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35 results on '"NSF's National Optical-Infrared Astronomy Research Laboratory"'

1. A dusty veil shading Betelgeuse during its Great Dimming

Author: Stefan Kraus, Eric Lagadec, E. Cannon, Florentin Millour, Guy Perrin, A. de Koter, John D. Monnier, Andrea Chiavassa, Xavier Haubois, Claudia Paladini, Narsireddy Anugu, Peter Scicluna, Andrea K. Dupree, L. Decin, Philippe Stee, Bruno Lopez, Gioia Rau, M. Montargès, William C. Danchi, K. Kravchenko, S. T. Ridgway, Ryan P. Norris, J. Sanchez-Bermudez, Pierre Kervella, Faustine Cantalloube, J-B. Le Bouquin, Markus Wittkowski, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Laboratoire Lagrange, Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS., Anton Pannenkoek Institute for Astronomy [University of Amsterdam], University of Amsterdam [Amsterdam] (UvA), Max Planck Institute for Astronomy (MPIA), Instituto de Astronomía, Univ. Nacional Autónoma de México, Universidad Nacional Autónoma de México (UNAM), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), School of Chemistry [Leeds], University of Leeds, Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], NSF’s National Optical-Infrared Astronomy Research Laboratory (NOIRLab), Steward Observatory, University of Arizona, School of Physics and Astronomy [Exeter], University of Exeter, Physics Department [New Mexico Institute of Mining and Technology], New Mexico Institute of Mining and Technology [New Mexico Tech] (NMT), GSFC Exoplanets and Stellar Astrophysics Laboratory, NASA Goddard Space Flight Center (GSFC), Department of Physics [Catholic University of America], Catholic University of America, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy University of Michigan, University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Low Energy Astrophysics (API, FNWI)
Subjects: Brightness, SURFACE, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, STELLAR CONVECTION, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Apparent magnitude, INTERSTELLAR SILICATE MINERALOGY, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, IIP SUPERNOVA, Red supergiant, 010306 general physics, 010303 astronomy & astrophysics, Stellar evolution, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Betelgeuse, Physics, Photosphere, Multidisciplinary, Science & Technology, Multidisciplinary Sciences, Supernova, Neutron star, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, [SDU]Sciences of the Universe [physics], NEAR-IR, Science & Technology - Other Topics, RED SUPERGIANTS, STEPS, Astrophysics::Earth and Planetary Astrophysics
Abstract: Red supergiants are the most common final evolutionary stage of stars that have initial masses between 8 and 35 times that of the Sun1. During this stage, which lasts roughly 100,000 years1, red supergiants experience substantial mass loss. However, the mechanism for this mass loss is unknown2. Mass loss may affect the evolutionary path, collapse and future supernova light curve3 of a red supergiant, and its ultimate fate as either a neutron star or a black hole4. From November 2019 to March 2020, Betelgeuse—the second-closest red supergiant to Earth (roughly 220 parsecs, or 724 light years, away)5,6—experienced a historic dimming of its visible brightness. Usually having an apparent magnitude between 0.1 and 1.0, its visual brightness decreased to 1.614 ± 0.008 magnitudes around 7–13 February 20207—an event referred to as Betelgeuse’s Great Dimming. Here we report high-angular-resolution observations showing that the southern hemisphere of Betelgeuse was ten times darker than usual in the visible spectrum during its Great Dimming. Observations and modelling support a scenario in which a dust clump formed recently in the vicinity of the star, owing to a local temperature decrease in a cool patch that appeared on the photosphere. The directly imaged brightness variations of Betelgeuse evolved on a timescale of weeks. Our findings suggest that a component of mass loss from red supergiants8 is inhomogeneous, linked to a very contrasted and rapidly changing photosphere. The southern hemisphere of Betelgeuse during its Great Dimming was an order of magnitude darker than usual, owing to a cool patch on the photosphere and associated dust formation.
Published: 2021
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2. Dark energy survey year 3 results: Galaxy sample for BAO measurement

Author: Josh Frieman, R. L. C. Ogando, J. Calcino, David J. James, Pablo Fosalba, F. J. Castander, Ramon Miquel, O. Alves, Elisabeth Krause, J. Mena-Fernández, Will J. Percival, N. Weaverdyck, Karl Glazebrook, D Burke, A Roodman, C. Lidman, B. E. Tucker, A. Brandao-Souza, Erin Sheldon, A. Choi, T. M. C. Abbott, M. Carrasco Kind, F. Andrade-Oliveira, Jennifer L. Marshall, K. Honscheid, J. Carretero, Michael Schubnell, Jack Elvin-Poole, Tamara M. Davis, Anais Möller, E. Bertin, Chun-Hao To, Agnès Ferté, E. J. Sanchez, Ashley J. Ross, Martin Crocce, I. Sevilla-Noarbe, M. Soares-Santos, R. Cawthon, Daniel Thomas, A. G. Kim, E. Suchyta, J. Gschwend, August E. Evrard, Tommaso Giannantonio, A. A. Plazas Malagón, Geraint F. Lewis, G. Tarle, W. Riquelme, Rob Sharp, Santiago Avila, E. Buckley-Geer, S. A. Uddin, Ofer Lahav, Alex Drlica-Wagner, Dragan Huterer, A. Porredon, W. G. Hartley, M. Costanzi, Felipe Menanteau, A. Carnero Rosell, K. D. Eckert, T. N. Varga, Peter Doel, Douglas L. Tucker, V. Scarpine, Daniela Carollo, Robert Morgan, Juan Garcia-Bellido, S. Desai, Kyler Kuehn, D. L. Hollowood, J. Annis, H. T. Diehl, Christopher J. Conselice, S. Serrano, I. Ferrero, L. N. da Costa, Ben Hoyle, K. C. Chan, Rogerio Rosenfeld, Enrique Gaztanaga, B. Flaugher, David J. Brooks, Antonella Palmese, Marcos Lima, M. A. G. Maia, M. Rodriguez-Monroy, U. Malik, Adriano Pieres, F. Paz-Chinchón, Joseph J. Mohr, J. De Vicente, M.E. da Silva Pereira, M. Smith, S. Everett, Daniel Gruen, H. Camacho, J. Muir, Samuel Hinton, D. W. Gerdes, G. Gutierrez, M. E. C. Swanson, Jacobo Asorey, Michel Aguena, D. Sanchez Cid, S. Allam, Robert A. Gruendl, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), DES, UAM. Departamento de Física Teórica, Rosell, A. C., Rodriguez-Monroy, M., Crocce, M., Elvin-Poole, J., Porredon, A., Ferrero, I., Mena-Fernandez, J., Cawthon, R., De Vicente, J., Gaztanaga, E., Ross, A. J., Sanchez, E., Sevilla-Noarbe, I., Alves, O., Andrade-Oliveira, F., Asorey, J., Avila, S., Brandao-Souza, A., Camacho, H., Chan, K. C., Ferte, A., Muir, J., Riquelme, W., Rosenfeld, R., Cid, D. S., Hartley, W. G., Weaverdyck, N., Abbott, T., Aguena, M., Allam, S., Annis, J., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D., Calcino, J., Carollo, D., Kind, M. C., Carretero, J., Castander, F., Choi, A., Conselice, C., Costanzi, M., Da Costa, L., Da Silva Pereira, M. E., Davis, T., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eckert, K., Everett, S., Evrard, A., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gerdes, D., Giannantonio, T., Glazebrook, K., Gruen, D., Gruendl, R., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., Hoyle, B., Huterer, D., James, D., Kim, A., Krause, E., Kuehn, K., Lahav, O., Lewis, G., Lidman, C., Lima, M., Maia, M., Malik, U., Marshall, J., Menanteau, F., Miquel, R., Mohr, J., Moller, A., Morgan, R., Ogando, R., Palmese, A., Paz-Chinchon, F., Percival, W., Pieres, A., Malagon, A. P., Roodman, A., Scarpine, V., Schubnell, M., Serrano, S., Sharp, R., Sheldon, E., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M., Tarle, G., Thomas, D., To, C., Tucker, B., Tucker, D., Uddin, S., Varga, T. N., Instituto de Astrofísica de Canarias, Dpto. Astrofísica, Laboratório Interinstitucional de E-Astronomia - LIneA, Medioambientales y Tecnológicas (CIEMAT), Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), The Ohio State University, University of Oslo, University of Wisconsin-Madison, University of Michigan, Universidade Estadual Paulista (UNESP), Universidad Autónoma de Madrid, Universidade Estadual de Campinas (UNICAMP), California Institute of Technology, Stanford University, University of Geneva, NSF's National Optical-Infrared Astronomy Research Laboratory, Fermi National Accelerator Laboratory, Institut d'Astrophysique de Paris, University College London, University of Chicago, SLAC National Accelerator Laboratory, University of Queensland, Astrophysical Observatory of Turin, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, University of Manchester, School of Physics and Astronomy, University of Trieste, Observatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, IIT Hyderabad, University of Pennsylvania, Santa Cruz Institute for Particle Physics, University of Cambridge, Swinburne University of Technology, Ludwig-Maximilians-Universität, Center for Astrophysics | Harvard and Smithsonian, Lawrence Berkeley National Laboratory, University of Arizona, Macquarie University, Lowell Observatory, The University of Sydney, The Australian National University, Australian National University, Universidade de São Paulo (USP), Texas A&M University, Institució Catalana de Recerca i Estudis Avançats, Max Planck Institute for Extraterrestrial Physics, LPC, University of Waterloo, Perimeter Institute for Theoretical Physics, Peyton Hall, Brookhaven National Laboratory, University of Southampton, Oak Ridge National Laboratory, University of Portsmouth, and The University of Texas at Austin
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology: observations, Large-Scale Structure of Universe [Cosmology], FOS: Physical sciences, Física, Astronomy and Astrophysics, observation [Cosmology], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Catalogues, Sample (graphics), Catalogue, Galaxy, Cosmology: large-scale structure of Universe, Observations [Cosmology], Space and Planetary Science, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Rosell, A., et al. (DES Collaboration), In this paper, we present and validate the galaxy sample used for the analysis of the baryon acoustic oscillation (BAO) signal in the Dark Energy Survey (DES) Y3 data. The definition is based on a colour and redshift-dependent magnitude cut optimized to select galaxies at redshifts higher than 0.5, while ensuring a high-quality determination. The sample covers ~4100 deg2 to a depth of i = 22.3 (AB) at 10s. It contains 7031 993 galaxies in the redshift range from z = 0.6 to 1.1, with a mean effective redshift of 0.835. Redshifts are estimated with the machine learning algorithm DNF, and are validated using the VIPERS PDR2 sample. We find a mean redshift bias of zbias~0.01 and a mean uncertainty, in units of 1 + z, of σ68~0.03. We evaluate the galaxy population of the sample, showing it is mostly built upon Elliptical to Sbc types. Furthermore, we find a low level of stellar contamination of ≤ 4 per cent. We present the method used to mitigate the effect of spurious clustering coming from observing conditions and other large-scale systematics.We apply it to the BAO sample and calculate weights that are used to get a robust estimate of the galaxy clustering signal. This paper is one of a series dedicated to the analysis of the BAO signal in DES Y3. In the companion papers, we present the galaxy mock catalogues used to calibrate the analysis and the angular diameter distance constraints obtained through the fitting to the BAO scale., The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838,PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). ACR acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under grant AYA2017-84061-P, co-financed by FEDER (European Regional Development Funds) and by the Spanish Space Research Program ‘Participation in the NISP instrument and preparation for the science of EUCLID’ (ESP2017-84272-C2-1-R). SA was supported by the MICUES project, funded by the EU’s H2020 MSCA grant agreement no. 713366 (InterTalentum UAM).
Published: 2022
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3. The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters

Author: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu, University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS), Williams College [Williamstown], Space Telescope Science Institute (STSci), University of Potsdam = Universität Potsdam, University of Texas at Austin [Austin], Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Johns Hopkins University (JHU), Universidad de La Serena (USERENA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF, Osservatorio Astronomico di Trieste, Italy, NSF’s National Optical-Infrared Astronomy Research Laboratory (NOIRLab), and Astronomy
Subjects: Ultraviolet astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Reionization (1383), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Galactic and extragalactic astronomy (563), Hubble Space Telescope (761) Supporting material: figure sets, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, machine-readable tables, Reionization, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Hubble Space Telescope, Ultraviolet astronomy (1736), Galactic and extragalactic astronomy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The origins of Lyman continuum (LyC) photons responsible for the reionization of the universe are as of yet unknown and highly contested. Detecting LyC photons from the epoch of reionization is not possible due to absorption by the intergalactic medium, which has prompted the development of several indirect diagnostics to infer the rate at which galaxies contribute LyC photons to reionize the universe by studying lower-redshift analogs. We present the Low-redshift Lyman Continuum Survey (LzLCS) comprising measurements made with HST/COS for a z=0.2-0.4 sample of 66 galaxies. After careful processing of the FUV spectra, we obtain a total of 35 Lyman continuum emitters (LCEs) detected with 97.725% confidence, nearly tripling the number of known local LCEs. We estimate escape fractions from the detected LyC flux and upper limits on the undetected LyC flux, finding a range of LyC escape fractions up to 50%. Of the 35 LzLCS LCEs, 12 have LyC escape fractions greater than 5%, more than doubling the number of known local LCEs with cosmologically relevant LyC escape., ApJS, accepted. 28 pages, 19 figures, 8 tables. Full machine readable tables will be made available by the publisher at the time of publication
Published: 2022
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4. The Dark Energy Survey Bright Arcs Survey: Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey 5000 Square Degree Footprint

