpc, and over \u00b1165 km s^(\u20131), the covering fraction of gas with Ly\u03b1 optical depth greater than unity is 100^(+0)_(\u201332%) (66% \u00b1 16%). Absorbers with \u03c4_(Ly\u03b1) > 0.1 are typically closer to galaxies than random. The mean galaxy overdensity around absorbers increases with the optical depth and also as the length scale over which the galaxy overdensity is evaluated is decreased. Absorbers with \u03c4_(Ly\u03b1) ~ 1 reside in regions where the galaxy number density is close to the cosmic mean on scales \u22650.25 Mpc. We clearly detect two types of redshift space anisotropies. On scales <200 km s^(\u20131), or <1 Mpc, the absorption is stronger along the line of sight than in the transverse direction. This \"finger of God\" effect may be due to redshift errors, but is probably dominated by gas motions within or very close to the halos. On the other hand, on scales of 1.4-2.0 Mpc the absorption is compressed along the line of sight (with >3\u03c3 significance), an effect that we attribute to large-scale infall (i.e., the Kaiser effect).", "date": "2012-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "751", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 94", "id_number": "CaltechAUTHORS:20120620-141602544", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120620-141602544", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/751/2/94", "primary_object": { "basename": "Rakic2012p18530Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/a4n9w-fzz83/files/Rakic2012p18530Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Rakic, Olivera; Schaye, Joop; et el." }, { "id": "https://authors.library.caltech.edu/records/kcq4t-zvt08", "eprint_id": 32365, "eprint_status": "archive", "datestamp": "2023-08-22 05:49:08", "lastmod": "2023-10-17 23:21:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brammer-G-B", "name": { "family": "Brammer", "given": "Gabriel B." }, "orcid": "0000-0003-2680-005X" }, { "id": "van-Dokkum-P-G", "name": { "family": "van Dokkum", "given": "Pieter G." }, "orcid": "0000-0002-8282-9888" }, { "id": "Franx-M", "name": { "family": "Franx", "given": "Marijn" }, "orcid": "0000-0002-8871-3026" }, { "id": "Fumagalli-M", "name": { "family": "Fumagalli", "given": "Mattia" }, "orcid": "0000-0001-6676-3842" }, { "id": "Patel-S-G", "name": { "family": "Patel", "given": "Shannon" } }, { "id": "Rix-H-W", "name": { "family": "Rix", "given": "Hans-Walter" }, "orcid": "0000-0003-4996-9069" }, { "id": "Skelton-R-E", "name": { "family": "Skelton", "given": "Rosalind E." } }, { "id": "Kriek-M", "name": { "family": "Kriek", "given": "Mariska" }, "orcid": "0000-0002-7613-9872" }, { "id": "Nelson-E-J", "name": { "family": "Nelson", "given": "Erica" }, "orcid": "0000-0002-7524-374X" }, { "id": "Schmidt-K-B", "name": { "family": "Schmidt", "given": "Kasper B." } }, { "id": "Bezanson-R", "name": { "family": "Bezanson", "given": "Rachel" } }, { "id": "da-Cunha-E", "name": { "family": "da Cunha", "given": "Elisabete" }, "orcid": "0000-0001-9759-4797" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Fan-Xiaohui", "name": { "family": "Fan", "given": "Xiaohui" }, "orcid": "0000-0003-3310-0131" }, { "id": "F\u00f6rster-Schreiber-N-M", "name": { "family": "F\u00f6rster Schreiber", "given": "Natascha" } }, { "id": "Illingworth-G-D", "name": { "family": "Illingworth", "given": "Garth D." }, "orcid": "0000-0002-6668-2011" }, { "id": "Labb\u00e9-I", "name": { "family": "Labb\u00e9", "given": "Ivo" }, "orcid": "0000-0002-2057-5376" }, { "id": "Leja-J", "name": { "family": "Leja", "given": "Joel" }, "orcid": "0000-0001-6755-1315" }, { "id": "Lundgren-B", "name": { "family": "Lundgren", "given": "Britt" } }, { "id": "Magee-D-K", "name": { "family": "Magee", "given": "Dan" } }, { "id": "Marchesini-D", "name": { "family": "Marchesini", "given": "Danilo" }, "orcid": "0000-0001-9002-3502" }, { "id": "McCarthy-P-J", "name": { "family": "McCarthy", "given": "Patrick" } }, { "id": "Momcheva-I-G", "name": { "family": "Momcheva", "given": "Ivelina" } }, { "id": "Muzzin-A", "name": { "family": "Muzzin", "given": "Adam" }, "orcid": "0000-0002-9330-9108" }, { "id": "Quadri-R", "name": { "family": "Quadri", "given": "Ryan" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Tal-Tomer", "name": { "family": "Tal", "given": "Tomer" } }, { "id": "Wake-D", "name": { "family": "Wake", "given": "David" } }, { "id": "Whitaker-K-E", "name": { "family": "Whitaker", "given": "Katherine E." }, "orcid": "0000-0001-7160-3632" }, { "id": "Williams-A", "name": { "family": "Williams", "given": "Anna" } } ] }, "title": "3D-HST: A Wide-field Grism Spectroscopic Survey with the Hubble Space Telescope", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; surveys", "note": "\u00a9 2012 The American Astronomical Society. \n\nReceived 2011 December 20; accepted for publication 2012 April 16; Published 2012 May 17. \n\nBased on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs 12177 and 12328. \n\nWe are grateful to the authors and maintainers of the aXe software package: Martin K\u00fcmmel, Harald Kuntschner, Jeremy Walsh, and Howard Bushouse. This research has made extensive use of NASA's Astrophysics Data System Bibliographic Services and of open source scientific Python libraries, including PyFITS and PyRAF produced by the Space Telescope Science Institute, which is operated by AURA for NASA. \n\nThe brown dwarf spectral templates are taken from the SpeX Prism Spectral Libraries, maintained by Adam Burgasser at http://pono.ucsd.edu/adam/browndwarfs/spexprism. 3D-HST is supported in part by grant HST-GO-12177 awarded by the Space Telescope Science Institute. Additional funding for this research was provided by the Marie Curie Actions of the European Commission (FP7-COFUND) and the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement 227749.\n\nPublished - Brammer2012p18775Astrophys_J_Suppl_S.pdf
", "abstract": "We present 3D-HST, a near-infrared spectroscopic Treasury program with the Hubble Space Telescope for studying\nthe physical processes that shape galaxies in the distant universe. 3D-HST provides rest-frame optical spectra for\na sample of \u223c7000 galaxies at 1 < z < 3.5, the epoch when \u223c60% of all star formation took place, the number\ndensity of quasars peaked, the first galaxies stopped forming stars, and the structural regularity that we see in\ngalaxies today must have emerged. 3D-HST will cover three quarters (625 arcmin^2) of the CANDELS Treasury\nsurvey area with two orbits of primary WFC3/G141 grism coverage and two to four orbits with the ACS/G800L\ngrism in parallel. In the IR, these exposure times yield a continuum signal-to-noise ratio of \u223c5 per resolution element\nat H_140 \u223c 23.1 and a 5\u03c3 emission-line sensitivity of \u223c5 \u00d7 10^(\u221217) erg s^\u22121 cm^(\u22122) for typical objects, improving by\na factor of \u223c2 for compact sources in images with low sky background levels. The WFC3/G141 spectra provide\ncontinuous wavelength coverage from 1.1 to 1.6\u03bcm at a spatial resolution of \u223c0.\"13, which, combined with their\ndepth, makes them a unique resource for studying galaxy evolution. We present an overview of the preliminary\nreduction and analysis of the grism observations, including emission-line and redshift measurements from combined\nfits to the extracted grism spectra and photometry from ancillary multi-wavelength catalogs. The present analysis\nyields redshift estimates with a precision of \u03c3(z) = 0.0034(1 + z), or \u03c3(v) \u2248 1000 km s^(\u22121). We illustrate how\nthe generalized nature of the survey yields near-infrared spectra of remarkable quality for many different types\nof objects, including a quasar at z = 4.7, quiescent galaxies at z \u223c 2, and the most distant T-type brown dwarf\nstar known. The combination of the CANDELS and 3D-HST surveys will provide the definitive imaging and\nspectroscopic data set for studies of the 1 < z < 3.5 universe until the launch of the James Webb Space Telescope.", "date": "2012-06", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "200", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 13", "id_number": "CaltechAUTHORS:20120711-142544942", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120711-142544942", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Marie Curie Fellowship", "grant_number": "FP7-COFUND" }, { "agency": "European Research Council (ERC)", "grant_number": "FP7/2007-2013" }, { "agency": "European Research Council (ERC)", "grant_number": "227749" } ] }, "doi": "10.1088/0067-0049/200/2/13", "primary_object": { "basename": "Brammer2012p18775Astrophys_J_Suppl_S.pdf", "url": "https://authors.library.caltech.edu/records/kcq4t-zvt08/files/Brammer2012p18775Astrophys_J_Suppl_S.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Brammer, Gabriel B.; van Dokkum, Pieter G.; et el." }, { "id": "https://authors.library.caltech.edu/records/hgr8t-fm882", "eprint_id": 29694, "eprint_status": "archive", "datestamp": "2023-08-19 10:53:37", "lastmod": "2023-10-24 22:22:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan F." }, "orcid": "0000-0002-6967-7322" }, { "id": "Rakic-O", "name": { "family": "Rakic", "given": "Olivera" } }, { "id": "Bogosavljevi\u0107-M", "name": { "family": "Bogosavljevi\u0107", "given": "Milan" } }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen" }, "orcid": "0000-0001-9687-4973" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" } ] }, "title": "The Gaseous Environment of High-z Galaxies: Precision Measurements of Neutral Hydrogen in the Circumgalactic Medium of z ~ 2-3 Galaxies in the Keck Baryonic Structure Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2014 galaxies: high-redshift \u2014 galaxies: evolution \u2014 galaxies: formation\u2014 intergalactic medium\u2014 quasars: absorption lines", "note": "\u00a9 2012 The American Astronomical Society. \n\nReceived 2011 December 13; accepted 2012 February 27; published 2012 April 17. \n\nBased on data obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration, and was made possible by the generous financial support of the W. M. Keck Foundation. \n\nThe authors would like to thank Ryan Cooke who contributed the fits to the Damped Profiles in our QSO spectra. \n\nWe are grateful to Bob Carswell for his assistance with the code VPFIT. Many thanks to Joop Schaye for his careful reading of the draft and insightful comments. We would also like to thank George Becker, Brian Siana, and Jean-Ren\u00e9 Gauthier for many helpful and interesting discussion. Thanks to Michele Fumagalli for providing the values listed in Table 5. \n\nWe wish to acknowledge the staff of the the W.M. Keck Observatory\nwhose efforts insure the telescopes and instruments perform reliably. Further, we extend our gratitude to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. \n\nThis work has been supported by the US National Science Foundation through grants AST-0606912 and AST-0908805. CCS acknowledges additional support from the John D. and Catherine T. MacArthur Foundation and the Peter and Patricia Gruber Foundation. Support for N.A.R. was provided by NASA through Hubble Fellowship grant HST-HF-01223.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555.\nThis research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. \n\nFacilities: Keck:I (LRIS), Keck:I (HIRES), Keck:II (NIRSPEC)\n\nPublished - 0004-637X_750_1_67.pdf
Submitted - 1202.6055v1.pdf
", "abstract": "We present results from the Keck Baryonic Structure Survey (KBSS), a unique spectroscopic survey of the\ndistant universe designed to explore the details of the connection between galaxies and intergalactic baryons\nwithin the same survey volumes, focusing particularly on scales from \u223c 50 kpc to a few Mpc. The KBSS is\noptimized for the redshift range z \u223c 2-3, combining S/N \u223c 100 Keck/HIRES spectra of 15 of the brightest\nQSOs in the sky at z \u2243 2.5-2.9 with very densely sampled galaxy redshift surveys within a few arcmin of each\nQSO sightline. In this paper, we present quantitative results on the distribution, column density, kinematics,\nand absorber line widths of neutral hydrogen (H_I) surrounding a subset of 886 KBSS star-forming galaxies\nwith 2.0 \u227e z \u227e 2.8 and with projected distances \u2264 3 physical Mpc from a QSO sightline. Using Voigt profile\ndecompositions of the full Ly\u03b1 forest region of all 15 QSO spectra, we compiled a catalog of \u223c6000 individual\nabsorbers in the redshift range of interest, with 12 \u2264 log(N_(HI)) \u2264 21. These are used to measure H I absorption\nstatistics near the redshifts of foreground galaxies as a function of projected galactocentric distance from the\nQSO sightline and for randomly chosen locations in the intergalacticmedium (IGM) within the survey volume.\nWe find that NHI and the multiplicity of velocity-associated H I components increase rapidly with decreasing\ngalactocentric impact parameter and as the systemic redshift of the galaxy is approached. The strongest H_I\nabsorbers within \u2243 100 physical kpc of galaxies have N_(HI) \u223c 3 orders of magnitude higher than those near\nrandom locations in the IGM. The circumgalactic zone of most significantly enhanced H_I absorption is found\nwithin transverse distances of \u227e 300 kpc and within \u00b1300 km s^(-1) of galaxy systemic redshifts. Taking this\nregion as the defining bounds of the circumgalactic medium (CGM), nearly half of absorbers with log(N_(HI))\n> 15.5 are found within the CGM of galaxies meeting our photometric selection criteria, while their CGM\noccupy only 1.5% of the cosmic volume. The spatial covering fraction, multiplicity of absorption components,\nand characteristic NHI remain significantly elevated to transverse distances of \u223c2 physical Mpc from galaxies\nin our sample. Absorbers with N_(HI) > 10^(14.5) cm^(-2) are tightly correlated with the positions of galaxies, while\nabsorbers with lower N_(HI) are correlated with galaxy positions only on \u2273 Mpc scales. Redshift anisotropies\non these larger scales indicate coherent infall toward galaxy locations, while on scales of \u223c 100 physical kpc\npeculiar velocities of \u0394v \u2243 \u00b1260 km s^(-1) with respect to the galaxies are indicated. The median Doppler widths\nof individual absorbers within 1-3 r_(vir) of galaxies are larger by \u2243 50% than randomly chosen absorbers of the\nsame NHI, suggesting higher gas temperatures and/or increased turbulence likely caused by some combination\nof accretion shocks and galactic winds around galaxies with M_(halo) \u2243 10^(12) M_\u2299 at z \u223c 2-3.", "date": "2012-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "750", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 67", "id_number": "CaltechAUTHORS:20120313-074331194", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120313-074331194", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-01223.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/750/1/67", "primary_object": { "basename": "0004-637X_750_1_67.pdf", "url": "https://authors.library.caltech.edu/records/hgr8t-fm882/files/0004-637X_750_1_67.pdf" }, "related_objects": [ { "basename": "1202.6055v1.pdf", "url": "https://authors.library.caltech.edu/records/hgr8t-fm882/files/1202.6055v1.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Rudie, Gwen C.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/q43e5-mf376", "eprint_id": 29952, "eprint_status": "archive", "datestamp": "2023-08-22 04:45:33", "lastmod": "2023-10-24 22:36:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Nagy-S-R", "name": { "family": "Nagy", "given": "Sarah R." } }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" } ] }, "title": "An HST/WFC3-IR Morphological Survey of Galaxies at z = 1.5-3.6. I. Survey Description and Morphological Properties of Star-forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: fundamental parameters; galaxies: high-redshift; galaxies: structure", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2011 July 15; accepted 2011 December 4; published 2012 January 3. \n\nBased in part on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. \n\nD.R.L., C.C.S., and S.R.N. have been supported by grant GO-11694 from the Space Telescope Science Institute. Support for D.R.L. and N.A.R. was also provided by NASA through Hubble Fellowship grants HF-51244.01 and HF-01223.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. C.C.S. has been supported by the US National Science Foundation through grants AST-0606912 and AST-0908805. A.E.S. acknowledges support from the David and Lucile Packard Foundation. D.R.L. appreciates productive conversations with A. Dutton and E. Bell, and thanks the referee (J. Lotz) for insightful comments that improved the final version of the manuscript. Finally, we extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests.\n\nPublished - Law2012p17615Astrophys_J.pdf
", "abstract": "We present the results of a 42-orbit Hubble Space Telescope Wide-Field Camera 3 (HST/WFC3) survey of the rest-frame optical morphologies of star-forming galaxies with spectroscopic redshifts in the range z = 1.5-3.6. The survey consists of 42 orbits of F160W imaging covering ~65 arcmin2 distributed widely across the sky and reaching a depth of 27.9 AB for a 5\u03c3 detection within a 0.2 arcsec radius aperture. Focusing on an optically selected sample of 306 star-forming galaxies with stellar masses in the range M_* = 10^9-10^(11) M_\u2609, we find that typical circularized effective half-light radii range from ~0.7 to 3.0 kpc and describe a stellar mass-radius relation as early as z ~ 3. While these galaxies are best described by an exponential surface brightness profile (S\u00e9rsic index n ~ 1), their distribution of axis ratios is strongly inconsistent with a population of inclined exponential disks and is better reproduced by triaxial stellar systems with minor/major and intermediate/major axis ratios ~0.3 and 0.7, respectively. While rest-UV and rest-optical morphologies are generally similar for a subset of galaxies with HST/Advanced Camera for Surveys imaging data, differences are more pronounced at higher masses M_* > 3 \u00d7 10^(10) M_\u2609. Finally, we discuss galaxy morphology in the context of efforts to constrain the merger fraction, finding that morphologically identified mergers/non-mergers generally have insignificant differences in terms of physical observables such as stellar mass and star formation rate, although merger-like galaxies selected according to some criteria have statistically smaller effective radii and correspondingly larger \u03a3_(SFR).", "date": "2012-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "745", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 85", "id_number": "CaltechAUTHORS:20120403-093455017", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120403-093455017", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO-11694" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HF-51244.01" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HF-01223.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/745/1/85", "primary_object": { "basename": "Law2012p17615Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/q43e5-mf376/files/Law2012p17615Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Law, David R.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/fk194-dv379", "eprint_id": 29951, "eprint_status": "archive", "datestamp": "2023-08-22 04:45:27", "lastmod": "2023-10-24 22:36:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kulas-K-R", "name": { "family": "Kulas", "given": "Kristin R." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Kollmeier-J-A", "name": { "family": "Kollmeier", "given": "Juna A." }, "orcid": "0000-0001-9852-1610" }, { "id": "Zheng-Zheng", "name": { "family": "Zheng", "given": "Zheng" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Hainline-K-N", "name": { "family": "Hainline", "given": "Kevin N." }, "orcid": "0000-0003-4565-8239" } ] }, "title": "The Kinematics of Multiple-Peaked Ly\u03b1 Emission in Star-Forming Galaxies at z ~ 2-3", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation; galaxies: high-redshift; galaxies: ISM; line: profiles; radiative transfer", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2011 July 18; accepted 2011 October 19; published 2011 December 28. \n\nBased, in part, on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. \n\nWe thank Mark Dijkstra for helpful discussions that enhanced the presentation of our results. K.R.K. and A.E.S. acknowledge support from the David and Lucile Packard Foundation. C.C.S. acknowledges additional support from the John D. and Catherine T. MacArthur Foundation, the Peter and Patricia Gruber Foundation, and NSF grants AST-0606912 and AST-0908805. Z.Z. gratefully acknowledges support from Yale Center for Astronomy and Astrophysics through a YCAA fellowship. \n\nWe wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible.\n\nPublished - Kulas2012p17614Astrophys_J.pdf
", "abstract": "We present new results on the Ly\u03b1 emission-line kinematics of 18 z ~ 2-3 star-forming galaxies with multiple-peaked Ly\u03b1 profiles. With our large spectroscopic database of UV-selected star-forming galaxies at these redshifts, we have determined that ~30% of such objects with detectable Ly\u03b1 emission display multiple-peaked emission profiles. These profiles provide additional constraints on the escape of Ly\u03b1 photons due to the rich velocity structure in the emergent line. Despite recent advances in modeling the escape of Ly\u03b1 from star-forming galaxies at high redshifts, comparisons between models and data are often missing crucial observational information. Using Keck II NIRSPEC spectra of H\u03b1 (z ~ 2) and [O III]\u03bb5007 (z ~ 3), we have measured accurate systemic redshifts, rest-frame optical nebular velocity dispersions, and emission-line fluxes for the objects in the sample. In addition, rest-frame UV luminosities and colors provide estimates of star formation rates and the degree of dust extinction. In concert with the profile sub-structure, these measurements provide critical constraints on the geometry and kinematics of interstellar gas in high-redshift galaxies. Accurate systemic redshifts allow us to translate the multiple-peaked Ly\u03b1 profiles into velocity space, revealing that the majority (11/18) display double-peaked emission straddling the velocity-field zero point with stronger red-side emission. Interstellar absorption-line kinematics suggest the presence of large-scale outflows for the majority of objects in our sample, with an average measured interstellar absorption velocity offset of (\u0394v_(abs))=\u2013230 km s^(\u20131). A comparison of the interstellar absorption kinematics for objects with multiple- and single-peaked Ly\u03b1 profiles indicate that the multiple-peaked objects are characterized by significantly narrower absorption line widths. We compare our data with the predictions of simple models for outflowing and infalling gas distributions around high-redshift galaxies. While popular \"shell\" models provide a qualitative match with many of the observations of Ly\u03b1 emission, we find that in detail there are important discrepancies between the models and data, as well as problems with applying the framework of an expanding thin shell of gas to explain high-redshift galaxy spectra. Our data highlight these inconsistencies, as well as illuminating critical elements for success in future models of outflow and infall in high-redshift galaxies.", "date": "2012-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "745", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 33", "id_number": "CaltechAUTHORS:20120403-092029054", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120403-092029054", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "David and Lucile Packard Foundation" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "Yale Center for Astronomy and Astrophysics" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/745/1/33", "primary_object": { "basename": "Kulas2012p17614Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/fk194-dv379/files/Kulas2012p17614Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Kulas, Kristin R.; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/w6gby-04495", "eprint_id": 28654, "eprint_status": "archive", "datestamp": "2023-08-22 04:21:25", "lastmod": "2023-10-24 18:03:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "van-Dokkum-P-G", "name": { "family": "van Dokkum", "given": "Pieter G." }, "orcid": "0000-0002-8282-9888" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "First Results from the 3D-HST Survey: The Striking Diversity of Massive Galaxies at z > 1", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution", "note": "\u00a9 2011 American Astronomical Society. \n\nReceived 2011 August 30; accepted 2011 October 13; published 2011 November 21.\n\nPublished - vanDokkum2011p16577Astrophys_J_Lett.pdf
", "abstract": "We present first results from the 3D-HST program, a near-IR spectroscopic survey performed with the Wide Field Camera 3 (WFC3) on the HST. We have used 3D-HST spectra to measure redshifts and H\u03b1 equivalent widths (EWH\u03b1) for a complete, stellar mass-limited sample of 34 galaxies at 1 < z < 1.5 with M_(star) > 10^(11) M_\u2609 in the COSMOS, GOODS, and AEGIS fields. We find that a substantial fraction of massive galaxies at this epoch are forming stars at a high rate: the fraction of galaxies with EW_(H\u03b1) >10 \u00c5 is 59%, compared to 10% among Sloan Digital Sky Survey galaxies of similar masses at z = 0.1. Galaxies with weak H\u03b1 emission show absorption lines typical of 2-4 Gyr old stellar populations. The structural parameters of the galaxies, derived from the associated WFC3 F140W imaging data, correlate with the presence of H\u03b1; quiescent galaxies are compact with high S\u00e9rsic index and high inferred velocity dispersion, whereas star-forming galaxies are typically large two-armed spiral galaxies, with low S\u00e9rsic index. Some of these star-forming galaxies might be progenitors of the most massive S0 and Sa galaxies. Our results challenge the idea that galaxies at fixed mass form a homogeneous population with small scatter in their properties. Instead, we find that massive galaxies form a highly diverse population at z > 1, in marked contrast to the local universe.", "date": "2011-12-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "743", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L15", "id_number": "CaltechAUTHORS:20120104-141106508", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120104-141106508", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1088/2041-8205/743/1/L15", "primary_object": { "basename": "vanDokkum2011p16577Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/w6gby-04495/files/vanDokkum2011p16577Astrophys_J_Lett.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "van Dokkum, Pieter G. and Steidel, Charles C." }, { "id": "https://authors.library.caltech.edu/records/ssyfm-ssn06", "eprint_id": 27225, "eprint_status": "archive", "datestamp": "2023-08-22 03:55:17", "lastmod": "2023-10-24 16:58:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Bogosavljevi\u0107-M", "name": { "family": "Bogosavljevi\u0107", "given": "Milan" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Filamentary Large-scale Structure Traced by Six Ly\u03b1 Blobs at z = 2.3", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift; large-scale structure of universe", "note": "\u00a9 2011 American Astronomical Society. \n\nReceived 2011 August 17; accepted 2011 September 9; published 2011 September 22. \n\nAlice Shapley, Naveen Reddy, and Max Pettini provided essential contributions to the survey on which this work is based. We also thank the staffs of Palomar and Keck Observatories for assistance with the observations, Yuichi Matsuda for useful suggestions, and the referee for helpful comments. D.K.E. acknowledges support from the University of Wisconsin Research Growth Initiative, and C.C.S. from the US National Science Foundation through grants AST-0606912 and AST-0908805, with additional support from the John D. and Catherine T. MacArthur Foundation and the Peter and Patricia Gruber Foundation.\n\nPublished - Erb2011p16046Astrophys_J_Lett.pdf
", "abstract": "Extended nebulae of Ly\u03b1 emission (\"Ly\u03b1 blobs\") are known to be associated with overdense regions at high redshift. Here we present six large Ly\u03b1 blobs in a previously known protocluster with galaxy overdensity \u03b4 ~ 7 at z = 2.3; this is the richest field of giant Ly\u03b1 blobs detected to date. The blobs have linear sizes of \u2273 100 kpc and Ly\u03b1 luminosities of ~10^(43) erg s^(\u20131). The positions of the blobs define two linear filaments with an extent of at least 12 comoving Mpc; these filaments intersect at the center of one of the blobs. Measurement of the position angles of the blobs indicates that five of the six are aligned with these filaments to within ~10\u00b0, suggesting a connection between the physical processes powering extended Ly\u03b1 emission and those driving structure on larger scales.", "date": "2011-10-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "740", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L31", "id_number": "CaltechAUTHORS:20111014-095153900", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111014-095153900", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "University of Wisconsin" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Peter and Patricia Gruber Foundation" } ] }, "doi": "10.1088/2041-8205/740/1/L31", "primary_object": { "basename": "Erb2011p16046Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/ssyfm-ssn06/files/Erb2011p16046Astrophys_J_Lett.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Erb, Dawn K.; Bogosavljevi\u0107, Milan; et el." }, { "id": "https://authors.library.caltech.edu/records/wyasa-mr612", "eprint_id": 27780, "eprint_status": "archive", "datestamp": "2023-08-22 03:48:55", "lastmod": "2023-10-24 17:25:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kacprzak-G-G", "name": { "family": "Kacprzak", "given": "Glenn G." } }, { "id": "Churchill-C-W", "name": { "family": "Churchill", "given": "Christopher W." } }, { "id": "Evans-J-L", "name": { "family": "Evans", "given": "Jessica L." } }, { "id": "Murphy-M-T", "name": { "family": "Murphy", "given": "Michael T." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Morphological properties of z ~ 0.5 absorption-selected galaxies: the role of galaxy inclination", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: haloes; galaxies: ISM; quasars: absorption lines", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 Royal Astronomical Society. \n\nAccepted 2011 June 15. Received 2011 June 15; in original form 2010 July 15. Article first published online: 11 Aug. 20. \n\nWe thank Simon Mutch for his contributions to the manuscript. We also thank Nicolas Bouch\u00e9 and Simon Lilly for carefully reading the manuscript and providing comments. We thank the anonymous referee for providing insightful comments and improving the paper. MTM thanks the Australian Research Council for a QEII Research Fellowship (DP0877998). CWC and JLE were partially supported by the National Science Foundation under Grant Number AST-\n0708210. This work is based in part on observations made with the NASA/ESA Hubble Space Telescope, or obtained from the data archive at the Space Telescope Institute (STScI), which is a collaboration between STScI/NASA, the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). Other observations were obtained with the ESOVery Large Telescope at the Paranal Observatories and with the W.M. Keck Observatory (some of which were generously provided by Jason X. Prochaska and by Wallace L. W. Sargent and\nMichael Rauch),which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. Keck Observatory was made possible by the generous financial support of the W.M. Keck Foundation.\n\nPublished - Kacprzak2011p16222Mon_Not_R_Astron_Soc.pdf
Supplemental Material - MNR_19261_sm_Figure1.zip
