[ { "id": "authors:t72fy-vsy96", "collection": "authors", "collection_id": "t72fy-vsy96", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200916-112912975", "type": "publication_whitepaper", "title": "Joint Survey Processing of LSST, Euclid and WFIRST: Enabling a broad array of astrophysics and cosmology through pixel level combinations of datasets", "author": [ { "family_name": "Chary", "given_name": "Ranga Ram", "orcid": "0000-0001-7583-0621", "clpid": "Chary-R-R" }, { "family_name": "Brammer", "given_name": "Gabriel", "orcid": "0000-0003-2680-005X", "clpid": "Brammer-G-B" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Dawson", "given_name": "William", "orcid": "0000-0003-0248-6123", "clpid": "Dawson-W" }, { "family_name": "Faisst", "given_name": "Andreas", "orcid": "0000-0002-9382-9832", "clpid": "Faisst-A-L" }, { "family_name": "Fajardo-Acosta", "given_name": "Sergio", "orcid": "0000-0001-9309-0102", "clpid": "Fajardo-Acosta-S-B" }, { "family_name": "Ferguson", "given_name": "Henry C.", "orcid": "0000-0001-7113-2738", "clpid": "Ferguson-H-C" }, { "family_name": "Grillmair", "given_name": "Carl J.", "orcid": "0000-0003-4072-169X", "clpid": "Grillmair-C-J" }, { "family_name": "Hemmati", "given_name": "Shoubaneh", "orcid": "0000-0003-2226-5395", "clpid": "Hemmati-Shoubaneh" }, { "family_name": "Koekemoer", "given_name": "Anton", "orcid": "0000-0002-6610-2048", "clpid": "Koekemoer-A-M" }, { "family_name": "Lee", "given_name": "Bomee", "orcid": "0000-0003-1954-5046", "clpid": "Lee-Bomee" }, { "family_name": "Lupton", "given_name": "Robert", "orcid": "0000-0003-1666-0962", "clpid": "Lupton-R-H" }, { "family_name": "Malhotra", "given_name": "Sangeeta", "orcid": "0000-0002-9226-5350", "clpid": "Malhotra-Sangeeta" }, { "family_name": "Melchior", "given_name": "Peter", "orcid": "0000-0002-8873-5065", "clpid": "Melchior-P" }, { "family_name": "Momcheva", "given_name": "Ivelina", "orcid": "0000-0003-1665-2073", "clpid": "Momcheva-I-G" }, { "family_name": "Newman", "given_name": "Jeffrey", "orcid": "0000-0001-8684-2222", "clpid": "Newman-J-A" }, { "family_name": "Masiero", "given_name": "Joseph", "orcid": "0000-0003-2638-720X", "clpid": "Masiero-J-R" }, { "family_name": "Paladini", "given_name": "Roberta", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Prakash", "given_name": "Abhishek", "orcid": "0000-0003-4451-4444", "clpid": "Prakash-Abhishek" }, { "family_name": "Rhodes", "given_name": "Jason", "orcid": "0000-0002-4485-8549", "clpid": "Rhodes-J-D" }, { "family_name": "Rusholme", "given_name": "Benjamin", "orcid": "0000-0001-7648-4142", "clpid": "Rusholme-B" }, { "family_name": "Schneider", "given_name": "Michael", "orcid": "0000-0002-8505-7094", "clpid": "Schneider-Michael" }, { "family_name": "Stickley", "given_name": "Nathaniel", "clpid": "Stickley-N-R" }, { "family_name": "Smith", "given_name": "Arfon", "orcid": "0000-0002-3957-2474", "clpid": "Smith-A-M" }, { "family_name": "Wood-Vasey", "given_name": "Michael", "orcid": "0000-0001-7113-1233", "clpid": "Wood-Vasey-W-M" }, { "family_name": "Berriman", "given_name": "G. Bruce", "orcid": "0000-0001-8388-534X", "clpid": "Berriman-G-B" } ], "abstract": "Joint survey processing (JSP) is the pixel level combination of LSST, Euclid, and WFIRST datasets. By combining the high spatial resolution of the space-based datasets with deep, seeing-limited, ground-based images in the optical bands, systematics like source confusion and astrometric mismatch can be addressed to derive the highest precision optical/infrared photometric catalogs. This white paper highlights the scientific motivation, computational and algorithmic needs to build joint pixel level processing capabilities, which the individual projects by themselves will not be able to support. Through this white paper, we request that the Astro2020 decadal committee recognize the JSP effort as a multi-agency project with the natural outcome being a collaborative effort among groups which are normally supported by a single agency. JSP will allow the U.S. (and international) astronomical community to manipulate the flagship data sets and undertake innovative science investigations ranging from solar system object characterization, exoplanet detections, nearby galaxy rotation rates and dark matter properties, to epoch of reionization studies. It will also result in the ultimate constraints on cosmological parameters and the nature of dark energy, with far smaller uncertainties and a better handle on systematics than by any one survey alone.", "doi": "10.48550/arXiv.1910.01259", "publisher": "arXiv", "publication_date": "2019-10-03" }, { "id": "authors:j9b6g-f5526", "collection": "authors", "collection_id": "j9b6g-f5526", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190813-084320751", "type": "publication_whitepaper", "title": "FOBOS: A Next-Generation Spectroscopic Facility at the W. M. Keck Observatory", "author": [ { "family_name": "Bundy", "given_name": "K.", "orcid": "0000-0001-9742-3138", "clpid": "Bundy-K-A" }, { "family_name": "Westfall", "given_name": "K." }, { "family_name": "MacDonald", "given_name": "N." }, { "family_name": "Kupke", "given_name": "R." }, { "family_name": "Savage", "given_name": "M." }, { "family_name": "Poppett", "given_name": "C." }, { "family_name": "Alabi", "given_name": "A." }, { "family_name": "Becker", "given_name": "G." }, { "family_name": "Burchett", "given_name": "J." }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Coil", "given_name": "A." }, { "family_name": "Cooper", "given_name": "M." }, { "family_name": "Cowley", "given_name": "D." }, { "family_name": "Deich", "given_name": "W." }, { "family_name": "Dillon", "given_name": "D." }, { "family_name": "Edelstein", "given_name": "J." }, { "family_name": "Guhathakurta", "given_name": "P." }, { "family_name": "Hennawi", "given_name": "J." }, { "family_name": "Kassis", "given_name": "M." }, { "family_name": "Lee", "given_name": "K.-G." }, { "family_name": "Masters", "given_name": "D." }, { "family_name": "Miller", "given_name": "T." }, { "family_name": "Newman", "given_name": "J." }, { "family_name": "O'Meara", "given_name": "J." }, { "family_name": "Prochaska", "given_name": "J. X." }, { "family_name": "Rau", "given_name": "M." }, { "family_name": "Rhodes", "given_name": "J." }, { "family_name": "Rich", "given_name": "R. M." }, { "family_name": "Rockosi", "given_name": "C." }, { "family_name": "Romanowsky", "given_name": "A." }, { "family_name": "Schafer", "given_name": "C." }, { "family_name": "Schlegel", "given_name": "D." }, { "family_name": "Shapley", "given_name": "A." }, { "family_name": "Siana", "given_name": "B." }, { "family_name": "Ting", "given_name": "Y. -S." }, { "family_name": "Weisz", "given_name": "D." }, { "family_name": "White", "given_name": "M." }, { "family_name": "Williams", "given_name": "B." }, { "family_name": "Wilson", "given_name": "G." }, { "family_name": "Wilson", "given_name": "M." }, { "family_name": "Yan", "given_name": "R." } ], "abstract": "High-multiplex and deep spectroscopic follow-up of upcoming panoramic deep-imaging surveys like LSST, Euclid, and WFIRST is a widely recognized and increasingly urgent necessity. No current or planned facility at a U.S. observatory meets the sensitivity, multiplex, and rapid-response time needed to exploit these future datasets. FOBOS, the Fiber-Optic Broadband Optical Spectrograph, is a near-term fiber-based facility that addresses these spectroscopic needs by optimizing depth over area and exploiting the aperture advantage of the existing 10m Keck II Telescope. The result is an instrument with a uniquely blue-sensitive wavelength range (0.31-1.0 um) at R~3500, high-multiplex (1800 fibers), and a factor 1.7 greater survey speed and order-of-magnitude greater sampling density than Subaru's Prime Focus Spectrograph (PFS). In the era of panoramic deep imaging, FOBOS will excel at building the deep, spectroscopic reference data sets needed to interpret vast imaging data. At the same time, its flexible focal plane, including a mode with 25 deployable integral-field units (IFUs) across a 20 arcmin diameter field, enables an expansive range of scientific investigations. Its key programmatic areas include (1) nested stellar-parameter training sets that enable studies of the Milky Way and M31 halo sub-structure, as well as local group dwarf galaxies, (2) a comprehensive picture of galaxy formation thanks to detailed mapping of the baryonic environment at z~2 and statistical linking of evolving populations to the present day, and (3) dramatic enhancements in cosmological constraints via precise photometric redshifts and determined redshift distributions. In combination with Keck I instrumentation, FOBOS also provides instant access to medium-resolution spectroscopy for transient sources with full coverage from the UV to the K-band.", "doi": "10.48550/arXiv.1907.07195", "publisher": "arXiv", "publication_date": "2019-07-16" }, { "id": "authors:sbcxm-knt45", "collection": "authors", "collection_id": "sbcxm-knt45", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190813-085750799", "type": "publication_whitepaper", "title": "WFIRST: The Essential Cosmology Space Observatory for the Coming Decade", "author": [ { "family_name": "Dor\u00e9", "given_name": "Olivier", "orcid": "0000-0001-7432-2932", "clpid": "Dor\u00e9-O" }, { "family_name": "Hirata", "given_name": "C.", "orcid": "0000-0002-2951-4932" }, { "family_name": "Wang", "given_name": "Y.", "clpid": "Wang-Yun" }, { "family_name": "Weinberg", "given_name": "D." }, { "family_name": "Eifler", "given_name": "T." }, { "family_name": "Foley", "given_name": "R. J." }, { "family_name": "Heinrich", "given_name": "C. He" }, { "family_name": "Krause", "given_name": "E." }, { "family_name": "Perlmutter", "given_name": "S." }, { "family_name": "Pisani", "given_name": "A." }, { "family_name": "Scolnic", "given_name": "D." }, { "family_name": "Spergel", "given_name": "D. N." }, { "family_name": "Suntzeff", "given_name": "N." }, { "family_name": "Aldering", "given_name": "G." }, { "family_name": "Baltay", "given_name": "C." }