Author: O’Donnell, JH, Wilkinson, RD, Diehl, HT, Aros-Bunster, C, Bechtol, K, Birrer, S, Buckley-Geer, EJ, Carnero Rosell, A, Carrasco Kind, M, Da Costa, LN, Gonzalez Lozano, SJ, Gruendl, RA, Hilton, M, Lin, H, Lindgren, KA, Martin, J, Pieres, A, Rykoff, ES, Sevilla-Noarbe, I, Sheldon, E, Sifón, C, Tucker, DL, Yanny, B, Abbott, TMC, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Bertin, E, Brooks, D, Burke, DL, Carretero, J, Costanzi, M, De Vicente, J, Desai, S, Dietrich, JP, Eckert, K, Everett, S, Ferrero, I, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gschwend, J, Gill, MSS, Gutierrez, G, Hinton, Hollowood, DL, Honscheid, K, James, DJ, Jeltema, T, Kuehn, K, Lahav, O, Lima, M, Maia, MAG, Marshall, JL, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, Nord, B, Ogando, RLC, Paz-Chinchón, F, Pereira, MES, Plazas Malagón, AA, Rodriguez-Monroy, M, Romer, AK, Roodman, A, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Smith, M, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, To, C, Varga, TN, O’Donnell, JH [0000-0003-4083-1530], Wilkinson, RD [0000-0002-3908-7313], Diehl, HT [0000-0002-8357-7467], Aros-Bunster, C [0000-0002-9441-3193], Birrer, S [0000-0003-3195-5507], Buckley-Geer, EJ [0000-0002-3304-0733], Carnero Rosell, A [0000-0003-3044-5150], Carrasco Kind, M [0000-0002-4802-3194], da Costa, LN [0000-0002-7731-277X], Gonzalez Lozano, SJ [0000-0001-7282-3864], Gruendl, RA [0000-0002-4588-6517], Hilton, M [0000-0002-8490-8117], Lin, H [0000-0002-7825-3206], Lindgren, KA [0000-0002-8414-7776], Pieres, A [0000-0001-9186-6042], Rykoff, ES [0000-0001-9376-3135], Sevilla-Noarbe, I [0000-0002-1831-1953], Sheldon, E [0000-0001-9194-0441], Sifón, C [0000-0002-8149-1352], Tucker, DL [0000-0001-7211-5729], Yanny, B [0000-0002-9541-2678], Abbott, TMC [0000-0003-1587-3931], Aguena, M [0000-0001-5679-6747], Annis, J [0000-0002-0609-3987], Bertin, E [0000-0002-3602-3664], Brooks, D [0000-0002-8458-5047], Burke, DL [0000-0003-1866-1950], Carretero, J [0000-0002-3130-0204], Costanzi, M [0000-0001-8158-1449], De Vicente, J [0000-0001-8318-6813], Desai, S [0000-0002-0466-3288], Eckert, K [0000-0002-1407-4700], Ferrero, I [0000-0002-1295-1132], Flaugher, B [0000-0002-2367-5049], Fosalba, P [0000-0002-1510-5214], Frieman, J [0000-0003-4079-3263], García-Bellido, J [0000-0002-9370-8360], Gaztanaga, E [0000-0001-9632-0815], Gerdes, DW [0000-0001-6942-2736], Gruen, D [0000-0003-3270-7644], Gschwend, J [0000-0003-3023-8362], Gill, MSS [0000-0003-2524-5154], Gutierrez, G [0000-0003-0825-0517], Hinton, SR [0000-0003-2071-9349], Hollowood, DL [0000-0002-9369-4157], Honscheid, K [0000-0002-6550-2023], James, DJ [0000-0001-5160-4486], Jeltema, T [0000-0001-6089-0365], Kuehn, K [0000-0003-0120-0808], Lahav, O [0000-0002-1134-9035], Lima, M [0000-0002-4719-3781], Maia, MAG [0000-0001-9856-9307], Marshall, JL [0000-0003-0710-9474], Melchior, P [0000-0002-8873-5065], Menanteau, F [0000-0002-1372-2534], Miquel, R [0000-0002-6610-4836], Morgan, R [0000-0002-7016-5471], Nord, B [0000-0001-6706-8972], Ogando, RLC [0000-0003-2120-1154], Paz-Chinchón, F [0000-0003-1339-2683], Plazas Malagón, AA [0000-0002-2598-0514], Rodriguez-Monroy, M [0000-0001-6163-1058], Romer, AK [0000-0002-9328-879X], Roodman, A [0000-0001-5326-3486], Sanchez, E [0000-0002-9646-8198], Schubnell, M [0000-0001-9504-2059], Smith, M [0000-0002-3321-1432], Suchyta, E [0000-0002-7047-9358], Swanson, MEC [0000-0002-1488-8552], Tarle, G [0000-0003-1704-0781], Thomas, D [0000-0002-6325-5671], To, C [0000-0001-7836-2261], Apollo - University of Cambridge Repository, Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, European Commission, European Research Council, UAM. Departamento de Física Teórica, University of California at Santa Cruz, University of Sussex, Fermi National Accelerator Laboratory, Pontificia Universidad Católica de Valparaíso, University of Wisconsin-Madison, Stanford University, 382 Via Pueblo Mall, University of Chicago, Laboratório Interinstitucional de E-Astronomia - LIneA, Observatório Nacional, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, Westville Campus, Brookhaven National Laboratory, Half Hollow Hills High School East, SLAC National Accelerator Laboratory, Medioambientales y Tecnológicas (CIEMAT), NSF's National Optical-Infrared Astronomy Research Laboratory, Universidade Estadual Paulista (UNESP), Institut d'Astrophysique de Paris, University College London, The Barcelona Institute of Science and Technology, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, IIT Hyderabad, Ludwig-Maximilians-Universität, University of Pennsylvania, Santa Cruz Institute for Particle Physics, University of Oslo, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE-CSIC), Universidad Autonoma de Madrid, University of Michigan, University of Queensland, The Ohio State University, Center for Astrophysics|Harvard and Smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas AandM University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Cambridge, Universität Hamburg, University of Southampton, Oak Ridge National Laboratory, University of Portsmouth, Giessenbachstrasse, Ludwig-Maximilians Universität München, A O'Donnell, J. H., Wilkinson, R. D., Diehl, H. T., Aros-Bunster, C., Bechtol, K., Birrer, S., Buckley-Geer, E. J., Carnero Rosell, A., Carrasco Kind, M., da Costa, L. N., Gonzalez Lozano, S. J., Gruendl, R. A., Hilton, M., Lin, H., Lindgren, K. A., Martin, J., Pieres, A., Rykoff, E. S., Sevilla-Noarbe, I., Sheldon, E., Sifón, C., Tucker, D. L., Yanny, B., Abbott, T. M. C., Aguena, M., Allam, S., Andrade- Oliveira, F., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Carretero, J., Costanzi, M., De Vicente, J., Desai, S., Dietrich, J. P., Eckert, K., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gschwend, J., Gill, M. S. S., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Nord, B., Ogando, R. L. C., Paz- Chinchón, F., Pereira, M. E. S., Plazas Malagón, A. A., Rodriguez- Monroy, M., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Varga, T. N.
Subjects: Física, Astronomy and Astrophysics, GALÁXIAS, 5109 Space Sciences, Galaxies, High-redshift galaxie, Lens, Space and Planetary Science, Strong gravitational lensing, High-redshift galaxies, 51 Physical Sciences, Quasars, Eye Disease and Disorders of Vision
Abstract: DES Collaboration: O’Donnell et al., We report the combined results of eight searches for strong gravitational lens systems in the full 5000 square degrees of Dark Energy Survey (DES) observations. The observations accumulated by the end of the third observing season fully covered the DES footprint in five filters (grizY), with an i-band limiting magnitude (at 10σ) of 23.44. In four searches, a list of potential candidates was identified using a color and magnitude selection from the object catalogs created from the first three observing seasons. Three other searches were conducted at the locations of previously identified galaxy clusters. Cutout images of potential candidates were then visually scanned using an object viewer. An additional set of candidates came from a data-quality check of a subset of the color–coadd tiles created from the full DES six-season data set. A short list of the most promising strong-lens candidates was then numerically ranked according to whether or not we judged them to be bona fide strong gravitational lens systems. These searches discovered a diverse set of 247 strong-lens candidate systems, of which 81 are identified for the first time. We provide the coordinates, magnitudes, and photometric properties of the lens and source objects, and an estimate of the Einstein radius for 81 new systems and 166 previously reported systems. This catalog will be of use for selecting interesting systems for detailed follow up, studies of galaxy cluster and group mass profiles, as well as a training/validation set for automated strong-lens searches., Funding for the DES projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at The Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l'Espai (IEEC/CSIC), the Institut de Física d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF's NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF's NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).
Published: 2022

5. GOODS-ALMA 2.0: Source catalog, number counts, and prevailing compact sizes in 1.1 mm galaxies

Author: Gómez-Guijarro, C., Elbaz, D., Xiao, M., Béthermin, M., Franco, M., Magnelli, B., Daddi, E., Dickinson, M., Demarco, R., Inami, H., Rujopakarn, W., Magdis, G.E., Shu, X., Chary, R., Zhou, L., Alexander, D.M., Bournaud, F., Ciesla, L., Ferguson, H.C., Finkelstein, S.L., Finlez, C., Giavalisco, M., Iono, D., Juneau, S., Kartaltepe, J.S., Lagache, G., Le Floc'H, E., Leiton, R., Lin, L., Messias, H., Motohara, K., Mullaney, J., Nagar, N.M., Okumura, K., Pannella, M., Papovich, C., Pope, A., Sargent, M.T., Silverman, J.D., Treister, E., Wang, T., Le Floc’h, E., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of Hertfordshire [Hatfield] (UH), NSF’s National Optical-Infrared Astronomy Research Laboratory (NOIRLab), Universidad de Concepción - University of Concepcion [Chile], Hiroshima University, Chulalongkorn University [Bangkok], Danmarks Tekniske Universitet = Technical University of Denmark (DTU), Anhui Normal University, California Institute of Technology (CALTECH), Nanjing University (NJU), Durham University, Space Telescope Science Institute (STSci), University of Texas at Austin [Austin], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS), National Astronomical Observatory of Japan (NAOJ), Rochester Institute of Technology, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Academia Sinica, The University of Tokyo (UTokyo), University of Sheffield [Sheffield], Università degli studi di Trieste = University of Trieste, Texas A&M University System, University of Sussex, Pontificia Universidad Católica de Chile (UC), Univ New South Wales, MERLin Sch Chem Engn, Sydney, NSW 2052, Australia, and We thank G. Pöpping, C. del P. Lagos, and J. A.Zavala for providing the predicted number counts from their models plotted in Fig. 11. M.F. acknowledges the support from STFC (grant number ST/R000905/1). G.E.M. acknowledges the Villum Fonden research grant 13160 ‘Gas to stars, stars to dust: tracing star formation across cosmic time’ and the Cosmic Dawn Center of Excellence funded by the Danish National Research Foundation under the grant No. 140. H.I. acknowledges support from JSPS KAKENHI Grant Number JP19K23462 and JP21H01129. M.T.S. acknowledges support from a Scientific Exchanges visitor fellowship (IZSEZO_202357) from the Swiss National Science Foundation. This papermakes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00543.S and ADS/JAO.ALMA#2017.1.00755.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. We are grateful to the anonymous referee, whose comments have been very useful to improving our work
Subjects: submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, structure [Galaxies], PHYSICAL-PROPERTIES, FOS: Physical sciences, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, star formation [Galaxies], 01 natural sciences, GMASS ULTRADEEP SPECTROSCOPY, high-redshift [Galaxies], galaxies [Submillimeter], galaxies: high-redshift, 0103 physical sciences, STAR-FORMING GALAXIES, Sensitivity (control systems), Continuum (set theory), DEEP FIELD-SOUTH, MAIN-SEQUENCE, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Effective radius, Physics, DEGREE EXTRAGALACTIC SURVEY, SUBMILLIMETER GALAXIES, 010308 nuclear & particles physics, photometry [Galaxies], Homogeneity (statistics), MASSIVE GALAXIES, Astronomy and Astrophysics, evolution [Galaxies], FAR-INFRARED PROPERTIES, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, galaxies: photometry, LUMINOSITY FUNCTION, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, galaxies: structure, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Submillimeter/millimeter observations of dusty star-forming galaxies with the Atacama Large Millimeter/submillimeter Array (ALMA) have shown that dust continuum emission generally occurs in compact regions smaller than the stellar distribution. However, it remains to be understood how systematic these findings are. Studies often lack homogeneity in the sample selection, target discontinuous areas with inhomogeneous sensitivities, and suffer from modest $uv$ coverage coming from single array configurations. GOODS-ALMA is a 1.1mm galaxy survey over a continuous area of 72.42arcmin$^2$ at a homogeneous sensitivity. In this version 2.0, we present a new low resolution dataset and its combination with the previous high resolution dataset from the survey, improving the $uv$ coverage and sensitivity reaching an average of $��= 68.4��$Jy beam$^{-1}$. A total of 88 galaxies are detected in a blind search (compared to 35 in the high resolution dataset alone), 50% at $S/N_{peak} \geq 5$ and 50% at $3.5 \leq S/N_{peak} \leq 5$ aided by priors. Among them, 13 out of the 88 are optically dark or faint sources ($H$- or $K$-band dropouts). The sample dust continuum sizes at 1.1mm are generally compact, with a median effective radius of $R_{e} = 0"10 \pm 0"05$ (a physical size of $R_{e} = 0.73 \pm 0.29$kpc at the redshift of each source). Dust continuum sizes evolve with redshift and stellar mass resembling the trends of the stellar sizes measured at optical wavelengths, albeit a lower normalization compared to those of late-type galaxies. We conclude that for sources with flux densities $S_{1.1mm} > 1$mJy, compact dust continuum emission at 1.1mm prevails, and sizes as extended as typical star-forming stellar disks are rare. The $S_{1.1mm} < 1$mJy sources appear slightly more extended at 1.1mm, although they are still generally compact below the sizes of typical star-forming stellar disks., Accepted by A&A. 30 pages, 18 figures
Published: 2022
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6. From the fire: a deeper look at the Phoenix stream