", "abstract": "We have used Galaxy IMage 2D (GIM2D) to quantify the morphological properties of 40 intermediate-redshift Mg ii absorption-selected galaxies [0.03 \u2264\u2002W_r(2796) \u2264 2.9 \u00c5], imaged with WFPC-2/Hubble Space Telescope\u2002(HST), and compared them to the halo gas properties measured from HIRES/Keck and UVES/VLT quasar spectra. We find that as the quasar\u2013galaxy separation,\u2002D, increases the Mg ii equivalent decreases with large scatter, implying that\u2002D\u2002 is not the only physical parameter affecting the distribution and quantity of halo gas. Our main result shows that inclination correlates with Mg ii absorption properties after normalizing out the relationship (and scatter) between the absorption properties and\u2002D. We find a 4.3\u03c3 correlation between\u2002W_r(2796) and galaxy inclination, normalized by impact parameter,\u2002i/D. Other measures of absorption optical depth also correlate with\u2002i/D\u2002at greater than 3.2\u03c3 significance. Overall, this result suggests that Mg ii gas has a co-planer geometry, not necessarily disc-like, that is coupled to the galaxy inclination. It is plausible that the absorbing gas arises from tidal streams, satellites, filaments, etc., which tend to have somewhat co-planer distributions. This result does not support a picture in which Mg ii absorbers with\u2002W_r(2796) \u2272 1 \u00c5 are predominantly produced by star formation driven winds.\n\nWe further find that: (1) Mg ii host galaxies have quantitatively similar bulge and disc scalelength distribution to field galaxies at similar redshifts and have a mean disc and bulge scalelength of 3.8 and 2.5 kpc, respectively; (2) Galaxy colour and luminosity do not correlate strongly with absorption properties, implying a lack of a connection between host galaxy star formation rates and absorption strength; and (3) parameters such as scalelengths and bulge-to-total ratios do not significantly correlate with the absorption parameters, suggesting that the absorption is independent of galaxy size or mass.", "date": "2011-10", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "416", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3118-3137", "id_number": "CaltechAUTHORS:20111115-094620008", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111115-094620008", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council", "grant_number": "DP0877998" }, { "agency": "NSF", "grant_number": "AST-0708210" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1111/j.1365-2966.2011.19261.x", "primary_object": { "basename": "Kacprzak2011p16222Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/wyasa-mr612/files/Kacprzak2011p16222Mon_Not_R_Astron_Soc.pdf" }, "related_objects": [ { "basename": "MNR_19261_sm_Figure1.zip", "url": "https://authors.library.caltech.edu/records/wyasa-mr612/files/MNR_19261_sm_Figure1.zip" } ], "resource_type": "article", "pub_year": "2011", "author_list": "Kacprzak, Glenn G.; Churchill, Christopher W.; et el." }, { "id": "https://authors.library.caltech.edu/records/xgyjk-40n30", "eprint_id": 28630, "eprint_status": "archive", "datestamp": "2023-08-22 03:51:22", "lastmod": "2023-10-24 18:01:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cooke-R-J", "name": { "family": "Cooke", "given": "Ryan" }, "orcid": "0000-0001-7653-5827" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Nissen-P-E", "name": { "family": "Nissen", "given": "Poul E." } } ] }, "title": "The most metal-poor damped Ly\u03b1 systems: insights into chemical\n evolution in the very metal-poor regime", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: abundances; galaxies: evolution; quasars: absorption lines", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. \n\nAccepted 2011 July 1. Received 2011 July 1; in original form 2011 April 4. Article first published online: 24 Aug 2011. \n\nBased on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile [VLT programme IDs 67.A-0078(A), 69.A-0613(A), 083.A-0042(A), 085.A-0109(A)], and at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. Keck telescope time was granted by NOAO, through the Telescope System Instrumentation Program (TSIP). TSIP is funded by NSF. \n\nWe are grateful to the relevant time assignment committees for their continuing support of this demanding observational programme, and to the staff astronomers at the VLT and Keck Observatories for their competent assistance with the observations. We also thank an anonymous referee who provided valuable comments that improved the presentation of this work. Tom Barlow and Michael Murphy generously shared their echelle data reduction software. Valuable advice and help with various aspects of the work described in this paper was provided by Bob Carswell, Paul Hewett and Regina Jorgenson. We thank the Hawaiian people for the opportunity to observe from Mauna Kea; without their hospitality, this work would not have been possible. RC is jointly funded by the Cambridge Overseas Trust and the Cambridge Commonwealth/Australia Trust with an Allen Cambridge Australia Trust Scholarship. CCS's research is partly supported by grants AST-0606912 and AST-0908805 from the US National Science Foundation.\n\nPublished - Cooke2011p16668Mon_Not_R_Astron_Soc.pdf
", "abstract": "We present a high spectral resolution survey of the most metal-poor damped Ly\u03b1 absorption systems (DLAs) aimed at probing the nature and nucleosynthesis of the earliest generations of stars. Our survey comprises 22 systems with iron abundance less than 1/100 solar; observations of seven of these are reported here for the first time. Together with recent measures of the abundances of C and O in Galactic metal-poor stars, we reinvestigate the trend of C/O in the very metal-poor (VMP) regime and we compare, for the first time, the O/Fe ratios in the most metal-poor DLAs and in halo stars. We confirm the near-solar values of C/O in DLAs at the lowest metallicities probed, and find that their distribution is in agreement with that seen in Galactic halo stars. We find that the O/Fe ratio in VMP DLAs is essentially constant, and shows very little dispersion, with a mean [\u3008O/Fe\u3009]=+0.39 \u00b1 0.12, in good agreement with the values measured in Galactic halo stars when the oxygen abundance is measured from the [O i] \u03bb6300 line. We speculate that such good agreement in the observed abundance trends points to a universal origin for these metals. In view of this agreement, we construct the abundance pattern for a typical VMP DLA and compare it to model calculations of Population II and Population III nucleosynthesis to determine the origin of the metals in VMP DLAs. Our results suggest that the most metal-poor DLAs may have been enriched by a generation of metal-free stars; however, given that abundance measurements are currently available for only a few elements, we cannot yet rule out an additional contribution from Population II stars.", "date": "2011-10", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "417", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1534-1558", "id_number": "CaltechAUTHORS:20120103-144527695", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120103-144527695", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Cambridge Overseas Trust" }, { "agency": "Cambridge Commonwealth/Australia Trust" }, { "agency": "Allen Cambridge Australia Trust Scholarship" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1111/j.1365-2966.2011.19365.x", "primary_object": { "basename": "Cooke2011p16668Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/xgyjk-40n30/files/Cooke2011p16668Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Cooke, Ryan; Pettini, Max; et el." }, { "id": "https://authors.library.caltech.edu/records/2qgfy-g3e97", "eprint_id": 25511, "eprint_status": "archive", "datestamp": "2023-08-22 03:43:35", "lastmod": "2023-10-24 15:56:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "F\u00f6rster-Schreiber-N-M", "name": { "family": "F\u00f6rster Schreiber", "given": "N. M." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "A. E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Genzel-Reinhard", "name": { "family": "Genzel", "given": "R." }, "orcid": "0000-0002-2767-9653" }, { "id": "Bouch\u00e9-N", "name": { "family": "Bouch\u00e9", "given": "N." } }, { "id": "Cresci-G", "name": { "family": "Cresci", "given": "G." } }, { "id": "Davies-R", "name": { "family": "Davies", "given": "R." } }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "D. K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Genel-S", "name": { "family": "Genel", "given": "S." }, "orcid": "0000-0002-3185-1540" }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Newman-S-Astro", "name": { "family": "Newman", "given": "S." } }, { "id": "Shapiro-K-L", "name": { "family": "Shapiro", "given": "K. L." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Sternberg-A", "name": { "family": "Sternberg", "given": "A." } }, { "id": "Tacconi-Linda-J", "name": { "family": "Tacconi", "given": "L. J." }, "orcid": "0000-0002-1485-9401" } ] }, "title": "Constraint on the Assembly and Dynamics of Galaxies. II. Properties of Kiloparsec-Scale Clumps in Rest-Frame Optical Emission of z ~ 2 Star-Forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: structure; infrared: galaxies", "note": "\u00a9 2011 The American Astronomical Society. \n\nReceived 2011 April 1; accepted 2011 July 4; published 2011 September 6. \n\nBased on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program no. 10924. Also based on observations obtained at the Very Large Telescope of the European Southern Observatory, Paranal, Chile (ESO Programme IDs 073.B-9018, 074.A-9011, 075.A-0466, 076.A-0527, 077.A-0576, 078.A-0600, 079.A-0341, 080.A-0330, and 080.A-0339). \n\nWe are grateful to our many colleagues for stimulating discussions and insightful comments on various aspects of this work, in particular A. Burkert, P. Johansson, T. Naab, A. Renzini, S. Wuyts, and the entire SINS team. We also wish to thank M. Swinbank and T. Jones for useful discussions and additional information about clumps in their lensed galaxy samples. We thank the referee for a thoughtful report and useful suggestions that improved the presentation of the results. Support for HST program no. 10924 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. N.M.F.S. acknowledges support by the Minerva program of the MPG. A.E.S. acknowledges support from the David and Lucile Packard Foundation. N.B. is supported by the Marie Curie grant PIOF-GA-2009-236012 from the European Commission. G.C. acknowledges support by ASI-INAF grant I/009/10/0. A.S. thanks the DFG for support via German-Israeli Project Cooperation Grant STE1868/1-1.GE625/15.1.\n\nPublished - Schreiber2011p15964Astrophys_J.pdf
", "abstract": "We study the properties of luminous stellar \"clumps\" identified in deep, high-resolution Hubble Space Telescope NIC2/F160W imaging at 1.6 \u03bcm of six z ~ 2 star-forming galaxies with existing near-infrared integral field spectroscopy from SINFONI at the Very Large Telescope. Individual clumps contribute ~0.5%-15% of the galaxy-integrated rest-frame \u22485000 \u00c5 emission, with median of \u22482%; the total contribution of clump light ranges from 10% to 25%. The median intrinsic clump size and stellar mass are ~1 kpc and ~10^9 M_\u2609, in the ranges for clumps identified in rest-UV or line emission in other studies. The clump sizes and masses in the subset of disks are broadly consistent with expectations for clump formation through gravitational instabilities in gas-rich, turbulent disks given the host galaxies' global properties. By combining the NIC2 data with Advanced Camera for Surveys (ACS)/F814W imaging available for one source, and adaptive-optics-assisted SINFONI H\u03b1 data for another, we infer modest color, M/L, and stellar age variations within each galaxy. In these two objects, sets of clumps identified at different wavelengths do not fully overlap; NIC2-identified clumps tend to be redder/older than ACS- or H\u03b1-identified clumps without rest-frame optical counterparts. There is evidence for a systematic trend of older ages at smaller galactocentric radii among the clumps, consistent with scenarios where inward migration of clumps transports material toward the central regions. From constraints on a bulge-like component at radii \u227e1-3 kpc, none of the five disks in our sample appears to contain a compact massive stellar core, and we do not discern a trend of bulge stellar mass fraction with stellar age of the galaxy. Further observations are necessary to probe the buildup of stellar bulges and the role of clumps in this process.", "date": "2011-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "739", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 45", "id_number": "CaltechAUTHORS:20110930-113320403", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110930-113320403", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "10924" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Marie Curie Fellowship", "grant_number": "PIOF-GA-2009-236012" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/009/10/0" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "STE1868/1-1.GE625/15.1" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "doi": "10.1088/0004-637X/739/1/45", "primary_object": { "basename": "Schreiber2011p15964Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/2qgfy-g3e97/files/Schreiber2011p15964Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "F\u00f6rster Schreiber, N. M.; Shapley, A. E.; et el." }, { "id": "https://authors.library.caltech.edu/records/4amrh-54010", "eprint_id": 25209, "eprint_status": "archive", "datestamp": "2023-08-22 03:24:28", "lastmod": "2023-10-24 15:42:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Bogosavljevi\u0107-M", "name": { "family": "Bogosavljevi\u0107", "given": "Milan" } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Kollmeier-J-A", "name": { "family": "Kollmeier", "given": "Juna A." }, "orcid": "0000-0001-9852-1610" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" } ] }, "title": "Diffuse Ly\u03b1 Emitting Halos: A Generic Property of High-redshift Star-forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: high-redshift", "note": "\u00a9 2011 The American Astronomical Society. \n\nReceived 2011 January 10; accepted 2011 May 24; published 2011 July 19. \n\nBased on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. \n\nThis work has been supported by the US National Science Foundation through grants AST-0606912 and AST-0908805 (C.C.S.), and by the David and Lucile Packard Foundation (A.E.S.). C.C.S. acknowledges additional support from the John D. and Catherine T. MacArthur Foundation and the Peter and Patricia Gruber Foundation. D.K.E. was supported by the National Aeronautics and Space Administration under Award No.NAS7-03001 and the California Institute of Technology. Gwen Rudie and Olivera Rakic each provided very helpful comments on an earlier draft of the paper; we also thank Kurt Adelberger for his early involvement in the work which made the new results possible. We are grateful to the staff of the W. M. Keck Observatory who keep the instruments and telescopes running effectively. A careful reading and constructive report by the referee is very much appreciated. Finally, we wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be\nguests.\n\nPublished - Steidel2011p15625Astrophys_J.pdf
", "abstract": "Using a sample of 92 UV continuum-selected, spectroscopically identified galaxies with langzrang = 2.65, all of which have been imaged in the Ly\u03b1 line with extremely deep narrow-band imaging, we examine galaxy Ly\u03b1 emission profiles to very faint surface brightness limits. The galaxy sample is representative of spectroscopic samples of Lyman break galaxies (LBGs) at similar redshifts in terms of apparent magnitude, UV luminosity, inferred extinction, and star formation rate and was assembled without regard to Ly\u03b1 emission properties. Approximately 45% (55%) of the galaxy spectra have Ly\u03b1 appearing in net absorption (emission), with \u224320% satisfying commonly used criteria for the identification of \"Ly\u03b1 emitters\" (LAEs; W 0(Ly\u03b1) \u2265 20 \u00c5). We use extremely deep stacks of rest-UV continuum and continuum-subtracted Ly\u03b1 images to show that all sub-samples exhibit diffuse Ly\u03b1 emission to radii of at least 10\" (~80 physical kpc). The characteristic exponential scale lengths for Ly\u03b1 line emission exceed that of the \u03bb_0 = 1220 \u00c5 UV continuum light by factors of ~5-10. The surface brightness profiles of Ly\u03b1 emission are strongly suppressed relative to the UV continuum light in the inner few kpc, by amounts that are tightly correlated with the galaxies' observed spectral morphology; however, all galaxy sub-subsamples, including that of galaxies for which Ly\u03b1 appears in net absorption in the spectra, exhibit qualitatively similar diffuse Ly\u03b1 emission halos. Accounting for the extended Ly\u03b1 emission halos, which generally would not be detected in the slit spectra of individual objects or with typical narrow-band Ly\u03b1 imaging, increases the total Ly\u03b1 flux (and rest equivalent width W _0(Ly\u03b1)) by an average factor of ~5, and by a much larger factor for the 80% of LBGs not classified as LAEs. We argue that most, if not all, of the observed Ly\u03b1 emission in the diffuse halos originates in the galaxy H II regions but is scattered in our direction by H I gas in the galaxy's circum-galactic medium. The overall intensity of Ly\u03b1 halos, but not the surface brightness distribution, is strongly correlated with the emission observed in the central ~1\" \u2014more luminous halos are observed for galaxies with stronger central Ly\u03b1 emission. We show that whether or not a galaxy is classified as a giant \"Ly\u03b1 blob\" (LAB) depends sensitively on the Ly\u03b1 surface brightness threshold reached by an observation. Accounting for diffuse Ly\u03b1 halos, all LBGs would be LABs if surveys were sensitive to 10 times lower Ly\u03b1 surface brightness thresholds; similarly, essentially all LBGs would qualify as LAEs.", "date": "2011-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "736", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 160", "id_number": "CaltechAUTHORS:20110902-103429209", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110902-103429209", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "NASA", "grant_number": "NAS7-03001" }, { "agency": "Caltech" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/736/2/160", "primary_object": { "basename": "Steidel2011p15625Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/4amrh-54010/files/Steidel2011p15625Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Steidel, Charles C.; Bogosavljevi\u0107, Milan; et el." }, { "id": "https://authors.library.caltech.edu/records/d2hm7-7t796", "eprint_id": 24624, "eprint_status": "archive", "datestamp": "2023-08-22 03:14:27", "lastmod": "2023-10-23 23:31:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nestor-D-B", "name": { "family": "Nestor", "given": "Daniel B." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Siana-Brian-D", "name": { "family": "Siana", "given": "Brian" }, "orcid": "0000-0002-4935-9511" } ] }, "title": "Narrowband Imaging of Escaping Lyman-continuum Emission in the SSA22 Field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; diffuse radiation; galaxies: high-redshift; intergalactic medium", "note": "\u00a9 2011 The American Astronomical Society. \n\nReceived 2011 January 31; accepted 2011 April 26; published 2011 June 29. \n\nBased, in part, on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. \n\nBased, in part, on data collected at the Subaru Telescope and obtained from the SMOKA archive, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan. \n\n We thank Andrew Blain for permitting our use of the NB3640 filter, Kevin Hainline for his helpful discussions regarding our photometric simulations, and the anonymous referee for constructive suggestions. D.B.N. and A.E.S. acknowledge support from the David and Lucile Packard Foundation. C.C.S. acknowledges additional support from the John D. and Catherine T. MacArthur Foundation, the Peter and Patricia Gruber Foundation, and NSF grants AST-0606912 and AST-0908805. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible.\n\nPublished - Nestor2011p15388Astrophys_J.pdf
", "abstract": "We present the results of an ultradeep, narrowband imaging survey for Lyman-continuum (LyC) emission at z ~ 3 in the SSA22a field. We employ a custom narrowband filter centered at \u03bb = 3640 \u00c5 (NB3640), which probes the LyC region for galaxies at z \u2265 3.06. We also analyze new and archival NB4980 imaging tuned to the wavelength of the Ly\u03b1 emission line at z = 3.09, and archival broadband B, V, and R images of the non-ionizing UV continuum. Our NB3640 images contain 26 z \u2265 3.06 Lyman break galaxies (LBGs) as well as a set of 130 Ly\u03b1 emitters (LAEs), identified by their excess NB4980 flux relative to the BV continuum. Six LBGs and 28 LAEs are detected in the NB3640 image. LBGs appear to span a range of NB3640-R colors, while LAEs appear bimodal in their NB3640-R properties. We estimate average UV-to-LyC flux density ratios, corrected for foreground contamination and intergalactic medium absorption, finding (F_(UV)/F_(LyC)^(LBG)_(corr) = 11.3^(+10.3)_(\u20135.4), which implies an LBG LyC escape fraction f^(LyC)_(esc) ~ 0.1, and (F_(UV)/F_(LyC)^(LAE)_(corr) = 2.2^(+0.9)_(\u20130.6). The strikingly blue LAE flux density ratios defy interpretation in terms of standard stellar population models. Assuming (F _(UV)/F_(LyC)^(LBG)_(corr) applies down to L = 0.1L^*, we estimate a galaxy contribution to the intergalactic hydrogen ionization rate that is consistent with independent estimates based on the Ly\u03b1 forest opacity at z sime 3. If we assume that (F_(UV)/F_(LyC)^(LAE)_(corr) holds at the faintest luminosities, the galaxy contribution significantly exceeds that inferred from the Ly\u03b1 forest. We interpret our results in terms of a model where LyC photons escape over only ~10%-20% of solid angle. When advantageously oriented, a galaxy will exhibit a low UV-to-LyC ratio, an effect enhanced for more compact galaxies. This model, however, does not adequately explain the extremely blue NB3640-R colors measured for some LAEs in our sample. Further follow-up study of these faint LAEs is crucial, given the potentially important contribution similar objects make to the process of reionization.", "date": "2011-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "736", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 18", "id_number": "CaltechAUTHORS:20110802-091358495", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110802-091358495", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "David and Lucile Packard Foundation" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/736/1/18", "primary_object": { "basename": "Nestor2011p15388Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/d2hm7-7t796/files/Nestor2011p15388Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Nestor, Daniel B.; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/d8x4z-fnk15", "eprint_id": 24874, "eprint_status": "archive", "datestamp": "2023-08-22 03:08:50", "lastmod": "2023-10-24 15:00:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nagy-S-R", "name": { "family": "Nagy", "given": "Sarah R." } }, { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "The Mass\u2013Radius Relation for Star-forming Galaxies at z ~ 1.5-3.0", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: fundamental parameters; galaxies: high-redshift; galaxies: structure", "note": "\u00a9 2011 The American Astronomical Society. \n\nReceived 2011 March 25; accepted 2011 May 16; published 2011 June 9. \n\nS.R.N., D.R.L., and C.C.S. have been supported by grant GO-11694 from the Space Telescope Science Institute. Support for D.R.L. was also provided by NASA through Hubble Fellowship grant no. HF-51244.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. A.E.S. acknowledges support from the David and Lucile Packard Foundation.\n\nPublished - Nagy2011p15504Astrophys_J_Lett.pdf
", "abstract": "We present early results from a Hubble Space Telescope WFC3/IR imaging survey of star-forming galaxies in the redshift range 1.5 < z < 3.0. When complete, this survey will consist of 42 orbits of F160W imaging distributed amongst 10 survey fields on the line of sight to bright background QSOs, covering 65 arcmin^2 to a depth of 27.9 AB with a point-spread function FWHM of 0\".18. In this contribution, we use a subset of these fields to explore the evolution of the galactic stellar mass-radius relation for a magnitude-limited sample of 102 spectroscopically confirmed star-forming galaxies ((SFR) ~ 30 M_\u2609 yr^(\u20131)) with stellar mass M_* ~ 10^(10) M_\u2609. Although the light profile of these galaxies often has an irregular, multi-component morphology, it is typically possible to describe the brightest component with a Sersic profile of index n ~ 1. The circularized half-light radius r e of the brightest component is on average r_e = 1.66 \u00b1 0.79 kpc (i.e., ~50%-70% the size of local late-type galaxies with similar stellar mass), consistent with recent theoretical models that incorporate strong feedback from star-forming regions. The mean half-light radius increases with stellar mass and, at fixed stellar mass, evolves with cosmic time as ~(1 + z)^(\u20131.42), suggesting that high-redshift star-forming galaxies may evolve onto the local stellar mass-radius relation by redshift z ~ 1.", "date": "2011-07-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "735", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L19", "id_number": "CaltechAUTHORS:20110816-082413937", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110816-082413937", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO-11694" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HF-51244.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "David and Lucile Packard Foundation" } ] }, "doi": "10.1088/2041-8205/735/1/L19", "primary_object": { "basename": "Nagy2011p15504Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/d8x4z-fnk15/files/Nagy2011p15504Astrophys_J_Lett.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Nagy, Sarah R.; Law, David R.; et el." }, { "id": "https://authors.library.caltech.edu/records/affq3-mgh65", "eprint_id": 24829, "eprint_status": "archive", "datestamp": "2023-08-22 03:03:35", "lastmod": "2023-10-24 14:57:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rakic-O", "name": { "family": "Rakic", "given": "Olivera" } }, { "id": "Schaye-J", "name": { "family": "Schaye", "given": "Joop" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" } ] }, "title": "Calibrating galaxy redshifts using absorption by the surrounding intergalactic medium", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; intergalactic medium; quasars: absorption lines", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. \n\nAccepted 2011 February 28. Received 2011 January 20; in original form 2010 November 2. Article first published online: 9 May 2011. \n\nBased on data obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA, and was made possible by the generous financial support of the W.M. Keck Foundation. \n\nWe are very grateful to Alice Shapley, Dawn Erb, Naveen Reddy, Milan Bogosavljev\u00edc and Max Pettini for their help with collecting and processing the data. We also thank the anonymous referee whose comments improved the clarity of the paper. This work was supported by an NWO VIDI grant (OR, JS), by the US National Science Foundation through grants AST-0606912 and AST-0908805, and by the David and Lucile Packard Foundation (CCS). CCS acknowledges additional support from the John D. and Catherine T. MacArthur Foundation and the Peter and Patricia Gruber Foundation. We thank the W. M. Keck Observatory staff for their assistance with the observations. We also thank the Hawaiian people, as without their hospitality the observations presented here would not have been possible.\n\nPublished - Rakic2011p15479Mon_Not_R_Astron_Soc.pdf
", "abstract": "Rest-frame UV spectral lines of star-forming galaxies are systematically offset from the galaxies' systemic redshifts, probably because of large-scale outflows. We calibrate galaxy redshifts measured from rest-frame UV lines by utilizing the fact that the mean H i Ly\u03b1 absorption profiles around the galaxies, as seen in spectra of background objects, must be symmetric with respect to the true galaxy redshifts if the galaxies are oriented randomly with respect to the lines of sight to the background objects. We use 15 bright QSOs at z\u22482.5\u20133 and more than 600 foreground galaxies with spectroscopic redshifts at z\u22481.9\u20132.5. All galaxies are within 2 Mpc proper from the lines of sight to the background QSOs. We find that Ly\u03b1 emission and ISM absorption redshifts require systematic shifts of \u2206\u03bd_Ly\u03b1 = -295^(+35)_(-35) and \u2206\u03bd_ISM = 145^(+70)_(-35) km s^(-1), respectively. Assuming a Gaussian distribution, we put 1\u03c3 upper limits on possible random redshift offsets of <220 km s^(-1) for Ly\u03b1 and <420 km s^(-1) for ISM redshifts. For the small subset (<10 per cent) of galaxies for which near-IR spectra have been obtained, we can compare our results to direct measurements based on rest-frame optical, nebular emission lines, which we confirm to mark the systemic redshifts. While our \u0394vISM agrees with the direct measurements, our \u0394v_Ly\u03b1 is significantly smaller. However, when we apply our method to the near-IR subsample which is characterized by slightly different selection effects, the best-fitting velocity offset comes into agreement with the direct measurement. This confirms the validity of our approach, and implies that no single number appropriately describes the whole population of galaxies, in line with the observation that the line offset depends on galaxy spectral morphology. This method provides accurate redshift calibrations and will enable studies of circumgalactic matter around galaxies for which rest-frame optical observations are not available.", "date": "2011-07", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "414", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3265-3271", "id_number": "CaltechAUTHORS:20110812-111221376", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110812-111221376", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1111/j.1365-2966.2011.18624.x", "primary_object": { "basename": "Rakic2011p15479Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/affq3-mgh65/files/Rakic2011p15479Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Rakic, Olivera; Schaye, Joop; et el." }, { "id": "https://authors.library.caltech.edu/records/7m400-jx918", "eprint_id": 23840, "eprint_status": "archive", "datestamp": "2023-08-22 02:44:59", "lastmod": "2023-10-23 20:04:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hainline-Kevin-N", "name": { "family": "Hainline", "given": "Kevin N." }, "orcid": "0000-0003-4565-8239" }, { "id": "Shapley-Alice-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Greene-Jenny-E", "name": { "family": "Greene", "given": "Jenny E." }, "orcid": "0000-0002-5612-3427" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "The Rest-frame Ultraviolet Spectra of UV-selected Active Galactic Nuclei at z ~ 2-3", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: evolution; galaxies: high-redshift; galaxies: nuclei", "note": "\u00a9 2011 The American Astronomical Society. \n\nReceived 2010 November 24; accepted 2011 March 16; published 2011 April 29. \n\nBased, in part, on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. \n\nWe thank Dawn Erb and Max Pettini for their helpful discussions. We also acknowledge the referee, David Alexander, for a thorough and constructive report, which significantly improved the paper. A.E.S. acknowledges support from the David and Lucile Packard Foundation. C.C.S. acknowledges additional support from the John D. and Catherine T. MacArthur Foundation and the Peter and Patricia Gruber Foundation. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible.\n\nPublished - Hainline2011p13968Astrophys_J.pdf
Accepted Version - 1012.0075.pdf
", "abstract": "We present new results for a sample of 33 narrow-lined UV-selected active galactic nuclei (AGNs), identified in the course of a spectroscopic survey for star-forming galaxies at z ~ 2-3. The rest-frame UV composite spectrum for our AGN sample shows several emission lines characteristic of AGNs, as well as interstellar absorption features detected in star-forming Lyman break galaxies (LBGs). We report a detection of N iv] \u03bb1486, which has been observed in high-redshift radio galaxies, as well as in rare optically selected quasars. The UV continuum slope of the composite spectrum is significantly redder than that of a sample of non-AGN UV-selected star-forming galaxies. Blueshifted Si iv absorption provides evidence for outflowing highly ionized gas in these objects at speeds of ~10^3 km s^(\u20131), quantitatively different from what is seen in the outflows of non-AGN LBGs. Grouping the individual AGNs by parameters such as the Ly\u03b1 equivalent width, redshift, and UV continuum magnitude allows for an analysis of the major spectroscopic trends within the sample. Stronger Ly\u03b1 emission is coupled with weaker low-ionization absorption, which is similar to what is seen in the non-AGN LBGs, and highlights the role that cool interstellar gas plays in the escape of Ly\u03b1 photons. However, the AGN composite does not show the same trends between Ly\u03b1 strength and extinction seen in the non-AGN LBGs. These results represent the first such comparison at high redshift between star-forming galaxies and similar galaxies that host AGN activity.", "date": "2011-05-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "733", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 31", "id_number": "CaltechAUTHORS:20110531-114638789", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110531-114638789", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "David and Lucile Packard Foundation" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/733/1/31", "primary_object": { "basename": "1012.0075.pdf", "url": "https://authors.library.caltech.edu/records/7m400-jx918/files/1012.0075.pdf" }, "related_objects": [ { "basename": "Hainline2011p13968Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/7m400-jx918/files/Hainline2011p13968Astrophys_J.pdf" } ], "resource_type": "article", "pub_year": "2011", "author_list": "Hainline, Kevin N.; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/yes84-5ep32", "eprint_id": 23639, "eprint_status": "archive", "datestamp": "2023-08-22 02:30:27", "lastmod": "2023-10-23 19:49:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "F\u00f6rster-Schreiber-N-M", "name": { "family": "F\u00f6rster Schreiber", "given": "N. M." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "A. E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "D. K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Genzel-Reinhard", "name": { "family": "Genzel", "given": "R." }, "orcid": "0000-0002-2767-9653" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Bouch\u00e9-N", "name": { "family": "Bouch\u00e9", "given": "N." } }, { "id": "Cresci-G", "name": { "family": "Cresci", "given": "G." } }, { "id": "Davies-R", "name": { "family": "Davies", "given": "R." } } ] }, "title": "Constraints on the Assembly and Dynamics of Galaxies. I. Detailed Rest-frame Optical Morphologies on Kiloparsec Scale of z ~ 2 Star-forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: kinematics and dynamics; galaxies: structure", "note": "\u00a9 2011 American Astronomical Society. \n\nReceived 2010 November 5; accepted 2011 February 8; published 2011 March 24. \n\nWe are grateful to M. Franx, L. Simard, A. Renzini, S. Wuyts, S. Genel, A. Sternberg, P. van Dokkum, and the entire SINS team for many stimulating discussions and insightful comments on various aspects of this work. We wish to thank in particular P. van Dokkum, L. Yan, and M. Kriek for kindly providing their reduced NIC2 images for the analysis, and N. Reddy for useful discussions on the IR properties of the sample. We thank S. Toft for advice on reducing NICMOS data and J. Greene for help with using GALFIT. We also thank the referee for a very constructive report and useful suggestions. N.M.F.S. acknowledges support by the Minerva program of the MPG. N.B. is supported by the Marie Curie grant PIOF-GA-2009-236012 from the European Commission. G.C. acknowledges support by the ASI-INAF grant I/009/10/0. \n\nBased on observations made with the NASA/ESA Hubble Space Telescope (HST), obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5\u221226555, and at the Very Large Telescope of the European Southern Observatory, Paranal, Chile (ESO Programme IDs 073.B-9018, 074.A-9011, 075.A-0466, 076.A-0527, 077.A-0576, 078.A-0600, 079.A-0341, 080.A-0330, and 080.A-0339).\n\nPublished - Schreiber2011p13753Astrophys_J.pdf