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Choi", "given_name": "A." }, { "family_name": "Deustua", "given_name": "S." }, { "family_name": "Dvorkin", "given_name": "C." }, { "family_name": "Fall", "given_name": "S. M." }, { "family_name": "Fang", "given_name": "X." }, { "family_name": "Fruchter", "given_name": "A." }, { "family_name": "Galbany", "given_name": "L." }, { "family_name": "Ho", "given_name": "S." }, { "family_name": "Hounsell", "given_name": "R." }, { "family_name": "Izard", "given_name": "A." }, { "family_name": "Jain", "given_name": "B." }, { "family_name": "Koekemoer", "given_name": "A. M." }, { "family_name": "Kruk", "given_name": "J." }, { "family_name": "Leauthaud", "given_name": "A." }, { "family_name": "Malhotra", "given_name": "S." }, { "family_name": "Mandelbaum", "given_name": "R." }, { "family_name": "Massara", "given_name": "E." }, { "family_name": "Masters", "given_name": "D." }, { "family_name": "Miyatake", "given_name": "H." }, { "family_name": "Plazas", "given_name": "A." }, { "family_name": "Rhoads", "given_name": "J." }, { "family_name": "Rhodes", "given_name": "J." }, { "family_name": "Rose", "given_name": "B." }, { "family_name": "Rubin", "given_name": "D." }, { "family_name": "Sako", "given_name": "M." }, { "family_name": "Samushia", "given_name": "L." }, { "family_name": "Shirasaki", "given_name": "M." }, { "family_name": "Simet", "given_name": "M." }, { "family_name": "Takada", "given_name": "M." }, { "family_name": "Troxel", "given_name": "M. A." }, { "family_name": "Wu", "given_name": "H." }, { "family_name": "Yoshida", "given_name": "N." }, { "family_name": "Zhai", "given_name": "Z.", "orcid": "0000-0001-7984-5476", "clpid": "Zhai-Zhongxu" } ], "abstract": "Two decades after its discovery, cosmic acceleration remains the most profound mystery in cosmology and arguably in all of physics. Either the Universe is dominated by a form of dark energy with exotic physical properties not predicted by standard model physics, or General Relativity is not an adequate description of gravity over cosmic distances. WFIRST emerged as a top priority of Astro2010 in part because of its ability to address the mystery of cosmic acceleration through both high precision measurements of the cosmic expansion history and the growth of cosmic structures with multiple and redundant probes. We illustrate in this white paper how mission design changes since Astro2010 have made WFIRST an even more powerful dark energy facility and have improved the ability of WFIRST to respond to changes in the experimental landscape. WFIRST is the space-based probe of DE the community needs in the mid-2020s.", "doi": "10.48550/arXiv.1904.01174", "publisher": "arXiv", "publication_date": "2019-04-02" }, { "id": "authors:bcv1w-4we73", "collection": "authors", "collection_id": "bcv1w-4we73", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191217-095259394", "type": "publication_whitepaper", "title": "Warm H\u2082 as a probe of massive accretion and feedback through shocks and turbulence across cosmic time", "author": [ { "family_name": "Appleton", "given_name": "Philip N.", "orcid": "0000-0002-7607-8766", "clpid": "Appleton-P-N" }, { "family_name": "Armus", "given_name": "Lee", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Boulanger", "given_name": "Fran\u00e7ois", "clpid": "Boulanger-F" }, { "family_name": "Bradford", "given_name": "Matt", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Braine", "given_name": "Jonathan", "clpid": "Braine-Jonathan" }, { "family_name": "Bromm", "given_name": "Volker", "clpid": "Bromm-V" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Cluver", "given_name": "Michelle", "orcid": "0000-0002-9871-6490", "clpid": "Cluver-M-E" }, { "family_name": "Cooray", "given_name": "Asantha", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "D\u00edaz-Santos", "given_name": "Tanio", "orcid": "0000-0003-0699-6083", "clpid": "D\u00edaz-Santos-T" }, { "family_name": "Egami", "given_name": "Eiichi", "clpid": "Egami-Eiichi" }, { "family_name": "Emonts", "given_name": "Bjorn", "clpid": "Emonts-B" }, { "family_name": "Guillard", "given_name": "Pierre", "orcid": "0000-0002-2421-1350", "clpid": "Guillard-P" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Lanz", "given_name": "Lauranne", "orcid": "0000-0002-3249-8224", "clpid": "Lanz-L" }, { "family_name": "Madden", "given_name": "Susanne", "clpid": "Madden-S" }, { "family_name": "Medling", "given_name": "Anne", "orcid": "0000-0001-7421-2944", "clpid": "Medling-A-M" }, { "family_name": "O'Sullivan", "given_name": "Ewan", "clpid": "O'Sullivan-E" }, { "family_name": "Ogle", "given_name": "Patrick", "orcid": "0000-0002-3471-981X", "clpid": "Ogle-P-M" }, { "family_name": "Pope", "given_name": "Alexandra", "orcid": "0000-0001-8592-2706", "clpid": "Pope-Alexandra" }, { "family_name": "Pineau des