Author: K. Tavangar, P. Ferguson, N. Shipp, A. Drlica-Wagner, S. Koposov, D. Erkal, E. Balbinot, J. García-Bellido, K. Kuehn, G. F. Lewis, T. S. Li, S. Mau, A. B. Pace, A. H. Riley, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, H. T. Diehl, S. Everett, I. Ferrero, B. Flaugher, J. Frieman, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, N. Kuropatkin, M. A. G. Maia, J. L. Marshall, F. Menanteau, R. Miquel, R. Morgan, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, M. Rodriguez-Monroy, E. Sanchez, V. Scarpine, S. Serrano, I. Sevilla-Noarbe, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, T. N. Varga, A. R. Walker, UAM. Departamento de Física Teórica, Tavangar, K [0000-0001-6584-6144], Ferguson, P [0000-0001-6957-1627], Shipp, N [0000-0003-2497-091X], Drlica-Wagner, A [0000-0001-8251-933X], Koposov, S [0000-0003-2644-135X], Erkal, D [0000-0002-8448-5505], Balbinot, E [0000-0002-1322-3153], García-Bellido, J [0000-0002-9370-8360], Kuehn, K [0000-0003-0120-0808], Lewis, GF [0000-0003-3081-9319], Li, TS [0000-0002-9110-6163], Mau, S [0000-0003-3519-4004], Pace, AB [0000-0002-6021-8760], Riley, AH [0000-0001-5805-5766], Aguena, M [0000-0001-5679-6747], Allam, S [0000-0002-7069-7857], Annis, J [0000-0002-0609-3987], Bertin, E [0000-0002-3602-3664], Brooks, D [0000-0002-8458-5047], Burke, DL [0000-0003-1866-1950], Carnero Rosell, A [0000-0003-3044-5150], Carrasco Kind, M [0000-0002-4802-3194], Carretero, J [0000-0002-3130-0204], Costanzi, M [0000-0001-8158-1449], De Vicente, J [0000-0001-8318-6813], Diehl, HT [0000-0002-8357-7467], Flaugher, B [0000-0002-2367-5049], Frieman, J [0000-0003-4079-3263], Gaztanaga, E [0000-0001-9632-0815], Gerdes, DW [0000-0001-6942-2736], Gruen, D [0000-0003-3270-7644], Gschwend, J [0000-0003-3023-8362], Gutierrez, G [0000-0003-0825-0517], Honscheid, K [0000-0002-6550-2023], James, DJ [0000-0001-5160-4486], Kuropatkin, N [0000-0003-2511-0946], Maia, MAG [0000-0001-9856-9307], Marshall, JL [0000-0003-0710-9474], Menanteau, F [0000-0002-1372-2534], Miquel, R [0000-0002-6610-4836], Ogando, RLC [0000-0003-2120-1154], Palmese, A [0000-0002-6011-0530], Paz-Chinchón, F [0000-0003-1339-2683], Pieres, A [0000-0001-9186-6042], Plazas Malagón, AA [0000-0002-2598-0514], Sanchez, E [0000-0002-9646-8198], Sevilla-Noarbe, I [0000-0002-1831-1953], Smith, M [0000-0002-3321-1432], Suchyta, E [0000-0002-7047-9358], Tarle, G [0000-0003-1704-0781], To, C [0000-0001-7836-2261], Walker, AR [0000-0002-7123-8943], Apollo - University of Cambridge Repository, Astronomy, University of Chicago, University of Wisconsin-Madison, Texas AandM University, MIT Kavli Institute for Astrophysics and Space Research, Fermi National Accelerator Laboratory, Royal Observatory, University of Cambridge, University of Surrey, University of Groningen, Universidad Autonoma de Madrid, Lowell Observatory, Macquarie University, The University of Sydney, University of Toronto, Observatories of the Carnegie Institution for Science, Princeton University, Stanford University, Carnegie Mellon University, NSF's National Optical-Infrared Astronomy Research Laboratory, Laboratório Interinstitucional de E-Astronomia-LIneA, Universidade Estadual Paulista (UNESP), Institut d'Astrophysique de Paris, University College London, SLAC National Accelerator Laboratory, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, University of Trieste, Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, Universität Hamburg, Medioambientales y Tecnológicas (CIEMAT), Santa Cruz Institute for Particle Physics, University of Oslo, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), Ludwig-Maximilians-Universität, University of Queensland, The Ohio State University, Center for Astrophysics | Harvard and Smithsonian, Institució Catalana de Recerca i Estudis Avançats, University of Southampton, Oak Ridge National Laboratory, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universität München, National Science Foundation (US), Department of Energy (US), German Research Foundation, Ministerio de Economía y Competitividad (España), European Commission, European Research Council, Generalitat de Catalunya, Tavangar, K., Ferguson, P., Shipp, N., Drlica-Wagner, A., Koposov, S., Erkal, D., Balbinot, E., García-Bellido, J., Kuehn, K., Lewis, G. F., T. S., Li, Mau, S., Pace, A. B., Riley, A. H., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuropatkin, N., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Varga, T. N., and Walker, A. R.
Subjects: Galaxy structure, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar stream, Stellar streams, FOS: Physical sciences, Física, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxies and Cosmology, Cosmology, Dark matter, Astronomy data modeling, Milky Way dynamics, Milky way dynamics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Tavangar et al., We use 6 yr of data from the Dark Energy Survey to perform a detailed photometric characterization of the Phoenix stellar stream, a 15° long, thin, dynamically cold, low-metallicity stellar system in the Southern Hemisphere. We use natural splines, a nonparametric modeling technique, to simultaneously fit the stream track, width, and linear density. This updated stream model allows us to improve measurements of the heliocentric distance (17.4 ± 0.1 (stat.) ±0.8 (sys.) kpc) and distance gradient (−0.009 ± 0.006 kpc deg−1) of Phoenix, which corresponds to a small change of 0.13 ± 0.09 kpc in heliocentric distance along the length of the stream. We measure linear intensity variations on degree scales, as well as deviations in the stream track on ∼2° scales, suggesting that the stream may have been disturbed during its formation and/or evolution. We recover three peaks and one gap in linear intensity along with fluctuations in the stream track. Compared to other thin streams, the Phoenix stream shows more fluctuations and, consequently, the study of Phoenix offers a unique perspective on gravitational perturbations of stellar streams. We discuss possible sources of perturbations to Phoenix, including baryonic structures in the Galaxy and dark matter subhalos., Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at The Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the LudwigMaximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-20160597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007–2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project No. CE110001020, and the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).
Published: 2022
Full Text: View/download PDF

7. Dark Energy Survey Year 3 results: A 2.7% measurement of baryon acoustic oscillation distance scale at redshift 0.835

Author: Abbott, T.M.C., Aguena, M., Allam, S., Amon, A., Andrade-Oliveira, F., Asorey, J., Avila, S., Bernstein, G.M., Bertin, E., Brandao-Souza, A., Brooks, D., Burke, D.L., Calcino, J., Camacho, H., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Castander, F.J., Cawthon, R., Chan, K.C., Choi, A., Conselice, C., Costanzi, M., Crocce, M., da Costa, L.N., Pereira, M.E.S., Davis, T.M., De Vicente, J., Desai, S., Diehl, H.T., Doel, P., Eckert, K., Elvin-Poole, J., Everett, S., Evrard, A.E., Fang, X., Ferrero, Ismael, Ferté, A., Flaugher, B., Fosalba, P., García-Bellido, J., Gaztanaga, E., Gerdes, D.W., Giannantonio, T., Glazebrook, K., Gomes, D., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Hinton, S.R., Hollowood, D.L., Honscheid, K., Huterer, D., Jain, B., James, D.J., Jeltema, T., Kokron, N., Krause, E., Kuehn, K., Lahav, O., Lewis, G.F., Lidman, C., Lima, M., Lin, H., Maia, M.A.G., Malik, U., Martini, P., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Mohr, J.J., Morgan, R., Muir, J., Myles, J., Möller, A., Palmese, A., Paz-Chinchón, F., Percival, W.J., Pieres, A., Plazas Malagón, A.A., Porredon, A., Prat, J., Reil, K., Rodriguez-Monroy, M., Romer, A.K., Roodman, A., Rosenfeld, R., Ross, A.J., Sanchez, E., Sanchez Cid, D., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., To, C., Troxel, M.A., Tucker, B.E., Tucker, D.L., Tutusaus, I., Uddin, S.A., Varga, T.N., Weller, J., Wilkinson, R.D., UAM. Departamento de Física Teórica, NSF's National Optical-Infrared Astronomy Research Laboratory, Laboratório Interinstitucional de E-Astronomia - LIneA, Fermi National Accelerator Laboratory, Stanford University, Universidade Estadual Paulista (UNESP), Medioambientales y Tecnológicas (CIEMAT), Universidad Autonoma de Madrid, University of Pennsylvania, Institut d'Astrophysique de Paris, Universidade Estadual de Campinas (UNICAMP), University College London, SLAC National Accelerator Laboratory, University of Queensland, Instituto de Astrofisica de Canarias, Dpto. Astrofísica, Astrophysical Observatory of Turin, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), University of Wisconsin-Madison, Sun Yat-sen University, The Ohio State University, University of Manchester, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, IIT Hyderabad, Santa Cruz Institute for Particle Physics, University of Arizona, University of Oslo, California Institute of Technology, University of Cambridge, Swinburne University of Technology, Universidade de São Paulo (USP), Ludwig-Maximilians-Universität, Center for Astrophysics | Harvard and Smithsonian, 382 Via Pueblo Mall, Macquarie University, Lowell Observatory, The University of Sydney, The Australian National University, Australian National University, Harvard University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, Max Planck Institute for Extraterrestrial Physics, LPC, University of Chicago, University of Waterloo, Perimeter Institute for Theoretical Physics, University of Sussex, Brookhaven National Laboratory, University of Southampton, Oak Ridge National Laboratory, University of Portsmouth, Duke University Durham, The University of Texas at Austin, Ludwig-Maximilians Universität München, Abbott, T. M. C., Aguena, M., Allam, S., Amon, A., Andrade-Oliveira, F., Asorey, J., Avila, S., Bernstein, G. M., Bertin, E., Brandao-Souza, A., Brooks, D., Burke, D. L., Calcino, J., Camacho, H., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Chan, K. C., Choi, A., Conselice, C., Costanzi, M., Crocce, M., Da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eckert, K., Elvin-Poole, J., Everett, S., Evrard, A. E., Fang, X., Ferrero, I., Ferte, A., Flaugher, B., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Glazebrook, K., Gomes, D., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., Jain, B., James, D. J., Jeltema, T., Kokron, N., Krause, E., Kuehn, K., Lahav, O., Lewis, G. F., Lidman, C., Lima, M., Lin, H., Maia, M. A. G., Malik, U., Martini, P., Melchior, P., Mena-Fernandez, J., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Muir, J., Myles, J., Moller, A., Palmese, A., Paz-Chinchon, F., Percival, W. J., Pieres, A., Plazas Malagon, A. A., Porredon, A., Prat, J., Reil, K., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Sanchez, E., Sanchez Cid, D., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tucker, B. E., Tucker, D. L., Tutusaus, I., Uddin, S. A., Varga, T. N., Weller, J., Wilkinson, R. D., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), DES, National Science Foundation (US), Department of Energy (US), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), European Commission, European Research Council, and Generalitat de Catalunya
Subjects: Astrophysic, Halo, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics, Cosmology and Nongalactic Astrophysics, FOS: Physical sciences, Red Shift, Física, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: T. M.C. Abbott et al., We present angular diameter measurements obtained by measuring the position of baryon acoustic oscillations (BAO) in an optimized sample of galaxies from the first three years of Dark Energy Survey data (DES Y3). The sample consists of 7 million galaxies distributed over a footprint of 4100 deg2 with 0.60.75. When combined with DES 3x2pt+SNIa, they lead to improvements in H0 and Ωm constraints by∼20%., Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University,the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV2016-0588, No. SEV-2016-0597, and No. MDM-20150509, some of which include ERDF funds from the European Union. I.F.A.E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grant Agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DEAC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2022
Full Text: View/download PDF

8. Dark Energy Survey Year 3 results: Cosmology from cosmic shear and robustness to modeling uncertainty

Author: Secco, L. F., Samuroff, S., Krause, E., Jain, B., Blazek, J., Raveri, M., Campos, A., Amon, A., Chen, A., Doux, C., Choi, A., Gruen, D., Bernstein, G. M., Chang, C., Derose, J., Myles, J., Ferté, A., Lemos, P., Huterer, D., Prat, J., Troxel, M. A., Maccrann, N., Liddle, A. R., Kacprzak, T., Fang, X., Sánchez, C., Pandey, S., Dodelson, S., Chintalapati, P., Hoffmann, K., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E. J., Bechtol, K., Becker, M. R., Brandao-Souza, A., Camacho, H., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Cordero, J. P., Crocce, M., Davis, C., Di Valentino, E., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elidaiana, M., Elsner, F., Elvin-Poole, J., Everett, S., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Jarvis, M., Jeffrey, N., Kuropatkin, N., Leget, P. -F., Muir, J., Mccullough, J., Navarro Alsina, A., Omori, Y., Park, Y., Porredon, A., Rollins, R., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E. S., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Diehl, H. T., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Scolnic, D., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Des, Collaboration, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Secco, L. F., Samuroff, S., Krause, E., Jain, B., Blazek, J., Raveri, M., Campos, A., Amon, A., Chen, A., Doux, C., Choi, A., Gruen, D., Bernstein, G. M., Chang, C., Derose, J., Myles, J., Ferte, A., Lemos, P., Huterer, D., Prat, J., Troxel, M. A., Maccrann, N., Liddle, A. R., Kacprzak, T., Fang, X., Sanchez, C., Pandey, S., Dodelson, S., Chintalapati, P., Hoffmann, K., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E. J., Bechtol, K., Becker, M. R., Brandao-Souza, A., Camacho, H., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Cordero, J. P., Crocce, M., Davis, C., Di Valentino, E., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elidaiana, M., Elsner, F., Elvin-Poole, J., Everett, S., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Jarvis, M., Jeffrey, N., Kuropatkin, N., Leget, P. -F., Muir, J., Mccullough, J., Navarro Alsina, A., Omori, Y., Park, Y., Porredon, A., Rollins, R., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E. S., Shin, T., Tutusaus, I., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., Da Costa, L. N., De Vicente, J., Diehl, H. T., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Petravick, D., Pieres, A., Plazas Malagon, A. A., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Scolnic, D., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), National Science Foundation (US), European Commission, Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Australian Research Council, University of Chicago, University of Pennsylvania, Carnegie Mellon University, Northeastern University, University of Arizona, École Polytechnique Fédérale de Lausanne (EPFL), Stanford University, University of Michigan, The Ohio State University, 382 Via Pueblo Mall, SLAC National Accelerator Laboratory, University of California, California Institute of Technology, University College London, Duke University, University of Cambridge, Universidade de Lisboa, University of Edinburgh, Perimeter Institute for Theoretical Physics, ETH Zürich, Northern Illinois University, University of Zürich, Argonne National Laboratory, Universidade Estadual Paulista (UNESP), Laboratório Interinstitucional de E-Astronomia - LIneA, University of Hawai'i, University of Wisconsin-Madison, Universidade Estadual de Campinas (UNICAMP), Medioambientales y Tecnológicas (CIEMAT), Instituto de Astrofísica de Canarias, Dpto. Astrofísica, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, University of Manchester, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Fermi National Accelerator Laboratory, Max Planck Institute für Extraterrestrial Physics, Santa Cruz Institute for Particle Physics, The Barcelona Institute of Science and Technology, Denys Wilkinson Building, Université de Genève, Université de Paris, Laboratoire de Physique de Clermont, Laboratoire de Physique Nucléaire et de Hautes Énergies, The University of Tokyo, Ohio State University, Brookhaven National Laboratory, Ludwig-Maximilians Universität München, NSF's National Optical-Infrared Astronomy Research Laboratory, University of Portsmouth, Institut d'Astrophysique de Paris, University of Sussex, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, Ludwig-Maximilians-Universität, University of Oslo, Universidad Autonoma de Madrid, University of Queensland, Max Planck Institute for Extraterrestrial Physics, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas A and M University, Harvard University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Southampton, Oak Ridge National Laboratory, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and UAM. Departamento de Física Teórica
Subjects: luminous red galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, Cosmological parameters, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, Sky surveys, Astrophysics, 01 natural sciences, large-scale structure, Astrophysic, weak-lensing surveys, Gravitational lenses, Cosmology and Nongalactic Astrophysics, 0103 physical sciences, Weak, baryonic feedback, 010303 astronomy & astrophysics, redshift inference, intrinsic galaxy shapes, Gravitational Lensing, 010308 nuclear & particles physics, Física, COSMOLOGIA, Dark Energy, 13. Climate action, 2-point correlation-functions, photometric data set, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Secco, L.F., et al. (DES Collaboration), This work and its companion paper, Amon et al. [Phys. Rev. D 105, 023514 (2022)PRVDAQ2470-001010.1103/PhysRevD.105.023514], present cosmic shear measurements and cosmological constraints from over 100 million source galaxies in the Dark Energy Survey (DES) Year 3 data. We constrain the lensing amplitude parameter S8σ8ωm/0.3 at the 3% level in ΛCDM: S8=0.759-0.023+0.025 (68% CL). Our constraint is at the 2% level when using angular scale cuts that are optimized for the ΛCDM analysis: S8=0.772-0.017+0.018 (68% CL). With cosmic shear alone, we find no statistically significant constraint on the dark energy equation-of-state parameter at our present statistical power. We carry out our analysis blind, and compare our measurement with constraints from two other contemporary weak lensing experiments: the Kilo-Degree Survey (KiDS) and Hyper-Suprime Camera Subaru Strategic Program (HSC). We additionally quantify the agreement between our data and external constraints from the Cosmic Microwave Background (CMB). Our DES Y3 result under the assumption of ΛCDM is found to be in statistical agreement with Planck 2018, although favors a lower S8 than the CMB-inferred value by 2.3σ (a p-value of 0.02). This paper explores the robustness of these cosmic shear results to modeling of intrinsic alignments, the matter power spectrum and baryonic physics. We additionally explore the statistical preference of our data for intrinsic alignment models of different complexity. The fiducial cosmic shear model is tested using synthetic data, and we report no biases greater than 0.3σ in the plane of S8×ωm caused by uncertainties in the theoretical models., The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-88861, No. FPA2015-68048, No. SEV-2012-0234, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020.
Published: 2022
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9. Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and weak lensing