", "abstract": "We present deep and high-resolution Hubble Space Telescope NIC2 F160W imaging at 1.6 \u03bcm of six z ~ 2 star-forming galaxies with existing near-infrared integral field spectroscopy from SINFONI at the Very Large Telescope. The unique combination of rest-frame optical imaging and nebular emission-line maps provides simultaneous insight into morphologies and dynamical properties. The overall rest-frame optical emission of the galaxies is characterized by shallow profiles in general (S\u00e9rsic index n < 1), with median effective radii of R_e ~ 5 kpc. The morphologies are significantly clumpy and irregular, which we quantify through a non-parametric morphological approach, estimating the Gini (G), multiplicity (\u03a8), and M_(20) coefficients. The estimated strength of the rest-frame optical emission lines in the F160W bandpass indicates that the observed structure is not dominated by the morphology of line-emitting gas, and must reflect the underlying stellar mass distribution of the galaxies. The sizes and structural parameters in the rest-frame optical continuum and H\u03b1 emission reveal no significant differences, suggesting similar global distributions of the ongoing star formation and more evolved stellar population. While no strong correlations are observed between stellar population parameters and morphology within the NIC2/SINFONI sample itself, a consideration of the sample in the context of a broader range of z ~ 2 galaxy types (K-selected quiescent, active galactic nucleus, and star forming; 24 \u03bcm selected dusty, infrared-luminous) indicates that these galaxies probe the high specific star formation rate and low stellar mass surface density part of the massive z ~ 2 galaxy population, with correspondingly large effective radii, low S\u00e9rsic indices, low G, and high \u03a8 and M_(20). The combined NIC2 and SINFONI data set yields insights of unprecedented detail into the nature of mass accretion at high redshift.", "date": "2011-04-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "731", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 65", "id_number": "CaltechAUTHORS:20110511-101501949", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110511-101501949", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Marie Curie Fellowship", "grant_number": "PIOF-GA-2009-236012" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/009/10/0" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "doi": "10.1088/0004-637X/731/1/65", "primary_object": { "basename": "Schreiber2011p13753Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/yes84-5ep32/files/Schreiber2011p13753Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "F\u00f6rster Schreiber, N. M.; Shapley, A. E.; et el." }, { "id": "https://authors.library.caltech.edu/records/z1p1m-6yq41", "eprint_id": 23461, "eprint_status": "archive", "datestamp": "2023-08-22 02:23:10", "lastmod": "2023-10-23 19:36:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cooke-R-J", "name": { "family": "Cooke", "given": "Ryan" }, "orcid": "0000-0001-7653-5827" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Jorgenson-R-A", "name": { "family": "Jorgenson", "given": "Regina A." } } ] }, "title": "A carbon-enhanced metal-poor damped Ly\u03b1 system: probing gas from Population III nucleosynthesis?", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: carbon; stars: Population III; galaxies: abundances; galaxies: evolution; quasars: absorption lines; quasars: individual: J0035\u22120918", "note": "\u00a9 2010 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2010 RAS. \n\nAccepted 2010 November 1. Received 2010 November 1; in original form 2010 July 29. Article first published online: 22 Dec. 2010. \n\nWe are grateful to the staff at the Keck and Magellan telescopes for their assistance with the observations, and to Tom Barlow, George\nBecker, Bob Carswell, Gary Ferland and Michael Murphy for providing much of the software used in the reduction and analysis of the data. We wish to thank Poul Nissen and Chris Tout for useful discussions regarding the stellar abundances. Chiaki Kobayashi and Nozomu Tominaga kindly helped with the interpretation of the results. A prompt and comprehensive referee report significantly improved\nthe paper.We thank the Hawaiian people for the opportunity to observe from Mauna Kea; without their hospitality, this work would not have been possible. RC is jointly funded by the Cambridge Overseas Trust and the Cambridge Commonwealth/Australia Trust with an Allen Cambridge Australia Trust Scholarship. CCS's research is partly supported by grants AST-0606912 and AST-0908805 from the US National Science Foundation.\n\nPublished - Cooke2011p13550Mon_Not_R_Astron_Soc.pdf
", "abstract": "We present high-resolution observations of an extremely metal-poor damped Ly\u03b1 system (DLA), at z_(abs) = 2.340 0972 in the spectrum of the QSO J0035\u22120918, exhibiting an abundance pattern consistent with model predictions for the supernova yields of Population III stars. Specifically, this DLA has [Fe/H]\u2243\u22123, shows a clear 'odd\u2013even' effect, and is C-rich with [C/Fe]=+1.53, a factor of \u223c20 greater than reported in any other DLA. In analogy to the carbon-enhanced metal-poor stars in the Galactic halo (with [C/Fe] > +1.0), this is the first known case of a carbon-enhanced DLA. We determine an upper limit to the mass of ^(12)C, M(^(12)C) \u2264 200 M_\u2299, which depends on the unknown gas density n(H); if n(H) > 1 cm^(\u22123) (which is quite likely for this DLA given its low velocity dispersion), then M(^(12)C) \u2264 2 M_\u2299, consistent with pollution by only a few prior supernovae. We speculate that DLAs such as the one discovered here may represent the 'missing link' between the yields of Population III stars and their later incorporation in the class of carbon-enhanced metal-poor stars which show no enhancement of neutron-capture elements (CEMP-no stars).", "date": "2011-04", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "412", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1047-1058", "id_number": "CaltechAUTHORS:20110426-092303862", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110426-092303862", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Cambridge Overseas Trust" }, { "agency": "Cambridge Commonwealth/Allen Cambridge Australia Trust Scholarship" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" } ] }, "doi": "10.1111/j.1365-2966.2010.17966.x", "primary_object": { "basename": "Cooke2011p13550Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/z1p1m-6yq41/files/Cooke2011p13550Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Cooke, Ryan; Pettini, Max; et el." }, { "id": "https://authors.library.caltech.edu/records/k431h-c3082", "eprint_id": 21542, "eprint_status": "archive", "datestamp": "2023-08-22 01:27:46", "lastmod": "2023-10-21 00:07:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cooke-R-J", "name": { "family": "Cooke", "given": "Ryan" }, "orcid": "0000-0001-7653-5827" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "King-L-J", "name": { "family": "King", "given": "Lindsay J." } }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Rakic-O", "name": { "family": "Rakic", "given": "Olivera" } } ] }, "title": "A newly discovered DLA and associated Ly\u03b1 emission in the spectra of the gravitationally lensed quasar UM 673A,B", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: abundances; galaxies: abundances; galaxies: evolution; galaxies: ISM; quasars: absorption lines; quasars: individual: UM673", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS. \n\nAccepted 2010 July 7; Received 2010 July 6; in original form 2010 February 10. \n\nBased on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. We are grateful to the staff astronomers at the Keck Observatory for their assistance with the observations. It is a pleasure to acknowledge advice and help with various aspects of the work described in this paper by George Becker, Sebastiano Cantalupo, Bob Carswell, Martin Haehnelt, Paul Hewett, Geraint Lewis, Eric Monier and Sam Rix. We thank the Hawaiian people for the opportunity to observe from Mauna Kea; without their hospitality, this work would not have been possible. RC is jointly funded by the Cambridge Overseas Trust and the Cambridge Commonwealth/Australia Trust with an Allen Cambridge Australia Trust Scholarship. CCS's research is partly supported by grants AST-0606912 and AST-0908805 from the US National Science Foundation. MP would like the express his gratitude to the members of the International Centre for Radio Astronomy Research at the University of Western Australia for their generous hospitality during the progress of this work.\n\nPublished - Cooke2010p12126Mon_Not_R_Astron_Soc.pdf
", "abstract": "The sightline to the brighter member of the gravitationally lensed quasar pair UM 673A,B intersects a damped Ly\u03b1 system (DLA) at z = 1.62650 which, because of its low redshift, has not been recognized before. Our high-quality echelle spectra of the pair, obtained with HIRES on the Keck I telescope, show a drop in neutral hydrogen column density N(H i) by a factor of at least 400 between UM 673A and UM 673B, indicating that the DLA's extent in this direction is much less than the 2.7 h^(\u22121)_(70) kpc separation between the two sightlines at z = 1.62650. By re-assessing this new case together with published data on other quasar pairs, we conclude that the typical size (radius) of DLAs at these redshifts is R \u2243 (5 \u00b1 3) h^(\u22121)_(70) kpc, smaller than previously realized. Highly ionized gas associated with the DLA is more extended, as we find only small differences in the C iv absorption profiles between the two sightlines.\n\nCoincident with UM 673B, we detect a weak and narrow Ly\u03b1\u2002emission line which we attribute to star formation activity at a rate SFR \u2273 0.2 M_\u2299 yr^(\u22121). The DLA in UM 673A is metal poor, with an overall metallicity Z_(DLA) \u2243 1/30 Z_\u2299, and has a very low internal velocity dispersion. It exhibits some apparent peculiarities in its detailed chemical composition, with the elements Ti, Ni and Zn being deficient relative to Fe by factors of 2\u20133. The [Zn/Fe] ratio is lower than those measured in any other DLA or Galactic halo star, presumably reflecting somewhat unusual previous enrichment by stellar nucleosynthesis. We discuss the implications of these results for the nature of the galaxy hosting the DLA.", "date": "2010-12", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "679-693", "id_number": "CaltechAUTHORS:20110103-110312343", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110103-110312343", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Cambridge Overseas Trust" }, { "agency": "Cambridge Commonwealth/Australia Trust" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1111/j.1365-2966.2010.17331.x", "primary_object": { "basename": "Cooke2010p12126Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/k431h-c3082/files/Cooke2010p12126Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Cooke, Ryan; Pettini, Max; et el." }, { "id": "https://authors.library.caltech.edu/records/e2h0p-3y711", "eprint_id": 20273, "eprint_status": "archive", "datestamp": "2023-08-22 00:51:38", "lastmod": "2023-10-20 22:23:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Digby-North-J-A", "name": { "family": "Digby-North", "given": "J. A." } }, { "id": "Nandra-K", "name": { "family": "Nandra", "given": "K." }, "orcid": "0000-0002-7150-9192" }, { "id": "Laird-E-S", "name": { "family": "Laird", "given": "E. S." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Georgakakis-A", "name": { "family": "Georgakakis", "given": "A." } }, { "id": "Bogosavljevi\u0107-M", "name": { "family": "Bogosavljevi\u0107", "given": "M." } }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "D. K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "A. E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "N. A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Aird-J-A", "name": { "family": "Aird", "given": "J." }, "orcid": "0000-0003-1908-8463" } ] }, "title": "Excess AGN activity in the z = 2.30 Protocluster in HS 1700+64", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: clusters: general; galaxies: high-redshift; surveys; X-rays: general", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS. \n\nAccepted 2010 May 6. Received 2010 May 6; in original form 2009 September 21. Article first published online: 18 Jun 2010. \n\nWe thank the anonymous referee for their comments which significantly improved this paper. JADN and ESL acknowledge generous financial support from the STFC. KN acknowledges the support of the Royal Society. This work is based on observations taken with the Chandra X-Ray Observatory, which is operated for NASA by the Smithsonian Astrophysical Observatory.\n\nPublished - DigbyNorth2010p11469Mon_Not_R_Astron_Soc.pdf
", "abstract": "We present the results of spectroscopic, narrow-band and X-ray observations of a z= 2.30 protocluster in the field of the QSO HS 1700+643. Using a sample of BX/MD galaxies, which are selected to be at z ~ 2.2\u20132.7 by their rest-frame ultraviolet colours, we find that there are five protocluster AGN which have been identified by characteristic emission-lines in their optical/near-IR spectra; this represents an enhancement over the field significant at >98.5 per cent confidence. Using a ~200-ks Chandra/ACIS-I observation of this field we detect a total of 161 X-ray point sources to a Poissonian false-probability limit of 4 \u00d7 10^(\u22126) and identify eight of these with BX/MD galaxies. Two of these are spectroscopically confirmed protocluster members and are also classified as emission-line AGN. When compared to a similarly selected field sample, the analysis indicates this is also evidence for an enhancement of X-ray selected BX/MD AGN over the field, significant at >99 per cent confidence. Deep Ly\u03b1 narrow-band imaging reveals that a total of 4/123 Ly\u03b1 emitters (LAEs) are found to be associated with X-ray sources, with two of these confirmed protocluster members and one highly likely member. We do not find a significant enhancement of AGN activity in this LAE sample over that of the field (result is significant at only 87 per cent confidence). The X-ray emitting AGN fractions for the BX/MD and LAE samples are found to be 6.9^(+9.2)_(\u22124.4) and 2.9^(+2.9)_(\u22121.6) per cent, respectively, for protocluster AGN with L_(2-10 keV)\u2265 4.6 \u00d7 10^(43) erg s^(\u22121) at z= 2.30. These findings are similar to results from the z= 3.09 protocluster in the SSA 22 field found by Lehmer et al. (2009), in that both suggest AGN activity is favoured in dense environments at z > 2.", "date": "2010-09-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "407", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "846-853", "id_number": "CaltechAUTHORS:20101004-101154180", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101004-101154180", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Royal Society" } ] }, "doi": "10.1111/j.1365-2966.2010.16977.x", "primary_object": { "basename": "DigbyNorth2010p11469Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/e2h0p-3y711/files/DigbyNorth2010p11469Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Digby-North, J. A.; Nandra, K.; et el." }, { "id": "https://authors.library.caltech.edu/records/fb3x1-d2151", "eprint_id": 19760, "eprint_status": "archive", "datestamp": "2023-08-22 00:38:20", "lastmod": "2023-10-20 21:21:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Physical Conditions in a Young, Unreddened, Low-metallicity Galaxy at High Redshift", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: abundances; galaxies: evolution; galaxies: high-redshift", "note": "\u00a9 2010 American Astronomical Society. \n\nReceived 2010 April 16; accepted 2010 June 23; published 2010 July 27. \n\nWe thank the anonymous referee for a constructive report; Gary Ferland for valuable assistance with the interpretation of the Cloudy results; Paul Crowther, Kristian Finlator, Jay Gallagher, Samantha Rix, and Elizabeth Stanway for useful conversations; and the staff of Keck Observatory for assistance with the observations. D.K.E. is supported by the Spitzer Fellowship Program of the National Aeronautics and Space Administration under Award No. NAS7-03001 and the California Institute of Technology. Additional support comes from the US National Science Foundation through grants AST-0606912 and AST-0908805, and the David and Lucile Packard Foundation (A.E.S. and C.C.S.). C.C.S. acknowledges additional support from the John D. and Catherine T. MacArthur Foundation. We wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests.\n\nPublished - Erb2010p11215Astrophys_J.pdf
", "abstract": "Increasingly large samples of galaxies are now being discovered at redshifts z ~ 5-6 and higher. Many of these objects are inferred to be young, low in mass, and relatively unreddened, but detailed analysis of their high quality spectra will not be possible until the advent of future facilities. In this paper, we shed light on the physical conditions in a plausibly similar low-mass galaxy by presenting the analysis of the rest-frame optical and UV spectra of Q2343-BX418, an L* galaxy at z = 2.3 with a very low mass-to-light ratio and unusual properties: BX418 is young (<100 Myr), low mass (M_* ~ 109 M_\u2609), low in metallicity (Z ~ 1/6 Z_\u2609), and unreddened (E(B \u2013 V) \u2243 0.02, UV continuum slope \u03b2 = \u20132.1). We infer a metallicity 12 + log(O/H) = 7.9 \u00b1 0.2 from the rest-frame optical emission lines. We also determine the metallicity via the direct, electron temperature method, using the ratio O III] \u03bb\u03bb1661, 1666/[O III] \u03bb5007 to determine the electron temperature and finding 12 + log(O/H) = 7.8 \u00b1 0.1. These measurements place BX418 among the most metal-poor galaxies observed in emission at high redshift. The rest-frame UV spectrum, which represents ~12 hr of integration with the Keck telescope, contains strong emission from Ly\u03b1 (with rest-frame equivalent width 54 \u00c5), He II \u03bb1640 (both stellar and nebular), C III] \u03bb\u03bb1907, 1909 and O III] \u03bb\u03bb1661, 1666. The C IV/C III] ratio indicates that the source of ionization is unlikely to be an active galactic nucleus. Analysis of the He II, O III], and C III] line strengths indicates a very high ionization parameter log U ~ \u20131, while Ly\u03b1 and the interstellar absorption lines indicate that outflowing gas is highly ionized over a wide range of velocities. It remains to be determined how many of BX418's unique spectral features are due to its global properties, such as low metallicity and dust extinction, and how many are indicative of a short-lived phase in the early evolution of an otherwise normal star-forming galaxy.", "date": "2010-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "719", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1168-1190", "id_number": "CaltechAUTHORS:20100901-164318892", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100901-164318892", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Spitzer Fellowship", "grant_number": "NAS7-03001" }, { "agency": "Caltech" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "John D. and Catherine T. MacArthur Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/719/2/1168", "primary_object": { "basename": "Erb2010p11215Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/fb3x1-d2151/files/Erb2010p11215Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Erb, Dawn K.; Pettini, Max; et el." }, { "id": "https://authors.library.caltech.edu/records/tz92d-1na85", "eprint_id": 18985, "eprint_status": "archive", "datestamp": "2023-08-22 00:18:15", "lastmod": "2023-10-20 19:15:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Bogosavljevi\u0107-M", "name": { "family": "Bogosavljevi\u0107", "given": "Milan" } }, { "id": "Rudie-G-C", "name": { "family": "Rudie", "given": "Gwen C." }, "orcid": "0000-0002-8459-5413" }, { "id": "Rakic-O", "name": { "family": "Rakic", "given": "Olivera" } } ] }, "title": "The Structure and Kinematics of the Circumgalactic Medium from Far-ultraviolet Spectra of z \u2243 2-3 Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: high-redshift", "note": "\u00a9 2010 American Astronomical Society. \n\nReceived 2010 February 22; accepted 2010 May 11; published 2010 June 10. \n\nBased on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. \n\nThis work has been supported by the US National Science Foundation through grants AST-0606912 and AST-0908805 (C.C.S.), and by the David and Lucile Packard Foundation (A.E.S., C.C.S.). C.C.S. acknowledges additional support from the John D. and Catherine T. MacArthur Foundation. D.K.E. is supported by the National Aeronautics and Space Administration under Award No. NAS7-03001 and the California Institute of Technology. We thank Juna Kollmeier and Joop Schaye for interesting and useful conversations, and Patrick Hall, Martin Haehnelt, and the referee for comments that significantly improved the final version of the paper. Kurt Adelberger played a major role in the early days of the survey used in this paper; his intellectual contributions have remained crucial though he has moved on to new challenges in the \"real\" world. Marc Kassis and the rest of the W. M. Keck Observatory staff keep the instruments and telescopes running effectively, for which we are extremely grateful.We extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests.\n\nPublished - Steidel2010p10605Astrophys_J.pdf
", "abstract": "We present new results on the kinematics and spatial distribution of metal-enriched gas within ~125 kpc of star-forming (\"Lyman break\") galaxies at redshifts 2 \u2272 z \u2272 3. In particular, we focus on constraints provided by the rest-frame far-ultraviolet (far-UV) spectra of faint galaxies, and demonstrate how galaxy spectra can be used to obtain key spatial and spectral information more efficiently than possible with QSO sightlines. Using a sample of 89 galaxies with z = 2.3 \u00b1 0.3 and with both rest-frame far-UV and H\u03b1 spectra, we re-calibrate the measurement of accurate galaxy systemic redshifts using only survey-quality rest-UV spectra. We use the velocity-calibrated sample to investigate the kinematics of the galaxy-scale outflows via the strong interstellar (IS) absorption lines and Ly\u03b1 emission (when present), as well as their dependence on other physical properties of the galaxies. We construct a sample of 512 close (1\"-15\") angular pairs of z ~ 2-3 galaxies with redshift differences indicating a lack of physical association. Sightlines to the background galaxies provide new information on the spatial distribution of circumgalactic gas surrounding the foreground galaxies. The close pairs sample galactocentric impact parameters 3-125 kpc (physical) at = 2.2, providing for the first time a robust map of cool gas as a function of galactocentric distance for a well-characterized population of galaxies. We propose a simple model of circumgalactic gas that simultaneously matches the kinematics, depth, and profile shape of IS absorption and Ly\u03b1 emission lines, as well as the observed variation of absorption line strength (H I and several metallic species) versus galactocentric impact parameter. Within the model, cool gas is distributed symmetrically around every galaxy, accelerating radially outward with v_(out)(r) increasing with r (i.e., the highest velocities are located at the largest galactocentric distances r). The inferred radial dependence of the covering fraction of cool gas (which modulates the absorption line strength) is f_c(r) \u221d r^(\u2013\u03b3) with 0.2 \u2272 \u03b3 \u2272 0.6 depending on transition. We discuss the results of the observations in the context of \"cold accretion,\" in which cool gas is accreting via filamentary streams directly onto the central regions of galaxies. At present, we find little observational evidence for cool infalling material, while evidence supporting the large-scale effects of superwind outflows is strong. This \"pilot\" study using faint galaxy spectra demonstrates the potential of using galaxies to trace baryons within galaxies, in the circumgalactic medium, and ultimately throughout the intergalactic medium.", "date": "2010-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "717", "number": "1", "publisher": "American Astronomical Society", "pagerange": "289-322", "id_number": "CaltechAUTHORS:20100709-165047127", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100709-165047127", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0908805" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "NASA", "grant_number": "NAS7-03001" }, { "agency": "Caltech" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/717/1/289", "primary_object": { "basename": "Steidel2010p10605Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/tz92d-1na85/files/Steidel2010p10605Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Steidel, Charles C.; Erb, Dawn K.; et el." }, { "id": "https://authors.library.caltech.edu/records/xsjhj-d7g20", "eprint_id": 17883, "eprint_status": "archive", "datestamp": "2023-08-21 23:42:32", "lastmod": "2023-10-20 15:22:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" } ] }, "title": "Dust Obscuration and Metallicity at High Redshift: New Inferences from UV, H\u03b1, and 8 \u03bcm Observations of z ~ 2 Star-forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: abundances; galaxies: evolution; galaxies: high-redshift; infrared: galaxies", "note": "\u00a9 2010 American Astronomical Society. \n\nReceived 2009 October 27; accepted for publication 2010 February 3; published 2010 March 10. \n\nWe thank the staff of the Keck and Palomar Observatories for their help in obtaining the data presented here. Support for N.A.R. was provided by NASA through Hubble Fellowship grant HST-HF-01223.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Additional support has been provided by research funding for the Spitzer Space Telescope Legacy Science Program, provided by NASA through contracts 1224666 and 1287778, issued by the Jet Propulsion Laboratory, California Institute of Technology. C.C.S. has been supported by grants AST 03-07263 and AST 06-06912 from the National Science Foundation and by the David and Lucile Packard Foundation.\n\nPublished - Reddy2010p7396Astrophys_J.pdf
", "abstract": "We use a sample of 90 spectroscopically confirmed Lyman break galaxies with H\u03b1 measurements and Spitzer MIPS 24 \u03bcm observations to constrain the relationship between rest-frame 8 \u03bcm luminosity (L_8) and star formation rate (SFR) for L* galaxies at z ~ 2. We find a tight correlation with 0.24 dex scatter between L_8 and H\u03b1 luminosity/SFR for z ~ 2 galaxies with 10^(10) L_\u2609 \u2272 L_(IR) \u2272 10^(12) L_\u2609. Employing this relationship with a larger sample of 392 galaxies with spectroscopic redshifts, we find that the UV slope \u03b2 can be used to recover the dust attenuation of the vast majority of moderately luminous L* galaxies at z ~ 2 to within a 0.4 dex scatter using the local correlation. Separately, young galaxies with ages \u2272100 Myr appear to be less dusty than their UV slopes would imply based on the local trend and may follow an extinction curve that is steeper than what is typically assumed. Consequently, very young galaxies at high redshift may be significantly less dusty than inferred previously. Our results provide the first direct evidence, independent of the UV slope, for a correlation between UV and bolometric luminosity (L_(bol)) at high redshift, in the sense that UV-faint galaxies are on average less infrared and less bolometrically luminous than their UV-bright counterparts. The L_(bol)-L_(UV) relation indicates that as the SFR increases, L_(UV) turns over (or \"saturates\") around the value of L* at z ~ 2, implying that dust obscuration may be largely responsible for modulating the bright end of the UV luminosity function. Finally, dust attenuation is found to correlate with oxygen abundance at z ~ 2. Accounting for systematic differences in local and high-redshift metallicity calibrations, we find that L* galaxies at z ~ 2, while at least an order of magnitude more bolometrically luminous, exhibit ratios of metals to dust that are similar to those of local starbursts. This result is expected if high-redshift galaxies are forming their stars in a less metal-rich environment compared to local galaxies of the same luminosity, thus naturally leading to a redshift evolution in both the bolometric luminosity-metallicity and bolometric luminosity-obscuration relations.", "date": "2010-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "712", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1070-1091", "id_number": "CaltechAUTHORS:20100407-095436265", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100407-095436265", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-01223.01" }, { "agency": "NASA", "grant_number": "1224666" }, { "agency": "NASA", "grant_number": "1287778" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "AST 03-07263" }, { "agency": "NSF", "grant_number": "AST 06-06912" }, { "agency": "David and Lucile Packard Foundation" } ] }, "doi": "10.1088/0004-637X/712/2/1070", "primary_object": { "basename": "Reddy2010p7396Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/xsjhj-d7g20/files/Reddy2010p7396Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Reddy, Naveen A.; Erb, Dawn K.; et el." }, { "id": "https://authors.library.caltech.edu/records/hwk92-kds45", "eprint_id": 17766, "eprint_status": "archive", "datestamp": "2023-08-21 23:34:25", "lastmod": "2023-10-20 00:13:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kacprzak-G-G", "name": { "family": "Kacprzak", "given": "Glenn G." } }, { "id": "Churchill-C-W", "name": { "family": "Churchill", "given": "Christopher W." } }, { "id": "Ceverino-D", "name": { "family": "Ceverino", "given": "Daniel" }, "orcid": "0000-0002-8680-248X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Klypin-A", "name": { "family": "Klypin", "given": "Anatoly" } }, { "id": "Murphy-M-T", "name": { "family": "Murphy", "given": "Michael T." } } ] }, "title": "Halo Gas and Galaxy Disk Kinematics Derived from Observations and \u039bCDM Simulations of Mg II Absorption-selected Galaxies at Intermediate Redshift", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: halos; galaxies: kinematics and dynamics; intergalactic medium; quasars: absorption lines", "note": "\u00a9 2010 The American Astronomical Society. \n\nIssue 2 (2010 March 10); received 2008 July 7, accepted for publication 2009 December 17; published 2010 February 16. \n\nWe thank Greg Wirth for his help and advice with ESI/Keck. We are grateful to A. Kravtsov for providing the hydro code. We are in debt to N. Gnedin creating the graphics package IFRIT. We thank Aneta Siemiginowska for her discussion regarding the X-ray data of Q127\u2212145. We express our gratitude to the anonymous referee for a careful reading and for insightful comments that lead to an improved manuscript. C.W.C and G.G.K were funded by the NSF grant AST 0708210. G.G.K was partially funded by the NMSU Graduate Research Enhancement Grant. M.T.M thanks the Australian Research Council for a QEII Research Fellowship (DP0877998). Most of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Some observations were made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5\u201326555. Some of this research was based on observations made with ESO Telescopes at the Paranal Observatories under program IDs listed in Table 1. The computer simulations presented in this paper were performed at the National Energy Research Scientific Computing Center (NERSC) of the Lawrence Berkeley National Laboratory.\n\nPublished - Kacprzak2010p7261Astrophys_J.pdf