For\u00eats", "given_name": "Guillaume", "clpid": "Pineau-des-For\u00eats-G" }, { "family_name": "Shull", "given_name": "J. Michael", "clpid": "Shull-J-M" }, { "family_name": "Smith", "given_name": "John-David", "orcid": "0000-0003-1545-5078", "clpid": "Smith-J-D-T" }, { "family_name": "Togi", "given_name": "Aditya", "orcid": "0000-0001-5042-3421", "clpid": "Togi-A" }, { "family_name": "Xu", "given_name": "C. Kevin", "orcid": "0000-0002-1588-6700", "clpid": "Xu-C-Kevin" } ], "abstract": "Galaxy formation depends on a complex interplay between gravitational collapse, gas accretion, merging, and feedback processes. Yet, after many decades of investigation, these concepts are poorly understood. This paper presents the argument that warm H\u2082 can be used as a tool to unlock some of these mysteries. Turbulence, shocks and outflows, driven by star formation, AGN activity or inflows, may prevent the rapid buildup of star formation in galaxies. Central to our understanding of how gas is converted into stars is the process by which gas can dissipate its mechanical energy through turbulence and shocks in order to cool. H\u2082 lines provide direct quantitative measurements of kinetic energy dissipation in molecular gas in galaxies throughout the Universe. Based on the detection of very powerful H\u2082 lines from z = 2 galaxies and proto-clusters at the detection limits of Spitzer, we are confident that future far-IR and UV H\u2082 observations will provide a wealth of new information and insight into galaxy evolution to high-z. Finally, at the very earliest epoch of star and galaxy formation, warm H\u2082 may also provide a unique glimpse of molecular gas collapse at 7 < z < 12 in massive dark matter (DM) halos on their way to forming the very first galaxies. Such measurements are beyond the reach of existing and planned observatories.", "doi": "10.48550/arXiv.1903.06653", "publisher": "arXiv", "publication_date": "2019-03-15" }, { "id": "authors:hy9b9-m1q58", "collection": "authors", "collection_id": "hy9b9-m1q58", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190626-104726557", "type": "publication_whitepaper", "title": "Warm H_2 as a probe of massive accretion and feedback through shocks and turbulence across cosmic time", "author": [ { "family_name": "Appleton", "given_name": "Philip N.", "orcid": "0000-0002-7607-8766", "clpid": "Appleton-P-N" }, { "family_name": "Armus", "given_name": "Lee", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Boulanger", "given_name": "Francois", "clpid": "Boulanger-F" }, { "family_name": "Bradford", "given_name": "Charles M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Braine", "given_name": "Jonathan", "clpid": "Braine-J" }, { "family_name": "Bromm", "given_name": "Volker", "clpid": "Bromm-V" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Cluver", "given_name": "Michelle", "orcid": "0000-0002-9871-6490", "clpid": "Cluver-M-E" }, { "family_name": "Cooray", "given_name": "Asantha", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "D\u00edaz-Santos", "given_name": "Tanio", "orcid": "0000-0003-0699-6083", "clpid": "D\u00edaz-Santos-T" }, { "family_name": "Egami", "given_name": "Eiichi", "clpid": "Egami-Eiichi" }, { "family_name": "Emonts", "given_name": "Bjorn", "clpid": "Emonts-B" }, { "family_name": "Guillard", "given_name": "Pierre", "orcid": "0000-0002-2421-1350", "clpid": "Guillard-P" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Lanz", "given_name": "Lauranne", "orcid": "0000-0002-3249-8224", "clpid": "Lanz-L" }, { "family_name": "Madden", "given_name": "Susanne", "clpid": "Madden-S" }, { "family_name": "Medling", "given_name": "Anne", "orcid": "0000-0001-7421-2944", "clpid": "Medling-A-M" }, { "family_name": "O'Sullivan", "given_name": "Ewan", "clpid": "O'Sullivan-E" }, { "family_name": "Ogle", "given_name": "Patrick", "orcid": "0000-0002-3471-981X", "clpid": "Ogle-P-M" }, { "family_name": "Pope", "given_name": "Alexandra", "orcid": "0000-0001-8592-2706", "clpid": "Pope-Alexandra" }, { "family_name": "Pineau des For\u00eats", "given_name": "Guillaume", "clpid": "Pineau-des-For\u00eats-G" }, { "family_name": "Shull", "given_name": "J. Michael", "clpid": "Shull-J-M" }, { "family_name": "Smith", "given_name": "John-David", "orcid": "0000-0003-1545-5078", "clpid": "Smith-J-D-T" }, { "family_name": "Togi", "given_name": "Aditya", "orcid": "0000-0001-5042-3421", "clpid": "Togi-A" }, { "family_name": "Xu", "given_name": "C. Kevin", "orcid": "0000-0002-1588-6700", "clpid": "Xu-C-Kevin" } ], "abstract": "Galaxy formation depends on a complex interplay between gravitational collapse, gas accretion, merging, and feedback processes. Yet, after many decades of investigation, these concepts are poorly understood. This paper presents the argument that warm H_2 can be used as a tool to unlock some of these mysteries. Turbulence, shocks and outflows, driven by star formation, AGN activity or inflows, may prevent the rapid buildup of star formation in galaxies. Central to our understanding of how gas is converted into stars is the process by which gas can dissipate its mechanical energy through turbulence and shocks in order to cool. H_2 lines provide direct quantitative measurements of kinetic energy dissipation in molecular gas