[ { "id": "https://authors.library.caltech.edu/records/x9ggm-2bt79", "eprint_id": 97861, "eprint_status": "archive", "datestamp": "2023-08-19 14:52:29", "lastmod": "2024-01-14 21:52:24", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Casey-C-M", "name": { "family": "Casey", "given": "Caitlin M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Staguhn-J-G", "name": { "family": "Staguhn", "given": "Johannes" }, "orcid": "0000-0002-8437-0433" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew" }, "orcid": "0000-0001-7489-5167" }, { "id": "B\u00e9thermin-Matthieu", "name": { "family": "B\u00e9thermin", "given": "Matthieu" }, "orcid": "0000-0002-3915-2015" }, { "id": "Champagne-J", "name": { "family": "Champagne", "given": "Jaclyn" }, "orcid": "0000-0002-6184-9097" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Coppin-K-E-K", "name": { "family": "Coppin", "given": "Kristen" } }, { "id": "Drew-P", "name": { "family": "Drew", "given": "Patrick" }, "orcid": "0000-0003-3627-7485" }, { "id": "Dwek-E", "name": { "family": "Dwek", "given": "Eli" }, "orcid": "0000-0001-8033-1181" }, { "id": "Finkelstein-S-L", "name": { "family": "Finkelstein", "given": "Steven" }, "orcid": "0000-0001-8519-1130" }, { "id": "Franco-M", "name": { "family": "Franco", "given": "Maximilien" }, "orcid": "0000-0002-3560-8599" }, { "id": "Geach-J-E", "name": { "family": "Geach", "given": "James" }, "orcid": "0000-0003-4964-4635" }, { "id": "Hodge-J-A", "name": { "family": "Hodge", "given": "Jacqueline" }, "orcid": "0000-0001-6586-8845" }, { "id": "Koprowski-M", "name": { "family": "Koprowski", "given": "Maciej" }, "orcid": "0000-0001-5785-1154" }, { "id": "Lagos-C-D-P", "name": { "family": "Lagos", "given": "Claudia" }, "orcid": "0000-0003-3021-8564" }, { "id": "Narayanan-D", "name": { "family": "Narayanan", "given": "Desika" }, "orcid": "0000-0002-7064-4309" }, { "id": "Pope-Alexandra", "name": { "family": "Pope", "given": "Alexandra" }, "orcid": "0000-0001-8592-2706" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "David" }, "orcid": "0000-0002-1233-9998" }, { "id": "Shivaei-Irene", "name": { "family": "Shivaei", "given": "Irene" } }, { "id": "Toft-S", "name": { "family": "Toft", "given": "Sune" }, "orcid": "0000-0003-3631-7176" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "Joaquin" } }, { "id": "Walter-F", "name": { "family": "Walter", "given": "Fabian" }, "orcid": "0000-0003-4793-7880" }, { "id": "Whitaker-K", "name": { "family": "Whitaker", "given": "Kate" } }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "Min" }, "orcid": "0000-0001-7095-7543" }, { "id": "Zavala-J", "name": { "family": "Zavala", "given": "Jorge" }, "orcid": "0000-0002-7051-1100" } ] }, "title": "Taking Census of Massive, Star-Forming Galaxies formed <1 Gyr After the Big Bang", "ispublished": "unpub", "full_text_status": "public", "note": "
Submitted - 1903.05634.pdf
", "abstract": "Two decades of effort have been poured into both single-dish and interferometric millimeter-wave surveys of the sky to infer the volume density of dusty star-forming galaxies (DSFGs, with SFR>100M\u2299 yr^(\u22121)) over cosmic time. Though obscured galaxies dominate cosmic star-formation near its peak at z\u223c2, the contribution of such heavily obscured galaxies to cosmic star-formation is unknown beyond z\u223c2.5 in contrast to the well-studied population of Lyman-break galaxies (LBGs) studied through deep, space- and ground-based pencil beam surveys in the near-infrared. Unlocking the volume density of DSFGs beyond z>3, particularly within the first 1 Gyr after the Big Bang is critical to resolving key open questions about early Universe galaxy formation: (1) What is the integrated star-formation rate density of the Universe in the first few Gyr and how is it distributed among low-mass galaxies (e.g. Lyman-break galaxies) and high-mass galaxies (e.g. DSFGs and quasar host galaxies)? (2) How and where do the first massive galaxies assemble? (3) What can the most extreme DSFGs teach us about the mechanisms of dust production (e.g. supernovae, AGB stars, grain growth in the ISM) <1 Gyr after the Big Bang? We summarize the types of observations needed in the next decade to address these