", "abstract": "We obtained ESI/Keck rotation curves of 10 Mg II absorption-selected galaxies (0.3 \u2264 z \u2264 1.0) for which we have WFPC-2/HST images and high-resolution HIRES/Keck and UVES/VLT quasar spectra of the Mg II absorption profiles. We perform a kinematic comparison of these galaxies and their associated halo Mg II absorption. For all 10 galaxies, the majority of the absorption velocities lie in the range of the observed galaxy rotation velocities. In 7/10 cases, the absorption velocities reside fully to one side of the galaxy systemic velocity and usually align with one arm of the rotation curve. In all cases, a constant rotating thick-disk model poorly reproduces the full spread of observed Mg II absorption velocities when reasonably realistic parameters are employed. In 2/10 cases, the galaxy kinematics, star formation surface densities, and absorption kinematics have a resemblance to those of high-redshift galaxies showing strong outflows. We find that Mg II absorption velocity spread and optical depth distribution may be dependent on galaxy inclination. To further aid in the spatial-kinematic relationships of the data, we apply quasar absorption-line techniques to a galaxy (v_c = 180 km s^(\u20131)) embedded in \u039bCDM simulations. In the simulations, Mg II absorption selects metal-enriched \"halo\" gas out to ~100 kpc from the galaxy, tidal streams, filaments, and small satellite galaxies. Within the limitations inherent in the simulations, the majority of the simulated Mg II absorption arises in the filaments and tidal streams and is infalling toward the galaxy with velocities between \u2013200 km s^(-1) \u2264 v_r \u2264 \u2013180 km s^(\u20131). The Mg II absorption velocity offset distribution (relative to the simulated galaxy) spans ~200 km s^(\u20131) with the lowest frequency of detecting Mg II at the galaxy systematic velocity.", "date": "2010-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "711", "number": "2", "publisher": "American Astronomical Society", "pagerange": "533-558", "id_number": "CaltechAUTHORS:20100317-113658511", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100317-113658511", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0708210" }, { "agency": "New Mexico State University" }, { "agency": "Australian Research Council", "grant_number": "DP0877998" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA", "grant_number": "NAS 5\u201326555" } ] }, "doi": "10.1088/0004-637X/711/2/533", "primary_object": { "basename": "Kacprzak2010p7261Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/hwk92-kds45/files/Kacprzak2010p7261Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Kacprzak, Glenn G.; Churchill, Christopher W.; et el." }, { "id": "https://authors.library.caltech.edu/records/1b7gs-1g970", "eprint_id": 17761, "eprint_status": "archive", "datestamp": "2023-08-21 23:34:15", "lastmod": "2023-10-20 00:12:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kornei-K-A", "name": { "family": "Kornei", "given": "Katherine A." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Bogosavljevi\u0107-M", "name": { "family": "Bogosavljevi\u0107", "given": "Milan" } } ] }, "title": "The Relationship between Stellar Populations and Ly\u03b1 Emission in Lyman Break Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: starburst", "note": "\u00a9 2010 The American Astronomical Society. \n\nReceived 2009 September 4; accepted 2010 January 22; published 2010 February 17. \n\nWe thank Kim Nilsson and Eric Gawiser for kindly providing their data for comparison. A.E.S. acknowledges support from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation. D.K.E. is supported by a Spitzer Fellowship through a NASA grant administrated by the Spitzer Science Center. C.C.S. has been supported by grants AST 03-07263 and AST 06-06912 from the National Science Foundation and by the David and Lucile Packard Foundation. Support for N.A.R. was provided by NASA through Hubble Fellowship grant HST-HF-01223.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. We also wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA.\n\nPublished - Kornei2010p7262Astrophys_J.pdf
", "abstract": "We present the results of a photometric and spectroscopic survey of 321 Lyman break galaxies (LBGs) at z ~ 3 to investigate systematically the relationship between Ly\u03b1 emission and stellar populations. Ly\u03b1 equivalent widths (W_(Ly\u03b1)) were calculated from rest-frame UV spectroscopy and optical/near-infrared/Spitzer photometry was used in population synthesis modeling to derive the key properties of age, dust extinction, star formation rate (SFR), and stellar mass. We directly compare the stellar populations of LBGs with and without strong Ly\u03b1 emission, where we designate the former group (W_(Ly\u03b1) \u2265 20 \u00c5) as Ly\u03b1 emitters (LAEs) and the latter group (W_(Ly\u03b1) < 20 \u00c5) as non-LAEs. This controlled method of comparing objects from the same UV luminosity distribution represents an improvement over previous studies in which the stellar populations of LBGs and narrowband-selected LAEs were contrasted, where the latter were often intrinsically fainter in broadband filters by an order of magnitude simply due to different selection criteria. Using a variety of statistical tests, we find that Ly\u03b1 equivalent width and age, SFR, and dust extinction, respectively, are significantly correlated in the sense that objects with strong Ly\u03b1 emission also tend to be older, lower in SFR, and less dusty than objects with weak Ly\u03b1 emission, or the line in absorption. We accordingly conclude that, within the LBG sample, objects with strong Ly\u03b1 emission represent a later stage of galaxy evolution in which supernovae-induced outflows have reduced the dust covering fraction. We also examined the hypothesis that the attenuation of Ly\u03b1 photons is lower than that of the continuum, as proposed by some, but found no evidence to support this picture.", "date": "2010-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "711", "number": "2", "publisher": "American Astronomical Society", "pagerange": "693-710", "id_number": "CaltechAUTHORS:20100317-111435674", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100317-111435674", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "David and Lucile Packard Foundation" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NASA Spitzer Fellowship" }, { "agency": "NSF", "grant_number": "AST 03-07263" }, { "agency": "NSF", "grant_number": "AST 06-06912" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-01223.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/711/2/693", "primary_object": { "basename": "Kornei2010p7262Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/1b7gs-1g970/files/Kornei2010p7262Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Kornei, Katherine A.; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/0m35g-vdw91", "eprint_id": 17642, "eprint_status": "archive", "datestamp": "2023-08-21 23:33:04", "lastmod": "2023-10-20 00:06:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Quider-A-M", "name": { "family": "Quider", "given": "Anna M." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Stark-D-P", "name": { "family": "Stark", "given": "Daniel P." } } ] }, "title": "A study of interstellar gas and stars in the gravitationally lensed galaxy 'the Cosmic Eye' from rest-frame ultraviolet spectroscopy", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: individual: Cosmic Eye; galaxies: starburst; cosmology: observations", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS. \n\nAccepted 2009 November 5. Received 2009 November 4; in original form 2009 October 5. \n\nWe are grateful to the staff at the W. M. Keck Observatory for their competent assistance with the observations. Valuable suggestions by an anonymous referee improved the final version of this paper. AMQ's research is funded by a scholarship from the Marshall Foundation, and a National Science Foundation graduate research fellowship. AES acknowledges support from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation, and CCS from NSF grant AST-0606912 and the John D. and Catherine T. MacArthur Foundation. DPS's research is supported by the UK STFC through the award of a postdoctoral fellowship. Finally, we wish to extend thanks to those of Hawaiian ancestry on whose mountain we are privileged to be guests.\n\nPublished - Quider2010p7173Mon_Not_R_Astron_Soc.pdf
", "abstract": "We report the results of a study of the rest-frame ultraviolet (UV) spectrum of the Cosmic Eye (J213512.73\u2212010143) , a luminous (L\u223c 2L*) Lyman break galaxy at z_(sys)= 3.07331 magnified by a factor of ~25 via gravitational lensing by foreground mass concentrations at z= 0.73 and 0.33. The spectrum, recorded at high resolution and signal-to-noise ratio with the Echellette Spectrograph and Imager (ESI) spectrograph on the Keck II telescope, is rich in absorption features from the gas and massive stars in this galaxy. The interstellar absorption lines are resolved into two components of approximately equal strength and each spanning several hundred km s^(\u22121) in velocity. One component has a net blueshift of \u221270 km s^(\u22121) relative to the stars and H II regions and presumably arises in a galaxy-scale outflow similar to those seen in most star-forming galaxies at z= 2\u20133 . The other is more unusual in showing a mean redshift of +350 km s^(\u22121) relative to z_(sys); possible interpretations include a merging clump, or material ejected by a previous star formation episode and now falling back on to the galaxy, or more simply a chance alignment with a foreground galaxy. In the metal absorption lines, both components only partially cover the OB stars against which they are being viewed. However, there must also be more pervasive diffuse gas to account for the near-total covering fraction of the strong damped Ly\u03b1 line, indicative of a column density N(HI) = (3.0 \u00b1 0.8) \u00d7 10^(21) cm^(\u22122) . We tentatively associate this neutral gas with the redshifted component, and propose that it provides the dust 'foreground screen' responsible for the low ratio of far-infrared to UV luminosities of the Cosmic Eye.\n\nThe C IV P Cygni line in the stellar spectrum is consistent with continuous star formation with a Salpeter initial mass function, stellar masses from 5 to 100 M_\u2299 , and a metallicity Z ~ 0.4 Z_\u2299. Compared to other well-studied examples of strongly lensed galaxies, we find that the young stellar population of the Cosmic Eye is essentially indistinguishable from those of the Cosmic Horseshoe and MS 1512\u2212cB58 . On the other hand, the interstellar spectra of all three galaxies are markedly different, attesting to the real complexity of the interplay between starbursts and ambient interstellar matter in young galaxies observed during the epoch when cosmic star formation was at its peak.", "date": "2010-03-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "402", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "1467-1479", "id_number": "CaltechAUTHORS:20100303-095354486", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100303-095354486", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Marshall Foundation" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "John D. and Catherine T. MacArthur Foundation" }, { "agency": "Science and Technology Facilities Council (STFC)" } ] }, "doi": "10.1111/j.1365-2966.2009.16005.x", "primary_object": { "basename": "Quider2010p7173Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/0m35g-vdw91/files/Quider2010p7173Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Quider, Anna M.; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/3aqts-8jq44", "eprint_id": 17514, "eprint_status": "archive", "datestamp": "2023-08-21 23:17:32", "lastmod": "2023-10-19 23:57:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aird-J-A", "name": { "family": "Aird", "given": "J." }, "orcid": "0000-0003-1908-8463" }, { "id": "Nandra-K", "name": { "family": "Nandra", "given": "K." }, "orcid": "0000-0002-7150-9192" }, { "id": "Laird-E-S", "name": { "family": "Laird", "given": "E. S." } }, { "id": "Georgakakis-A", "name": { "family": "Georgakakis", "given": "A." } }, { "id": "Ashby-M-L-N", "name": { "family": "Ashby", "given": "M. L. N." }, "orcid": "0000-0002-3993-0745" }, { "id": "Barmby-P", "name": { "family": "Barmby", "given": "P." }, "orcid": "0000-0003-2767-0090" }, { "id": "Coil-A-L", "name": { "family": "Coil", "given": "A. L." } }, { "id": "Huang-J-S", "name": { "family": "Huang", "given": "J.-S." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Willmer-C-N-A", "name": { "family": "Willmer", "given": "C. N. A." } } ] }, "title": "The evolution of the hard X-ray luminosity function of AGN", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: evolution; galaxies: luminosity function, mass function; X-rays: galaxies", "note": "\u00a9 2010 RAS. \n\nAccepted 2009 October 5. Received 2009 September 3; in original form 2009 April 29. \n\nWe acknowledge financial support from STFC (JA, ESL). Some\nobservations reported here were obtained at the MMT Observatory,\na joint facility of the Smithsonian Institution and the University\nof Arizona. Also based in part on observations obtained with\nMegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA,\nat the CFHT which is operated by the National Research Council\n(NRC) of Canada, the Institut National des Sciences de l'Univers of\nthe Centre National de la Recherche Scientifique (CNRS) of France\nand the University of Hawaii. This work is based in part on data\nproducts produced at TERAPIX and the Canadian Astronomy Data\nCentre as part of the CFHTLS, a collaborative project of NRC and CNRS.\n\nPublished - Aird2010p7031Mon_Not_R_Astron_Soc.pdf
", "abstract": "We present new observational determinations of the evolution of the 2\u201310 keV X-ray luminosity function (XLF) of active galactic nuclei (AGN). We utilize data from a number of surveys including both the 2 Ms Chandra Deep Fields and the AEGIS-X 200 ks survey, enabling accurate measurements of the evolution of the faint end of the XLF. We combine direct, hard X-ray selection and spectroscopic follow-up or photometric redshift estimates at z < 1.2 with a rest-frame UV colour pre-selection approach at higher redshifts to avoid biases associated with catastrophic failure of the photometric redshifts. Only robust optical counterparts to X-ray sources are considered using a likelihood ratio matching technique. A Bayesian methodology is developed that considers redshift probability distributions, incorporates selection functions for our high-redshift samples and allows robust comparison of different evolutionary models. We statistically account for X-ray sources without optical counterparts to correct for incompleteness in our samples. We also account for Poissonian effects on the X-ray flux estimates and sensitivities and thus correct for the Eddington bias. We find that the XLF retains the same shape at all redshifts, but undergoes strong luminosity evolution out to z ~ 1 , and an overall negative density evolution with increasing redshift, which thus dominates the evolution at earlier times. We do not find evidence that a luminosity-dependent density evolution, and the associated flattening of the faint-end slope, is required to describe the evolution of the XLF. We find significantly higher space densities of low-luminosity, high-redshift AGN than in prior studies, and a smaller shift in the peak of the number density to lower redshifts with decreasing luminosity. The total luminosity density of AGN peaks at z= 1.2 \u00b1 0.1 , but there is a mild decline to higher redshifts. We find that >50 per cent of black hole growth takes place at z > 1 , with around half in L_X < 10^(44) erg s^(\u22121) AGN.", "date": "2010-02", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "401", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "2531-2551", "id_number": "CaltechAUTHORS:20100218-101337738", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100218-101337738", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)" } ] }, "doi": "10.1111/j.1365-2966.2009.15829.x", "primary_object": { "basename": "Aird2010p7031Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/3aqts-8jq44/files/Aird2010p7031Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Aird, J.; Nandra, K.; et el." }, { "id": "https://authors.library.caltech.edu/records/46cfy-xc155", "eprint_id": 16925, "eprint_status": "archive", "datestamp": "2023-08-21 22:50:55", "lastmod": "2023-10-19 22:39:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "F\u00f6rster-Schreiber-N-M", "name": { "family": "F\u00f6rster Schreiber", "given": "N. M." } }, { "id": "Genzel-Reinhard", "name": { "family": "Genzel", "given": "R." }, "orcid": "0000-0002-2767-9653" }, { "id": "Bouch\u00e9-N", "name": { "family": "Bouch\u00e9", "given": "N." } }, { "id": "Cresci-G", "name": { "family": "Cresci", "given": "G." } }, { "id": "Davies-R", "name": { "family": "Davies", "given": "R." } }, { "id": "Buschkamp-P", "name": { "family": "Buschkamp", "given": "P." } }, { "id": "Shapiro-K-L", "name": { "family": "Shapiro", "given": "K." } }, { "id": "Tacconi-Linda-J", "name": { "family": "Tacconi", "given": "L. J." }, "orcid": "0000-0002-1485-9401" }, { "id": "Hicks-E-K-S", "name": { "family": "Hicks", "given": "E. K. S." } }, { "id": "Genel-S", "name": { "family": "Genel", "given": "S." }, "orcid": "0000-0002-3185-1540" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "A. E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "D. K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Eisenhauer-F", "name": { "family": "Eisenhauer", "given": "F." } }, { "id": "Gillessen-S", "name": { "family": "Gillessen", "given": "S." } }, { "id": "Sternberg-A", "name": { "family": "Sternberg", "given": "A." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "Kurk-J", "name": { "family": "Kurk", "given": "J." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Kong-X", "name": { "family": "Kong", "given": "X." } }, { "id": "Lehnert-Matthew-D", "name": { "family": "Lehnert", "given": "M. D." }, "orcid": "0000-0003-1939-5885" }, { "id": "Nesvadba-N-P-H", "name": { "family": "Nesvadba", "given": "N." } }, { "id": "Verma-A", "name": { "family": "Verma", "given": "A." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H." }, "orcid": "0000-0002-9489-7765" }, { "id": "Arimoto-Nobuo", "name": { "family": "Arimoto", "given": "N." } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "M." } }, { "id": "Onodera-Masato", "name": { "family": "Onodera", "given": "M." } } ] }, "title": "The SINS Survey: SINFONI Integral Field Spectroscopy of z ~ 2 Star-forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: kinematics and dynamics; infrared: galaxies", "note": "\u00a9 2009 American Astronomical Society. \n\nPrint publication: Issue 2 (2009 December 1); received 2009 March 10; accepted for publication 2009 October 19; published 2009 November 11. \n\nWe thank the ESO staff, and in particular at Paranal Observatory, for their helpful and enthusiastic support during the many observing runs and several years over which SINFONI GTO were carried out. We also thank the SINFONI and PARSEC teams for their hard work on the instrument and the laser, which allowed our observational program to be carried out so successfully. We thank the referee for useful comments and suggestions that helped improve the quality and presentation of the paper. This paper and the SINS survey have benefited from many constructive, insightful, and enthusiastic discussions with many colleagues whom we are very grateful to, especially Marijn Franx for numerous inspiring discussions, as well as\nAndi Burkert, Thorsten Naab, Peter Johansson, Ortwin Gerhard, Avishai Dekel, Pieter van Dokkum, Guinevere Kauffmann, Simon White, Hans-Walter Rix, St\u00b4ephane Courteau, Martin Bureau, Claudia Maraston, among many others.We are grateful to Ian Smail, Scott Chapman, and Rob Ivison for providing the necessary information and imaging data of SMGs targeted as part of our SINS survey. N.M.F.S. acknowledges support by the Schwerpunkt\nProgramme SPP1177 of the Deutsche Forschungsgemeinschaft\nand by the Minerva Program of the Max-Planck-Gesellschaft. N.A. is supported by a Grant-in-Aid for Science Research (19549245) by the Japanese Ministry of Education, Culture, Sports, Science and Technology.\n\nPublished - Schreiber2009p6523Astrophys_J_Lett.pdf
", "abstract": "We present the Spectroscopic Imaging survey in the near-infrared (near-IR) with SINFONI (SINS) of high-redshift galaxies. With 80 objects observed and 63 detected in at least one rest-frame optical nebular emission line, mainly H\u03b1, SINS represents the largest survey of spatially resolved gas kinematics, morphologies, and physical properties of star-forming galaxies at z ~ 1-3. We describe the selection of the targets, the observations, and the data reduction. We then focus on the \"SINS H\u03b1 sample,\" consisting of 62 rest-UV/optically selected sources at 1.3 < z < 2.6 for which we targeted primarily the H\u03b1 and [N II] emission lines. Only \u224830% of this sample had previous near-IR spectroscopic observations. The galaxies were drawn from various imaging surveys with different photometric criteria; as a whole, the SINS H\u03b1 sample covers a reasonable representation of massive M_* \u2273 10^(10) M_\u2609 star-forming galaxies at z \u2248 1.5-2.5, with some bias toward bluer systems compared to pure K-selected samples due to the requirement of secure optical redshift. The sample spans 2 orders of magnitude in stellar mass and in absolute and specific star formation rates, with median values \u22483 \u00d7 10^(10) M_\u2609, \u224870 M_\u2609 yr^(\u20131), and \u22483 Gyr^(\u20131). The ionized gas distribution and kinematics are spatially resolved on scales ranging from \u22481.5 kpc for adaptive optics assisted observations to typically \u22484-5 kpc for seeing-limited data. The H\u03b1 morphologies tend to be irregular and/or clumpy. About one-third of the SINS H\u03b1 sample galaxies are rotation-dominated yet turbulent disks, another one-third comprises compact and velocity dispersion-dominated objects, and the remaining galaxies are clear interacting/merging systems; the fraction of rotation-dominated systems increases among the more massive part of the sample. The H\u03b1 luminosities and equivalent widths suggest on average roughly twice higher dust attenuation toward the H II regions relative to the bulk of the stars, and comparable current and past-averaged star formation rates.", "date": "2009-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "706", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1364-1428", "id_number": "CaltechAUTHORS:20091209-112844140", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091209-112844140", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "19549245" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/706/2/1364", "primary_object": { "basename": "Schreiber2009p6523Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/46cfy-xc155/files/Schreiber2009p6523Astrophys_J_Lett.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "F\u00f6rster Schreiber, N. M.; Genzel, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/fmsn3-7s057", "eprint_id": 15488, "eprint_status": "archive", "datestamp": "2023-08-21 22:06:52", "lastmod": "2023-10-19 14:30:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shapiro-K-L", "name": { "family": "Shapiro", "given": "Kristen L." } }, { "id": "Genzel-Reinhard", "name": { "family": "Genzel", "given": "Reinhard" }, "orcid": "0000-0002-2767-9653" }, { "id": "Quataert-E", "name": { "family": "Quataert", "given": "Eliot" }, "orcid": "0000-0001-9185-5044" }, { "id": "F\u00f6rster-Schreiber-N-M", "name": { "family": "F\u00f6rster Schreiber", "given": "Natascha M." } }, { "id": "Davies-R", "name": { "family": "Davies", "given": "Richard" } }, { "id": "Tacconi-Linda-J", "name": { "family": "Tacconi", "given": "Linda" }, "orcid": "0000-0002-1485-9401" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Bouch\u00e9-N", "name": { "family": "Bouch\u00e9", "given": "Nicolas" } }, { "id": "Buschkamp-P", "name": { "family": "Buschkamp", "given": "Peter" } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "Andrea" } }, { "id": "Cresci-G", "name": { "family": "Cresci", "given": "Giovanni" } }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "Emanuele" }, "orcid": "0000-0002-3331-9590" }, { "id": "Eisenhauer-F", "name": { "family": "Eisenhauer", "given": "Frank" } }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Genel-S", "name": { "family": "Genel", "given": "Shy" }, "orcid": "0000-0002-3185-1540" }, { "id": "Hicks-E-K-S", "name": { "family": "Hicks", "given": "Erin K. S." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "Simon J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "Dieter" }, "orcid": "0000-0003-0291-9582" }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "Alvio" }, "orcid": "0000-0002-7093-7355" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice" }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Sternberg-A", "name": { "family": "Sternberg", "given": "Amiel" } } ] }, "title": "The SINS Survey: Broad Emission Lines in High-Redshift Star-Forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: evolution; galaxies: high-redshift", "note": "\u00a9 2009 American Astronomical Society. \n\nPrint publication: Issue 2 (2009 August 20); received 2009 February 11; accepted for publication 2009 June 16; published 2009 July 28. \n\nWe thank the ESO staff, especially those at Paranal Observatory, for their helpful and enthusiastic support during the many observing runs and several years over which the SINS project was carried out. We also acknowledge the SINFONI and PARSEC teams, whose hard work on the instrument and laser paved the way for the success of the SINS observations. This paper has additionally benefited significantly from many enlightening conversations with colleagues, including Fr\u00e9d\u00e9ric Bournaud, Mohan Ganeshalingam, Kevin Heng, Phil Hopkins, Chris McKee, Jeffrey Silverman, and Thea Steele. Finally, we thank the referee, whose detailed and insightful comments greatly improved the quality of this paper.\n\nPublished - Shapiro2009p5720Astrophys_J.pdf
", "abstract": "High signal-to-noise, representative spectra of star-forming galaxies at z ~ 2, obtained via stacking, reveal a high-velocity component underneath the narrow H\u03b1 and [NII] emission lines. When modeled as a single Gaussian, this broad component has FWHM 1500 km s\u20131; when modeled as broad wings on the H\u03b1 and [N II] features, it has FWHM \u2273 500 km s^(\u20131). This feature is preferentially found in the more massive and more rapidly star-forming systems, which also tend to be older and larger galaxies. We interpret this emission as evidence of either powerful starburst-driven galactic winds or active supermassive black holes (SMBHs). If galactic winds are responsible for the broad emission, the observed luminosity and velocity of this gas imply mass outflow rates comparable to the star formation rate. On the other hand, if the broad-line regions of active black holes account for the broad feature, the corresponding black holes masses are estimated to be an order of magnitude lower than those predicted by local scaling relations, suggesting a delayed assembly of SMBHs with respect to their host bulges.", "date": "2009-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "701", "number": "2", "publisher": "American Astronomical Society", "pagerange": "955-963", "id_number": "CaltechAUTHORS:20090831-131328673", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090831-131328673", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/701/2/955", "primary_object": { "basename": "Shapiro2009p5720Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/fmsn3-7s057/files/Shapiro2009p5720Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Shapiro, Kristen L.; Genzel, Reinhard; et el." }, { "id": "https://authors.library.caltech.edu/records/7dftj-fge90", "eprint_id": 16171, "eprint_status": "archive", "datestamp": "2023-08-21 22:03:21", "lastmod": "2023-10-19 22:00:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Quider-A-M", "name": { "family": "Quider", "given": "Anna M." } }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "The ultraviolet spectrum of the gravitationally lensed galaxy 'the Cosmic Horseshoe': a close-up of a star-forming galaxy at z\u223c 2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: individual: Cosmic Horseshoe; galaxies: starburst; cosmology: observations", "note": "Journal compilation \u00a9 2009 RAS. \n\nAccepted 2009 June 8. Received 2009 June 7; in original form 2009 May 1. \n\nWe are grateful to the staff at the W. M. Keck Observatory for their competent assistance with the observations, to Sam Rix and Dan Nestor who generously provided some of the software used in the analysis of the spectra and to Simon Dye for clarifications concerning\nthe lensing models. Lindsay King kindly allowed us to reproduce\nher ESO/FORS2 image of the Cosmic Horseshoe in Fig. 1. We also thank the anonymous referee for helpful comments which have improved the paper. AMQ's research is funded by a scholarship from the Marshall Foundation. AES acknowledges support from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation, and CCS acknowledges support from NSF grant AST-0606912 and the John D. and Catherine T. MacArthur Foundation. Finally, we wish to extend thanks to those of Hawaiian ancestry on whose mountain we are privileged to be guests.\n\nPublished - Quider2009p5965Mon_Not_R_Astron_Soc.pdf
", "abstract": "Taking advantage of strong gravitational lensing, we have recorded the rest-frame ultraviolet (UV) spectrum of the z= 2.38115 galaxy 'the Cosmic Horseshoe' (J1148+1930) at higher resolution and signal-to-noise ratio than is currently feasible for unlensed galaxies at z= 2\u20133 . With a star formation rate of ~100 M_\u2299 yr^(\u22121) , dynamical mass M_vir\u2243 1 \u00d7 10^(10) M_\u2299 , half-solar metallicity and moderate reddening E(B\u2212V) = 0.15 , the Cosmic Horseshoe is a good example of the population of galaxies responsible for most of the star formation activity at these redshifts.\nFrom the analysis of stellar spectral features we conclude that a continuous mode of star formation with a Salpeter slope for stars in the mass range 5\u2013100 M_\u2299 gives a good representation of the UV spectrum, ruling out significant departures from a 'standard' initial mass function. Generally, we find good agreement between the values of metallicity deduced from stellar and nebular tracers. Interstellar absorption is present over a velocity range \u0394v\u2243 1000 km s^(\u22121) , from \u2212800 to +250 km s^(\u22121) relative to the stars and their H ii regions, but we still lack a model relating the kinematic structure of the gas to its location within the galaxy. There is evidence to suggest that the outflowing interstellar gas is patchy, covering only \u223c60 per cent of the UV stellar continuum.\nThe Ly\u03b1 line shares many of the characteristics of the so-called Ly\u03b1 emitters; its double-peaked profile can be reproduced by models of Ly\u03b1 photons resonantly scattered by an expanding shell of gas and dust, with \u223c10\u201315 per cent of the photons escaping the galaxy. Many of the physical properties of the Cosmic Horseshoe are similar to those of the only other galaxy at z= 2\u20133 studied in comparable detail up to now: MS 1512\u2212cB58. The fact that these two galaxies have drastically different Ly\u03b1 lines may be due simply to orientation effects, or differences in the covering factor of outflowing gas, and cautions against classifying high-z galaxies only on the basis of spectral features, such as Ly\u03b1, whose appearance can be affected by a variety of different parameters.", "date": "2009-08-10", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "398", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "1263-1278", "id_number": "CaltechAUTHORS:20091002-133653002", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091002-133653002", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Marshall Foundation" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "John D. and Catherine T. MacArthur Foundation" } ] }, "doi": "10.1111/j.1365-2966.2009.15234.x", "primary_object": { "basename": "Quider2009p5965Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/7dftj-fge90/files/Quider2009p5965Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Quider, Anna M.; Pettini, Max; et el." }, { "id": "https://authors.library.caltech.edu/records/sw86a-sz432", "eprint_id": 15665, "eprint_status": "archive", "datestamp": "2023-08-21 21:46:16", "lastmod": "2023-10-19 14:42:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wright-S-A", "name": { "family": "Wright", "given": "Shelley A." }, "orcid": "0000-0003-1034-8054" }, { "id": "Larkin-J-E", "name": { "family": "Larkin", "given": "James E." }, "orcid": "0000-0001-7687-3965" }, { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" } ] }, "title": "Dynamics of Galactic Disks and Mergers at z ~ 1.6: Spatially Resolved Spectroscopy with Keck Laser Guide Star Adaptive Optics", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: kinematics and dynamics; infrared: galaxies", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2008 June 20; accepted 2009 April 29; published 2009 June 11. \n\nThe authors acknowledge the dedicated members of the Keck Observatory staff, particularly Marcos van Dam, Jim Lyke, Randy Campbell, and Al Conrad, who helped greatly with the success of our observations. Our referee offered interesting insight and beneficial suggestions. We would like to thank the generous funding from the Center of Adaptive Optics which supported this research program. Data presented herein were obtained at W.M. Keck Observatory, which is operated as a scientific partnership between the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by generous financial support of the W.M. Keck Foundation. The authors recognize and acknowledge the 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 \"heiau\" mountain.\n\nPublished - Wright2009p4801Astrophys_J.pdf