Author: DES Collaboration, Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Alves, O., Amon, A., Andrade-Oliveira, F., Annis, J., Avila, S., Bacon, D., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Bhargava, S., Birrer, S., Blazek, J., Brandao-Souza, A., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Camacho, H., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, A., Chen, R., Choi, A., Conselice, C., Cordero, J., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. da Silva, Davis, C., Davis, T. M., De Vicente, J., DeRose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Evrard, A. E., Fang, X., Farahi, A., Fernandez, E., Ferrero, I., Fert��, A., Fosalba, P., Friedrich, O., Frieman, J., Garc��a-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Harrison, I., Hartley, W. G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huff, E. M., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeffrey, N., Jeltema, T., Kovacs, A., Krause, E., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Leget, P. -F., Lemos, P., Liddle, A. R., Lidman, C., Lima, M., Lin, H., MacCrann, N., Maia, M. A. G., Marshall, J. L., Martini, P., McCullough, J., Melchior, P., Mena-Fern��ndez, J., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Muir, J., Myles, J., Nadathur, S., Navarro-Alsina, A., Nichol, R. C., Ogando, R. L. C., Omori, Y., Palmese, A., Pandey, S., Park, Y., Paz-Chinch��n, F., Petravick, D., Pieres, A., Malag��n, A. A. Plazas, Porredon, A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., S��nchez, C., Sanchez, E., Sanchez, J., Cid, D. Sanchez, Scarpine, V., Schubnell, M., Scolnic, D., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tabbutt, M., Tarle, G., Thomas, D., To, C., Troja, A., Troxel, M. A., Tucker, D. L., Tutusaus, I., Varga, T. N., Walker, A. R., Weaverdyck, N., Wechsler, R., Weller, J., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Alves, O., Amon, A., Andrade-Oliveira, F., Annis, J., Avila, S., Bacon, D., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Bhargava, S., Birrer, S., Blazek, J., Brandao-Souza, A., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, A., Chen, R., Choi, A., Conselice, C., Cordero, J., Costanzi, M., Crocce, M., Da Costa, L. N., Da Silva Pereira, M. E., Davis, C., Davis, T. M., De Vicente, J., Derose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Evrard, A. E., Fang, X., Farahi, A., Fernandez, E., Ferrero, I., Ferte, A., Fosalba, P., Friedrich, O., Frieman, J., Garcia-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Harrison, I., Hartley, W. G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huff, E. M., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeffrey, N., Jeltema, T., Kovacs, A., Krause, E., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Leget, P. -F., Lemos, P., Liddle, A. R., Lidman, C., Lima, M., Lin, H., Maccrann, N., Maia, M. A. G., Marshall, J. L., Martini, P., Mccullough, J., Melchior, P., Mena-Fernandez, J., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Muir, J., Myles, J., Nadathur, S., Navarro-Alsina, A., Nichol, R. C., Ogando, R. L. C., Omori, Y., Palmese, A., Pandey, S., Park, Y., Paz-Chinchon, F., Petravick, D., Pieres, A., Plazas Malagon, A. A., Porredon, A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sanchez, C., Sanchez, E., Sanchez, J., Sanchez Cid, D., Scarpine, V., Schubnell, M., Scolnic, D., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tabbutt, M., Tarle, G., Thomas, D., To, C., Troja, A., Troxel, M. A., Tucker, D. L., Tutusaus, I., Varga, T. N., Walker, A. R., Weaverdyck, N., Wechsler, R., Weller, J., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, European Commission, Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), Department of Energy (US), Generalitat de Catalunya, National Aeronautics and Space Administration (US), National Science Foundation (US), NSF's National Optical-Infrared Astronomy Research Laboratory, Laboratório Interinstitucional de E-Astronomia - LIneA, Argonne National Laboratory, Fermi National Accelerator Laboratory, University of Michigan, Universidade Estadual Paulista (UNESP), Stanford University, Universidad Autonoma de Madrid, University of Portsmouth, University of Hawai'i, University of Wisconsin-Madison, University of Pennsylvania, University of Sussex, 450 Serra Mall, Northeastern University, Observatoire de Sauverny, Universidade Estadual de Campinas (UNICAMP), University of Manchester, University College London, University of Chicago, SLAC National Accelerator Laboratory, Carnegie Mellon University, Instituto de Astrofisica de Canarias, Dpto. Astrofísica, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Duke University, The Ohio State University, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Queensland, Medioambientales y Tecnológicas (CIEMAT), Lawrence Berkeley National Laboratory, IIT Hyderabad, Ludwig-Maximilians-Universität, University of Arizona, California Institute of Technology, Santa Cruz Institute for Particle Physics, University of Texas at Austin, University of Oslo, University of Cambridge, 382 Via Pueblo Mall, Denys Wilkinson Building, University of Geneva, Center for Astrophysics and Harvard and Smithsonian, Université de Paris, Macquarie University, Lowell Observatory, University of Edinburgh, Universidade de Lisboa, Perimeter Institute for Theoretical Physics, The Australian National University, Australian National University, Universidade de São Paulo (USP), Texas AandM University, Harvard University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, Max Planck Institute for Extraterrestrial Physics, The University of Tokyo, Brookhaven National Laboratory, University of Southampton, Oak Ridge National Laboratory, Ludwig-Maximilians Universität München, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), DES, UAM. Departamento de Física Teórica, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: luminous red galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, parameter constraints, supernova legacy survey, Astrophysics, 01 natural sciences, Astrophysic, Cosmology and Nongalactic Astrophysics, 0103 physical sciences, LENTES GRAVITACIONAIS, Weak, 010303 astronomy & astrophysics, mass correlation-function, Gravitational Lensing, extragalactic objects, 010308 nuclear & particles physics, Física, Dark Energy, ia supernovae, digital sky survey, power-spectrum, photometric data set, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic shear, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: T. M. C. Abbott et al., We present the first cosmology results from large-scale structure using the full 5000 deg2 of imaging data from the Dark Energy Survey (DES) Data Release 1. We perform an analysis of large-scale structure combining three two-point correlation functions (3×2pt): (i) cosmic shear using 100 million source galaxies, (ii) galaxy clustering, and (iii) the cross-correlation of source galaxy shear with lens galaxy positions, galaxy–galaxy lensing. To achieve the cosmological precision enabled by these measurements has required updates to nearly every part of the analysis from DES Year 1, including the use of two independent galaxy clustering samples, modeling advances, and several novel improvements in the calibration of gravitational shear and photometric redshift inference. The analysis was performed under strict conditions to mitigate confirmation or observer bias; we describe specific changes made to the lens galaxy sample following unblinding of the results and tests of the robustness of our results to this decision. We model the data within the flat ΛCDM and wCDM cosmological models, marginalizing over 25 nuisance parameters. We find consistent cosmological results between the three two-point correlation functions; their combination yields clustering amplitude S8=0.776+0.017−0.017 and matter density Ωm=0.339+0.032−0.031 in ΛCDM, mean with 68% confidence limits; S8=0.775+0.026−0.024, Ωm=0.352+0.035−0.041, and dark energy equation-of-state parameter w=−0.98+0.32−0.20 in wCDM. These constraints correspond to an improvement in signal-to-noise of the DES Year 3 3×2pt data relative to DES Year 1 by a factor of 2.1, about 20% more than expected from the increase in observing area alone. This combination of DES data is consistent with the prediction of the model favored by the Planck 2018 cosmic microwave background (CMB) primary anisotropy data, which is quantified with a probability-to-exceed p=0.13–0.48. We find better agreement between DES 3×2pt and Planck than in DES Y1, despite the significantly improved precision of both. When combining DES 3×2pt data with available baryon acoustic oscillation, redshift-space distortion, and type Ia supernovae data, we find p=0.34. Combining all of these datasets with Planck CMB lensing yields joint parameter constraints of S8=0.812+0.008−0.008, Ωm=0.306+0.004−0.005, h=0.680+0.004−0.003, and ∑mν, Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ci`encies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements No. 240672, No. 291329, and No. 306478.We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant No. 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. This work also used resources on Duke Compute Cluster (DCC), the CCAPP condo of the Ruby Cluster at the Ohio Supercomputing Center [232], and computing resources at SLAC National Accelerator Laboratory. We also thank the staff of the Fermilab Computing Sector for their support. Plots in this manuscript were produced partly with MATPLOTLIB [233], and it has been prepared using NASA’s Astrophysics Data System Bibliographic Services.
Published: 2022