questions.", "date": "2019-08-13", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20190813-100440817", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190813-100440817", "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": "10.48550/arXiv.1903.05634", "primary_object": { "basename": "1903.05634.pdf", "url": "https://authors.library.caltech.edu/records/x9ggm-2bt79/files/1903.05634.pdf" }, "resource_type": "monograph", "pub_year": "2019", "author_list": "Casey, Caitlin M.; Capak, Peter; et el." }, { "id": "https://authors.library.caltech.edu/records/2q184-ja103", "eprint_id": 60280, "eprint_status": "archive", "datestamp": "2023-08-20 01:09:16", "lastmod": "2023-10-24 16:23:08", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "Frank" }, "orcid": "0000-0002-1707-1775" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James" }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-M-C", "name": { "family": "Bradford", "given": "Matt" } }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. Darren" } }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "Jason" }, "orcid": "0000-0001-7527-2017" }, { "id": "Goldsmith-P-F", "name": { "family": "Goldsmith", "given": "Paul" }, "orcid": "0000-0002-6622-8396" }, { "id": "Harwit-M", "name": { "family": "Harwit", "given": "Martin" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D." }, "orcid": "0000-0003-1545-5078" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Stacey-G-J", "name": { "family": "Stacey", "given": "Gordon" } }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "Joaquin" } }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "Min" }, "orcid": "0000-0001-7095-7543" }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" } } ] }, "title": "A complete view of galaxy evolution: panchromatic luminosity functions and the generation of metals", "ispublished": "unpub", "full_text_status": "public", "note": "Submitted on 6 Mar 2009.\n\nSubmitted - 0903.1272v1.pdf
", "abstract": "When and how did galaxies form and their metals accumulate? Over the last decade, this has moved from an archeological question to a live investigation: there is now a broad picture of the evolution of galaxies in dark matter halos: their masses, stars, metals and supermassive blackholes. Galaxies have been found and studied in which these formation processes are taking place most vigorously, all the way back in cosmic time to when the intergalactic medium (IGM) was still largely neutral. However, the details of how and why the interstellar medium (ISM) in\ndistant galaxies cools, is processed, recycled and enriched in metals by stars, and fuels active\ngalactic nuclei (AGNs) remain uncertain. In particular, the cooling of gas to fuel star formation,\nand the chemistry and physics of the most intensely active regions is hidden from view at optical\nwavelengths, but can be seen and diagnosed at mid- & far-infrared (IR) wavelengths. Rest-frame\nIR observations are important first to identify the most luminous, interesting and important\ngalaxies, secondly to quantify accurately their total luminosity, and finally to use spectroscopy to\ntrace the conditions in the molecular and atomic gas out of which stars form. In order to map out\nthese processes over the full range of environments and large-scale structures found in the\nuniverse - from the densest clusters of galaxies to the emptiest voids \u2013 we require tools for deep,\nlarge area surveys, of millions of galaxies out to z~5, and for detailed follow-up spectroscopy.\nThe necessary tools can be realized technically. Here, we outline the requirements for gathering\nthe crucial information to build, validate and challenge models of galaxy evolution.", "date": "2015-09-16", "date_type": "published", "id_number": "CaltechAUTHORS:20150916-130227932", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150916-130227932", "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": "10.48550/arXiv.0903.1272", "primary_object": { "basename": "0903.1272v1.pdf", "url": "https://authors.library.caltech.edu/records/2q184-ja103/files/0903.1272v1.pdf" }, "resource_type": "monograph", "pub_year": "2015", "author_list": "Blain, Andrew W.; Armus, Lee; et el." } ]