", "abstract": "We present 0\".2 resolution near-infrared integral field spectroscopy of H\u03b1 emission from six star-forming galaxies at z ~ 1.6 (a look-back time of ~9.6 Gyr). These observations were obtained with OSIRIS using the Keck Laser Guide Star Adaptive Optics system. All sources have a compact spatial extent of ~1\", with an average half-light radius of r_(1/2) = 2.9 kpc and an average dereddened star formation rate of 22 M\u2299 yr^(\u20131). Based on H\u03b1 kinematics we find that these six galaxies are dynamically distinguishable, and we classify them as either irregular/merger or disk candidate systems. We find three systems (HDF-BX1287, HDF-BX1315, and Q1623-BX491) with varying geometries and dynamical properties. Three galaxies (HDF-BMZ1299, Q2343-BX344, and Q2343-BM145) are well fitted by an inclined-disk model with low-velocity residuals (20 to 46 km s^(\u20131)). An average plateau velocity of \u03bd(p) = 185 km s^(\u20131) is achieved within 1.0 kpc. The majority of observed velocity dispersions (\u03c3 ~ 88 km s^(\u20131)) can be explained by the residual seeing halo, and are not intrinsic to our sources. However, one irregular and one disk candidate have high-velocity dispersions (\u03c3_(obs) \u2273 200 km s^(\u20131)) that cannot be solely explained by beam smearing. For two disk candidates, we detect [N II] emission and are able to map the [N II]/H\u03b1 ratio on kiloparsec scales. In both cases, [N II] emission is more concentrated than H\u03b1 emission (\u227e0\".2), and peak ratios are best explained by the presence of an active galactic nucleus (AGN). These are among the weakest known AGNs at high redshift; however their emission is strong enough to impact high-redshift metallicity studies that use nebular ratios. All disk candidates have likely to be completed only a few orbital periods, and if left unperturbed are excellent candidates to become present-day spiral galaxies.", "date": "2009-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "699", "number": "1", "publisher": "American Astronomical Society", "pagerange": "421-440", "id_number": "CaltechAUTHORS:20090908-091007755", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090908-091007755", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/699/1/421", "primary_object": { "basename": "Wright2009p4801Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/sw86a-sz432/files/Wright2009p4801Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Wright, Shelley A.; Larkin, James E.; et el." }, { "id": "https://authors.library.caltech.edu/records/cj044-gjk08", "eprint_id": 15409, "eprint_status": "archive", "datestamp": "2023-08-21 21:36:06", "lastmod": "2023-10-18 21:45:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Larkin-J-E", "name": { "family": "Larkin", "given": "James E." }, "orcid": "0000-0001-7687-3965" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Wright-S-A", "name": { "family": "Wright", "given": "Shelley A." }, "orcid": "0000-0003-1034-8054" } ] }, "title": "The Kiloparsec-scale Kinematics of High-redshift Star-forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: kinematics and dynamics; galaxies: starburst", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2009 January 19; accepted 2009 March 27; published 2009 May 18. \n\nThe authors thank Randy Campbell, Al Conrad, and Jim Lyke for their invaluable assistance obtaining the observations presented herein. D.R.L. also thanks Andrew Benson and Mark Swinbank for constructive discussions, Naveen Reddy for providing stellar mass function data, and the anonymous referee for helpful suggestions which improved the final draft of this manuscript. D.R.L. and C.C.S. have been supported by grants AST-0606912 and AST-0307263 from the US National Science Foundation. Additional support for this work was provided by NASA through Hubble Fellowship grant HF-01221.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Finally, we wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests.\n\nPublished - Law2009p4290Astrophys_J.pdf
", "abstract": "We present the results of a spectroscopic survey of the kinematic structure of star-forming galaxies at redshift z ~ 2-3 using Keck/OSIRIS integral field spectroscopy. Our sample is comprised of 12 galaxies between redshifts z ~ 2.0 and 2.5 and one galaxy at z ~ 3.3 which are well detected in either H\u03b1 or [O III] emission. These galaxies are generally representative of the mean stellar mass of star-forming galaxies at similar redshifts, although they tend to have star formation rate surface densities slightly higher than the mean. These observations were obtained in conjunction with the Keck laser guide star adaptive optics system, with a typical angular resolution after spatial smoothing ~0\".15 (approximately 1 kpc at the redshift of the target sample). At most five of these 13 galaxies have spatially resolved velocity gradients consistent with rotation while the remaining galaxies have relatively featureless or irregular velocity fields. All of our galaxies show local velocity dispersions ~60-100 km s^(\u20131), suggesting that (particularly for those galaxies with featureless velocity fields) rotation about a preferred axis may not be the dominant mechanism of physical support. While some galaxies show evidence for major mergers such evidence is unrelated to the kinematics of individual components (one of our strongest merger candidates also exhibits unambiguous rotational structure), refuting a simple bimodal disk/merger classification scheme. We discuss these data in light of complementary surveys and extant UV-IR spectroscopy and photometry, concluding that the dynamical importance of cold gas may be the primary factor governing the observed kinematics of z ~ 2 galaxies. We conclude by speculating on the importance of mechanisms for accreting low angular momentum gas and the early formation of quasi-spheroidal systems in the young universe.", "date": "2009-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "697", "number": "2", "publisher": "American Astronomical Society", "pagerange": "2057-2082", "id_number": "CaltechAUTHORS:20090828-114836846", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090828-114836846", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0606912" }, { "agency": "NSF", "grant_number": "AST-0307263" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HF-01221.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "doi": "10.1088/0004-637X/697/2/2057", "primary_object": { "basename": "Law2009p4290Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/cj044-gjk08/files/Law2009p4290Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Law, David R.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/37h2f-ww625", "eprint_id": 16142, "eprint_status": "archive", "datestamp": "2023-08-21 20:47:26", "lastmod": "2023-10-19 21:58:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "A Steep Faint-End Slope of the UV Luminosity Function at z ~ 2-3: Implications for the Global Stellar Mass Density and Star Formation in Low-Mass Halos", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: luminosity function, mass function", "note": "\u00a9 2009. The American Astronomical Society. \n\nReceived 2008 July 15; accepted 2008 October 10; published 2009 February 20. \n\nBased, in part, on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation.\n\nPublished - Reddy2009p15110.10880004-637X6921778.pdf
", "abstract": "We use the deep ground-based optical photometry of the Lyman Break Galaxy (LBG) Survey to derive robust measurements of the faint-end slope (\u03b1) of the UV luminosity function (LF) at redshifts 1.9 \u2264 z \u2264 3.4. Our sample includes >2000 spectroscopic redshifts and 31000 LBGs in 31 spatially independent fields over a total area of 3261 arcmin^2. These data allow us to select galaxies to 0.07L^* and 0.10L^* at z ~ 2 and z ~ 3, respectively. A maximum-likelihood analysis indicates steep values of \u03b1(z = 2) = \u20131.73 \u00b1 0.07 and \u03b1(z = 3) = \u20131.73 \u00b1 0.13. This result is robust to luminosity-dependent systematics in the Ly\u03b1 equivalent width and reddening distributions, and is similar to the steep values advocated at z 4, and implies that 93% of the unobscured UV luminosity density at z ~ 2-3 arises from sub-L^* galaxies. With a realistic luminosity-dependent reddening distribution, faint to moderately luminous galaxies account for 70% and 25% of the bolometric luminosity density and present-day stellar mass density, respectively, when integrated over 1.9 \u2264 z < 3.4. We find a factor of 8-9 increase in the star-formation rate density between z ~ 6 and z ~ 2, due to both a brightening of L^* and an increasing dust correction proceeding to lower redshifts. Combining the UV LF with stellar mass estimates suggests a relatively steep low-mass slope of the stellar mass function at high redshift. The previously observed discrepancy between the integral of the star-formation history and stellar mass density measurements at z ~ 2 may be reconciled by invoking a luminosity-dependent reddening correction to the star-formation history combined with an accounting for the stellar mass contributed by UV-faint galaxies. The steep and relatively constant faint-end slope of the UV LF at z 2 contrasts with the shallower slope inferred locally, suggesting that the evolution in the faint-end slope may be dictated simply by the availability of low-mass halos capable of supporting star formation at z 2.", "date": "2009-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "692", "number": "1", "publisher": "American Astronomical Society", "pagerange": "778-803", "id_number": "CaltechAUTHORS:20091001-100336792", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091001-100336792", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/692/1/778", "primary_object": { "basename": "Reddy2009p15110.10880004-637X6921778.pdf", "url": "https://authors.library.caltech.edu/records/37h2f-ww625/files/Reddy2009p15110.10880004-637X6921778.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Reddy, Naveen A. and Steidel, Charles C." }, { "id": "https://authors.library.caltech.edu/records/jvmb0-bas71", "eprint_id": 12915, "eprint_status": "archive", "datestamp": "2023-08-22 13:54:42", "lastmod": "2023-10-17 21:14:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Zych-B-J", "name": { "family": "Zych", "given": "Berkeley J." } }, { "id": "Murphy-M-T", "name": { "family": "Murphy", "given": "Michael T." } }, { "id": "Lewis-A", "name": { "family": "Lewis", "given": "Antony" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Deuterium abundance in the most metal-poor damped Lyman alpha system: converging on \u03a9b,0h^2", "ispublished": "pub", "full_text_status": "public", "keywords": "quasars: absorption lines; quasars: individual: Q0913+072; cosmology: observations", "note": "\u00a9 2008 The Authors. Journal compilation \u00a9 2008 RAS. \n\nAccepted 2008 September 5. Received 2008 September 2; in original form 2008 May 1. Published Online: 24 November 2008. \n\nThe work presented in this paper is based on UVES observations made with the ESO VLT/Kueyen telescope at Paranal, Chile, obtained in programme 078.A-0185(A) and from the public data archive. We are grateful to the ESO time assignment committee, and to the staff astronomers at VLT, for their help in conducting the observations. Bob Carswell, Jim Lewis and Sam Rix kindly helped with various aspects of the data analysis, and John O'Meara and Gary Steigman offered valuable comments on an earlier version of the paper. We also thank the anonymous referee for useful suggestions on the presentation of the data. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. MTM thanks the Australian Research Council for a QEII research fellowship (DP0877998). CCS's research is partly supported by grant AST-0606912 from the US National Science Foundation.\n\nPublished - PETmnras08b.pdf
", "abstract": "The most metal-poor damped Ly\u03b1 system known to date, at zabs= 2.61843 in the spectrum of the QSO Q0913+072, with an oxygen abundance of only \u223c1/250 of the solar value, shows six well-resolved DI Lyman series transitions in high-quality echelle spectra recently obtained with the European Southern Observatory (ESO) VLT. We deduce a value of the deuterium abundance log (D/H) =\u22124.56 \u00b1 0.04 which is in good agreement with four out of the six most reliable previous determinations of this ratio in QSO absorbers. We find plausible reasons why in the other two cases the 1\u03c3 errors may have been underestimated by about a factor of two. The addition of this latest data point does not significantly change the mean value of the primordial abundance of deuterium, suggesting that we are now converging to a reliable measure of this quantity. We conclude that\u3008log (D/H)p\u3009=\u22124.55 \u00b1 0.03 and \u03a9b,0h2(BBN) = 0.0213 \u00b1 0.0010 (68 per cent confidence limits). Including the latter as a prior in the analysis of the Wilkinson Microwave Anisotropy Probe (WMAP) five-year data leads to a revised best-fitting value of the power-law index of primordial fluctuations ns= 0.956 \u00b1 0.013 (1\u03c3) and ns < 0.990 with 99 per cent confidence. Considering together the constraints provided by WMAP 5, (D/H)p, baryon oscillations in the galaxy distribution, and distances to Type Ia supernovae, we arrive at the current best estimates \u03a9b,0h2= 0.0224 \u00b1 0.0005 and ns= 0.959 \u00b1 0.013.", "date": "2008-12-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "391", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "1499-1510", "id_number": "CaltechAUTHORS:PETmnras08b", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:PETmnras08b", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Southern Observatory", "grant_number": "078.A-0185(A)" }, { "agency": "NASA" }, { "agency": "Australian Research Council" }, { "agency": "NSF", "grant_number": "AST-0606912" } ] }, "doi": "10.1111/j.1365-2966.2008.13921.x", "primary_object": { "basename": "PETmnras08b.pdf", "url": "https://authors.library.caltech.edu/records/jvmb0-bas71/files/PETmnras08b.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Pettini, Max; Zych, Berkeley J.; et el." }, { "id": "https://authors.library.caltech.edu/records/kzjzy-fh293", "eprint_id": 14293, "eprint_status": "archive", "datestamp": "2023-08-22 13:32:24", "lastmod": "2023-10-18 16:27:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Genzel-Reinhard", "name": { "family": "Genzel", "given": "R." }, "orcid": "0000-0002-2767-9653" }, { "id": "Burkert-A", "name": { "family": "Burkert", "given": "A." } }, { "id": "Bouch\u00e9-N", "name": { "family": "Bouch\u00e9", "given": "N." } }, { "id": "Cresci-G", "name": { "family": "Cresci", "given": "G." } }, { "id": "F\u00f6rster-Schreiber-N-M", "name": { "family": "F\u00f6rster Schreiber", "given": "N. M." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "A." }, "orcid": "0000-0003-3509-4855" }, { "id": "Shapiro-K-L", "name": { "family": "Shapiro", "given": "K." } }, { "id": "Tacconi-Linda-J", "name": { "family": "Tacconi", "given": "L. J." }, "orcid": "0000-0002-1485-9401" }, { "id": "Buschkamp-P", "name": { "family": "Buschkamp", "given": "P." } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "Davies-R", "name": { "family": "Davies", "given": "R." } }, { "id": "Eisenhauer-F", "name": { "family": "Eisenhauer", "given": "F." } }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "D. K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Genel-S", "name": { "family": "Genel", "given": "S." }, "orcid": "0000-0002-3185-1540" }, { "id": "Gerhard-O", "name": { "family": "Gerhard", "given": "O." } }, { "id": "Hicks-E-K-S", "name": { "family": "Hicks", "given": "E." } }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Naab-T", "name": { "family": "Naab", "given": "T." } }, { "id": "Ott-T", "name": { "family": "Ott", "given": "T." } }, { "id": "Rabien-S", "name": { "family": "Rabien", "given": "S." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Sternberg-A", "name": { "family": "Sternberg", "given": "A." } }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S. J." }, "orcid": "0000-0002-6423-3597" } ] }, "title": "From Rings to Bulges: Evidence for Rapid Secular Galaxy Evolution at z ~ 2 from Integral Field Spectroscopy in the SINS Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: high-redshift; infrared: galaxies", "note": "\u00a9 2008 The American Astronomical Society. \n\nReceived 2008 April 13, accepted for publication 2008 July 7. \n\nWe thank the staff of Paranal Observatory for their support. This work would have been impossible without the dedicated work of the ESOLGSF team at ESO,MPE and MPIA Heidelberg. We are grateful to Norm Murray, Eve Ostriker, and Chris McKee for enlightening discussions on star formation processes and to Avishai Dekel and an anonymous referee for valuable comments on the paper.\n\nPublished - GENapj08.pdf
", "abstract": "We present H\u03b1 integral field spectroscopy of well-resolved, UV/optically selected z ~ 2 star-forming galaxies as part of the SINS survey with SINFONI on the ESO VLT. Our laser guide star adaptive optics and good seeing data show the presence of turbulent rotating star-forming outer rings/disks, plus central bulge/inner disk components, whose mass fractions relative to the total dynamical mass appear to scale with the [N II]/H\u03b1 flux ratio and the star formation age. We propose that the buildup of the central disks and bulges of massive galaxies at z ~ 2 can be driven by the early secular evolution of gas-rich proto-disks. High-redshift disks exhibit large random motions. This turbulence may in part be stirred up by the release of gravitational energy in the rapid \"cold\" accretion flows along the filaments of the cosmic web. As a result, dynamical friction and viscous processes proceed on a timescale of <1 Gyr, at least an order of magnitude faster than in z ~ 0 disk galaxies. Early secular evolution thus drives gas and stars into the central regions and can build up exponential disks and massive bulges, even without major mergers. Secular evolution along with increased efficiency of star formation at high surface densities may also help to account for the short timescales of the stellar buildup observed in massive galaxies at z ~ 2.", "date": "2008-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "687", "number": "1", "publisher": "American Astronomical Society", "pagerange": "59-77", "id_number": "CaltechAUTHORS:20090524-210427908", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090524-210427908", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1086/591840", "primary_object": { "basename": "GENapj08.pdf", "url": "https://authors.library.caltech.edu/records/kzjzy-fh293/files/GENapj08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Genzel, R.; Burkert, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/pedw3-vxt86", "eprint_id": 14095, "eprint_status": "archive", "datestamp": "2023-08-22 12:32:11", "lastmod": "2023-10-18 16:06:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shapiro-K-L", "name": { "family": "Shapiro", "given": "Kristen L." } }, { "id": "Genzel-Reinhard", "name": { "family": "Genzel", "given": "Reinhard" }, "orcid": "0000-0002-2767-9653" }, { "id": "F\u00f6rster-Schreiber-N-M", "name": { "family": "F\u00f6rster Schreiber", "given": "Natascha M." } }, { "id": "Tacconi-Linda-J", "name": { "family": "Tacconi", "given": "Linda J." }, "orcid": "0000-0002-1485-9401" }, { "id": "Bouch\u00e9-N", "name": { "family": "Bouch\u00e9", "given": "Nicolas" } }, { "id": "Cresci-G", "name": { "family": "Cresci", "given": "Giovanni" } }, { "id": "Davies-R", "name": { "family": "Davies", "given": "Richard" } }, { "id": "Eisenhauer-F", "name": { "family": "Eisenhauer", "given": "Frank" } }, { "id": "Johansson-P-H", "name": { "family": "Johansson", "given": "Peter H." } }, { "id": "Krajnovi\u0107-D", "name": { "family": "Krajnovi\u0107", "given": "Davor" } }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "Dieter" }, "orcid": "0000-0003-0291-9582" }, { "id": "Naab-T", "name": { "family": "Naab", "given": "Thorsten" } }, { "id": "Arimoto-Nobuo", "name": { "family": "Arimoto", "given": "Nobuo" } }, { "id": "Arribas-S", "name": { "family": "Arribas", "given": "Santiago" }, "orcid": "0000-0001-7997-1640" }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "Andrea" } }, { "id": "Colina-L", "name": { "family": "Colina", "given": "Luis" }, "orcid": "0000-0002-9090-4227" }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "Emanuele" }, "orcid": "0000-0002-3331-9590" }, { "id": "Daigle-O", "name": { "family": "Daigle", "given": "Olivier" } }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn" }, "orcid": "0000-0001-9714-2758" }, { "id": "Hernandez-O", "name": { "family": "Hernandez", "given": "Olivier" } }, { "id": "Kong-Xu", "name": { "family": "Kong", "given": "Xu" } }, { "id": "Mignoli-M", "name": { "family": "Mignoli", "given": "Marco" } }, { "id": "Onodera-Masato", "name": { "family": "Onodera", "given": "Masato" } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "Alvio" }, "orcid": "0000-0002-7093-7355" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice" }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Kinemetry of SINS high-redshift star-forming galaxies : distinguishing rotating disks from major mergers", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: interactions; galaxies: kinematics and dynamics; methods: data analysis; techniques: spectroscopic", "note": "\u00a9 2008 The American Astronomical Society. \n\nReceived 2007 November 16; accepted 2008 February 5. \n\nWe are very grateful to the entire SINS team, whose input greatly improved the quality of this work. We also thank Carl Heiles for many useful discussions and the anonymous referee for helpful comments. N. M. F. S. acknowledges support by the Schwerpunkt Programm SPP1177 of the Deutsche Forschungsgemeinschaft. N. A. acknowledges support from a Grant-in-Aid for Scientific Research (19540245) by the Japanese Ministry of Education, Culture, Sports, and Science. S. A. and L. C. have been supported by the Spanish Ministry for Education and Science under grants PNE2005-01480 and ESP2007-65475-C02-01.\n\nPublished - SHAapj08.pdf
", "abstract": "We present a simple set of kinematic criteria that can distinguish between galaxies dominated by ordered rotational motion and those involved in major merger events. Our criteria are based on the dynamics of the warm ionized gas (as traced by H\u03b1) within galaxies, making this analysis accessible to high-redshift systems, whose kinematics are primarily traceable through emission features. Using the method of kinemetry (developed by Krajnovi\u0107 and coworkers), we quantify asymmetries in both the velocity and velocity dispersion maps of the warm gas, and the resulting criteria enable us to empirically differentiate between nonmerging and merging systems at high redshift. We apply these criteria to 11 of our best-studied rest-frame UV/optical-selected z ~ 2 galaxies for which we have near-infrared integral-field spectroscopic data from SINFONI on the VLT. Of these 11 systems, we find that >50% have kinematics consistent with a single rotating disk interpretation, while the remaining systems are more likely undergoing major mergers. This result, combined with the short formation timescales of these systems, provides evidence that rapid, smooth accretion of gas plays a significant role in galaxy formation at high redshift.", "date": "2008-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "682", "number": "1", "publisher": "American Astronomical Society", "pagerange": "231-251", "id_number": "CaltechAUTHORS:20090428-075610786", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090428-075610786", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "Schwerpunkt Programm SPP1177" }, { "agency": "Ministry of Education, Culture, Sports, Science, and Technology (MEXT)", "grant_number": "19540245" }, { "agency": "Ministerio de Educaci\u00f3n y Ciencia (MEC)", "grant_number": "PNE2005-01480" }, { "agency": "Ministerio de Educaci\u00f3n y Ciencia (MEC)", "grant_number": "ESP2007-65475-C02-01" } ] }, "doi": "10.1086/587133", "primary_object": { "basename": "SHAapj08.pdf", "url": "https://authors.library.caltech.edu/records/pedw3-vxt86/files/SHAapj08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Shapiro, Kristen L.; Genzel, Reinhard; et el." }, { "id": "https://authors.library.caltech.edu/records/pat5g-nv881", "eprint_id": 14263, "eprint_status": "archive", "datestamp": "2023-08-22 11:35:31", "lastmod": "2023-10-18 16:26:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Zych-B-J", "name": { "family": "Zych", "given": "Berkeley J." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Chaffee-F-H", "name": { "family": "Chaffee", "given": "Fred H." } } ] }, "title": "C, N, O abundances in the most metal-poor damped Lyman alpha systems", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: abundances; galaxies: evolution; galaxies: ISM; cosmology: observations; quasars: absorption lines", "note": "\u00a9 2008 The Authors. Journal compilation \u00a9 2008 RAS. \n\nAccepted 2008 January 10. Received 2008 January 8; in original form 2007 November 29. \n\nWe are grateful to the Keck and ESO time assignment committees\nfor their support of this programme and to the staff astronomers at\nthe Keck and VLT observatories for their help in conducting the observations. \n\nTom Barlow, Bob Carswell, Thiago Gon\u00b8calves, Michael Murphy and Sam Rix kindly helped with different aspects of the data reduction and analysis. Martin Asplund, Damian Fabbian, Dick Henry, Poul Nissen and an anonymous referee made valuable suggestions which improved the paper. We thank the Hawaiian people for the opportunity to observe from Mauna Kea; without their hospitality, this work would not have been possible. CCS's research is partly supported by grant AST-0606912 from the US National Science Foundation. Some of this work was carried out during a visit by Fred Chaffee to the Institute of Astronomy, Cambridge, supported by the Institute's visitor grant.\n\nPublished - PETmnras08a.pdf
", "abstract": "This study focuses on some of the most metal-poor damped Ly\u03b1 (DLA) absorbers known in the spectra of high-redshift QSOs, using new and archival observations obtained with ultraviolet-sensitive echelle spectrographs on the Keck and VLT telescopes. The weakness and simple velocity structure of the absorption lines in these systems allow us to measure the abundances of several elements, and in particular those of C, N and O, a group that is difficult to study in DLAs of more typical metallicities. We find that when the oxygen abundance is less than \u223c1/100 of solar, the C/O ratio in high-redshift DLAs and sub-DLAs matches that of halo stars of similar metallicity and shows higher values than expected from galactic chemical evolution models based on conventional stellar yields. Furthermore, there are indications that at these low metallicities the N/O ratio may also be above simple expectations and may exhibit a minimum value, as proposed by Centuri\u00f3n and her collaborators in 2003. Both results can be interpreted as evidence for enhanced production of C and N by massive stars in the first few episodes of star formation, in our Galaxy and in the distant protogalaxies seen as QSO absorbers. The higher stellar yields implied may have an origin in stellar rotation which promotes mixing in the stars' interiors, as considered in some recent model calculations. We briefly discuss the relevance of these results to current ideas on the origin of metals in the intergalactic medium and the universality of the stellar initial mass function.", "date": "2008-04-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "385", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "2011-2024", "id_number": "CaltechAUTHORS:20090519-090047352", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090519-090047352", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0606912" } ] }, "doi": "10.1111/j.1365-2966.2008.12951.x", "primary_object": { "basename": "PETmnras08a.pdf", "url": "https://authors.library.caltech.edu/records/pat5g-nv881/files/PETmnras08a.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Pettini, Max; Zych, Berkeley J.; et el." }, { "id": "https://authors.library.caltech.edu/records/trfg0-asz89", "eprint_id": 13849, "eprint_status": "archive", "datestamp": "2023-08-22 11:30:05", "lastmod": "2023-10-18 14:30:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gon\u00e7alves-T-S", "name": { "family": "Gon\u00e7alves", "given": "Thiago S." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" } ] }, "title": "Detection of the transverse proximity effect : radiative feedback from bright QSOs", "ispublished": "pub", "full_text_status": "public", "keywords": "intergalactic medium; quasars: absorption lines; quasars: general", "note": "\u00a9 2008 The American Astronomical Society. \n\nReceived 2007 August 16; accepted 2007 November 20. \n\nWe would like to thank Dawn Erb, Naveen Reddy, and Alice Shapley for their collaboration in the large survey which supplied the LRIS spectroscopic redshifts of galaxies and AGNs in the field of Q1623+268. In addition, Dawn and Alice obtained the near-IR spectra used to determine the systemic redshifts of the QSOs, and Naveen kindly provided the Spitzer results on the QSOs prior to publication. Kurt Adelberger is thanked for many discussions and for his participation in the early stages of the project. We would also like to thank Tom Barlow, Rob Simcoe, George Becker, and Bob Carswell for assistance with the software used to reduce HIRES data. Rob Simcoe also provided us with measurements from his previous work, for which we are grateful. Wal Sargent provided us with his HIRES spectra of KP 76 and KP 77, which were combined with the new data presented here. An anonymous referee and Juna Kollmeier provided constructive comments which significantly improved the paper. Finally, we wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. This work was supported by grants AST 03-07263 and AST 06-06912 from the US National Science Foundation and by the David and Lucile Packard Foundation.\n\nPublished - GONapj08.pdf
", "abstract": "Measuring the response of the intergalactic medium (IGM) to a blast of ionizing radiation allows one to infer the physical properties of the medium and, in principle, the lifetime and isotropy of the radiating source. The most sensitive such measurements can be made if the source of radiation is near the line of sight to a bright background QSO. We present results based on deep Keck HIRES observations of the QSO triplet KP 76, KP 77, and KP 78 at z \u2243 2.5, with separations of 2'-3' on the plane of the sky. Using accurate systemic redshifts of the QSOs from near-IR spectroscopy, we quantify the state of the IGM gas in the proximity regions where the expected ionizing flux from the foreground QSOs exceeds that of the metagalactic background by factors of 10-200, assuming constant and isotropic emission. Based on the unusual ionization properties of the absorption systems with detected H I, C IV, and O VI, we conclude that the gas has been significantly affected by the UV radiation from the nearby QSOs. Aided by observations of the galaxy density near the foreground QSOs, we discuss several effects that may explain why the transverse proximity effect has eluded most previous attempts to detect it. Our observations suggest that the luminosities of KP 76 and KP 77 have remained comparable to current values over timescales of, respectively, \u0394 t > 25 Myr and 16 Myr < \u0394 t < 33 Myr , consistent with typical QSO lifetimes estimated from independent, less direct methods. There is no evidence that the UV radiation from either QSO was significantly anisotropic during these intervals.", "date": "2008-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "676", "number": "2", "publisher": "American Astronomical Society", "pagerange": "816-835", "id_number": "CaltechAUTHORS:GONapj08", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:GONapj08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 03-07263" }, { "agency": "NSF", "grant_number": "AST 06-06912" }, { "agency": "David and Lucile Packard Foundation" } ] }, "doi": "10.1086/527313", "primary_object": { "basename": "GONapj08.pdf", "url": "https://authors.library.caltech.edu/records/trfg0-asz89/files/GONapj08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Gon\u00e7alves, Thiago S.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/3sqrq-nw049", "eprint_id": 13465, "eprint_status": "archive", "datestamp": "2023-08-22 11:13:51", "lastmod": "2023-10-17 23:54:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kacprzak-G-G", "name": { "family": "Kacprzak", "given": "Glenn G." } }, { "id": "Churchill-C-W", "name": { "family": "Churchill", "given": "Christopher W." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Murphy-M-T", "name": { "family": "Murphy", "given": "Michael T." } } ] }, "title": "Halo gas cross sections and covering fractions of MgII absorption selected galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: halos; galaxies: ISM; quasars: absorption lines", "note": "\u00a9 2008 American Astronomical Society. \n\nReceived 2007 August 29; accepted 2007 October 29; published 2008 February 5. \n\nPartial support from program no. 10644 which was provided by NASA through a grant from the Space Telescope Science Institute. Partial support for G.G.K was also provided by Sigma-Xi Grants in Aid of Research. G.G.K thanks NMSU for funding from the Graduate Student Enhancement Grant. M.T.M. thanks PPARC for and Advanced Fellowship. We thank Hsiao-Wen Chen for discussions regarding k-corrections. We also thank the anonymous referee for insightful comments. Some of the data presented herein are based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Institute. STScI is operated by the association of Universities for Research in Astronomy, Inc. under the NASA contract NAS 5-26555. Some spectroscopic data were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA. The Observatory was made possible by the generous financial support of theW. M.Keck Foundation. Additional spectroscopic data are based on observations made with European Southern Observatory Very Large Telescope at the Paranal Observatories under various programs.\n\nPublished - KACaj08.pdf