10. The mass and galaxy distribution around SZ-selected clusters

Author: Edward J. Wollack, S. Goldstein, Erin S. Sheldon, Jochen Weller, L. N. da Costa, J. Elvin-Poole, Suzanne T. Staggs, Simone Ferraro, Marco Raveri, Mark J. Devlin, J. P. Dietrich, Sahar S. Allam, T. N. Varga, David Brooks, S. Pandey, M. Lokken, Brian Yanny, Maria E. S. Pereira, A. Amsellem, J. DeRose, Maria Salatino, J. McCullough, M. E. C. Swanson, M. Costanzi, C. Doux, Chun-Hao To, Cristóbal Sifón, E. J. Sanchez, Joseph J. Mohr, I. Tutusaus, I. Sevilla-Noarbe, Gary Bernstein, B. Partridge, John P. Hughes, Carlos Solans Sanchez, G. Tarle, Scott Dodelson, Chihway Chang, V. Scarpine, Keith Bechtol, Ian Harrison, Enrique Gaztanaga, B. Flaugher, Peter Doel, Nick Battaglia, Alex Drlica-Wagner, J. Myles, David J. James, N. P. Kuropatkin, H. T. Diehl, David Bacon, Kavilan Moodley, Niall MacCrann, T. M. C. Abbott, David H. Weinberg, Kyler Kuehn, M. Gatti, J. Prat, Adriano Pieres, Samuel Hinton, Bhuvnesh Jain, K. Eckert, J. De Vicente, T. Dacunha, Marcelle Soares-Santos, E. Suchyta, E. J. Baxter, D. Gruen, A. Carnero Rosell, J. Carretero, Matt Hilton, M. Belyakov, Michael Troxel, J. C. Hill, F. Paz-Chinchón, A. Alarcon, Richard P. Rollins, Antonio Campos, Ramon Miquel, S. Desai, Federico Nati, Michael D. Niemack, Sebastian Bocquet, M. Smith, M. Aguena, A. K. Romer, Daniel Thomas, E. Buckley-Geer, L. A. Page, Emmanuel Bertin, Antonella Palmese, Andrés N. Salcedo, Jeff McMahon, Agnès Ferté, Blake D. Sherwin, M. A. G. Maia, D. W. Gerdes, Ofer Lahav, I. Ferrero, Mathew S. Madhavacheril, Robert Morgan, M. Rodriguez-Monroy, Yanxi Zhang, A. A. Plazas Malagón, Andrey V. Kravtsov, S. Everett, Marco A. P. Lima, S. Adhikari, Patricio A. Gallardo, Matthew R. Becker, Basilio X. Santiago, D. L. Burke, J. Frieman, J. R. Bond, Robert A. Gruendl, M. Carrasco Kind, F. Andrade-Oliveira, Tesla E. Jeltema, Ricardo L. C. Ogando, M. Jarvis, R. Chen, Ami Choi, Elisabeth Krause, Peter Melchior, Eli S. Rykoff, Eve M. Vavagiakis, G. Gutierrez, A. Navarro-Alsina, Santiago Serrano, B. Yin, Alexandra Amon, Felipe Menanteau, James Annis, Brian J. Koopman, L. F. Secco, W. G. Hartley, Alessandro Schillaci, Devon L. Hollowood, T. Shin, University of Pennsylvania, University of Chicago, University of Hawaii, The Ohio State University, Cornell University, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians-Universität, NSF’s National Optical-Infrared Astronomy Research Laboratory, Universidade de São Paulo (USP), Laboratório Interinstitucional de e-Astronomia – LIneA, Argonne National Laboratory, Fermi National Accelerator Laboratory, Stanford University, Universidade Estadual Paulista (UNESP), University of Portsmouth, University of Wisconsin-Madison, Institut d’Astrophysique de Paris, University of Toronto, University College London, Carnegie Mellon University, Duke University, Instituto de Astrofisica de Canarias, Dpto. Astrofísica, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, Lawrence Berkeley National Laboratory, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, IIT Hyderabad, Medioambientales y Tecnológicas (CIEMAT), Santa Cruz Institute for Particle Physics, University of Oslo, California Institute of Technology, Institut d’Estudis Espacials de Catalunya (IEEC), CSIC), University of Michigan, SLAC National Accelerator Laboratory, Denys Wilkinson Building, University of Manchester, University of Geneva, Columbia University, Flatiron Institute, Westville Campus, University of Queensland, The State University of New Jersey, Center for Astrophysics | Harvard & Smithsonian, Yale University, University of Arizona, Macquarie University, Lowell Observatory, Dunlap Institute of Astronomy & Astrophysics, University of Cambridge, Perimeter Institute for Theoretical Physics, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Milano-Bicocca, Universidade Estadual de Campinas (UNICAMP), Princeton University, Haverford College, University of Sussex, UFRGS, Brookhaven National Laboratory, Pontificia Universidad Católica de Valparaíso, University of Southampton, Oak Ridge National Laboratory, NASA/Goddard Space Flight Center, Shin, T, Jain, B, Adhikari, S, Baxter, E, Chang, C, Pandey, S, Salcedo, A, Weinberg, D, Amsellem, A, Battaglia, N, Belyakov, M, Dacunha, T, Goldstein, S, Kravtsov, A, Varga, T, Abbott, T, Aguena, M, Alarcon, A, Allam, S, Amon, A, Andrade-Oliveira, F, Annis, J, Bacon, D, Bechtol, K, Becker, M, Bernstein, G, Bertin, E, Bocquet, S, Bond, J, Brooks, D, Buckley-Geer, E, Burke, D, Campos, A, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Chen, R, Choi, A, Costanzi, M, da Costa, L, Derose, J, Desai, S, de Vicente, J, Devlin, M, Diehl, H, Dietrich, J, Dodelson, S, Doel, P, Doux, C, Drlica-Wagner, A, Eckert, K, Elvin-Poole, J, Everett, S, Ferraro, S, Ferrero, I, Ferte, A, Flaugher, B, Frieman, J, Gallardo, P, Gatti, M, Gaztanaga, E, Gerdes, D, Gruen, D, Gruendl, R, Gutierrez, G, Harrison, I, Hartley, W, Hill, J, Hilton, M, Hinton, S, Hollowood, D, Hughes, J, James, D, Jarvis, M, Jeltema, T, Koopman, B, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Lokken, M, Maccrann, N, Madhavacheril, M, Maia, M, Mccullough, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Mohr, J, Moodley, K, Morgan, R, Myles, J, Nati, F, Navarro-Alsina, A, Niemack, M, Ogando, R, Page, L, Palmese, A, Partridge, B, Paz-Chinchon, F, Pereira, M, Pieres, A, Plazas Malagon, A, Prat, J, Raveri, M, Rodriguez-Monroy, M, Rollins, R, Romer, A, Rykoff, E, Salatino, M, Sanchez, C, Sanchez, E, Santiago, B, Scarpine, V, Schillaci, A, Secco, L, Serrano, S, Sevilla-Noarbe, I, Sheldon, E, Sherwin, B, Sifon, C, Smith, M, Soares-Santos, M, Staggs, S, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, To, C, Troxel, M, Tutusaus, I, Vavagiakis, E, Weller, J, Wollack, E, Yanny, B, Yin, B, Zhang, Y, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), Univ Penn, Univ Chicago, Univ Hawaii, Ohio State Univ, Cornell Univ, Max Planck Inst Extraterr Phys, Ludwig Maximilians Univ Munchen, NSFs Natl Opt Infrared Astron Res Lab, Lab Interinst E Astron LIneA, Argonne Natl Lab, Fermilab Natl Accelerator Lab, Stanford Univ, Univ Portsmouth, Univ Wisconsin, Inst Astrophys Paris, Sorbonne Univ, Univ Toronto, UCL, Carnegie Mellon Univ, Duke Univ, Inst Astrofis Canarias, Univ La Laguna, Natl Ctr Supercomp Applicat, Univ Illinois, Barcelona Inst Sci & Technol, Lawrence Berkeley Natl Lab, Univ Trieste, INAF Osservatorio Astron Trieste, Inst Fundamental Phys Universe, Observ Nacl, Ctr Invest Energet Medioambientales & Tecnol CIEM, Santa Cruz Inst Particle Phys, Univ Oslo, CALTECH, Inst Estudis Espacials Catalunya IEEC, CSIC, Univ Michigan, SLAC Natl Accelerator Lab, Univ Oxford, Univ Manchester, Univ Geneva, Columbia Univ, Flatiron Inst, Univ KwaZulu Natal, Univ Queensland, Rutgers State Univ, Ctr Astrophys Harvard & Smithsonian, Yale Univ, Univ Arizona, Macquarie Univ, Lowell Observ, Dunlap Inst Astron & Astrophys, Univ Cambridge, Perimeter Inst Theoret Phys, Princeton Univ, Inst Catalana Recerca & Estudis Avancats, Univ Milano Bicocca, Haverford Coll, Univ Sussex, Univ Fed Rio Grande do Sul, Brookhaven Natl Lab, Pontificia Univ Catolica Valparaiso, Univ Southampton, Oak Ridge Natl Lab, NASA, Shin, T., Jain, B., Adhikari, S., Baxter, E. J., Chang, C., Pandey, S., Salcedo, A., Weinberg, D. H., Amsellem, A., Battaglia, N., Belyakov, M., Dacunha, T., Goldstein, S., Kravtsov, A. V., Varga, T. N., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Amon, A., Andrade-Oliveira, F., Annis, J., Bacon, D., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Bocquet, S., Bond, J. R., Brooks, D., Buckley-Geer, E., Burke, D. L., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Chen, R., Choi, A., Costanzi, M., da Costa, L. N., Derose, J., Desai, S., de Vicente, J., Devlin, M. J., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferraro, S., Ferrero, I., Ferte, A., Flaugher, B., Frieman, J., Gallardo, P. A., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hartley, W. G., Hill, J. C., Hilton, M., Hinton, S. R., Hollowood, D. L., Hughes, J. P., James, D. J., Jarvis, M., Jeltema, T., Koopman, B. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lokken, M., Maccrann, N., Madhavacheril, M. S., Maia, M. A. G., Mccullough, J., Mcmahon, J., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moodley, K., Morgan, R., Myles, J., Nati, F., Navarro-Alsina, A., Niemack, M. D., Ogando, R. L. C., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchon, F., Pereira, M. E. S., Pieres, A., Plazas Malagon, A. A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Rykoff, E. S., Salatino, M., Sanchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schillaci, A., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Sherwin, B. D., Sifon, C., Smith, M., Soares-Santos, M., Staggs, S. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tutusaus, I., Vavagiakis, E. M., Weller, J., Wollack, E. J., Yanny, B., Yin, B., and Zhang, Y.
Subjects: Cold dark matter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], Cosmology: observation, Cosmology, Galaxies clusters general, observations [Cosmology], Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Cosmology observation, Physics, Cosmology: observations, Galaxies: evolution, Astronomy and Astrophysics, evolution [Galaxies], Cosmology observations, Galaxies evolution, Galaxy, Redshift, Galaxies: clusters: general, Space and Planetary Science, Atacama Cosmology Telescope, Dark energy, Halo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Shin, T., et al., We present measurements of the radial profiles of the mass and galaxy number density around Sunyaev–Zel’dovich (SZ)-selected clusters using both weak lensing and galaxy counts. The clusters are selected from the Atacama Cosmology Telescope Data Release 5 and the galaxies from the Dark Energy Survey Year 3 data set. With signal-to-noise ratio of 62 (45) for galaxy (weak lensing) profiles over scales of about 0.2–20 h Mpc, these are the highest precision measurements for SZ-selected clusters to date. Because SZ selection closely approximates mass selection, these measurements enable several tests of theoretical models of the mass and light distribution around clusters. Our main findings are: (1) The splashback feature is detected at a consistent location in both the mass and galaxy profiles and its location is consistent with predictions of cold dark matter N-body simulations. (2) The full mass profile is also consistent with the simulations. (3) The shapes of the galaxy and lensing profiles are remarkably similar for our sample over the entire range of scales, from well inside the cluster halo to the quasilinear regime. We measure the dependence of the profile shapes on the galaxy sample, redshift, and cluster mass. We extend the Diemer & Kravtsov model for the cluster profiles to the linear regime using perturbation theory and show that it provides a good match to the measured profiles. We also compare the measured profiles to predictions of the standard halo model and simulations that include hydrodynamics. Applications of these results to cluster mass estimation, cosmology, and astrophysics are discussed., The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant no. 465376/2014-2).
Published: 2021

11. C/2014 UN271(Bernardinelli-Bernstein): The Nearly Spherical Cow of Comets

Author: David J. James, R. Cawthon, H. T. Diehl, Maria E. S. Pereira, Josh Frieman, Ramon Miquel, Y.-H. Zhang, David J. Brooks, D. L. Hollowood, S. Serrano, Enrique Gaztanaga, Benjamin T. Montet, Marcelle Soares-Santos, Robert Weryk, A. Carnero Rosell, G. Tarle, R. L. C. Ogando, E. Bertin, Juan Garcia-Bellido, I. Ferrero, M. Costanzi, J. Carretero, Chun-Hao To, E. J. Sanchez, A. Roodman, Richard J. Wainscoat, A. A. Plazas Malagón, J. Gschwend, Adriano Pieres, M. A. G. Maia, M. Rodriguez-Monroy, Salcedo Romero de Ávila, A. R. Walker, M. Carrasco Kind, B. Flaugher, Gary Bernstein, Samuel Hinton, Robert Morgan, S. Everett, M. N. K. Smith, F. Andrade-Oliveira, G. Gutierrez, J. De Vicente, A. K. Romer, Pedro H. Bernardinelli, K. Kuehn, Michael Troxel, E. Suchyta, Jennifer L. Marshall, J. Annis, Michael Schubnell, O. Lahav, D. L. Burke, S. Allam, Robert A. Gruendl, C. J. Conselice, Michel Aguena, I. Sevilla-Noarbe, N. Kuropatkin, T. N. Varga, L. N. da Costa, Felipe Menanteau, K. Honscheid, M. E. C. Swanson, F. Paz-Chinchón, Daniel Gruen, D. W. Gerdes, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), UAM. Departamento de Física Teórica, University of Pennsylvania, University of New South Wales, University of Western Ontario, University of Hawaii, Laboratório Interinstitucional de E-Astronomia - LIneA, Fermi National Accelerator Laboratory, Universidade Estadual Paulista (UNESP), Universidad Autonoma de Madrid, Institut d'Astrophysique de Paris, University College London, Stanford University, SLAC National Accelerator Laboratory, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Barcelona Institute of Science and Technology, University of Wisconsin-Madison, University of Manchester, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, Universitat Hamburg, Medioambientales y Tecnológicas (CIEMAT), Santa Cruz Institute for Particle Physics, University of Oslo, University of Chicago, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Ludwig-Maximilians-Universitat, University of Queensland, Ohio State University, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Texas A and M University, Institució Catalana de Recerca i Estudis Avancats, University of Cambridge, Peyton Hall, University of Sussex, University of Southampton, Oak Ridge National Laboratory, 382 Via Pueblo Mall, Duke University, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universitat München, NSF's National Optical-Infrared Astronomy Research Laboratory, Bernardinelli, P. H., Bernstein, G. M., Montet, B. T., Weryk, R., Wainscoat, R., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Kind, M. C., Carretero, J., Cawthon, R., Conselice, C., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Ogando, R. L. C., Paz-Chinchon, F., Pieres, A., Malagon, A. A. P., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Troxel, M. A., Varga, T. N., Walker, A. R., and Zhang, Y.
Subjects: Rotation period, Absolute magnitude, Brightness, Long period comets, Small Solar System bodies, Comet nuclei, Comet dynamics, Comet origins, 933, 1469, 2160, 2213, 2203, Astrophysics - Earth and Planetary Astrophysics, Comet, FOS: Physical sciences, Astrophysics, 01 natural sciences, Comet origin, Long Period Comets (933), Geometric albedo, 0103 physical sciences, Comet Nuclei (2160), Surface brightness, 010303 astronomy & astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Long period comet, Small Solar System Bodies (1469), 05 social sciences, Uranus, 050301 education, Física, Astronomy and Astrophysics, Comet dynamic, Radiative equilibrium, Small Solar System bodie, Comet Dynamics (2213), Comet Origins (2203), Space and Planetary Science, 0503 education
Abstract: Comet C/2014 UN271 (Bernardinelli-Bernstein), incoming from the Oort cloud, is remarkable in having the brightest (and presumably largest) nucleus of any well-measured comet and having been discovered at the heliocentric distance r h ≈ 29 au, farther than any Oort cloud comet. In this work, we describe the discovery process and observations and the properties that can be inferred from images recorded until the first reports of activity in 2021 June. The orbit has i = 95°, with a perihelion of 10.97 au to be reached in 2031 and a previous aphelion at 40,400 ± 260 au. Backward integration of the orbit under a standard Galactic tidal model and known stellar encounters suggests a perihelion of q ≈ 18 au on its previous perihelion passage 3.5 Myr ago; hence, the current data could be the first ever obtained of a comet that has not been inside Uranus's orbit in 4 Gyr. The photometric data show an unresolved nucleus with absolute magnitude H r = 8.0, colors that are typical of comet nuclei or Damocloids, and no secular trend as it traversed the range 34-23 au. For the r-band geometric albedo p r , this implies a diameter of km. There is strong evidence of brightness fluctuations at the ±0.2 mag level, but no rotation period can be discerned. A coma, nominally consistent with a "stationary"1/ρ surface brightness distribution, grew in scattering cross section at an exponential rate from A f ρ ≈ 1 to ≈150 m as the comet approached from 28 to 20 au. The activity rate is consistent with a very simple model of sublimation of a surface species in radiative equilibrium with the Sun. The inferred enthalpy of sublimation matches those of CO2 and NH3. More volatile species, such as N2, CH4, and CO, must be far less abundant on the sublimating surfaces., The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007–2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).
Published: 2021