in galaxies throughout the Universe. Based on the detection of very powerful H_2 lines from z = 2 galaxies and proto-clusters at the detection limits of Spitzer, we are confident that future far-IR and UV H_2 observations will provide a wealth of new information and insight into galaxy evolution to high-z. Finally, at the very earliest epoch of star and galaxy formation, warm H_2 may also provide a unique glimpse of molecular gas collapse at 7 < z < 12 in massive dark matter (DM) halos on their way to forming the very first galaxies. Such measurements are beyond the reach of existing and planned observatories.", "doi": "10.48550/arXiv.1903.06653", "publisher": "arXiv", "publication_date": "2019-03-15" }, { "id": "authors:5f4rf-p8x96", "collection": "authors", "collection_id": "5f4rf-p8x96", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190626-140614418", "type": "publication_whitepaper", "title": "Observing Galaxy Evolution in the Context of Large-Scale Structure", "author": [ { "family_name": "Dickinson", "given_name": "Mark", "orcid": "0000-0001-5414-5131", "clpid": "Dickinson-Mark-E" }, { "family_name": "Wang", "given_name": "Yun", "clpid": "Wang-Yun" }, { "family_name": "Bartlett", "given_name": "James", "clpid": "Bartlett-James" }, { "family_name": "Behroozi", "given_name": "Peter", "clpid": "Behroozi-P-S" }, { "family_name": "Brinchmann", "given_name": "Jarle", "clpid": "Brinchmann-J" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Chary", "given_name": "Ranga", "orcid": "0000-0001-7583-0621", "clpid": "Chary-R-R" }, { "family_name": "Cimatti", "given_name": "Andrea", "clpid": "Cimatti-A" }, { "family_name": "Coil", "given_name": "Alison", "clpid": "Coil-A-L" }, { "family_name": "Conroy", "given_name": "Charlie", "orcid": "0000-0002-1590-8551", "clpid": "Conroy-C" }, { "family_name": "Daddi", "given_name": "Emanuele", "orcid": "0000-0002-3331-9590", "clpid": "Daddi-Emanuele" }, { "family_name": "Donahue", "given_name": "Megan", "orcid": "0000-0002-2808-0853", "clpid": "Donahue-Megan" }, { "family_name": "Eisenhardt", "given_name": "Peter", "clpid": "Eisenhardt-P-R-M" }, { "family_name": "Ferguson", "given_name": "Henry C.", "orcid": "0000-0001-7113-2738", "clpid": "Ferguson-H-C" }, { "family_name": "Furlanetto", "given_name": "Steve", "orcid": "0000-0002-0658-1243", "clpid": "Furlanetto-S-R" }, { "family_name": "Glazebrook", "given_name": "Karl", "clpid": "Glazebrook-K" }, { "family_name": "Gonzalez", "given_name": "Anthony", "orcid": "0000-0002-0933-8601", "clpid": "Gonzalez-A-H" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Hopkins", "given_name": "Philip F.", "orcid": "0000-0003-3729-1684", "clpid": "Hopkins-P-F" }, { "family_name": "Kartaltepe", "given_name": "Jeyhan", "orcid": "0000-0001-9187-3605", "clpid": "Kartaltepe-J" }, { "family_name": "Lee", "given_name": "Janice", "orcid": "0000-0002-2278-9407", "clpid": "Lee-Janice-C" }, { "family_name": "Malhotra", "given_name": "Sangeeta", "orcid": "0000-0002-9226-5350", "clpid": "Malhotra-S" }, { "family_name": "Marshall", "given_name": "Jennifer", "clpid": "Marshall-J-L" }, { "family_name": "Newman", "given_name": "Jeffrey A.", "orcid": "0000-0001-8684-2222", "clpid": "Newman-J-A" }, { "family_name": "Orsi", "given_name": "Alvaro", "clpid": "Orsi-Alvaro" }, { "family_name": "Rhoads", "given_name": "James", "orcid": "0000-0002-1501-454X", "clpid": "Rhoads-J-E" }, { "family_name": "Rhodes", "given_name": "Jason", "orcid": "0000-0002-4485-8549", "clpid": "Rhodes-J-D" }, { "family_name": "Shapley", "given_name": "Alice", "orcid": "0000-0003-3509-4855", "clpid": "Shapley-A-E" }, { "family_name": "Wechsler", "given_name": "Risa H.", "orcid": "0000-0003-2229-011X", "clpid": "Wechsler-R-H" } ], "abstract": "Galaxies form and evolve in the context of their local and large-scale environments. Their baryonic content that we observe with imaging and spectroscopy is intimately connected to the properties of their dark matter halos, and to their location in the \"cosmic web\" of large-scale structure. Very large spectroscopic surveys of the local universe (e.g., SDSS and GAMA) measure galaxy positions (location within large-scale structure), statistical clustering (a direct constraint on dark matter halo masses), and spectral features (measuring physical conditions of the gas and stars within the galaxies, as well as internal velocities). Deep surveys with the James Webb Space Telescope (JWST) will revolutionize spectroscopic measurements of redshifts and spectral properties for galaxies out to the epoch of reionization, but with numerical statistics and over cosmic volumes that are too small to map large-scale structure and to constrain halo properties via clustering. Here, we consider advances in understanding galaxy evolution that would be enabled by very large spectroscopic surveys at high redshifts: very large numbers of galaxies (outstanding statistics) over large co-moving volumes (large-scale structure on all scales) over broad redshift ranges (evolution over most of cosmic history). The required