", "abstract": "We examine halo gas cross sections and covering fractions, fc, of intermediate-redshift Mg II absorption selected galaxies. We computed statistical absorber halo radii, Rx, using current values of dN/dz and Schechter luminosity function parameters, and have compared these values to the distribution of impact parameters and luminosities from a sample of 37 galaxies. For equivalent widths Wr(2796) \u2265 0.3 \u00c5, we find 43 \u2264 Rx \u2264 88 kpc, depending on the lower luminosity cutoff and the slope, \u03b2, of the Holmberg-like luminosity scaling, R \u221d \u03b1 L^\u03b2 . The observed distribution of impact parameters, D, are such that several absorbing galaxies lie at D > Rx and several non-absorbing galaxies lie at D < Rx. We deduced that fc must be less than unity and obtain a mean of ~ 0.5 for our sample. Moreover, the data suggest that halo radii of Mg II absorbing galaxies do not follow a luminosity scaling with \u03b2 in the range of 0.2\u20130.28, if fc = 1 as previously reported. However, provided fc ~ 0.5, we find that halo radii can remain consistent with a Holmberg-like luminosity relation with \u03b2 \u2243 0.2 and R\u2217 = Rx/\u221a(fc) ~ 110 kpc. No luminosity scaling (\u03b2 = 0) is also consistent with the observed distribution of impact parameters if fc \u2264 0.37. The data support a scenario in which gaseous halos are patchy and likely have non-symmetric geometric distributions about the galaxies. We suggest that halo gas distributions may not be governed primarily by galaxy mass/luminosity but also by stochastic processes local to the galaxy.", "date": "2008-03", "date_type": "published", "publication": "Astronomical Journal", "volume": "135", "number": "3", "publisher": "University of Chicago Press", "pagerange": "922-927", "id_number": "CaltechAUTHORS:KACaj08", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:KACaj08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "Sigma Xi" }, { "agency": "New Mexico State University" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-6256/135/3/922", "primary_object": { "basename": "KACaj08.pdf", "url": "https://authors.library.caltech.edu/records/3sqrq-nw049/files/KACaj08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Kacprzak, Glenn G.; Churchill, Christopher W.; et el." }, { "id": "https://authors.library.caltech.edu/records/gey18-cap65", "eprint_id": 14310, "eprint_status": "archive", "datestamp": "2023-08-22 11:14:38", "lastmod": "2023-10-18 16:28:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Adelberger-K-L", "name": { "family": "Adelberger", "given": "Kurt L." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Dickinson-Mark-E", "name": { "family": "Dickinson", "given": "Mark" }, "orcid": "0000-0001-5414-5131" } ] }, "title": "Multiwavelength constraints on the cosmic star formation history from spectroscopy: the rest-frame ultraviolet, H\u03b1, and infrared luminosity functions at redshifts 1.9 \u227e z \u227e 3.4", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: luminosity function, mass function; galaxies: starburst; infrared: galaxies", "note": "\u00a9 2008 The American Astronomical Society. \n\nPrint publication: Issue 1 (2008 March). Received 2007 May 21, accepted for publication 2007 June 16. \n\nWe acknowledge useful conversations with Rychard Bouwens, Emeric Le Floc'h,Casey Papovich, Marcin Sawicki, and Lin Yan. We thank Emeric Le Floc'h for providing data from Le Floc'h et al. (2005) in electronic format, Rychard Bouwens for a careful reading of the manuscript, and the referee for helpful suggestions to improve the clarity of the paper. This work would not have been possible without the support of the staff of the Keck Observatory. The work presented here has been supported by grants AST 03-07263 and AST 06-06912 from the National Science Foundation and by the David and Lucile Packard Foundation.\n\nPublished - REDapjss08.pdf
", "abstract": "We use a sample of rest-frame UV-selected and spectroscopically observed galaxies at redshifts 1.9 \u2264 z < 3.4, combined with ground-based spectroscopic H\u03b1 and Spitzer MIPS 24 \u03bcm data, to derive the most robust measurements of the rest-frame UV, H\u03b1, and infrared (IR) luminosity functions (LFs) at these redshifts. Our sample is by far the largest of its kind, with over 2000 spectroscopic redshifts in the range 1.9 \u2264 z < 3.4 and ~15,000 photometric candidates in 29 independent fields covering a total area of almost a square degree. Our method for computing the LFs takes into account a number of systematic effects, including photometric scatter, Ly\u03b1 line perturbations to the observed optical colors of galaxies, and contaminants. Taking into account the latter, we find no evidence for an excess of UV-bright galaxies over what was inferred in early z ~ 3 LBG studies. The UV LF appears to undergo little evolution between z ~ 4 and z ~ 2. Corrected for extinction, the UV luminosity density (LD) at z ~ 2 is at least as large as the value at z ~ 3 and a factor of ~9 larger than the value at z ~ 6, primarily reflecting an increase in the number density of bright galaxies between z ~ 6 and z ~ 2. Our analysis yields the first constraints anchored by extensive spectroscopy on the infrared and bolometric LFs for faint and moderately luminous (L_(bol) \u227e 10^(12) L\u2299) galaxies. Adding the IR to the emergent UV luminosity, incorporating independent measurements of the LD from ULIRGs, and assuming realistic dust attenuation values for UV-faint galaxies, indicates that galaxies with L_(bol) < 10^(12) L\u2299 account for \u224880% of the bolometric LD and SFRD at z ~ 2\u20133. This suggests that previous estimates of the faint end of the Lbol LF may have underestimated the steepness of the faint-end slope at L_(bol) < 10^(12) L\u2299. Our multiwavelength constraints on the global SFRD indicate that approximately one-third of the present-day stellar mass density was formed in subultraluminous galaxies between redshifts z = 1.9\u20133.4.", "date": "2008-03", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "175", "number": "1", "publisher": "American Astronomical Society", "pagerange": "48-85", "id_number": "CaltechAUTHORS:20090527-080644843", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090527-080644843", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 03-07263" }, { "agency": "NSF", "grant_number": "AST 06-06912" }, { "agency": "David and Lucile Packard Foundation" } ] }, "doi": "10.1086/521105", "primary_object": { "basename": "REDapjss08.pdf", "url": "https://authors.library.caltech.edu/records/gey18-cap65/files/REDapjss08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Reddy, Naveen A.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/dpev3-4df48", "eprint_id": 16516, "eprint_status": "archive", "datestamp": "2023-08-22 10:41:13", "lastmod": "2023-10-19 22:19:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bouch\u00e9-N", "name": { "family": "Bouch\u00e9", "given": "N." } }, { "id": "Cresci-G", "name": { "family": "Cresci", "given": "G." } }, { "id": "Davies-R", "name": { "family": "Davies", "given": "R." } }, { "id": "Eisenhauer-F", "name": { "family": "Eisenhauer", "given": "F." } }, { "id": "F\u00f6rster-Schreiber-N-M", "name": { "family": "F\u00f6rster Schreiber", "given": "N. M." } }, { "id": "Genzel-Reinhard", "name": { "family": "Genzel", "given": "R." }, "orcid": "0000-0002-2767-9653" }, { "id": "Gillessen-S", "name": { "family": "Gillessen", "given": "S." } }, { "id": "Lehnert-Matthew-D", "name": { "family": "Lehnert", "given": "M." }, "orcid": "0000-0003-1939-5885" }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Nesvadba-N-P-H", "name": { "family": "Nesvadba", "given": "N." } }, { "id": "Shapiro-K-L", "name": { "family": "Shapiro", "given": "K. L." } }, { "id": "Sternberg-A", "name": { "family": "Sternberg", "given": "A." } }, { "id": "Tacconi-Linda-J", "name": { "family": "Tacconi", "given": "L. J." }, "orcid": "0000-0002-1485-9401" }, { "id": "Verma-A", "name": { "family": "Verma", "given": "A." } }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "A." } }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "D. K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "A." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Dynamical Properties of z ~ 2 Star-forming Galaxies and a Universal Star Formation Relation", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology : observations; galaxies : evolution; infrared : galaxies", "note": "\u00a9 2007 The American Astronomical Society. \n\nReceived 2007 March 21; accepted 2007 July 28. \n\nWe are grateful to the staff of Paranal Observatory for their support, and the SINFONI team for their hard work on the instrument that has made this research possible. We also thank the SMG team, A. Blain, F. Bertoldi, S. Chapman, P. Cox, T. Greve, R. Ivison, R. Neri, A. Omont, and I. Smail. We acknowledge useful discussions with A. Burkert, A. Dekel, T. Naab, and E. Quataert. N. M. F. S. acknowledges support by the Priority Programme 1177 of the Deutsche Forschungsgemeinschatt. We thank the anonymous referee for his/her critical comments that led to an improved manuscript.\n\nPublished - BOUapj07.pdf
", "abstract": "We present the first comparison of the dynamical properties of different samples of z ~ 1.4-3.4 star-forming galaxies from spatially resolved imaging spectroscopy from SINFONI/VLT integral field spectroscopy and IRAM CO millimeter interferometry. Our samples include 16 rest-frame UV-selected, 16 rest-frame optically selected, and 13 submillimeter galaxies (SMGs). We find that rest-frame UV and optically bright (K < 20) z ~ 2 star forming galaxies are dynamically similar, and follow the same velocity-size relation as disk galaxies at z ~ 0. In the theoretical framework of rotating disks forming from dissipative collapse in dark matter halos, the two samples require a spin parameter <\u03bb> ranging from 0.06 to 0.2. In contrast, bright SMGs (S_(850) \u03bcm \u2265 5 mJy) have larger velocity widths and are much more compact. Hence, SMGs have lower angular momenta and higher matter densities than either the UV or optically selected populations. This indicates that dissipative major mergers may dominate the SMGs population, resulting in early spheroids, and that a significant fraction of the UV/optically bright galaxies have evolved less violently, either in a series of minor mergers, or in rapid dissipative collapse from the halo, given that either process may leads to the formation of early disks. These early disks may later evolve into spheroids via disk instabilities or mergers. Because of their small sizes and large densities, SMGs lie at the high surface density end of a universal (out to z = 2.5) \"Schmidt-Kennicutt\" relation between gas surface density and star formation rate surface density. The best-fit relation suggests that the star formation rate per unit area scales as the surface gas density to a power of ~1.7, and that the star formation efficiency increases by a factor of 4 between non-starbursts and strong starbursts.", "date": "2007-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "671", "number": "1", "publisher": "American Astronomical Society", "pagerange": "303-309", "id_number": "CaltechAUTHORS:20091029-090949441", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091029-090949441", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "Priority Programme 1177" } ] }, "doi": "10.1086/522221", "primary_object": { "basename": "BOUapj07.pdf", "url": "https://authors.library.caltech.edu/records/dpev3-4df48/files/BOUapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Bouch\u00e9, N.; Cresci, G.; et el." }, { "id": "https://authors.library.caltech.edu/records/4k4pc-tny67", "eprint_id": 16629, "eprint_status": "archive", "datestamp": "2023-08-22 10:28:53", "lastmod": "2023-10-19 22:26:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rix-Samantha-A", "name": { "family": "Rix", "given": "Samantha A." } }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Adelberger-K-L", "name": { "family": "Adelberger", "given": "Kurt L." } }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" } ] }, "title": "The Sightline to Q2343-BX415: Clues to Galaxy Formation in a Quasar Environment", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology : observations; galaxies : abundances; galaxies : evolution; galaxies : high-redshift; quasars : absorption lines; quasars : individual (Q2343-BX415)", "note": "\u00a9 2007 The American Astronomical Society. \n\nReceived 2007 February 22; accepted 2007 July 23. \n\nIt is a pleasure to acknowledge illuminating discussions with Bob Carswell, Gary Ferland, and Paul Hewett, and valuable suggestions from the referee, which have improved this paper. We are indebted to Art Wolfe, who generously helped with the interpretation of the C ii* absorption. Part of this work was carried out during visits by Sam Rix and Art Wolfe to the Institute of Astronomy, Cambridge, supported by the Institute's visitors' grant. S. Rix also acknowledges the support of a PPARC Postdoctoral Research Fellowship. We thank the staff of the Keck Observatory for their expert assistance with the ESI and NIRSPEC observations, and the Hawaiian people for the opportunity to observe from Mauna Kea.\nWithout their hospitality, this work would not have been possible.\n\nPublished - RIXapj07.pdf
", "abstract": "We have discovered a strong DLA coincident in redshift with the faint QSO Q2343-BX415 (R = 20.2, z_(em) = 2.57393). Follow-up observations at intermediate spectral resolution reveal that the metal lines associated with this proximate DLA (PDLA) consist of two sets of absorption components. One set is moving toward the quasar with velocities of ~150-600 km s^(-1); this gas is highly ionized and does not fully cover the continuum source, suggesting that it is physically close to the active nucleus. The other, which accounts for most of the neutral gas, is blueshifted relative to the QSO, with the strongest component at ~-160 km s^(-1). We consider the possibility that the PDLA arises in the outflowing interstellar medium of the host galaxy of Q2343-BX415, an interpretation supported by strong C IV and N V absorption at nearby velocities, and by the intense radiation field longward of the Lyman limit implied by the high C II*/H I ratio. If Q2343-BX415 is the main source of these UV photons, then the PDLA is located at either ~8 or ~37 kpc from the active nucleus. Alternatively, the absorber may be a foreground star-forming galaxy unrelated to the quasar and coincidentally at the same redshift, but our deep imaging and follow-up spectroscopy of the field of Q2343-BX415 has not yet produced a likely candidate. We measure the abundances of 14 elements in the PDLA, finding an overall metallicity of ~1/5 solar and a normal pattern of relative element abundances for this metallicity. Thus, in this PDLA there is no evidence for the supersolar metallicities that have been claimed for some proximate, high-ionization, systems.", "date": "2007-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "670", "number": "1", "publisher": "American Astronomical Society", "pagerange": "15-38", "id_number": "CaltechAUTHORS:20091109-143310813", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091109-143310813", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Institute of Astronomy, Cambridge" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" } ] }, "doi": "10.1086/521808", "primary_object": { "basename": "RIXapj07.pdf", "url": "https://authors.library.caltech.edu/records/4k4pc-tny67/files/RIXapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Rix, Samantha A.; Pettini, Max; et el." }, { "id": "https://authors.library.caltech.edu/records/kkw2e-dh068", "eprint_id": 11612, "eprint_status": "archive", "datestamp": "2023-08-22 10:24:57", "lastmod": "2023-10-17 15:10:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Larkin-J-E", "name": { "family": "Larkin", "given": "James E." }, "orcid": "0000-0001-7687-3965" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Wright-S-A", "name": { "family": "Wright", "given": "Shelley A." }, "orcid": "0000-0003-1034-8054" } ] }, "title": "Integral field spectroscopy of high-redshift star-forming galaxies with laser-guided adaptive optics: Evidence for dispersion-dominated kinematics", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: kinematics and dynamics; galaxies: starburst", "note": "\u00a9 2007 The American Astronomical Society. \n\nReceived 2007 May 16; accepted 2007 July 16. \n\nWe would like to thank Andrew Benson and Juna Kollmeier for numerous helpful discussions, and Naveen Reddy for providing Spitzer photometry for Q1623-BX453. The authors also thank Randy Campbell, Al Conrad, David LeMignant, and Jim Lyke for their invaluable help obtaining the observations presented herein. D.R.L. and C.C.S. have been supported by grants AST 06-06912 and AST 03-07263 from the US National Science Foundation. Finally, we wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. \n\nBased on data obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W.M. Keck Foundation.\n\nPublished - LAWapj07b.pdf
", "abstract": "We present early results from an ongoing study of the kinematic structure of star-forming galaxies at redshift z similar to 2-3 using integral-field spectroscopy of rest-frame optical nebular emission lines in combination with Keck laser guide star adaptive optics (LGSAO). We show kinematic maps of three target galaxies Q1623-BX453, Q0449-BX93, and DSF 2237a-C2 located at redshifts z = 2.1820, 2.0067, and 3.3172, respectively, each of which is well resolved with a PSF measuring approximately 0.11\"-0.15\" (similar to 900-1200 pc at z similar to 2-3) after cosmetic smoothing. Neither galaxy at z similar to 2 exhibits substantial kinematic structure on scales greater than or similar to 30 km s^(-1); both are instead consistent with largely dispersion-dominated velocity fields with sigma similar to 80 km s^(-1) along any given line of sight into the galaxy. In contrast, DSF 2237a-C2 presents a well-resolved gradient in velocity over a distance of similar to 4 kpc with peak-to-peak amplitude of 140 km s(-1). It is unlikely that DSF 2237a-C2 represents a dynamically cold rotating disk of ionized gas as the local velocity dispersion of the galaxy (sigma = 79 km s^(-1))is comparable to the observed shear. While some gas cooling models reproduce the observed kinematics better than a simple rotating disk model, even these provide a poor overall description of the target galaxies, suggesting that our current understanding of gas cooling mechanisms in galaxies in the early universe is (at best) incomplete.", "date": "2007-11-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "669", "number": "2", "publisher": "American Astronomical Society", "pagerange": "929-946", "id_number": "CaltechAUTHORS:LAWapj07b", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:LAWapj07b", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 06-06912" }, { "agency": "NSF", "grant_number": "AST 03-07263" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1086/521786", "primary_object": { "basename": "LAWapj07b.pdf", "url": "https://authors.library.caltech.edu/records/kkw2e-dh068/files/LAWapj07b.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Law, David R.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/svcsk-bkt64", "eprint_id": 12989, "eprint_status": "archive", "datestamp": "2023-08-22 10:13:12", "lastmod": "2023-10-17 21:41:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Peter-A-H-G", "name": { "family": "Peter", "given": "Annika H. G." }, "orcid": "0000-0002-8040-6785" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" } ] }, "title": "Morphologies of Galaxies in and around a Protocluster at z = 2.300", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: clusters: general; galaxies: high-redshift; galaxies: structure", "note": "\u00a9 2007. The American Astronomical Society. \n\nReceived 2007 February 27; accepted 2007 June 16. Print publication: Issue 1 (2007 October 10). \n\nBased on observations made with the NASA ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program HST-GO-10581.07-A. Support for program HST-GO-10581.07-A was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. A.E.S. acknowledges support from the David and Lucile Packard Foundation. C.C.S. and D.R.L. have been supported by grants AST 06-06912 from the US National Science Foundation and HST-AR-10311 from NASA through the Space Telescope Science Institute. We thank Jennifer Lotz for providing us with her morphological analysis of the GOODS-N field, Mauro Giavalisco for useful discussions, and an anonymous referee, whose comments improved the paper.\n\nPublished - PETapj07.pdf
", "abstract": "We present results from the first robust investigation of galaxy morphology as a function of environment at z > 1.5. Our study is motivated by the fact that star-forming galaxies contained within a protocluster at z = 2.3 in the HS 1700+64 field have significantly older ages and larger stellar masses on average than those at similar redshifts but more typical environmental densities. In the analysis of HST ACS images, we apply nonparametric statistics to characterize the rest-frame UV morphologies of a sample of 85 UV-selected star-forming galaxies at z = 1.7-2.9, 22 of which are contained in the protocluster. The remaining 63 control sample galaxies are not in the protocluster but have a similar mean redshift of zbar ~ 2.3. We find no environmental dependence for the distributions of morphological properties. Combining the measured morphologies with the results of population synthesis modeling, we find only weak correlations, if any, between morphological and stellar population properties such as stellar mass, age, extinction, and star formation rate. Given the incomplete census of the protocluster galaxy population, and the lack of correlation between rest-frame UV morphology and star formation history at z ~ 2 within our sample, the absence of environmental trends in the distribution of morphological properties is not surprising. In addition, using a larger sample of photometric candidates, we compare morphological distributions for 282 UV-selected and 43 near-IR-selected galaxies. While the difference in the degree of nebulosity between the two samples appears to be a by-product of the fainter average rest-frame UV surface brightness of the near-IR-selected galaxies, we find that, among the lowest surface brightness galaxies, the near-IR-selected objects have significantly smaller angular sizes.", "date": "2007-10-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "668", "number": "1", "publisher": "American Astronomical Society", "pagerange": "23-44", "id_number": "CaltechAUTHORS:PETapj07", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:PETapj07", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NASA", "grant_number": "HST-GO-10581.07-A" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "NSF", "grant_number": "AST 06-06912" }, { "agency": "NASA", "grant_number": "HST-AR-10311" } ] }, "doi": "10.1086/521184", "primary_object": { "basename": "PETapj07.pdf", "url": "https://authors.library.caltech.edu/records/svcsk-bkt64/files/PETapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Peter, Annika H. G.; Shapley, Alice E.; et el." }, { "id": "https://authors.library.caltech.edu/records/p12pg-0a536", "eprint_id": 18081, "eprint_status": "archive", "datestamp": "2023-08-22 09:16:42", "lastmod": "2023-10-20 15:34:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Churchill-C-W", "name": { "family": "Churchill", "given": "Christopher W." } }, { "id": "Kacprzak-G-G", "name": { "family": "Kacprzak", "given": "Glenn G." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Evans-J-L", "name": { "family": "Evans", "given": "Jessica L." } } ] }, "title": "On the Heterogeneity of Metal-Line and Ly\u03b1 Absorption in Galaxy \"Halos\" at z ~ 0.7", "ispublished": "pub", "full_text_status": "public", "keywords": "quasars: absorption lines; quasars: individual (QSO B1317+274, QSO B1317+274)", "note": "\u00a9 2007 American Astronomical Society. \n\nReceived 2006 May 19; accepted 2006 December 20. \n\nSupport for this research through grant HST-AR-10644.01-A was provided by NASA via the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. G. G. K. acknowledges support from Sigma-Xi Grants in Aid of Research. J. L. E. acknowledges support from Research Cluster Fellowship from NMSU and a Graduate Student Fellowship from NASA's New Mexico Space Grant Consortium. \n\nFacilities: HST (WFPC-2, STIS, FOS), Keck:I (HIRES, LRIS)\n\nPublished - CHUapj07.pdf
", "abstract": "We examine the properties of two galaxy \"halos\" at z ~ 0.7 in the Ton 153 (z_(em) = 1.01) quasar field. The first absorber-galaxy pair (G1) is a z = 0.672, L_B = 4.3L*_B, E/S0 galaxy probed at D = 58 kpc. G1 is associated with a remarkable five-component Ly\u03b1 complex having \u03c4_(LL) \u2264 0.4, W_(r)(Ly\u03b1) = 2.8 \u00c5, and a velocity spread of \u0394v = 1420 km s^(-1). We find no Mg II, C IV, N V, nor O VI absorption in these clouds and infer metallicity upper limits of -3 \u2264 log Z/Z_\u2609 \u2264 -1, depending on assumptions of photoionized or collisionally ionized gas. The second absorber-galaxy pair (G2) is a z = 0.661, L_B = 1.8 L*_B, Sab galaxy probed at D = 103 kpc. G2 is associated with metal-enriched (log Z/Z_\u2609 \u2243 -0.4) photoionized gas having N(H I) \u2243 18.3 (cm^(-2)) and a velocity spread of \u0394v = 200 km s^(-1). The very different G1 and G2 systems both have gas-galaxy properties inconsistent with the standard luminosity-dependent galaxy \"halo\" model commonly invoked for quasar absorption line surveys. We emphasize that mounting evidence is revealing that extended galactic gaseous envelopes in the regime of D \u2264 100 kpc do not exhibit a level of homogeneity supporting a standardized halo model. Selection effects may have played a central role in the development of a simple model. We discuss the G1 and G2 systems in the context of \u039bCDM models of galaxy formation and suggest that the heterogeneous properties of absorber-galaxy pairs is likely related to the range of overdensities from which galaxies and gas structures arise.", "date": "2007-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "661", "number": "2", "publisher": "American Astronomical Society", "pagerange": "714-718", "id_number": "CaltechAUTHORS:20100429-113357034", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100429-113357034", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-AR-10644.01-A" }, { "agency": "Sigma-Xi" }, { "agency": "New Mexico State University" }, { "agency": "New Mexico Space Consortium" } ] }, "doi": "10.1086/512113", "primary_object": { "basename": "CHUapj07.pdf", "url": "https://authors.library.caltech.edu/records/p12pg-0a536/files/CHUapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Churchill, Christopher W.; Kacprzak, Glenn G.; et el." }, { "id": "https://authors.library.caltech.edu/records/d2s23-kgz69", "eprint_id": 11611, "eprint_status": "archive", "datestamp": "2023-08-22 08:27:05", "lastmod": "2023-10-17 15:10:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Adelberger-K-L", "name": { "family": "Adelberger", "given": "Kurt L." } }, { "id": "Simenc-David-J", "name": { "family": "Simenc", "given": "David J." } } ] }, "title": "The physical nature of rest-UV galaxy morphology during the peak epoch of galaxy formation", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: fundamental parameters; galaxies: high-redshift; galaxies: irregular; galaxies: starburst; galaxies: structure", "note": "\u00a9 2007 The American Astronomical Society. \n\nReceived 2006 August 8; accepted 2006 October 22. \n\nD.R.L. and C.C.S. have been supported by grant AST 03-07263 from the US National Science Foundation and archival grant HST-AR 10311 from the Space Telescope Science Institute. The authors thank Rupali Chandar and Christy Tremonti for helpful communications.\n\nPublished - LAWapj07.pdf
", "abstract": "Motivated by the irregular and little-understood morphologies of z similar to 2-3 galaxies, we use nonparametric coefficients to quantify the morphologies of 216 galaxies that have been spectroscopically confirmed to lie at redshifts z = 1.8-3.4 in the GOODS-N field. Using measurements of UV and optical spectral lines, multiband photometric data, and stellar population models, we statistically assess possible correlations between galaxy morphology and physical observables such as stellar mass, star formation rate, and the strength of galaxy-scale outflows. We find evidence that dustier galaxies have more nebulous UV morphologies and that larger, more luminous galaxies may drive stronger outflows, but we otherwise conclude that UV morphology is either statistically decoupled from the majority of physical observables or determined by too complex a combination of physical processes to provide characterizations with predictive power. Given the absence of strong correlations between UV morphology and physical parameters such as star formation rates, we are therefore unable to support the hypothesis that morphologically irregular galaxies predominantly represent major galaxy mergers. Comparing galaxy samples, we find that IR-selected BzK galaxies and radio-selected submillimeter galaxies have UV morphologies similar to the optically selected sample, while distant red galaxies are more nebulous.", "date": "2007-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "656", "number": "1", "publisher": "American Astronomical Society", "pagerange": "1-26", "id_number": "CaltechAUTHORS:LAWapj07", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:LAWapj07", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 03-07263" }, { "agency": "NASA", "grant_number": "HST-AR 10311" } ] }, "doi": "10.1086/510357", "primary_object": { "basename": "LAWapj07.pdf", "url": "https://authors.library.caltech.edu/records/d2s23-kgz69/files/LAWapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Law, David R.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/mb1qc-49725", "eprint_id": 24589, "eprint_status": "archive", "datestamp": "2023-08-22 07:52:21", "lastmod": "2023-10-23 23:29:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" } ] }, "title": "A Spectroscopic Survey of Redshift 1.4 \u227e z \u227e 3.0 Galaxies in the GOODS-North Field: Survey Description, Catalogs, and Properties", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: evolution; galaxies: high-redshift; galaxies: starburst; galaxies: stellar content", "note": "\u00a9 2006 The American Astronomical Society. \n\nReceived 2006 May 7; accepted 2006 September 1. \n\nBased on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA and was made possible by the generous financial support of the W. M. Keck Foundation. \n\nWe thank David Law for setting up the Web site where the galaxy photometry and SEDfits are available to the public. We are grateful to the staff of the Keck and Palomar Observatories for their help in obtaining the data presented here. This work has been supported by grant AST 03-07263 from the National Science Foundation and by the David and Lucile Packard Foundation.\n\nPublished - REDapj06.pdf