12. DES Y1 results: Splitting growth and geometry to test $\Lambda$CDM

Author: Muir, J., Baxter, E., Miranda, V, Doux, C., Ferte, A., Leonard, C. D., Huterer, D., Jain, B., Lemos, P., Raveri, M., Nadathur, S., Campos, A. [UNESP], Chen, A., Dodelson, S., Elvin-Poole, J., Lee, S., Secco, L. F., Troxel, M. A., Weaverdyck, N., Zuntz, J., Brout, D., Choi, A., Crocce, M., Davis, T. M., Gruen, D., Krause, E., Lidman, C., MacCrann, N., Moller, A., Prat, J., Ross, A. J., Sako, M., Samuroff, S., Sanchez, C., Scolnic, D., Zhang, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Burke, D. L., Carnero Rosell, A., Kind, M. Carrasco, Carretero, J., Cawthon, R., Costanzi, M., Costa, L. N. da, Pereira, M. E. S., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Estrada, J., Everett, S., Evrard, A. E., Ferrero, I, Flaugher, B., Frieman, J., Garcia-Bellido, J., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Menanteau, F., Miquel, R., Morgan, R., Myles, J., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V, Serrano, S., Sevilla-Noarbe, I, Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Weller, J., Wilkinson, R. D., DES Collaboration, Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), Stanford University, University of Hawaii, University of Arizona, University of Pennsylvania, California Institute of Technology, Newcastle University, University of Michigan, University College London, University of Chicago, University of Portsmouth, Carnegie Mellon University, Universidade Estadual Paulista (UNESP), Ohio State University, Duke University, University of Edinburgh, Harvard and Smithsonian, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE-CSIC, University of Queensland, 382 Via Pueblo Mall, SLAC National Accelerator Laboratory, Australian National University, LPC, NSF's National Optical-Infrared Astronomy Research Laboratory, Universidade de São Paulo (USP), Laboratório Interinstitucional de E-Astronomia-LIneA, Fermi National Accelerator Laboratory, Universidad Autonoma de Madrid, Institut d'Astrophysique de Paris, University of Sussex, University of Manchester, Instituto de Astrofisica de Canarias, Universidad de la Laguna, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, Barcelona Institute of Science and Technology, University of Wisconsin-Madison, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, IIT Hyderabad, Ludwig-Maximilians-Universität, Santa Cruz Institute for Particle Physics, University of Oslo, University of Cambridge, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universität München, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Institució Catalana de Recerca i Estudis Avançats, Peyton Hall, Medioambientales y Tecnológicas (CIEMAT), University of Southampton, Oak Ridge National Laboratory, Stanford Univ, Univ Hawaii, Univ Arizona, Univ Penn, CALTECH, Newcastle Univ, Univ Michigan, UCL, Univ Chicago, Univ Portsmouth, Carnegie Mellon Univ, Universidade Estadual Paulista (Unesp), Ohio State Univ, Duke Univ, Univ Edinburgh, Harvard & Smithsonian, Inst Estudis Espacials Catalunya IEEC, CSIC, Univ Queensland, SLAC Natl Accelerator Lab, Australian Natl Univ, Univ Clermont Auvergne, Cerro Tololo Interamer Observ, Lab Interinst E Astron LIneA, Fermilab Natl Accelerator Lab, Univ Autonoma Madrid, Inst Astrophys Paris, Sorbonne Univ, Univ Sussex, Univ Manchester, Inst Astrofis Canarias, Univ La Laguna, Univ Illinois, Natl Ctr Supercomp Applicat, Barcelona Inst Sci & Technol, Univ Wisconsin, INAF Osservatorio Astron Trieste, Inst Fundamental Phys Universe, Observ Nacl, Ludwig Maximilians Univ Munchen, Santa Cruz Inst Particle Phys, Univ Oslo, Univ Cambridge, Max Planck Inst Extraterr Phys, Macquarie Univ, Lowell Observ, Inst Catalana Recerca & Estudis Avancats, Princeton Univ, Ctr Invest Energet Medioambientales & Tecnol CIEM, Univ Southampton, Oak Ridge Natl Lab, UAM. Departamento de Física Teórica, Muir, J., Baxter, E., Miranda, V., Doux, C., Ferte, A., Leonard, C. D., Huterer, D., Jain, B., Lemos, P., Raveri, M., Nadathur, S., Campos, A., Chen, A., Dodelson, S., Elvin-Poole, J., Lee, S., Secco, L. F., Troxel, M. A., Weaverdyck, N., Zuntz, J., Brout, D., Choi, A., Crocce, M., Davis, T. M., Gruen, D., Krause, E., Lidman, C., Maccrann, N., Moller, A., Prat, J., Ross, A. J., Sako, M., Samuroff, S., Sanchez, C., Scolnic, D., Zhang, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cawthon, R., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Estrada, J., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Menanteau, F., Miquel, R., Morgan, R., Myles, J., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Weller, J., and Wilkinson, R. D.
Subjects: General relativity, Cosmological parameters, Geometry, Astrophysics::Cosmology and Extragalactic Astrophysics, Lambda, Sky surveys, 01 natural sciences, Omega, Evolution of the Universe, Cosmology, Cosmic microwave background, Cosmologial constant, symbols.namesake, 0103 physical sciences, Dark energy, RADIAÇÃO DE FUNDO, Astrophysical studies of gravity, Weak, Large-scale structure of the Universe, Planck, 010306 general physics, Weak gravitational lensing, Gravitational Lensing, Physics, 010308 nuclear & particles physics, Física, symbols, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Muir, J., et al. (DES Collaboration), We analyze Dark Energy Survey (DES) data to constrain a cosmological model where a subset of parameters - focusing on ωm - are split into versions associated with structure growth (e.g., ωmgrow) and expansion history (e.g., ωmgeo). Once the parameters have been specified for the ΛCDM cosmological model, which includes general relativity as a theory of gravity, it uniquely predicts the evolution of both geometry (distances) and the growth of structure over cosmic time. Any inconsistency between measurements of geometry and growth could therefore indicate a breakdown of that model. Our growth-geometry split approach therefore serves both as a (largely) model-independent test for beyond-ΛCDM physics, and as a means to characterize how DES observables provide cosmological information. We analyze the same multiprobe DES data as [Phys. Rev. Lett. 122, 171301 (2019)PRLTAO0031-900710.1103/PhysRevLett.122.171301]: DES Year 1 (Y1) galaxy clustering and weak lensing, which are sensitive to both growth and geometry, as well as Y1 BAO and Y3 supernovae, which probe geometry. We additionally include external geometric information from BOSS DR12 BAO and a compressed Planck 2015 likelihood, and external growth information from BOSS DR12 RSD. We find no significant disagreement with ωmgrow=ωmgeo. When DES and external data are analyzed separately, degeneracies with neutrino mass and intrinsic alignments limit our ability to measure ωmgrow, but combining DES with external data allows us to constrain both growth and geometric quantities. We also consider a parametrization where we split both ωm and w, but find that even our most constraining data combination is unable to separately constrain ωmgrow and wgrow. Relative to ΛCDM, splitting growth and geometry weakens bounds on σ8 but does not alter constraints on h., The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2).
Published: 2021
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13. Constraints on dark matter to dark radiation conversion in the late universe with DES-Y1 and external data

Author: Chen, Angela, Huterer, Dragan, Lee, Sujeong, Ferté, Agnès, Weaverdyck, Noah, Alves, Otavio Alonso, Leonard, C. Danielle, MacCrann, Niall, Raveri, Marco, Porredon, Anna, Di Valentino, Eleonora, Muir, Jessica, Lemos, Pablo, Liddle, Andrew, Blazek, Jonathan, Campos, Andresa, Cawthon, Ross, Choi, Ami, Dodelson, Scott, Elvin-Poole, Jack, Gruen, Daniel, Ross, Ashley, Secco, Lucas F., Sevilla, Ignacio, Sheldon, Erin, Troxel, Michael A., Zuntz, Joe, Abbott, Tim, Aguena, Michel, Allam, Sahar, Annis, James, Avila, Santiago, Bertin, Emmanuel, Bhargava, Sunayana, Bridle, Sarah, Brooks, David, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, Costanzi, Matteo, Crocce, Martin, da Costa, Luiz, Pereira, Maria Elidaiana da Silva, Davis, Tamara, Doel, Peter, Eifler, Tim, Ferrero, Ismael, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Gerdes, David, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hinton, Samuel, Hollowood, Devon L., Honscheid, Klaus, Hoyle, Ben, James, David, Jarvis, Mike, Kuehn, Kyler, Lahav, Ofer, Maia, Marcio, Marshall, Jennifer, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Palmese, Antonella, Paz-Chinchon, Francisco, Malagón, Andrés Plazas, Roodman, Aaron, Sanchez, Eusebio, Scarpine, Vic, Schubnell, Michael, Serrano, Santiago, Smith, Mathew, Suchyta, Eric, Tarle, Gregory, Thomas, Daniel, To, Chun-Hao, Varga, Tamas Norbert, Weller, Jochen, Wilkinson, Reese, UAM. Departamento de Física Teórica, National Science Foundation (US), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, University of Michigan, Duke University, California Institute of Technology, Universidade Estadual Paulista (UNESP), Newcastle Unviersity, Ohio State University, University of Chicago, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), University of Manchester, Stanford University, University College London, Universidade de Lisboa, University of Edinburgh, Perimeter Institute for Theoretical Physics, Observatoire de Sauverny, Carnegie Mellon University, University of Wisconsin-Madison, 382 Via Pueblo Mall, Menlo Park, University of Pennsylvania, Medioambientales y Tecnológicas (CIEMAT), Brookhaven National Laboratory, NSF's National Optical-Infrared Astronomy Research Laboratory, Universidade de São Paulo (USP), LIneA, Fermi National Accelerator Laboratory, Universidad Autonoma de Madrid, Institut d'Astrophysique de Paris, University of Sussex, Instituto de Astrofisica de Canarias, Dpto. Astrofísica, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, Barcelona Institute of Science and Technology, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Queensland, University of Arizona, University of Oslo, Santa Cruz Institute for Particle Physics, Ludwig-Maximilians-Universität, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universität München, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Texas AandM University, Institució Catalana de Recerca i Estudis Avançats, University of Cambridge, Peyton Hall, University of Southampton, Oak Ridge National Laboratory, University of Portsmouth, Chen, Angela, Huterer, Dragan, Lee, Sujeong, Ferté, Agnè, Weaverdyck, Noah, Alonso Alves, Otavio, Leonard, C. Danielle, Maccrann, Niall, Raveri, Marco, Porredon, Anna, Di Valentino, Eleonora, Muir, Jessica, Lemos, Pablo, Liddle, Andrew, Blazek, Jonathan, Campos, Andresa, Cawthon, Ro, Choi, Ami, Dodelson, Scott, Elvin-Poole, Jack, Gruen, Daniel, Ross, Ashley, Secco, Lucas F., Sevilla, Ignacio, Sheldon, Erin, Troxel, Michael A., Zuntz, Joe, Abbott, Tim, Aguena, Michel, Allam, Sahar, Annis, Jame, Avila, Santiago, Bertin, Emmanuel, Bhargava, Sunayana, Bridle, Sarah, Brooks, David, Carnero Rosell, Aurelio, Carrasco Kind, Matia, Carretero, Jorge, Costanzi, Matteo, Crocce, Martin, da Costa, Luiz, Elidaiana da Silva Pereira, Maria, Davis, Tamara, Doel, Peter, Eifler, Tim, Ferrero, Ismael, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Gerdes, David, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hinton, Samuel, Hollowood, Devon L., Honscheid, Klau, Hoyle, Ben, James, David, Jarvis, Mike, Kuehn, Kyler, Lahav, Ofer, Maia, Marcio, Marshall, Jennifer, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Palmese, Antonella, Paz-Chinchon, Francisco, Plazas Malagón, André, Roodman, Aaron, Sanchez, Eusebio, Scarpine, Vic, Schubnell, Michael, Serrano, Santiago, Smith, Mathew, Suchyta, Eric, Tarle, Gregory, Thomas, Daniel, Chun-Hao, To, Varga, Tamas Norbert, Weller, Jochen, and Wilkinson, Reese
Subjects: matter: power spectrum, Cosmic microwave background, cosmic background radiation: polarization, Astrophysics, power spectrum, 01 natural sciences, Cosmology, hubble constant, High Energy Physics - Phenomenology (hep-ph), Scale Structure, cosmological model: parameter space, Power Spectrum, Dark energy, Astrophysics - Cosmology and Nongalactic Astrophysic, Large-scale structure of the Universe, 010303 astronomy & astrophysics, media_common, Physics, Energy, massive neutrinos, Hubble Constant, tension, Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology, halo-model, statistics, dark energy: density, Dark radiation, symbols, Halo-Model, energy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Dark matter, Cosmological parameters, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter: density, galaxy formation, Evolution of the Universe, symbols.namesake, scale structure, 0103 physical sciences, supernova, Galaxy formation and evolution, Self-Interactions, Massive Neutrinos, STFC, Sdss, 010308 nuclear & particles physics, RCUK, resolution, Física, self-interactions, inconsistent, Universe, cosmic background radiation: temperature, 13. Climate action, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Galaxy Formation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], sdss, Hubble's law
Abstract: Chen, A., et al. DES Collaboration, We study a phenomenological class of models where dark matter converts to dark radiation in the low redshift epoch. This class of models, dubbed DMDR, characterizes the evolution of comoving dark-matter density with two extra parameters, and may be able to help alleviate the observed discrepancies between early and late-time probes of the Universe. We investigate how the conversion affects key cosmological observables such as the cosmic microwave background (CMB) temperature and matter power spectra. Combining 3x2pt data from Year 1 of the Dark Energy Survey, Planck-2018 CMB temperature and polarization data, supernovae (SN) Type Ia data from Pantheon, and baryon acoustic oscillation (BAO) data from BOSS DR12, MGS and 6dFGS, we place new constraints on the amount of dark matter that has converted to dark radiation and the rate of this conversion. The fraction of the dark matter that has converted since the beginning of the Universe in units of the current amount of dark matter, ζ, is constrained at 68% confidence level to be, he DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (Grant No. FP7/2007-2013) including ERC Grants Agreement No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2).
Published: 2021
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14. Dark Energy Survey Year 3 results: Curved-sky weak lensing mass map reconstruction