observational facility can be established as part of the probe portfolio by NASA within the next decade.", "doi": "10.48550/arXiv.1903.07409", "publisher": "arXiv", "publication_date": "2019-03-14" }, { "id": "authors:fr3ve-naf15", "collection": "authors", "collection_id": "fr3ve-naf15", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190812-144155775", "type": "publication_whitepaper", "title": "The Nature of Low-Density Star Formation", "author": [ { "family_name": "Thilker", "given_name": "David", "orcid": "0000-0002-8528-7340", "clpid": "Thilker-D-A" }, { "family_name": "Lee", "given_name": "Janice", "orcid": "0000-0002-2278-9407", "clpid": "Lee-Janice-C" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Cook", "given_name": "David", "orcid": "0000-0002-6877-7655", "clpid": "Cook-D-O" }, { "family_name": "Dale", "given_name": "Daniel", "orcid": "0000-0002-5782-9093", "clpid": "Dale-D-A" }, { "family_name": "Elmegreen", "given_name": "Bruce", "orcid": "0000-0002-1723-6330", "clpid": "Elmegreen-B-G" }, { "family_name": "Gil de Paz", "given_name": "Armando", "orcid": "0000-0001-6150-2854", "clpid": "Gil-de-Paz-A" }, { "family_name": "Gallagher", "given_name": "John", "clpid": "Gallagher-J-S" }, { "family_name": "Hunter", "given_name": "Deidre", "orcid": "0000-0002-3322-9798", "clpid": "Hunter-D-A" }, { "family_name": "Leroy", "given_name": "Adam", "orcid": "0000-0002-2545-1700", "clpid": "Leroy-A-K" }, { "family_name": "Meurer", "given_name": "Gerhardt", "orcid": "0000-0002-0163-2507", "clpid": "Meurer-G-R" }, { "family_name": "Pisano", "given_name": "D. J.", "clpid": "Pisano-D-J" }, { "family_name": "Rafelski", "given_name": "Marc", "orcid": "0000-0002-9946-4731", "clpid": "Rafelski-M" }, { "family_name": "Tosi", "given_name": "Monica", "clpid": "Tosi-Monica" }, { "family_name": "Wofford", "given_name": "Aida", "clpid": "Wofford-A" } ], "abstract": "How do stars manage to form within low-density, HI-dominated gas? Such environments provide a laboratory for studying star formation with physical conditions distinct from starbursts and the metal-rich disks of spiral galaxies where most effort has been invested. Here we outline fundamental open questions about the nature of star formation at low-density. We describe the wide-field, high-resolution UV-optical-IR-radio observations of stars, star clusters and gas clouds in nearby galaxies needed in the 2020's to provide definitive answers, essential for development of a complete theory of star formation.", "doi": "10.48550/arXiv.1903.05745", "publisher": "arXiv", "publication_date": "2019-03-13" }, { "id": "authors:x9ggm-2bt79", "collection": "authors", "collection_id": "x9ggm-2bt79", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190813-100440817", "type": "publication_whitepaper", "title": "Taking Census of Massive, Star-Forming Galaxies formed <1 Gyr After the Big Bang", "author": [ { "family_name": "Casey", "given_name": "Caitlin M.", "orcid": "0000-0002-0930-6466", "clpid": "Casey-C-M" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Staguhn", "given_name": "Johannes", "orcid": "0000-0002-8437-0433", "clpid": "Staguhn-J-G" }, { "family_name": "Armus", "given_name": "Lee", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Blain", "given_name": "Andrew", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "B\u00e9thermin", "given_name": "Matthieu", "orcid": "0000-0002-3915-2015", "clpid": "B\u00e9thermin-Matthieu" }, { "family_name": "Champagne", "given_name": "Jaclyn", "orcid": "0000-0002-6184-9097", "clpid": "Champagne-J" }, { "family_name": "Cooray", "given_name": "Asantha", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "Coppin", "given_name": "Kristen", "clpid": "Coppin-K-E-K" }, { "family_name": "Drew", "given_name": "Patrick", "orcid": "0000-0003-3627-7485", "clpid": "Drew-P" }, { "family_name": "Dwek", "given_name": "Eli", "orcid": "0000-0001-8033-1181", "clpid": "Dwek-E" }, { "family_name": "Finkelstein", "given_name": "Steven", "orcid": "0000-0001-8519-1130", "clpid": "Finkelstein-S-L" }, { "family_name": "Franco", "given_name": "Maximilien", "orcid": "0000-0002-3560-8599", "clpid": "Franco-M" }, { "family_name": "Geach", "given_name": "James", "orcid": "0000-0003-4964-4635", "clpid": "Geach-J-E" }, { "family_name": "Hodge", "given_name": "Jacqueline", "orcid": "0000-0001-6586-8845", "clpid": "Hodge-J-A" }, { "family_name": "Koprowski", "given_name": "Maciej", "orcid": "0000-0001-5785-1154", "clpid": "Koprowski-M" }, { "family_name": "Lagos", "given_name": "Claudia", "orcid": "0000-0003-3021-8564", "clpid": "Lagos-C-D-P" }, { "family_name": "Narayanan", "given_name": "Desika", "orcid": "0000-0002-7064-4309", "clpid": "Narayanan-D" }, { "family_name": "Pope", "given_name": "Alexandra", "orcid": "0000-0001-8592-2706", "clpid": "Pope-Alexandra" }, { "family_name": "Sanders", "given_name": "David", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-D-B" }, { "family_name": "Shivaei", "given_name": "Irene", "clpid": "Shivaei-Irene" }, { "family_name": "Toft", "given_name": "Sune", "orcid": "0000-