", "abstract": "We present the results of a spectroscopic survey with LRIS-B on Keck of more than 280 star-forming galaxies and AGNs at redshifts 1.4 \u227e z \u227e 3.0 in the GOODS-N field. Candidates are selected by their U_nGR colors using the \"BM/BX\" criteria to target redshift 1.4 \u227e z \u227e 2.5 galaxies and the LBG criteria to target redshift z ~ 3 galaxies; combined these samples account for ~25%-30% of the R and K_s band counts to R = 25.5 and K_s(AB) = 24.4, respectively. The 212 BM/BX galaxies and 74 LBGs constitute the largest spectroscopic sample of galaxies at z > 1.4 in GOODS-N. Extensive multiwavelength data allow us to investigate the stellar populations, stellar masses, bolometric luminosities (L_(bol)), and extinction of z ~ 2 galaxies. Deep Chandra and Spitzer data indicate that the sample includes galaxies with a wide range in L_(bol) (\u224310^(10) to >10^(12) L_\u2609) and 4 orders of magnitude in dust obscuration (L_(bol)/L_(UV)). The sample includes galaxies with a large dynamic range in evolutionary state, from very young galaxies (ages \u224350 Myr) with small stellar masses (M* \u2243 10^9 M_\u2609) to evolved galaxies with stellar masses comparable to the most massive galaxies at these redshifts (M* > 10^(11) M_\u2609). Spitzer data indicate that the optical sample includes some fraction of the obscured AGN population at high redshifts: at least 3 of 11 AGNs in the z > 1.4 sample are undetected in the deep X-ray data but exhibit power-law SEDs longward of ~2 \u03bcm (rest frame) indicative of obscured AGNs. The results of our survey indicate that rest-frame UV selection and spectroscopy presently constitute the most timewise efficient method of culling large samples of high-redshift galaxies with a wide range in intrinsic properties, and the data presented here will add significantly to the multiwavelength legacy of GOODS.", "date": "2006-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "653", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1004-1026", "id_number": "CaltechAUTHORS:20110728-143023640", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110728-143023640", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 03-07263" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1086/508851", "primary_object": { "basename": "REDapj06.pdf", "url": "https://authors.library.caltech.edu/records/mb1qc-49725/files/REDapj06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Reddy, Naveen A.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/2nfhb-fq227", "eprint_id": 11170, "eprint_status": "archive", "datestamp": "2023-08-22 07:38:23", "lastmod": "2023-10-16 23:19:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Laird-E-S", "name": { "family": "Laird", "given": "E. S." } }, { "id": "Nandra-K", "name": { "family": "Nandra", "given": "K." }, "orcid": "0000-0002-7150-9192" }, { "id": "Hobbs-A", "name": { "family": "Hobbs", "given": "A." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "The X-ray emission of Lyman break galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "active galaxies; high-redshift galaxies; starburst galaxies; X-ray astronomy", "note": "\u00a9 2006 The Authors. Journal compilation \u00a9 2006 RAS. \n\nAccepted 2006 August 30. Received 2006 August 25; in original form 2006 May 2. \n\nWe acknowledge the financial support of PPARC (ESL) and the Leverhulme Trust (KN). This work has made use of data from the Chandra archive hosted at CfA. We are grateful to those who built and operate the Chandra X-ray Observatory.\n\nPublished - LAImnras06.pdf
", "abstract": "We present an analysis of the X-ray emission of a large sample of z\u223c3 Lyman break galaxies (LBGs), based on Chandra/ACIS observations of several LBG survey fields. A total of 24 LBGs are directly detected in the X-ray, approximately doubling the number of known detections. Thirteen of the LBGs have optical spectroscopic signatures of active galactic nucleus (AGN) activity, but almost all the other X-ray detections are also likely to host an accreting black hole based on their X-ray properties. The AGN exhibit a wide range in X-ray luminosity, from weak Seyferts to bright quasi-stellar objects (QSOs). An optical spectroscopy identified approximately one-third of the X-ray-detected sources as broad-line QSOs, one-third as narrow-line AGN (NLAGN) and one-third as normal star-forming LBGs. The fraction of X-ray-detected LBGs is 3 per cent, much lower than that which has been found for submillimetre-selected galaxies. Two galaxies have X-ray luminosities, spectra and fX/fopt values that are consistent with emission from star formation processes and are identified as candidate X-ray bright, pure starburst galaxies at z\u223c 3. If powered solely by star formation, the sources would have star formation rates (SFRs) of 300\u2013500 M\u2299 yr\u22121. X-ray spectral analysis of the LBGs shows a mean photon index of \u0393= 1.96 , similar to local AGN. There is evidence for absorption in at least 40 per cent of the objects. Significantly more absorption is evident in the NLAGN, which is consistent with AGN unification schemes. After correction for absorption, the narrow- and broad-line objects show the same average luminosity. X-ray-detected LBGs, spectroscopically classified as normal galaxies, however, are less luminous in both soft and hard X-ray bands, indicating that the host galaxy is outshining any optical AGN signature. Turning to the X-ray emission from LBGs without direct detections, stacking the X-ray flux in the two deepest Chandra fields under consideration [the Hubble Deep Field-North (HDF-N) and Groth\u2013Westphal Strip (GWS)] produced significant detections in each, although the GWS result was marginal. The detection in the HDF-N gives an X-ray-derived SFR of 42.4 \u00b1 7.8 M\u2299 yr^\u22121 per LBG and, by comparing with the ultraviolet (UV) SFR, the implied UV extinction correction is 4.1 \u00b1 0.8. The LBG sample was split into three bins based on UV magnitude to examine the correlation between UV and X-ray emission: for the limited statistics available, there was no evidence of any correlation.", "date": "2006-11-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "373", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "217-230", "id_number": "CaltechAUTHORS:LAImnras06", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:LAImnras06", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "Leverhulme Trust" } ] }, "doi": "10.1111/j.1365-2966.2006.11002.x", "primary_object": { "basename": "LAImnras06.pdf", "url": "https://authors.library.caltech.edu/records/2nfhb-fq227/files/LAImnras06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Laird, E. S.; Nandra, K.; et el." }, { "id": "https://authors.library.caltech.edu/records/z2pja-cem57", "eprint_id": 24574, "eprint_status": "archive", "datestamp": "2023-08-22 07:13:15", "lastmod": "2023-10-23 23:28:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Adelberger-K-L", "name": { "family": "Adelberger", "given": "Kurt L." } }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" } ] }, "title": "The Direct Detection of Lyman Continuum Emission from Star-forming Galaxies at z~3", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; diffuse radiation; galaxies: high-redshift; intergalactic medium", "note": "\u00a9 2006 American Astronomical Society. \n\nReceived 2006 March 14; accepted 2006 June 23. \n\nBased, in part, on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA and was made possible by the generous financial support of the W. M. Keck Foundation. We would like to thank our collaborators in the LBG survey for their assistance in various stages of the project and an anonymous referee, whose comments improved the paper. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible. We also thank the staff at the W. M. Keck Observatory for their assistance with the LRIS observations. Finally, we gratefully acknowledge Michael Santos and Jerry Ostriker for extensive and enlightening discussions and Robert Lupton for statistical insights. C. C. S. and D. K. E. have been supported by grants AST 00-70773 and AST 03-07263 from the US National Science Foundation and by the David and Lucile Packard Foundation. A. E. S. acknowledges support from the Miller Foundation for Basic Research in Science.\n\nPublished - SHAapj06.pdf
", "abstract": "We present the results of rest-frame UV spectroscopic observations of a sample of 14 z ~ 3 star-forming galaxies in the SSA 22a field. These spectra are characterized by unprecedented depth in the Lyman continuum region. For the first time, we have detected escaping ionizing radiation from individual galaxies at high redshift, with 2 of the 14 objects showing significant emission below the Lyman limit. We also measured the ratio of emergent flux density at 1500 \u00c5 to that in the Lyman continuum region, for the individual detections (C49 and D3) and the sample average. If a correction for the average IGM opacity is applied to the spectra of the objects C49 and D3, we find f_(1500)/f_(900,corr,C49) = 4.5 and f_(1500)/f_(900,corr,D3) = 2.9. The average emergent flux density ratio in our sample is = 22, implying an escape fraction ~4.5 times lower than inferred from the composite spectrum from Steidel and coworkers. If this new estimate is representative of LBGs, their contribution to the metagalactic ionizing radiation field is J_\u03bd(900) ~ 2.6 \u00d7 10^(-22) ergs s^(-1) cm^(-2) Hz^(-1) sr^(-1), comparable to the contribution of optically selected quasars at the same redshift. The sum of the contributions from galaxies and quasars is consistent with recent estimates of the level of the ionizing background at z ~ 3, inferred from the H I Ly\u03b1 forest optical depth. There is significant variance among the emergent far-UV spectra in our sample, yet the factors controlling the detection or nondetection of Lyman continuum emission from galaxies are not well determined. Because we do not yet understand the source of this variance, significantly larger samples will be required to obtain robust constraints on the galaxy contribution to the ionizing background at z ~ 3 and beyond.", "date": "2006-11-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "651", "number": "2", "publisher": "American Astronomical Society", "pagerange": "688-703", "id_number": "CaltechAUTHORS:20110727-154144547", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110727-154144547", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 00-70773" }, { "agency": "NSF", "grant_number": "AST 03-07263" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Miller Foundation for Basic Research in Science" } ] }, "doi": "10.1086/507511", "primary_object": { "basename": "SHAapj06.pdf", "url": "https://authors.library.caltech.edu/records/z2pja-cem57/files/SHAapj06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Shapley, Alice E.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/x7bnm-4de65", "eprint_id": 23664, "eprint_status": "archive", "datestamp": "2023-08-22 06:28:29", "lastmod": "2023-10-23 19:50:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Georgakakis-A", "name": { "family": "Georgakakis", "given": "A." } }, { "id": "Nandra-K", "name": { "family": "Nandra", "given": "K." }, "orcid": "0000-0002-7150-9192" }, { "id": "Laird-E-S", "name": { "family": "Laird", "given": "E. S." } }, { "id": "Gwyn-S", "name": { "family": "Gwyn", "given": "S." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Sarajedini-V-L", "name": { "family": "Sarajedini", "given": "V. L." } }, { "id": "Barmby-P", "name": { "family": "Barmby", "given": "P." }, "orcid": "0000-0003-2767-0090" }, { "id": "Faber-S-M", "name": { "family": "Faber", "given": "S. M." }, "orcid": "0000-0003-4996-214X" }, { "id": "Coil-A-L", "name": { "family": "Coil", "given": "A. L." } }, { "id": "Cooper-M-C", "name": { "family": "Cooper", "given": "M. C." }, "orcid": "0000-0003-1371-6019" }, { "id": "Davis-M-E-Astro", "name": { "family": "Davis", "given": "M." } }, { "id": "Newman-J-A", "name": { "family": "Newman", "given": "J. A." }, "orcid": "0000-0001-8684-2222" } ] }, "title": "A deep Chandra survey of the Groth Strip \u2013 II. Optical identification of the X-ray sources", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys; galaxies: active; cosmology: observations; X-rays: diffuse background; X-rays: galaxies", "note": "\u00a9 2006 The Authors. Journal compilation \u00a9 2006 Royal Astronomical Society. \n\nAccepted 2006 May 25. Received 2006 May 18; in original form 2005 November 7. Article first published online: 24 Jul. 2006. \n\nWe thank the anonymous referee for valuable comments and suggestions. AG acknowledges funding from PPARC and the Marie-Curie Fellowship grant MEIF-CT-2005-025108. This work uses data obtained with support of the National Science Foundation grants AST 95-29028 and AST 00-71198. Funding for the DEEP2 survey has been provided by NSF grant AST-0071048 and AST-0071198. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the\nCalifornia Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The DEEP2 team and Keck Observatory acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community and appreciate the opportunity to conduct observations from this mountain. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the CFHT which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France and the University of Hawaii. This work is based in part on data products produced at the Canadian Astronomy Data Centre as part of the CFHTLS, a collaborative project of NRC and CNRS.\n\nPublished - GEOmnras06.pdf
", "abstract": "In this paper, we discuss the optical and X-ray spectral properties of the sources detected in a single 200-ks Chandra pointing in the Groth-Westphal Strip region. A wealth of optical photometric and spectroscopic data are available in this field providing optical identifications and redshift determinations for the X-ray population. The optical photometry and spectroscopy used here are primarily from the Deep Extragalactic Evolutionary Probe 2 (DEEP2) survey with additional redshifts obtained from the literature. These are complemented with the deeper (r \u2248 26 mag) multiwaveband data (ugriz) from the Canada\u2013France\u2013Hawaii Telescope Legacy Survey to estimate photometric redshifts and to optically identify sources fainter than the DEEP2 magnitude limit (R_(AB)\u2248 24.5 mag). We focus our study on the 2\u201310 keV selected sample comprising 97 sources to the limit \u2248 8 \u00d7 10^(\u22121)6 erg s^(\u22121) cm^(\u22122), this being the most complete in terms of optical identification rate (86 per cent) and redshift determination fraction (63 per cent; both spectroscopic and photometric). We first construct the redshift distribution of the sample which shows a peak at z\u2248 1. This is in broad agreement with models where less luminous active galactic nuclei (AGNs) evolve out to z\u2248 1 with powerful quasi-stellar objects (QSOs) peaking at higher redshift, z\u2248 2. Evolution similar to that of broad-line QSOs applied to the entire AGN population (both types I and II) does not fit the data. We also explore the observedNH distribution of the sample and estimate a fraction of obscured AGN (N_H > 10^(22) cm^(\u22122)) of 48 \u00b1 9 per cent. This is found to be consistent with both a luminosity-dependent intrinsic N_H distribution, where less luminous systems comprise a higher fraction of type II AGNs and models with a fixed ratio 2:1 between types I and II AGNs. We further compare our results with those obtained in deeper and shallower surveys. We argue that a luminosity-dependent parametrization of the intrinsic NH distribution is required to account for the fraction of obscured AGN observed in different samples over a wide range of fluxes.", "date": "2006-09-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "371", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "221-234", "id_number": "CaltechAUTHORS:20110513-112624137", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110513-112624137", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "Marie Curie Fellowship", "grant_number": "MEIF-CT-2005-025108" }, { "agency": "NSF", "grant_number": "AST 95-29028" }, { "agency": "NSF", "grant_number": "AST 00-71198" } ] }, "doi": "10.1111/j.1365-2966.2006.10634.x", "primary_object": { "basename": "GEOmnras06.pdf", "url": "https://authors.library.caltech.edu/records/x7bnm-4de65/files/GEOmnras06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Georgakakis, A.; Nandra, K.; et el." }, { "id": "https://authors.library.caltech.edu/records/wwyy4-afx03", "eprint_id": 22531, "eprint_status": "archive", "datestamp": "2023-08-22 06:18:57", "lastmod": "2023-10-23 16:58:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Adelberger-K-L", "name": { "family": "Adelberger", "given": "Kurt L." } } ] }, "title": "H\u03b1 Observations of a Large Sample of Galaxies at z ~ 2: Implications for Star Formation in High-Redshift Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; stars: formation", "note": "\u00a9 2006 American Astronomical Society. \n\nReceived 2006 February 14; accepted 2006 April 18. \n\nBased on data obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. \n\nWe thank Andrew Blain, Jonathan Bird, David Kaplan, and Shri Kulkarni for obtaining near-IR images of some of our targets, and the staffs of the Keck and Palomar observatories for their assistance with the observations. We also thank the anonymous referee for a useful report. C. C. S., D. K. E., and N. A. R. have been supported by grant AST 03-07263 from the US National Science Foundation and by the David and Lucile Packard Foundation. A. E. S. acknowledges support from the Miller Institute for Basic Research in Science, and K. L. A. from the Carnegie Institution of Washington. Finally, we wish to extend special thanks to those of Hawaiian ancestry on whose \nsacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible.\n\nPublished - ERBapj06b.pdf
", "abstract": "Using H\u03b1 spectra of 114 rest-frame UV-selected galaxies at z ~ 2, we compare inferred star formation rates (SFRs) with those determined from the UV continuum luminosity. After correcting for extinction using standard techniques based on the UV continuum slope, we find excellent agreement between the indicators, with = 31 M_\u2609 yr^(-1) and = 29 M_\u2609 yr^(-1). The agreement between the indicators suggests that the UV luminosity is attenuated by a typical factor of ~4.5 (ranging from no attenuation to a factor of ~100 for the most obscured object in the sample), in good agreement with estimates of obscuration from X-ray, radio, and mid-IR data. The H\u03b1 luminosity is attenuated by a factor of ~1.7 on average, and the maximum H\u03b1 attenuation is a factor of ~5. In agreement with X-ray and mid-IR studies, we find that the SFR increases with increasing stellar mass and at brighter K magnitudes to ~ 60 M_\u2609 yr^(-1) for galaxies with K_s < 20; the correlation between K magnitude and SFR is much stronger than the correlation between stellar mass and SFR. All galaxies in the sample have SFRs per unit area \u03a3_(SFR) in the range observed in local starbursts. We compare the instantaneous SFRs and the past average SFRs as inferred from the ages and stellar masses, finding that for most of the sample, the current SFR is an adequate representation of the past average. There is some evidence that the most massive galaxies (M_* > 10^(11) M_\u2609) have had higher SFRs in the past.", "date": "2006-08-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "647", "number": "1", "publisher": "American Astronomical Society", "pagerange": "128-139", "id_number": "CaltechAUTHORS:20110225-160800612", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110225-160800612", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 03-07263" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Miller Institute for Basic Research in Science" }, { "agency": "Carnegie Institution of Washington" } ] }, "doi": "10.1086/505341", "primary_object": { "basename": "ERBapj06b.pdf", "url": "https://authors.library.caltech.edu/records/wwyy4-afx03/files/ERBapj06b.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Erb, Dawn K.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/547h9-1ec02", "eprint_id": 22535, "eprint_status": "archive", "datestamp": "2023-08-19 18:18:54", "lastmod": "2023-10-23 16:58:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Erb-D-K", "name": { "family": "Erb", "given": "Dawn K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "Naveen A." }, "orcid": "0000-0001-9687-4973" }, { "id": "Adelberger-K-L", "name": { "family": "Adelberger", "given": "Kurt. L." } } ] }, "title": "The Stellar, Gas, and Dynamical Masses of Star-forming Galaxies at z ~ 2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2014 galaxies: high-redshift \u2014 galaxies: kinematics and dynamics", "note": "\u00a9 2006 American Astronomical Society. \nReceived 2006 February 3, accepted for publication 2006 March 31. \n\nBased on data obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. We thank Andrew Blain, Jonathan Bird, David Kaplan, and Shri Kulkarni for obtaining near-IR images of some of our targets;\nthe staffs of the Keck and Palomar observatories for their assistance\nwith the observations; and the anonymous referee for a thoroughly helpful report that significantly improved the paper. C. C. S., D. K. E., and N. A. R. have been supported by grant AST 03-07263 from the US National Science Foundation and by the David and Lucile Packard Foundation. A. E. S. acknowledges support from the Miller Institute for Basic Research in Science, and K. L. A. acknowledges support from the Carnegie Institution of Washington. Finally, we wish to extend special thanks to those of Hawaiian ancestry, on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented here would not have been possible.\n\nPublished - ERBapj06a.pdf
", "abstract": "We present analysis of the near-infrared spectra of 114 rest-frame UV-selected star-forming galaxies at z ~ 2. By combining the H\u03b1 spectra with photometric measurements from observed 0.3-8 \u03bcm, we assess the relationships among kinematics, dynamical masses, inferred gas fractions, and stellar masses and ages. The H\u03b1 line widths give a mean dynamical mass M_(dyn) = (6.9 \u00b1 0.6) \u00d7 10^(10) M_\u2299 within a typical radius of ~6 kpc, after excluding AGNs. The average dynamical mass is ~2 times larger than the average stellar mass, and the two agree to within a factor of several for most objects. However, ~15% of the sample has M_(dyn)\u226b M. These objects are best fit by young stellar populations and tend to have high H\u03b1 equivalent widths, W_(H\u03b1) \u2273 200 \u00c5, suggesting that they are young starbursts with large gas masses. Rest-frame optical luminosity and velocity dispersion are correlated with 4 \u03c3 significance. Using the local empirical correlation between star formation rate per unit area and gas surface density, we estimate the mass of the gas associated with star formation and find a mean gas fraction of ~50% and a strong decrease in gas fraction with increasing stellar mass. The masses of gas and stars combined are considerably better correlated with the dynamical masses than are the stellar masses alone, and agree to within a factor of 3 for 85% of the sample. The combination of kinematic measurements, estimates of gas masses, and stellar population properties suggest that the factor of ~500 range in stellar mass across the sample cannot be fully explained by intrinsic differences in the total masses of the galaxies, which vary by a factor of ~40; the remaining variation is due to the evolution of the stellar population and the conversion of gas into stars.", "date": "2006-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "646", "number": "1", "publisher": "American Astronomical Society", "pagerange": "107-132", "id_number": "CaltechAUTHORS:20110228-084159205", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110228-084159205", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 03-07263" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Miller Institute for Basic Research in Science" }, { "agency": "Carnegie Institution of Washington" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1086/504891", "primary_object": { "basename": "ERBapj06a.pdf", "url": "https://authors.library.caltech.edu/records/547h9-1ec02/files/ERBapj06a.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Erb, Dawn K.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/hqsd6-5ma33", "eprint_id": 24497, "eprint_status": "archive", "datestamp": "2023-08-22 06:03:37", "lastmod": "2023-10-23 22:46:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "F\u00f6rster-Schreiber-N-M", "name": { "family": "F\u00f6rster Schreiber", "given": "N. M." } }, { "id": "Genzel-Reinhard", "name": { "family": "Genzel", "given": "R." }, "orcid": "0000-0002-2767-9653" }, { "id": "Lehnert-Matthew-D", "name": { "family": "Lehnert", "given": "M. D." }, "orcid": "0000-0003-1939-5885" }, { "id": "Bouch\u00e9-N", "name": { "family": "Bouch\u00e9", "given": "N." } }, { "id": "Verma-A", "name": { "family": "Verma", "given": "A." } }, { "id": "Erb-D-K", "name": { "family": "Erb", "given": "D. K." }, "orcid": "0000-0001-9714-2758" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "A. E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Davies-R", "name": { "family": "Davies", "given": "R." } }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Nesvadba-N-P-H", "name": { "family": "Nesvadba", "given": "N." } }, { "id": "Tacconi-Linda-J", "name": { "family": "Tacconi", "given": "L. J." }, "orcid": "0000-0002-1485-9401" }, { "id": "Eisenhauer-F", "name": { "family": "Eisenhauer", "given": "F." } }, { "id": "Abuter-R", "name": { "family": "Abuter", "given": "R." } }, { "id": "Gilbert-A-C", "name": { "family": "Gilbert", "given": "A." } }, { "id": "Gillessen-S", "name": { "family": "Gillessen", "given": "S." } }, { "id": "Sternberg-A", "name": { "family": "Sternberg", "given": "A." } } ] }, "title": "SINFONI Integral Field Spectroscopy of z ~ 2 UV-selected Galaxies: Rotation Curves and Dynamical Evolution", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: kinematics and dynamics; infrared: galaxies", "note": "\u00a9 2006 American Astronomical Society. \n\nReceived 2006 January 21; accepted 2006 March 19. \n\nBased on observations obtained at the Very Large Telescope (VLT) of the European Southern Observatory, Paranal, Chile (ESO program IDs 073.B-9018, 074.A-9011, 075.A-0466, and 076.A-0527). \n\nWe wish to thank the ESO staff for helpful and enthusiastic support during the observations. We thank the referee for useful comments that helped improve the paper.We are also grateful to Norman Murray, Eliot Quataert, Todd Thompson, Ortwin Gerhard, and Sune Toft for interesting discussions and insightful comments on various aspects of this work.\n\nPublished - SCHRapj06.pdf
", "abstract": "We present ~0\".5 resolution near-infrared integral field spectroscopy of the H\u03b1 line emission of 14 z ~ 2 UV-selected BM/BX galaxies, obtained with SINFONI at the ESO Very Large Telescope. The average H\u03b1 half-light radius is r_(1/2)\u2248 4 h^(-1)_(70) kpc, and line emission is detected over \u227320 h^(-1)_(70)kpc in several sources. In nine galaxies, we detect spatially resolved velocity gradients, from 40 to 410 km s^(-1) over ~10 h^(-1)_(70) kpc. The kinematics of the larger systems are generally consistent with orbital motions. Four galaxies are well described by rotating clumpy disks, and we extracted rotation curves out to radii \u227310 h^(-1)_(70) kpc. One or two galaxies exhibit signatures more consistent with mergers. Analyzing all 14 galaxies in the framework of rotating disks, we infer mean inclination- and beam-corrected maximum circular velocities of v_c ~ 180 \u00b1 90 km s^(-1) and dynamical masses from ~0.5 to 25 \u00d7 10^(10) h^(-1)_(70) M_\u2609 within r_(1/2). The specific angular momenta of our BM/BX galaxies are similar to those of local late-type galaxies. Moreover, the specific angular momenta of their baryons are comparable to those of their dark matter halos. Extrapolating from the average vc at 10 himg1.gif kpc, the virial mass of the typical halo of a galaxy in our sample is 10^(11.7\u00b10.5) h^(-1)_(70) M_\u2609. Kinematic modeling of the three best cases implies a ratio of v_c to local velocity dispersion v_(c)/\u03c3 ~ 2-4 and, accordingly, a large geometric thickness. We argue that this suggests a mass accretion (alternatively, gas exhaustion) timescale of ~500 Myr. We also argue that if our BM/BX galaxies were initially gas-rich, their clumpy disks would subsequently lose their angular momentum and form compact bulges on a timescale of ~1 Gyr.", "date": "2006-07-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "645", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1062-1075", "id_number": "CaltechAUTHORS:20110721-114249847", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110721-114249847", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1086/504403", "primary_object": { "basename": "SCHRapj06.pdf", "url": "https://authors.library.caltech.edu/records/hqsd6-5ma33/files/SCHRapj06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "F\u00f6rster Schreiber, N. M.; Genzel, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/thfw6-ss396", "eprint_id": 22341, "eprint_status": "archive", "datestamp": "2023-08-22 05:41:56", "lastmod": "2023-10-23 15:52:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Berger-Edo", "name": { "family": "Berger", "given": "E." }, "orcid": "0000-0002-9392-9681" }, { "id": "Penprase-B-E", "name": { "family": "Penprase", "given": "B. E." } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Fox-D-B", "name": { "family": "Fox", "given": "D. B." }, "orcid": "0000-0002-3714-672X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "N. A." }, "orcid": "0000-0001-9687-4973" } ] }, "title": "Spectroscopy of GRB 050505 at z = 4.275: A log N(H I) = 22.1 DLA host galaxy and the nature of the progenitor", "ispublished": "pub", "full_text_status": "public", "keywords": "gamma rays: bursts; ISM: abundances; ISM: kinematics and dynamics; stars: mass loss; stars: Wolf-Rayet", "note": "\u00a9 2006 American Astronomical Society. \n\nReceived 2005 November 16; accepted 2006 January 12. \n\nWe thank Michael Rauch for helpful discussions and comments, and Allard-Jan vanMarle for information on Wolf-Rayet winds. E. B. is supported is supported by NASA through Hubble Fellowship grant HST-01171.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.\n\nPublished - BERapj06.pdf
", "abstract": "We present optical spectroscopy of the afterglow of GRB 050505 obtained with the Keck I 10 m telescope. The spectrum exhibits three absorption systems with the highest, at z = 4.2748, arising in the host galaxy. The host absorption is marked by a DLA with log N(H i) = 22.05 \u00b1 0.10, higher than that of any QSO-DLA detected to date but similar to several other recent measurements from GRB spectra. We further deduce a metallicity of Z \u2248 0.06 Z_\u2299, with a depletion pattern that is similar to that of the Galactic warm halo or warm disk. More importantly, we detect strong absorption from Si II^* indicating a dense environment, n_H \u2273 10^2 cm^(-3), in the vicinity of the burst, with a size of ~4 pc. The C IV absorption system spans a velocity range of about 10^3 km s^(-1), most likely arising in the progenitor stellar wind. In this context the lack of corresponding Si IV absorption indicates that the progenitor had a mass \u227e 25 M_\u2299 and a metallicity \u227e 0.1 Z_\u2299, and therefore required a binary companion to eject its hydrogen envelope prior to the GRB explosion. Finally, by extending the GRB-DLA sample to z \u2248 4.3 we show that these objects appear to follow a similar metallicity-redshift relation as in QSO-DLAs, but with systematically higher metallicities. It remains to be seen whether this trend is simply due to the higher neutral hydrogen columns in GRB-DLAs and/or sight lines which probe star-forming regions, or if it is a manifestation of different star formation properties in GRB-DLAs.", "date": "2006-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "642", "number": "2", "publisher": "American Astronomical Society", "pagerange": "979-988", "id_number": "CaltechAUTHORS:20110217-090330627", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110217-090330627", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-01171.01" }, { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/501162", "primary_object": { "basename": "BERapj06.pdf", "url": "https://authors.library.caltech.edu/records/thfw6-ss396/files/BERapj06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Berger, E.; Penprase, B. E.; et el." }, { "id": "https://authors.library.caltech.edu/records/anwxj-ybx45", "eprint_id": 22539, "eprint_status": "archive", "datestamp": "2023-08-22 05:36:46", "lastmod": "2023-10-23 16:58:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Crowther-P-A", "name": { "family": "Crowther", "given": "Paul A." } }, { "id": "Prinja-R-K", "name": { "family": "Prinja", "given": "Raman K." } }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "On the reliability of C IV \u03bb 1549 as an abundance indicator for high-redshift star-forming galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: abundances; galaxies: starburst; ultraviolet: galaxies", "note": "\u00a9 2006 The Authors. Journal compilation \u00a9 2006 RAS. \n\nAccepted 2006 February 7. Received 2006 January 24. Article first published online: 23 Mar. 2006. \n\nBased, in part, on the observations with the NASA/ESA HST, obtained from the ESO/ST-ECF Science Archive Facility. PAC gratefully acknowledges financial support from the Royal Society. We thank Sam Rix for providing her synthetic UV spectra of star-forming galaxies.\n\nPublished - CROmnras06.pdf