Author: Sunayana Bhargava, Jennifer L. Marshall, David J. Brooks, Carlos Solans Sanchez, G. Tarle, Samuel Hinton, G. Gutierrez, Alexandra Amon, Peter Doel, Ami Choi, Ben Hoyle, Marco Raveri, B. Flaugher, F. Andrade-Oliveira, Jochen Weller, R. P. Rollins, H. T. Diehl, D. L. Burke, Felipe Menanteau, Alex Drlica-Wagner, J. DeRose, F. J. Castander, David Bacon, E. Suchyta, Dragan Huterer, Christopher J. Conselice, Brian Yanny, Jack Elvin-Poole, U. Demirbozan, Maria E. S. Pereira, Niall MacCrann, Keith Bechtol, Erin Sheldon, Martin Crocce, V. Scarpine, T. M. C. Abbott, Peter Melchior, D. L. Hollowood, S. Serrano, Agnès Ferté, J. De Vicente, J. Cordero, P. F. Leget, A. Campos, Eli S. Rykoff, C. Doux, Chun-Hao To, E. J. Sanchez, K. Herner, F. Paz-Chinchón, J. Carretero, Antonella Palmese, Marcos Lima, J. Myles, I. Harrison, G. Pollina, A. Roodman, David J. James, Tommaso Giannantonio, D. Zeurcher, M. A. G. Maia, M. Rodriguez-Monroy, Joe Zuntz, A. Alarcon, B. Yin, S. Allam, Robert A. Gruendl, A. Kovács, Matthew R. Becker, Pablo Fosalba, B. Mawdsley, Ashley J. Ross, S. Pandey, J. Muir, Joseph J. Mohr, Michael Troxel, I. Ferrero, Matt J. Jarvis, A. Carnero Rosell, J. McCullough, P. Vielzeuf, Yanxi Zhang, Seshadri Nadathur, M. Carrasco Kind, M. March, S. Everett, M. Smith, M. Costanzi, Jean-Luc Starck, Daniel Gruen, I. Tutusaus, Francois Lanusse, Chihway Chang, Daniel Thomas, J. Prat, L. Whiteway, F. Elsner, S. Desai, I. Sevilla-Noarbe, M. Soares-Santos, G. Giannini, W. G. Hartley, D. W. Gerdes, R. Cawthon, N. Kuropatkin, Ramon Miquel, K. D. Eckert, T. N. Varga, L. N. da Costa, J. P. Dietrich, Juan Garcia-Bellido, E. Bertin, E. M. Huff, R. Chen, Michel Aguena, Enrique Gaztanaga, R. L. C. Ogando, Bhuvnesh Jain, M Gatti, Ofer Lahav, Niall Jeffrey, Robert Morgan, L. F. Secco, Nico Hamaus, A. A. Plazas, A. Navarro-Alsina, T. Shin, T. Kacprzak, C. Davis, J. Gschwend, Gary Bernstein, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), University of Portsmouth, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Jeffrey, N., Gatti, M., Chang, C., Whiteway, L., Demirbozan, U., Kovacs, A., Pollina, G., Bacon, D., Hamaus, N., Kacprzak, T., Lahav, O., Lanusse, F., Mawdsley, B., Nadathur, S., Starck, J. L., Vielzeuf, P., Zeurcher, D., Alarcon, A., Amon, A., Bechtol, K., Bernstein, G. M., Campos, A., Rosell, A. C., Kind, M. C., Cawthon, R., Chen, R., Choi, A., Cordero, J., Davis, C., Derose, J., Doux, C., Drlica-Wagner, A., Eckert, K., Elsner, F., Elvin-Poole, J., Everett, S., Ferte, A., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Kuropatkin, N., Jarvis, M., Leget, P. F., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Pandey, S., Prat, J., Raveri, M., Rollins, R. P., Ross, A. J., Rykoff, E. S., Sanchez, C., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troxel, M. A., Tutusaus, I., Varga, T. N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Becker, M. R., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carretero, J., Castander, F. J., Conselice, C., Costanzi, M., Crocce, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Hoyle, B., Jain, B., James, D. J., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Rodriguez-Monroy, M., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Weller, J., Université de Paris, University College London, Barcelona Institute of Science and Technology, University of Pennsylvania, University of Chicago, Calle Viá Láctea, Universidad de La Laguna (ULL), Ludwig-Maximilians Universität München, ETH Zurich, Argonne National Laboratory, Stanford University, University of Wisconsin-Madison, CarnegieMellon University, Instituto de Astrofisica de Canarias, Laboratorio Interinstitucional de e-Astronomia-LIneA, Dpto. Astrofisica, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Duke University, Ohio State University, University of Manchester, University of California,Berkeley, Santa Cruz Institute for Particle Physics, Fermi National Accelerator Laboratory, California Institute of Technology, SLAC National Accelerator Laboratory, Denys Wilkinson Building, University of Geneva, University of Michigan, University of Cambridge, Universidade Estadual de Campinas (UNICAMP), Medioambientales y Tecnologicas (CIEMAT), Brookhaven National Laboratory, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), Max Planck Institute for Extraterrestrial Physics, University of Edinburgh, NSF's National Optical-Infrared Astronomy Research Laboratory, Universidade de Saõ Paul, Universidade Estadual Paulista (UNESP), Institut d'Astrophysique deParis, Institut d'Astrophysique de Paris, University of Sussex, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, IIT Hyderabad, Ludwig-Maximilians-Universitat, University of Oslo, Universidad Autonoma de Madrid, University of Queensland, Center for Astrophysics | Harvard and Smithsonian, Texas A and M University, Princeton University, Institucio Catalana de Recerca i Estudis Avancats, University of Southampton, Oak Ridge National Laboratory, and Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris)
Subjects: statistical [Methods], Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Gravitational lensing: weak, 0103 physical sciences, Prior probability, Maximum a posteriori estimation, 010303 astronomy & astrophysics, STFC, Weak gravitational lensing, Methods: statistical, media_common, Physics, ST/M001334/1, 010308 nuclear & particles physics, RCUK, Astronomy and Astrophysics, Celestial sphere, gravitational lensing: Weak, large-scale structure of Universe, methods: Statistical, ST/R000476/1, Galaxy, Space and Planetary Science, Sky, astro-ph.CO, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], weak [Gravitational lensing], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Jeffrey, N., et al. DES Collaboration, We present reconstructed convergence maps, mass maps, from the Dark Energy Survey (DES) third year (Y3) weak gravitational lensing data set. The mass maps are weighted projections of the density field (primarily dark matter) in the foreground of the observed galaxies. We use four reconstruction methods, each is a maximum a posteriori estimate with a different model for the prior probability of the map: Kaiser–Squires, null B-mode prior, Gaussian prior, and a sparsity prior. All methods are implemented on the celestial sphere to accommodate the large sky coverage of the DES Y3 data. We compare the methods using realistic ΛCDM simulations with mock data that are closely matched to the DES Y3 data. We quantify the performance of the methods at the map level and then apply the reconstruction methods to the DES Y3 data, performing tests for systematic error effects. The maps are compared with optical foreground cosmic-web structures and are used to evaluate the lensing signal from cosmic-void profiles. The recovered dark matter map covers the largest sky fraction of any galaxy weak lensing map to date., The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This paper has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. NJ has been supported by funding from l’Ecole Normale Supérieure, Paris. OL and NJ acknowledge support from a European Research Council Advanced Grant TESTDE (FP7/291329) and STFC Consolidated Grants ST/M001334/1 and ST/R000476/1. AK has been supported by a Juan de la Cierva fellowship from MINECO with project number IJC2018-037730-I, and funding for this project was also available in part through SEV-2015-0548 and AYA2017-89891-P. Cosmic voids computational work has been performed on the UK SCIAMA High Performance Computing cluster supported by the ICG, SEPNet, and the University of Portsmouth.
Published: 2021
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15. CHARA array adaptive optics: complex operational software and performance

Author: T. ten Brummelaar, Douglas R. Gies, Laszlo Sturmann, Denis Mourard, Matthew D. Anderson, Philippe Berio, Cyril Petit, John Monnier, Stefan Kraus, C. B. Lim, Michel Tallon, Michael J. Ireland, Norm Vargas, Judit Sturmann, Chris Farrington, Stephen T. Ridgway, Narsireddy Anugu, Jean Baptiste Le Bouquin, Olli Majoinen, Gail H. Schaefer, Nils H. Turner, Steward Observatory, University of Arizona, Georgia State University, University System of Georgia (USG), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Australian National University (ANU), University of Michigan [Ann Arbor], University of Michigan System, Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), NSF’s National Optical-Infrared Astronomy Research Laboratory (NOIRLab), School of Physics and Astronomy [Exeter], University of Exeter, DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), DOTA, ONERA, Université Paris Saclay [Châtillon], Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)
Subjects: Physics - Instrumentation and Detectors, CHARA, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Active galactic nucleus, Computer science, Young stellar object, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, EMCCD, 01 natural sciences, CHARA array, law.invention, 010309 optics, Telescope, [SPI]Engineering Sciences [physics], Software, Optics, Wavefront sensor, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Sensitivity (control systems), Adaptive optics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Throughput (business), ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Shack-Hartmann, Long baseline interferometry, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, business
Abstract: The CHARA Array is the longest baseline optical interferometer in the world. Operated with natural seeing, it has delivered landmark sub-milliarcsecond results in the areas of stellar imaging, binaries, and stellar diameters. However, to achieve ambitious observations of faint targets such as young stellar objects and active galactic nuclei, higher sensitivity is required. For that purpose, adaptive optics are developed to correct atmospheric turbulence and non-common path aberrations between each telescope and the beam combiner lab. This paper describes the AO software and its integration into the CHARA system. We also report initial on-sky tests that demonstrate an increase of scientific throughput by sensitivity gain and by extending useful observing time in worse seeing conditions. Our 6 telescopes and 12 AO systems with tens of critical alignments and control loops pose challenges in operation. We describe our methods enabling a single scientist to operate the entire system., Comment: SPIE, Optical and Infrared Interferometry and Imaging VII, Proceedings Volume 11446, 1144622, Dec 14, 2020 "See, https://doi.org/10.1117/12.2561560"
Published: 2020
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16. COLDz: A High Space Density of Massive Dusty Starburst Galaxies ~1 Billion Years after the Big Bang

Author: Emanuele Daddi, Peter Capak, Chelsea E. Sharon, Manuel Aravena, Dominik A. Riechers, Fabian Walter, Pierre Cox, Jacqueline Hodge, Jeff Wagg, Chris Carilli, Elisabete da Cunha, Riccardo Pavesi, Roberto Decarli, Helmut Dannerbauer, Rob Ivison, Roberto Neri, Mark Dickinson, Ian Smail, Department of Astronomy [Ithaca], Cornell University [New York], Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, European Southern Observatory (ESO), Yale-NUS College, Department of Physics [Durham University], Durham University, Universidad Diego Portales [Santiago] (UDP), Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA, National Radio Astronomy Observatory [Socorro] (NRAO), National Radio Astronomy Observatory (NRAO), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Research School of Astronomy and Astrophysics [Canberra] (RSAA), Australian National University (ANU), Instituto de Astrofisica de Canarias (IAC), NSF’s National Optical-Infrared Astronomy Research Laboratory (NOIRLab), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), SKA Organization, Lower Withington Macclesfield, and Universiteit Leiden
Subjects: Physics, [PHYS]Physics [physics], Active galactic nucleus, 010504 meteorology & atmospheric sciences, Star formation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Billion years, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Submillimetre astronomy, 13. Climate action, Space and Planetary Science, Observational cosmology, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Galaxy formation and evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: We report the detection of CO($J$=2$\to$1) emission from three massive dusty starburst galaxies at $z$$>$5 through molecular line scans in the NSF's Karl G. Jansky Very Large Array (VLA) CO Luminosity Density at High Redshift (COLDz) survey. Redshifts for two of the sources, HDF 850.1 ($z$=5.183) and AzTEC-3 ($z$=5.298), were previously known. We revise a previous redshift estimate for the third source GN10 ($z$=5.303), which we have independently confirmed through detections of CO $J$=1$\to$0, 5$\to$4, 6$\to$5, and [CII] 158 $��$m emission with the VLA and the NOrthern Extended Milllimeter Array (NOEMA). We find that two currently independently confirmed CO sources in COLDz are "optically dark", and that three of them are dust-obscured galaxies at $z$$>$5. Given our survey area of $\sim$60 arcmin$^2$, our results appear to imply a $\sim$6-55 times higher space density of such distant dusty systems within the first billion years after the Big Bang than previously thought. At least two of these $z$$>$5 galaxies show star-formation rate surface densities consistent with so-called "maximum" starbursts, but we find significant differences in CO excitation between them. This result may suggest that different fractions of the massive gas reservoirs are located in the dense, star-forming nuclear regions - consistent with the more extended sizes of the [CII] emission compared to the dust continuum and higher [CII]-to-far-infrared luminosity ratios in those galaxies with lower gas excitation. We thus find substantial variations in the conditions for star formation between $z$$>$5 dusty starbursts, which typically have dust temperatures $\sim$57%$\pm$25% warmer than starbursts at $z$=2-3 due to their enhanced star formation activity., 30 pages, 15 figures, 8 tables, to appear in ApJ (accepted April 21, 2020) [v2: fixed one latex issue and a few typos, no content changes]
Published: 2020
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17. The Dark Side of Pluto

Author: William B. McKinnon, Jeffrey M. Moore, Leslie A. Young, John R. Spencer, Tod R. Lauer, Kirby Runyon, Harold A. Weaver, Tanguy Bertrand, Catherine B. Olkin, Ross A. Beyer, Kimberly Ennico, S. Alan Stern, Oliver L. White, NSF’s National Optical-Infrared Astronomy Research Laboratory (NOIRLab), Southwest Research Institute [Boulder] (SwRI), NASA Ames Research Center (ARC), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), McDonnell Center for Space Sciences, and Washington University in Saint Louis (WUSTL)
Subjects: Sunlight, Moonlight, Haze, 0211 other engineering and technologies, Flux, Astronomy, Astronomy and Astrophysics, 02 engineering and technology, Albedo, 01 natural sciences, Pluto, Atmosphere, Geophysics, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), 010303 astronomy & astrophysics, Southern Hemisphere, Geology, 021101 geological & geomatics engineering
Abstract: International audience; During its departure from Pluto, New Horizons used its LORRI camera to image a portion of Pluto's southern hemisphere that was in a decades-long seasonal winter darkness, but still very faintly illuminated by sunlight reflected by Charon. Recovery of this faint signal was technically challenging. The bright ring of sunlight forwardscattered by haze in the Plutonian atmosphere encircling the nightside hemisphere was severely overexposed, defeating the standard smeared-charge removal required for LORRI images. Reconstruction of the overexposed portions of the raw images, however, allowed adequate corrections to be accomplished. The small solar elongation of Pluto during the departure phase also generated a complex scattered-sunlight background in the images that was three orders of magnitude stronger than the estimated Charon-light flux (the Charon-light flux is similar to the flux of moonlight on Earth a few days before first quarter). A model background image was constructed for each Pluto image based on principal component analysis applied to an ensemble of scattered-sunlight images taken at identical Sun−spacecraft geometry to the Pluto images. The recovered Charon-light image revealed a high-albedo region in the southern hemisphere. We argue that this may be a regional deposit of N 2 or CH 4 ice. The Charon-light image also shows that the south polar region currently has markedly lower albedo than the north polar region of Pluto, which may reflect the sublimation of N 2 ice or the deposition of haze particulates during the recent southern summer.
Published: 2021
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18. A dormant overmassive black hole in the early Universe.