0003-3631-7176", "clpid": "Toft-S" }, { "family_name": "Vieira", "given_name": "Joaquin", "clpid": "Vieira-J-D" }, { "family_name": "Walter", "given_name": "Fabian", "orcid": "0000-0003-4793-7880", "clpid": "Walter-F" }, { "family_name": "Whitaker", "given_name": "Kate", "clpid": "Whitaker-K" }, { "family_name": "Yun", "given_name": "Min", "orcid": "0000-0001-7095-7543", "clpid": "Yun-Min-S" }, { "family_name": "Zavala", "given_name": "Jorge", "orcid": "0000-0002-7051-1100", "clpid": "Zavala-J" } ], "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.", "doi": "10.48550/arXiv.1903.05634", "publisher": "arXiv", "publication_date": "2019-03-13" }, { "id": "authors:wwqa0-56508", "collection": "authors", "collection_id": "wwqa0-56508", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190813-083044401", "type": "publication_whitepaper", "title": "Simultaneous Measurements of Star Formation and Supermassive Black Hole Growth in Galaxies", "author": [ { "family_name": "Pope", "given_name": "Alexandra", "orcid": "0000-0001-8592-2706", "clpid": "Pope-Alexandra" }, { "family_name": "Armus", "given_name": "Lee", "orcid": "0000-0003-3498-2973", "clpid": "Armus-Lee" }, { "family_name": "Murphy", "given_name": "Eric" }, { "family_name": "Aalto", "given_name": "Susanne", "orcid": "0000-0002-5828-7660", "clpid": "Aalto-Susanne" }, { "family_name": "Alexander", "given_name": "David" }, { "family_name": "Appleton", "given_name": "Philip", "orcid": "0000-0002-7607-8766", "clpid": "Appleton-P-N" }, { "family_name": "Barger", "given_name": "Amy" }, { "family_name": "Bradford", "given_name": "Matt" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Casey", "given_name": "Caitlin" }, { "family_name": "Charmandaris", "given_name": "Vassilis" }, { "family_name": "Chary", "given_name": "Ranga", "orcid": "0000-0001-7583-0621", "clpid": "Chary-Ranga-Ram" }, { "family_name": "Cooray", "given_name": "Asantha" }, { "family_name": "Condon", "given_name": "Jim" }, { "family_name": "Diaz Santos", "given_name": "Tanio", "orcid": "0000-0003-0699-6083" }, { "family_name": "Dickinson", "given_name": "Mark" }, { "family_name": "Farrah", "given_name": "Duncan" }, { "family_name": "Ferkinhoff", "given_name": "Carl" }, { "family_name": "Grogin", "given_name": "Norman" }, { "family_name": "Hickox", "given_name": "Ryan" }, { "family_name": "Kirkpatrick", "given_name": "Allison" }, { "family_name": "Kotaro", "given_name": "Kohno" }, { "family_name": "Matthews", "given_name": "Allison" }, { "family_name": "Narayanan", "given_name": "Desika" }, { "family_name": "Riechers", "given_name": "Dominik" }, { "family_name": "Sajina", "given_name": "Anna" }, { "family_name": "Sargent", "given_name": "Mark" }, { "family_name": "Scott", "given_name": "Douglas" }, { "family_name": "Smith", "given_name": "J. D." }, { "family_name": "Stacey", "given_name": "Gordon" }, { "family_name": "Veilleux", "given_name": "Sylvain" }, { "family_name": "Vieira", "given_name": "Joaquin" } ], "abstract": "Galaxies grow their supermassive black holes in concert with their stars, although the relationship between these major galactic components is poorly understood. Observations of the cosmic growth of stars and black holes in galaxies suffer from disjoint samples and the strong effects of dust attenuation. The thermal infrared holds incredible potential for simultaneously measuring both the star formation and black hole accretion rates in large samples of galaxies covering a wide range of physical conditions. Spitzer demonstrated this potential at low redshift, and by observing some of the most luminous galaxies at z~2. JWST will apply these methods to normal galaxies at these epochs, but will not be able to generate large spectroscopic samples or access the thermal infrared at high-redshift. An order of magnitude gap in our wavelength coverage will persist between JWST and ALMA. A large, cold infrared telescope can fill this gap to determine when (in cosmic time), and where (within the cosmic web), stars and black holes co-evolve, by measuring these processes simultaneously in statistically complete and unbiased samples of galaxies to z>8. A next-generation radio interferometer will have the resolution and sensitivity to measure star-formation and nuclear accretion in even the dustiest galaxies. Together, the thermal infrared and radio can uniquely determine how stars and supermassive blackholes co-evolve in galaxies over cosmic time.", "doi": "10.48550/arXiv.1903.05110", "publisher": "arXiv", "publication_date": "2019-03-12" }, { "id": "authors:70ksa-c7e09", "collection": "authors", "collection_id": "70ksa-c7e09", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190814-080308839", "type": "publication_whitepaper", "title": "LSST Observing Strategy White Paper: LSST Observations of WFIRST Deep Fields", "author": [ { "family_name": "Foley", "given_name": "R. J.", "clpid": "Foley-R-J" }, { "family_name": "Koekemoer", "given_name": "A. M.", "orcid": "0000-0002-6610-2048", "clpid": "Koekemoer-A-M" }, { "family_name": "Spergel", "given_name": "D. N.", "orcid": "0000-0002-5151-0006", "clpid": "Spergel-D-N" }, { "family_name": "Bianco", "given_name": "F. B.", "orcid": "0000-0003-1953-8727", "clpid": "Bianco-F-B" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Dai", "given_name": "L.", "clpid": "Dai-L" }, { "family_name": "Dor\u00e9", "given_name": "O.", "orcid": "0000-0001-7432-2932", "clpid": "Dor\u00e9-O" }, { "family_name": "Fazio", "given_name": "G. G.", "orcid": "0000-0002-0670-0708", "clpid": "Fazio-G-G" }, { "family_name": "Ferguson", "given_name": "H.", "orcid": "0000-0001-7113-2738", "clpid": "Ferguson-H-C" }, { "family_name": "Filippenko", "given_name": "A. V.", "orcid": "0000-0003-3460-0103", "clpid": "Filippenko-A-V" }, { "family_name": "Frye", "given_name": "B.", "clpid": "Frye-Brenda-L" }, { "family_name": "Galbany", "given_name": "L.", "orcid": "0000-0002-1296-6887", "clpid": "Galbany-L" }, { "family_name": "Gawiser", "given_name": "E.", "clpid": "Gawiser-E" }, { "family_name": "Gronwall", "given_name": "C.", "clpid": "Gronwall-C" }, { "family_name": "Hathi", "given_name": "N. P.", "orcid": "0000-0001-6145-5090", "clpid": "Hathi-N-P" }, { "family_name": "Hirata", "given_name": "C.", "orcid": "0000-0002-2951-4932", "clpid": "Hirata-C-M" }, { "family_name": "Hounsell", "given_name": "R.", "clpid": "Hounsell-R-A" }, { "family_name": "Jha", "given_name": "S. W.", "orcid": "0000-0001-8738-6011", "clpid": "Jha-S-W" }, { "family_name": "Kim", "given_name": "A. G.", "clpid": "Kim-Alex-G" }, { "family_name": "Kelly", "given_name": "P. L.", "orcid": "0000-0003-3142-997X", "clpid": "Kelly-P-L" }, { "family_name": "Kruk", "given_name": "J. W.", "orcid": "0000-0002-5861-7236", "clpid": "Kruk-J-W" }, { "family_name": "Malhotra", "given_name": "S.", "orcid": "0000-0002-9226-5350", "clpid": "Malhotra-S" }, { "family_name": "Mandel", "given_name": "K. S.", "orcid": "0000-0001-9846-4417", "clpid": "Mandel-K-S" }, { "family_name": "Margutti", "given_name": "R.", "orcid": "0000-0003-4768-7586", "clpid": "Margutti-R" }, { "family_name": "Marrone", "given_name": "D.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "McQuinn", "given_name": "K. B. W.", "clpid": "McQuinn-K-B-W" }, { "family_name": "Melchior", "given_name": "P.", "orcid": "0000-0002-8873-5065", "clpid": "Melchior-P" }, { "family_name": "Moustakas", "given_name": "L.", "orcid": "0000-0003-3030-2360", "clpid": "Moustakas-L-A" }, { "family_name": "Newman", "given_name": "J. A.", "orcid": "0000-0001-8684-2222", "clpid": "Newman-J-A" }, { "family_name": "Peek", "given_name": "J. E. G.", "orcid": "0000-0003-4797-7030", "clpid": "Peek-J-E-G" }, { "family_name": "Perlmutter", "given_name": "S.", "clpid": "Perlmutter-S" }, { "family_name": "Rhodes", "given_name": "J. D.", "orcid": "0000-0002-4485-8549", "clpid": "Rhodes-J-D" }, { "family_name": "Robertson", "given_name": "B.", "orcid": "0000-0002-4271-0364", "clpid": "Robertson-B-E" }, { "family_name": "Rubin", "given_name": "D.", "clpid": "Rubin-D-M" }, { "family_name": "Scolnic", "given_name": "D.", "orcid": "0000-0002-4934-5849", "clpid": "Scolnic-D" }, { "family_name": "Somerville", "given_name": "R.", "clpid": "Somerville-R-S" }, { "family_name": "Street", "given_name": "R.", "orcid": "0000-0001-6279-0552", "clpid": "Street-R-A" }, { "family_name": "Wang", "given_name": "Y.", "clpid": "Wang-Yun" }, { "family_name": "Whalen", "given_name": "D. J.", "clpid": "Whalen-D-J" }, { "family_name": "Windhorst", "given_name": "R. A.", "clpid": "Windhorst-R-A" }, { "family_name": "Wollack", "given_name": "E. J.", "orcid": "0000-0002-7567-4451", "clpid": "Wollack-E-J" }, { "literal": "WFIRST Deep Field Working Group" }, { "literal": "WFIRST Science Investigation Team Members" } ], "abstract": "The Wide-Field Infrared Survey Telescope (WFIRST) is expected to launch in the mid-2020s. With its wide-field near-infrared (NIR) camera, it will survey the sky to unprecedented detail. As part of normal operations and as the result of multiple expected dedicated surveys, WFIRST will produce several relatively wide-field (tens of square degrees) deep (limiting magnitude of 28 or fainter) fields. In particular, a planned supernova survey is expected to image 3 deep fields in the LSST footprint roughly every 5 days over 2 years. Stacking all data, this survey will produce, over all WFIRST supernova fields in the LSST footprint, ~12-25 deg^2 and ~5-15 deg^2 regions to depths of ~28 mag and ~29 mag, respectively. We suggest LSST undertake mini-surveys that will match the WFIRST cadence and simultaneously observe the supernova survey fields during the 2-year WFIRST supernova survey, achieving a stacked depth similar to that of the WFIRST data. We also suggest additional observations of these same regions throughout the LSST survey to get deep images earlier, have long-term monitoring in the fields, and produce deeper images overall. These fields will provide a legacy for cosmology, extragalactic, and transient/variable science.", "doi": "10.48550/arXiv.1812.00514", "publisher": "arXiv", "publication_date": "2018-11-30" } ]