", "abstract": "We reconsider the use of the equivalent width of C IV \u03bb 1549, EW(C IV), as an indicator of the oxygen abundance in star-forming galaxies, as proposed by Heckman et al. for nearby starbursts. We refine the local calibration of EW(C IV) versus log (O/H) by using a restricted wavelength window which minimizes blending with interstellar absorption lines. When applied to the stellar component only of the complex C IV \u03bb 1549 features in two high-redshift galaxies with good quality spectra, MS 1512-cB58 (z = 2.7268) and Q1307-BM1163 (z = 1.4105), the local calibration gives values of the oxygen abundance which are in good agreement with other metallicity determinations based on nebular emission and interstellar absorption lines. Our main conclusion is that for this method to give reliable results at high redshifts, it should only be used on data of sufficiently high spectral resolution (R \u2273 1000) for stellar and interstellar C IV components to be clearly separated. Oxygen abundances will be systematically overestimated if the local calibration is applied to spectra of high-redshift galaxies obtained with the low resolving powers (R \u2243 200 - 300) of many current wide-field surveys. It will also be necessary to understand better the causes of the scatter in the local relation, before we can be confident of inferences from it at high z.", "date": "2006-05", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "368", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "895-902", "id_number": "CaltechAUTHORS:20110228-090445852", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110228-090445852", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" } ] }, "doi": "10.1111/j.1365-2966.2006.10164.x", "primary_object": { "basename": "CROmnras06.pdf", "url": "https://authors.library.caltech.edu/records/anwxj-ybx45/files/CROmnras06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Crowther, Paul A.; Prinja, Raman K.; et el." }, { "id": "https://authors.library.caltech.edu/records/c6c0m-qd540", "eprint_id": 75920, "eprint_status": "archive", "datestamp": "2023-08-22 04:09:09", "lastmod": "2023-10-25 15:25:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Adelberger-K-L", "name": { "family": "Adelberger", "given": "Kurt L." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "A Possible Correlation between the Luminosities and Lifetimes of Active Galactic Nuclei", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; large-scale structure of universe; quasars: general", "note": "\u00a9 2005. The American Astronomical Society. \n\nReceived 2005 March 10; accepted 2005 May 11. \n\n K. L. A. would like to thank L. Ho, L. Hernquist, L. Ferrarese, and J. Kollmeier for many interesting conversations and an anonymous referee for encouraging us to discuss the physical interpretation of the duty cycle. Our collaborators in the Lyman break survey did most of the work in taking and reducing these data. We are grateful that they let us proceed with the analysis. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. \n\nBased, in part, on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership between the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation.\n\nPublished - pdf
Submitted - 0505210.pdf
", "abstract": "We use the clustering of galaxies around distant AGNs to show with ~90% confidence that fainter AGNs are longer lived. Our argument is simple: since the measured galaxy-AGN cross-correlation length r_0 ~ 5 h^(-1) Mpc does not vary significantly over a 10 mag range in AGN optical luminosity, faint and bright AGNs must reside in dark matter halos with similar masses. The halos that host bright and faint AGNs must therefore have similar abundances, and bright AGNs are rare partly because their lifetimes are short.", "date": "2005-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "630", "number": "1", "publisher": "American Astronomical Society", "pagerange": "50-58", "id_number": "CaltechAUTHORS:20170408-141820229", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170408-141820229", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Carnegie Trust" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/431789", "primary_object": { "basename": "0505210.pdf", "url": "https://authors.library.caltech.edu/records/c6c0m-qd540/files/0505210.pdf" }, "related_objects": [ { "basename": "pdf", "url": "https://authors.library.caltech.edu/records/c6c0m-qd540/files/pdf" } ], "resource_type": "article", "pub_year": "2005", "author_list": "Adelberger, Kurt L. and Steidel, Charles C." }, { "id": "https://authors.library.caltech.edu/records/18ry8-04f13", "eprint_id": 76067, "eprint_status": "archive", "datestamp": "2023-08-19 13:28:57", "lastmod": "2023-10-25 15:30:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hunt-M-P", "name": { "family": "Hunt", "given": "Matthew P." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Adelberger-K-L", "name": { "family": "Adelberger", "given": "Kurt L." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" } ] }, "title": "The Faint End of the QSO Luminosity Function at z = 3", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2004. The American Astronomical Society. \n\nReceived 2003 September 16; accepted 2003 December 1. \n\nWe wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, most of the observations presented herein would not have been possible. We would also like to thank the staffs at the Keck and Palomar observatories for their invaluable assistance with the observations, and the anonymous referee for helpful suggestions. M. P. H., C. C. S., and A. E. S. have been supported by grant AST 00-70773 from the US National Science Foundation and by the David and Lucile Packard Foundation. \n\nBased, in part, on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation.\n\nPublished - pdf
Submitted - 0312041v2.pdf
", "abstract": "We present the first measurement of the faint end of the QSO luminosity function at z = 3. The QSOs, which range from M_(1450) = -21 to M_(1450) = -27, were discovered in 17 fields totaling 0.43 deg^2 using multicolor selection criteria (the Lyman break technique) and spectroscopic follow-up. We find that the faint-end slope of the luminosity function is \u03b2_l = 1.24 \u00b1 0.07 (\u03a6 \u221d L^(-\u03b2_t)), flatter than the value of \u03b2_l = 1.64 \u00b1 0.18 measured at lower redshift. The integrated rest 1450 \u00c5 UV luminosity of z = 3 QSOs is only 50% of most previous estimates and only sime8% of that produced by Lyman break galaxies at the same redshifts. Assuming that ionizing photons from faint QSOs are as successful in escaping their host galaxies as bright QSOs, we estimate the total contribution of QSOs to the ionizing flux J912 at z ~ 3, J912 \u2243 2.4 \u00d7 10^(-22) ergs s^(-1) cm^(-2) Hz^(-1). This estimate, which we regard as an upper limit, remains consistent with rough estimates of J_(912) based on the Ly\u03b1 forest \"proximity effect.\"", "date": "2004-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "605", "number": "2", "publisher": "American Astronomical Society", "pagerange": "625-630", "id_number": "CaltechAUTHORS:20170408-154715902", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170408-154715902", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "NSF", "grant_number": "AST 00-70773" } ] }, "doi": "10.1086/381727", "primary_object": { "basename": "0312041v2.pdf", "url": "https://authors.library.caltech.edu/records/18ry8-04f13/files/0312041v2.pdf" }, "related_objects": [ { "basename": "pdf", "url": "https://authors.library.caltech.edu/records/18ry8-04f13/files/pdf" } ], "resource_type": "article", "pub_year": "2004", "author_list": "Hunt, Matthew P.; Steidel, Charles C.; et el." }, { "id": "https://authors.library.caltech.edu/records/ekw54-ftj07", "eprint_id": 99153, "eprint_status": "archive", "datestamp": "2023-08-19 09:46:29", "lastmod": "2023-10-18 17:54:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" }, { "id": "Rix-Samantha-A", "name": { "family": "Rix", "given": "Samantha A." } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Chuck C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Hunt-M-P", "name": { "family": "Hunt", "given": "Matthew P." } }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice E." }, "orcid": "0000-0003-3509-4855" }, { "id": "Adelberger-K-L", "name": { "family": "Adelberger", "given": "Kurt L." } } ] }, "title": "MS 1512\u2013cB58: A case study of star formation, metal enrichment and superwinds in Lyman break galaxies", "ispublished": "pub", "full_text_status": "restricted", "keywords": "Galaxies: evolution \u2013 galaxies: starburst \u2013 galaxies: individual (MS 1512\u2212cB58)", "note": "\u00a9 Kluwer Academic Publishers 2002.", "abstract": "Recent advances in instrumentation and observing techniques have made it possible to begin to study in detail the stellar populations and the interstellar media of galaxies at redshift z = 3, when the universe was still in its 'teen years'. I illustrate recent progress in this field with the latest observations of the gravitationally lensed galaxy MS 1512- cB58.", "date": "2002-07", "date_type": "published", "publication": "Astrophysics and Space Science", "volume": "281", "number": "1/2", "publisher": "Springer", "pagerange": "461-466", "id_number": "CaltechAUTHORS:20191008-111636046", "issn": "0004-640X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191008-111636046", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1023/a:1019500911063", "resource_type": "article", "pub_year": "2002", "author_list": "Pettini, Max; Rix, Samantha A.; et el." }, { "id": "https://authors.library.caltech.edu/records/qp14j-9qs15", "eprint_id": 74575, "eprint_status": "archive", "datestamp": "2023-08-21 20:58:07", "lastmod": "2023-10-24 22:46:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hogg-D-W", "name": { "family": "Hogg", "given": "David W." }, "orcid": "0000-0003-2866-9403" }, { "id": "Pahre-M-A", "name": { "family": "Pahre", "given": "Michael A." } }, { "id": "Adelberger-K-L", "name": { "family": "Adelberger", "given": "Kurt L." } }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger" }, "orcid": "0000-0002-1854-5506" }, { "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673" }, { "id": "Gautier-T-N-III", "name": { "family": "Gautier", "given": "T. N." } }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "Thomas" }, "orcid": "0000-0002-4939-734X" }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Caltech Faint Galaxy Redshift Survey. IX. Source Detection and Photometry in the Hubble Deep Field Region", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: fundamental parameters; galaxies: photometry", "note": "\u00a9 2000 American Astronomical Society. \n\nReceived 1999 July 26. Accepted 1999 October 25. \n\nThe Hubble Deep Field (HDF) database was planned, taken, reduced, and made public by a large team at the Space Telescope Science Institute headed by B. Williams. We thank the referee, A. Dressler, for timely and helpful criticism. This study is based on observations made at the Palomar Observatory, which is owned and operated by the California Institute of Technology; and with the NASA/ESA Hubble Space Telescope, which is operated by AURA under NASA contract NAS 5-26555. Primary financial support was provided under NSF grant AST 95-29170. Some additional support was provided by Hubble Fellowship grants HF-01093.01-97A and HF-01099.01-97A from STScI, which is operated by AURA under NASA contract NAS 5-26555.\n\nPublished - Hogg_2000_ApJS_127_1.pdf
Submitted - 9909360.pdf
", "abstract": "Detection and photometry of sources in the U_n, G, \u211b, and K_s bands in a 9 \u00d7 9 arcmin^2 region of the sky, centered on the Hubble Deep Field, are described. The data permit construction of complete photometric catalogs to roughly U_n = 25, G = 26, \u211b = 25.5, K_s = 20 mag and significant photometric measurements somewhat fainter. The galaxy number density is 1.3 \u00d7 10^5 deg^(-2) to \u211b = 25.0 mag. Galaxy number counts have slopes d log N/dm = 0.42, 0.33, 0.27, and 0.31 in the U_n, G, \u211b, and K_s bands, consistent with previous studies and the trend that fainter galaxies are, on average, bluer. Galaxy catalogs selected in the \u211b and K_s bands are presented, containing 3607 and 488 sources in field areas of 74.8 and 59.4 arcmin^2, to \u211b = 25.5 and K_s = 20 mag.", "date": "2000-03", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "127", "number": "1", "publisher": "American Astronomical Society", "pagerange": "1-9", "id_number": "CaltechAUTHORS:20170228-080833641", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170228-080833641", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF", "grant_number": "AST 95-29170" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HF-01093.01-97A" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HF-01099.01-97A" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1086/313318", "primary_object": { "basename": "9909360.pdf", "url": "https://authors.library.caltech.edu/records/qp14j-9qs15/files/9909360.pdf" }, "related_objects": [ { "basename": "Hogg_2000_ApJS_127_1.pdf", "url": "https://authors.library.caltech.edu/records/qp14j-9qs15/files/Hogg_2000_ApJS_127_1.pdf" } ], "resource_type": "article", "pub_year": "2000", "author_list": "Hogg, David W.; Pahre, Michael A.; et el." }, { "id": "https://authors.library.caltech.edu/records/q63vs-ysk36", "eprint_id": 52160, "eprint_status": "archive", "datestamp": "2023-08-19 04:14:44", "lastmod": "2023-10-18 19:37:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Observing the epoch of galaxy formation", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1999 National Academy of Sciences.\n\nPublished - PNAS-1999-Steidel-4232-5.pdf
", "abstract": "Significant observational progress in addressing the question of the origin and early evolution of galaxies has been made in the past few years, allowing for direct comparison of the epoch when most of the stars in the universe were forming to prevailing theoretical models. There is currently broad consistency between theoretical expectations and the observations, but rapid improvement in the data will provide much more critical tests of theory in the coming years.", "date": "1999-04-13", "date_type": "published", "publication": "Proceedings of the National Academy of Sciences of the United States of America", "volume": "96", "number": "8", "publisher": "National Academy of Sciences", "pagerange": "4232-4235", "id_number": "CaltechAUTHORS:20141125-150513174", "issn": "0027-8424", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141125-150513174", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1073/pnas.96.8.4232", "pmcid": "PMC33559", "primary_object": { "basename": "PNAS-1999-Steidel-4232-5.pdf", "url": "https://authors.library.caltech.edu/records/q63vs-ysk36/files/PNAS-1999-Steidel-4232-5.pdf" }, "resource_type": "article", "pub_year": "1999", "author_list": "Steidel, Charles C." }, { "id": "https://authors.library.caltech.edu/records/1rgnv-jdc66", "eprint_id": 105651, "eprint_status": "archive", "datestamp": "2023-08-22 13:30:57", "lastmod": "2023-10-20 22:14:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Adelberger-K-L", "name": { "family": "Adelberger", "given": "K." } }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Dickinson-M", "name": { "family": "Dickinson", "given": "M." } }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "M." }, "orcid": "0000-0002-5139-4359" }, { "id": "Kellogg-M", "name": { "family": "Kellogg", "given": "M." } } ] }, "title": "Galaxy clustering at z \u223c 3", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology; large-scale structure; galaxy formation; observational cosmology", "note": "\u00a9 1999 The Royal Society. \n\nDiscussion Meeting Issue 'Large\u2013scale structure in the Universe' organized by G. P. Efstathiou, R. S. Ellis, J. E. Gunn and D. York. \n\nMuch of the work described would not have been possible without the generous gift from the W. M. Keck Foundation that allowed the construction of the Keck Observatory, and the many people involved in building and supporting the telescopes and the low-resolution imaging spectrograph. This work has been financially supported by the US National Science foundation (C.S., K.A., M.K.) and by grant HF-01071.01-94A from the Space Telescope Science Institute (M.G.).\n\nSubmitted - 9805267.pdf
", "abstract": "Galaxies at very high redshift (z \u223c 3 or greater) are now accessible to wholesale observation, making possible for the first time a robust statistical assessment of their spatial distribution at look\u2013back times approaching ca. 90% of the age of the universe. This paper summarizes recent progress in understanding the nature of these early galaxies, concentrating in particular on the clustering properties. Direct comparison of the data to predictions and physical insights provided by galaxy and structure formation models is particularly straightforward at these early epochs, and results in critical tests of the 'biased' hierarchical galaxy formation paradigm.", "date": "1999-01-15", "date_type": "published", "publication": "Philosophical Transactions A: Mathematical, Physical and Engineering Sciences", "volume": "357", "number": "1750", "publisher": "Royal Society of London", "pagerange": "153-166", "id_number": "CaltechAUTHORS:20200929-143507369", "issn": "1364-503X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200929-143507369", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NSF" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HF-01071.01-94A" } ] }, "doi": "10.1098/rsta.1999.0320", "primary_object": { "basename": "9805267.pdf", "url": "https://authors.library.caltech.edu/records/1rgnv-jdc66/files/9805267.pdf" }, "resource_type": "article", "pub_year": "1999", "author_list": "Steidel, C.; Adelberger, K.; et el." }, { "id": "https://authors.library.caltech.edu/records/wnzmz-sbr18", "eprint_id": 52172, "eprint_status": "archive", "datestamp": "2023-08-19 02:24:12", "lastmod": "2023-10-18 19:38:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Galaxies and large scale structure at high redshifts", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1998 by The National Academy of Sciences. \n\nThis paper was presented at a colloquium entitled ''The Age of the Universe, Dark Matter, and Structure Formation,'' organized by David N. Schramm, held March 21\u201323, 1997, sponsored by the National Academy of Sciences at the Beckman Center in Irvine, CA. \n\nIt is a pleasure to thank my collaborators and colleagues, Kurt Adelberger, Mark Dickinson, Mauro Giavalisco, Mindy Kellogg, and\nMax Pettini, for allowing me to present the results of our joint work.\nI would like also to acknowledge financial support from the National\nScience Foundation through the Young Investigator Program, as well\nas the Alfred P. Sloan Foundation. The Keck Observatory, without\nwhich much of the work described above would not have been possible, is operated jointly by the California Institute of Technology and the University of California, and was made possible by a generous gift from the W. M. Keck Foundation.\n\nPublished - PNAS-1998-Steidel-22-8.pdf
", "abstract": "It is now straightforward to assemble large samples of very high redshift (z \u223c 3) field galaxies selected by their pronounced spectral discontinuity at the rest frame Lyman limit of hydrogen (at 912 \u00c5). This makes possible both statistical analyses of the properties of the galaxies and the first direct glimpse of the progression of the growth of their large-scale distribution at such an early epoch. Here I present a summary of the progress made in these areas to date and some preliminary results of and future plans for a targeted redshift survey at z = 2.7\u20133.4. Also discussed is how the same discovery method may be used to obtain a \"census\" of star formation in the high redshift Universe, and the current implications for the history of galaxy formation as a function of cosmic epoch.", "date": "1998-01-06", "date_type": "published", "publication": "Proceedings of the National Academy of Sciences of the United States of America", "volume": "95", "number": "1", "publisher": "National Academy of Sciences", "pagerange": "22-28", "id_number": "CaltechAUTHORS:20141126-095046793", "issn": "0027-8424", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141126-095046793", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1073/pnas.95.1.22", "pmcid": "PMC34185", "primary_object": { "basename": "PNAS-1998-Steidel-22-8.pdf", "url": "https://authors.library.caltech.edu/records/wnzmz-sbr18/files/PNAS-1998-Steidel-22-8.pdf" }, "resource_type": "article", "pub_year": "1998", "author_list": "Steidel, Charles C." }, { "id": "https://authors.library.caltech.edu/records/39zgd-xp565", "eprint_id": 38032, "eprint_status": "archive", "datestamp": "2023-08-22 11:46:37", "lastmod": "2023-10-23 19:42:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Metzger-M-R", "name": { "family": "Metzger", "given": "M. R." } }, { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "S. G." }, "orcid": "0000-0002-0603-3087" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C. C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Adelberger-K-L", "name": { "family": "Adelberger", "given": "K. L." } }, { "id": "Frail-D-A", "name": { "family": "Frail", "given": "D. A." } }, { "id": "Costa-E", "name": { "family": "Costa", "given": "E." } }, { "id": "Frontera-F", "name": { "family": "Frontera", "given": "F." } } ] }, "title": "Spectral constraints on the redshift of the optical counterpart to the \u03b3-ray burst of 8 May 1997", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 1997 Macmillan Publishers Ltd. \n\nReceived 21 May; accepted 3 June 1997. \n\nWe thank the BeppoSAX team for their efforts in disseminating information to observers for rapid identification of an optical transient, making this work possible. We thank W. Sargent and M. Pahre for discussions, and the Keck Observatory staff for assistance at the telescope. This work is based on observations obtained at the W. M. Keck Observatory, which is jointly operated by the California Institute of Technology and the University of California. M.R.M. was supported by Caltech; S.R.K. was supported by NASA and NSF; S.G.D. was supported by NSF and the Bressler Foundation; C.C.S. was supported by NSF and the Sloan Foundation.", "abstract": "Brief, intense bursts of y-rays occur approximately daily from random directions in space, but their origin has remained unknown since their initial detection almost 25 years ago. Arguments based on their observed isotropy and apparent brightness distribution are not sufficient to constrain the location of the bursts to a local or cosmological origin. The recent detection of a counterpart to a y-ray burst at other wavelengths has therefore\nraised the hope that the sources of these energetic events might soon be revealed. Here we report spectroscopic observations of the possible optical counterpart to the y-ray burst GRB970508. The spectrum is mostly featureless, except for a few prominent absorption lines which we attribute to the presence of an absorption system along the line of sight at redshift z = 0.835. Coupled with the absence of Lyman-\u03b1 forest features in the spectra, our\nresults imply that the optical transient lies at 0.835 \u227e z \u227e 2.3. If the optical transient is indeed the counterpart of GRB970508, our results provide the first direct limits on the distance to a y-ray burst, confirming that at least some of these events lie at cosmological distances, and are thus highly energetic.", "date": "1997-06-26", "date_type": "published", "publication": "Nature", "volume": "387", "number": "6636", "publisher": "Nature Publishing Group", "pagerange": "878-880", "id_number": "CaltechAUTHORS:20130419-091322811", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130419-091322811", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech" }, { "agency": "NASA" }, { "agency": "NSF" }, { "agency": "Bressler Foundation" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "local_group": { "items": [ { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "resource_type": "article", "pub_year": "1997", "author_list": "Metzger, M. R.; Djorgovski, S. G.; et el." }, { "id": "https://authors.library.caltech.edu/records/dxw0d-m3y49", "eprint_id": 52281, "eprint_status": "archive", "datestamp": "2023-08-19 01:14:06", "lastmod": "2023-10-18 19:44:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Spergel-D-N", "name": { "family": "Spergel", "given": "David N." }, "orcid": "0000-0002-5151-0006" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "Simon J." }, "orcid": "0000-0002-6423-3597" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "The epoch of galaxy formation", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 1997 National Academy of Sciences. \n\nThis paper serves as a summary of a symposium session as part of the Frontiers of Science series, held November 7\u20139, 1996, at the Arnold and Mabel Beckman Center of the National Academies of Sciences and Engineering in Irvine, CA.\n\nPublished - PNAS-1997-Spergel-2783-4.pdf
", "abstract": "Recent advances in technology have enabled astronomers to observe fainter, and more distant, galaxies and to study the processes of galaxy formation and evolution. Recent observations suggest that the bulk of the stars in the universe formed between z = 3 (\u223c1 \u00d7 10^9 years after the big bang) and the present. The star formation rate appears to have peaked at z \u223c 1\u20132 (\u223c 2\u20134 \u00d7 10^9 years after the big bang). While galactic disks appear to form primarily around z = 1, the central regions of spiral galaxies and most elliptical galaxies appear to have been assembled at higher redshift.", "date": "1997-04-01", "date_type": "published", "publication": "Proceedings of the National Academy of Sciences of the United States of America", "volume": "94", "number": "7", "publisher": "National Academy of Sciences", "pagerange": "2783-2784", "id_number": "CaltechAUTHORS:20141202-134228071", "issn": "0027-8424", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141202-134228071", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechAUTHORS", "doi": "10.1073/pnas.94.7.2783", "pmcid": "PMC34147", "primary_object": { "basename": "PNAS-1997-Spergel-2783-4.pdf", "url": "https://authors.library.caltech.edu/records/dxw0d-m3y49/files/PNAS-1997-Spergel-2783-4.pdf" }, "resource_type": "article", "pub_year": "1997", "author_list": "Spergel, David N.; Lilly, Simon J.; et el." }, { "id": "https://authors.library.caltech.edu/records/c9b91-dsk42", "eprint_id": 76429, "eprint_status": "archive", "datestamp": "2023-08-19 00:42:37", "lastmod": "2023-10-25 15:59:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Madau-P", "name": { "family": "Madau", "given": "Piero" } }, { "id": "Ferguson-H-C", "name": { "family": "Ferguson", "given": "Henry C." }, "orcid": "0000-0001-7113-2738" }, { "id": "Dickinson-Mark-E", "name": { "family": "Dickinson", "given": "Mark E." }, "orcid": "0000-0001-5414-5131" }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "Mauro" }, "orcid": "0000-0002-7831-8751" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Fruchter-A-S", "name": { "family": "Fruchter", "given": "Andrew" } } ] }, "title": "High-redshift galaxies in the Hubble Deep Field: colour selection and star formation history to z ~ 4", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: formation, galaxies: evolution, intergalactic medium, quasars: absorption lines, cosmology: observations, ultraviolet: galaxies", "note": "\u00a9 1996 RAS. \n\nAccepted 1996 August 15. Received 1996 August 1; in original fonn 1996 July 10. \n\nWe have benefited from discussions with M. Fall, D. Hogg, C. Leitherer, S. Lilly, Y. Pei, M. Pettini and M. Shull. Support for this work, which was based on observations made with the NASA/ESA Hubble Space Telescope, was provided by NASA through grant AR-06337.10-94A from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. MO acknowledges support from the Hubble Fellowship program through grant number HF-01071.01-94A. CCS acknowledges support from the Sloan Foundation and from the NSF through grant AST-9457446.\n\nPublished - 1388.full.pdf
Submitted - 9607172
", "abstract": "The Lyman decrement associated with the cumulative effect of H I in QSO absorption systems along the line of sight provides a distinctive feature for identifying galaxies at z \u2273 2.5. Colour criteria, which are sensitive to the presence of a Lyman continuum break superposed on an otherwise flat UV spectrum, have been shown, through Keck spectroscopy, to successfully identify a substantial population of star-forming galaxies at 3 \u2272 z \u2272 3.5. Such objects have proven to be surprisingly elusive in field galaxy redshift surveys; quantification of their surface densities and morphologies is crucial for determining how and when galaxies formed. The Hubble Deep Field (HDF) observations offer the opportunity to exploit the ubiquitous effect of intergalactic absorption and obtain useful statistical constraints on the redshift distribution of galaxies to considerably fainter limits than the current spectroscopic limits. We model the H I cosmic opacity as a function of redshift, including scattering in resonant lines of the Lyman series and Lyman continuum absorption, and use stellar population synthesis models with a wide variety of ages, metallicities, dust contents and redshifts to derive colour selection criteria that provide a robust separation between high-redshift and low-redshift galaxies. From the HDF images we construct a sample of star-forming galaxies at 2 \u2272z \u2272 4.5. While none of the \u223c 60 objects in the HDF having known Keck/Low-Resolution Imaging Spectrograph (LRIS) spectroscopic redshifts in the range 0 \u2272 z \u22721.4 is found to contaminate our high-redshift sample, our colour criteria are able to efficiently select the 2.6 \u2272 z \u2272 3.2 galaxies identified by Steidel et al. \n\nThe ultraviolet (and blue) dropout technique opens up the possibility of investigating cosmic star and element formation in the early Universe. We set a lower limit to the ejection rate of heavy elements per unit comoving volume from Type II supernovae at \u3008z\u3009 = 2.75 of \u2248 3.6 \u00d7 10^(\u22124) M_\u2299 yr^(\u22121) Mpc^(\u22123) (for q_0 = 0.5 and H_0 = 50 km s^(\u22121) Mpc^(\u22121)), which is 3 times higher than the local value but still 4 times lower than the rate observed at z \u2248 1. At \u3008z\u3009 = 4, our lower limit to the cosmic metal ejection rate is \u2248 3 times lower than the \u3008z\u3009 = 2.75 value. We discuss the implications of these results on models of galaxy formation, and on the chemical enrichment and ionization history of the intergalactic medium.", "date": "1996-12-31", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "283", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "1388-1404", "id_number": "CaltechAUTHORS:20170409-071151363", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170409-071151363", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "AR-06337.10-94A" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HF-01071.01-94A" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF", "grant_number": "AST-9457446" } ] }, "collection": "CaltechAUTHORS", "doi": "10.1093/mnras/283.4.1388", "primary_object": { "basename": "9607172", "url": "https://authors.library.caltech.edu/records/c9b91-dsk42/files/9607172" }, "related_objects": [ { "basename": "1388.full.pdf", "url": "https://authors.library.caltech.edu/records/c9b91-dsk42/files/1388.full.pdf" } ], "resource_type": "article", "pub_year": "1996", "author_list": "Madau, Piero; Ferguson, Henry C.; et el." }, { "id": "https://authors.library.caltech.edu/records/20zen-n9n07", "eprint_id": 95319, "eprint_status": "archive", "datestamp": "2023-08-19 18:43:29", "lastmod": "2023-10-20 19:07:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." } }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Hazard-C", "name": { "family": "Hazard", "given": "Cyril" } }, { "id": "McMahon-R-G", "name": { "family": "McMahon", "given": "Richard G." } } ] }, "title": "Spectrum of a QSO with redshift 3.8", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 Nature Publishing Group 1986. \n\nReceived 18 February; accepted 9 May 1986. \n\nWe thank J. Henning, C. Price, S. Staples and D. Tennant for assistance at Palomar Observatory. This research was supported by NSF grant AST84-16704 (W.L.W.S.) and by the Miller Institute for Basic Research in Science (A.V.F.).", "abstract": "Hazard et al. have described the circumstances leading to the identification of a quasi-stellar object (QSO) (1208 + 1011) with z = 3.82 \u00b1 0.04. Here we present a moderate-resolution optical spectrum of this object. Its precise redshift, z = 3.803 \u00b1 0.005, is the highest ever recorded.", "date": "1986-07-03", "date_type": "published", "publication": "Nature", "volume": "322", "number": "6074", "publisher": "Nature Publishing Group", "pagerange": "40-42", "id_number": "CaltechAUTHORS:20190507-145525566", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190507-145525566", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 84-16704" }, { "agency": "Miller Institute for Basic Research in Science" } ] }, "doi": "10.1038/322040a0", "resource_type": "article", "pub_year": "1986", "author_list": "Sargent, Wallace L. W.; Filippenko, Alexei V.; et el." } ]