Author: Juodžbalis I, Maiolino R, Baker WM, Tacchella S, Scholtz J, D'Eugenio F, Witstok J, Schneider R, Trinca A, Valiante R, DeCoursey C, Curti M, Carniani S, Chevallard J, de Graaff A, Arribas S, Bennett JS, Bourne MA, Bunker AJ, Charlot S, Jiang B, Koudmani S, Perna M, Robertson B, Sijacki D, Übler H, Williams CC, and Willott C
Abstract: Recent observations have found a large number of supermassive black holes already in place in the first few hundred million years after the Big Bang, many of which seem to be overmassive relative to their host galaxy stellar mass when compared with local relation 1-9 . Several different models have been proposed to explain these findings, ranging from heavy seeds to light seeds experiencing bursts of high accretion rate 10-16 . Yet, current datasets are unable to differentiate between these various scenarios. Here we report the detection, from the JADES survey, of broad Hα emission in a galaxy at z = 6.68, which traces a black hole with a mass of about 4 × 10 8 M ⊙ and accreting at a rate of only 0.02 times the Eddington limit. The black hole to host galaxy stellar mass ratio is about 0.4-that is, about 1,000 times above the local relation-whereas the system is closer to the local relations in terms of dynamical mass and velocity dispersion of the host galaxy. This object is most likely an indication of a much larger population of dormant black holes around the epoch of reionization. Its properties are consistent with scenarios in which short bursts of super-Eddington accretion have resulted in black hole overgrowth and massive gas expulsion from the accretion disk; in between bursts, black holes spend most of their life in a dormant state., Competing Interests: Competing interests: The authors declare no competing interests., (© 2024. The Author(s).)
Published: 2024
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19. Accelerated formation of ultra-massive galaxies in the first billion years.

Author: Xiao M, Oesch PA, Elbaz D, Bing L, Nelson EJ, Weibel A, Illingworth GD, van Dokkum P, Naidu RP, Daddi E, Bouwens RJ, Matthee J, Wuyts S, Chisholm J, Brammer G, Dickinson M, Magnelli B, Leroy L, Schaerer D, Herard-Demanche T, Lim S, Barrufet L, Endsley R, Fudamoto Y, Gómez-Guijarro C, Gottumukkala R, Labbé I, Magee D, Marchesini D, Maseda M, Qin Y, Reddy NA, Shapley A, Shivaei I, Shuntov M, Stefanon M, Whitaker KE, and Wyithe JSB
Abstract: Recent James Webb Space Telescope (JWST) observations have revealed an unexpected abundance of massive-galaxy candidates in the early Universe, extending further in redshift and to lower luminosity than what had previously been found by submillimetre surveys 1-6 . These JWST candidates have been interpreted as challenging the Λ cold dark-matter cosmology (where Λ is the cosmological constant) 7-9 , but, so far, these studies have mostly relied on only rest-frame ultraviolet data and have lacked spectroscopic confirmation of their redshifts 10-16 . Here we report a systematic study of 36 massive dust-obscured galaxies with spectroscopic redshifts between 5 and 9 from the JWST FRESCO survey. We find no tension with the Λ cold dark-matter model in our sample. However, three ultra-massive galaxies (logM ★ /M ⊙ ≳ 11.0, where M ★ is the stellar mass and M ⊙ is the mass of the Sun) require an exceptional fraction of 50 per cent of baryons converted into stars-two to three times higher than the most efficient galaxies at later epochs. The contribution from an active galactic nucleus is unlikely because of their extended emission. Ultra-massive galaxies account for as much as 17 per cent of the total cosmic star-formation-rate density 17 at redshifts between about five and six., Competing Interests: Competing interests The authors declare no competing interests., (© 2024. The Author(s), under exclusive licence to Springer Nature Limited.)
Published: 2024
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20. Using JADES NIRCam photometry to investigate the dependence of stellar mass inferences on the IMF in the early universe.

Author: Woodrum C, Rieke M, Ji Z, Baker WM, Bhatawdekar R, Bunker AJ, Charlot S, Curtis-Lake E, Eisenstein DJ, Hainline K, Hausen R, Helton JM, Hviding RE, Johnson BD, Robertson B, Sun F, Tacchella S, Whitler L, Williams CC, and Willmer CNA
Abstract: The detection of numerous and relatively bright galaxies at redshifts z > 9 has prompted new investigations into the star-forming properties of high-redshift galaxies. Using local forms of the initial mass function (IMF) to estimate stellar masses of these galaxies from their light output leads to galaxy masses that are at the limit allowed for the state of the Lambda Cold Dark Matter (ΛCDM) Universe at their redshift. We explore how varying the IMF assumed in studies of galaxies in the early universe changes the inferred values for the stellar masses of these galaxies. We infer galaxy properties with the spectral energy distribution (SED) fitting code Prospector using varying IMF parameterizations for a sample of 102 galaxies with photometry from the James Webb Space Telescope, JWST Advanced Deep Extragalactic Survey that are spectroscopically confirmed to be at [Formula: see text], with additional photometry from the JWST Extragalactic Medium Band Survey for twenty-one of the galaxies. We demonstrate that models with stellar masses reduced by a factor of three or more do not affect the modeled SED., Competing Interests: Competing interests statement:The authors declare no competing interest.
Published: 2024
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21. Spectroscopic confirmation of two luminous galaxies at a redshift of 14.

Author: Carniani S, Hainline K, D'Eugenio F, Eisenstein DJ, Jakobsen P, Witstok J, Johnson BD, Chevallard J, Maiolino R, Helton JM, Willott C, Robertson B, Alberts S, Arribas S, Baker WM, Bhatawdekar R, Boyett K, Bunker AJ, Cameron AJ, Cargile PA, Charlot S, Curti M, Curtis-Lake E, Egami E, Giardino G, Isaak K, Ji Z, Jones GC, Kumari N, Maseda MV, Parlanti E, Pérez-González PG, Rawle T, Rieke G, Rieke M, Del Pino BR, Saxena A, Scholtz J, Smit R, Sun F, Tacchella S, Übler H, Venturi G, Williams CC, and Willmer CNA
Abstract: The first observations of the James Webb Space Telescope (JWST) have revolutionized our understanding of the Universe by identifying galaxies at redshift z ≈ 13 (refs. 1-3 ). In addition, the discovery of many luminous galaxies at Cosmic Dawn (z > 10) has suggested that galaxies developed rapidly, in apparent tension with many standard models 4-8 . However, most of these galaxies lack spectroscopic confirmation, so their distances and properties are uncertain. Here we present JWST Advanced Deep Extragalactic Survey-Near-Infrared Spectrograph spectroscopic confirmation of two luminous galaxies at z = 14.32 - 0.20 + 0.08 and z = 13.90 ± 0.17. The spectra reveal ultraviolet continua with prominent Lyman-α breaks but no detected emission lines. This discovery proves that luminous galaxies were already in place 300 million years after the Big Bang and are more common than what was expected before JWST. The most distant of the two galaxies is unexpectedly luminous and is spatially resolved with a radius of 260 parsecs. Considering also the very steep ultraviolet slope of the second galaxy, we conclude that both are dominated by stellar continuum emission, showing that the excess of luminous galaxies in the early Universe cannot be entirely explained by accretion onto black holes. Galaxy formation models will need to address the existence of such large and luminous galaxies so early in cosmic history., (© 2024. The Author(s).)
Published: 2024
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22. Author Correction: A small and vigorous black hole in the early Universe.

Author: Maiolino R, Scholtz J, Witstok J, Carniani S, D'Eugenio F, de Graaff A, Übler H, Tacchella S, Curtis-Lake E, Arribas S, Bunker A, Charlot S, Chevallard J, Curti M, Looser TJ, Maseda MV, Rawle TD, Rodríguez Del Pino B, Willott CJ, Egami E, Eisenstein DJ, Hainline KN, Robertson B, Williams CC, Willmer CNA, Baker WM, Boyett K, DeCoursey C, Fabian AC, Helton JM, Ji Z, Jones GC, Kumari N, Laporte N, Nelson EJ, Perna M, Sandles L, Shivaei I, and Sun F
Published: 2024
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23. A recently quenched galaxy 700 million years after the Big Bang.

Author: Looser TJ, D'Eugenio F, Maiolino R, Witstok J, Sandles L, Curtis-Lake E, Chevallard J, Tacchella S, Johnson BD, Baker WM, Suess KA, Carniani S, Ferruit P, Arribas S, Bonaventura N, Bunker AJ, Cameron AJ, Charlot S, Curti M, de Graaff A, Maseda MV, Rawle T, Rix HW, Del Pino BR, Smit R, Übler H, Willott C, Alberts S, Egami E, Eisenstein DJ, Endsley R, Hausen R, Rieke M, Robertson B, Shivaei I, Williams CC, Boyett K, Chen Z, Ji Z, Jones GC, Kumari N, Nelson E, Perna M, Saxena A, and Scholtz J
Subjects: Time Factors, Stars, Celestial, Extraterrestrial Environment chemistry, Galaxies
Abstract: Local and low-redshift (z < 3) galaxies are known to broadly follow a bimodal distribution: actively star-forming galaxies with relatively stable star-formation rates and passive systems. These two populations are connected by galaxies in relatively slow transition. By contrast, theory predicts that star formation was stochastic at early cosmic times and in low-mass systems 1-4 . These galaxies transitioned rapidly between starburst episodes and phases of suppressed star formation, potentially even causing temporary quiescence-so-called mini-quenching events 5,6 . However, the regime of star-formation burstiness is observationally highly unconstrained. Directly observing mini-quenched galaxies in the primordial Universe is therefore of utmost importance to constrain models of galaxy formation and transformation 7,8 . Early quenched galaxies have been identified out to redshift z < 5 (refs. 9-12 ) and these are all found to be massive (M ⋆ > 10 10 M ⊙ ) and relatively old. Here we report a (mini-)quenched galaxy at z = 7.3, when the Universe was only 700 Myr old. The JWST/NIRSpec spectrum is very blue (U-V = 0.16 ± 0.03 mag) but exhibits a Balmer break and no nebular emission lines. The galaxy experienced a short starburst followed by rapid quenching; its stellar mass (4-6 × 10 8 M ⊙ ) falls in a range that is sensitive to various feedback mechanisms, which can result in perhaps only temporary quenching., (© 2024. The Author(s).)
Published: 2024
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24. A contact binary satellite of the asteroid (152830) Dinkinesh.

Author: Levison HF, Marchi S, Noll KS, Spencer JR, Statler TS, Bell JF 3rd, Bierhaus EB, Binzel R, Bottke WF, Britt D, Brown ME, Buie MW, Christensen PR, Dello Russo N, Emery JP, Grundy WM, Hahn M, Hamilton VE, Howett C, Kaplan H, Kretke K, Lauer TR, Manzoni C, Marschall R, Martin AC, May BH, Mottola S, Olkin CB, Pätzold M, Parker JW, Porter S, Preusker F, Protopapa S, Reuter DC, Robbins SJ, Salmon J, Simon AA, Stern SA, Sunshine JM, Wong I, Weaver HA, Adam C, Ancheta S, Andrews J, Anwar S, Barnouin OS, Beasley M, Berry KE, Birath E, Bolin B, Booco M, Burns R, Campbell P, Carpenter R, Crombie K, Effertz M, Eifert E, Ellis C, Faiks P, Fischetti J, Fleming P, Francis K, Franco R, Freund S, Gallagher C, Geeraert J, Gobat C, Gorgas D, Granat C, Gray S, Haas P, Harch A, Hegedus K, Isabelle C, Jackson B, Jacob T, Jennings S, Kaufmann D, Keeney BA, Kennedy T, Lauffer K, Lessac-Chenen E, Leonard R, Levine A, Lunsford A, Martin T, McAdams J, Mehall G, Merkley T, Miller G, Montanaro M, Montgomery A, Murphy G, Myers M, Nelson DS, Ocampo A, Olds R, Pelgrift JY, Perkins T, Pineau J, Poland D, Ramanan V, Rose D, Sahr E, Short O, Solanki I, Stanbridge D, Sutter B, Talpas Z, Taylor H, Treiu B, Vermeer N, Vincent M, Wallace M, Weigle G, Wibben DR, Wiens Z, Wilson JP, and Zhao Y
Abstract: Asteroids with diameters less than about 5 km have complex histories because they are small enough for radiative torques (that is, YORP, short for the Yarkovsky-O'Keefe-Radzievskii-Paddack effect) 1 to be a notable factor in their evolution 2 . (152830) Dinkinesh is a small asteroid orbiting the Sun near the inner edge of the main asteroid belt with a heliocentric semimajor axis of 2.19 AU; its S-type spectrum 3,4 is typical of bodies in this part of the main belt 5 . Here we report observations by the Lucy spacecraft 6,7 as it passed within 431 km of Dinkinesh. Lucy revealed Dinkinesh, which has an effective diameter of only 720 m, to be unexpectedly complex. Of particular note is the presence of a prominent longitudinal trough overlain by a substantial equatorial ridge and the discovery of the first confirmed contact binary satellite, now named (152830) Dinkinesh I Selam. Selam consists of two near-equal-sized lobes with diameters of 210 m and 230 m. It orbits Dinkinesh at a distance of 3.1 km with an orbital period of about 52.7 h and is tidally locked. The dynamical state, angular momentum and geomorphologic observations of the system lead us to infer that the ridge and trough of Dinkinesh are probably the result of mass failure resulting from spin-up by YORP followed by the partial reaccretion of the shed material. Selam probably accreted from material shed by this event., (© 2024. The Author(s).)
Published: 2024
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25. A high black-hole-to-host mass ratio in a lensed AGN in the early Universe.

Author: Furtak LJ, Labbé I, Zitrin A, Greene JE, Dayal P, Chemerynska I, Kokorev V, Miller TB, Goulding AD, de Graaff A, Bezanson R, Brammer GB, Cutler SE, Leja J, Pan R, Price SH, Wang B, Weaver JR, Whitaker KE, Atek H, Bogdán Á, Charlot S, Curtis-Lake E, van Dokkum P, Endsley R, Feldmann R, Fudamoto Y, Fujimoto S, Glazebrook K, Juneau S, Marchesini D, Maseda MV, Nelson E, Oesch PA, Plat A, Setton DJ, Stark DP, and Williams CC
Abstract: Early JWST observations have uncovered a population of red sources that might represent a previously overlooked phase of supermassive black hole growth 1-3 . One of the most intriguing examples is an extremely red, point-like object that was found to be triply imaged by the strong lensing cluster Abell 2744 (ref. 4 ). Here we present deep JWST/NIRSpec observations of this object, Abell2744-QSO1. The spectroscopy confirms that the three images are of the same object, and that it is a highly reddened (A V ≃ 3) broad emission line active galactic nucleus at a redshift of z spec = 7.0451 ± 0.0005. From the width of Hβ (full width at half-maximum = 2,800 ± 250 km s -1 ), we derive a black hole mass of M BH = 4 - 1 + 2 × 1 0 7 M ⊙ . We infer a very high ratio of black-hole-to-galaxy mass of at least 3%, an order of magnitude more than that seen in local galaxies 5 and possibly as high as 100%. The lack of strong metal lines in the spectrum together with the high bolometric luminosity (L bol = (1.1 ± 0.3) × 10 45 erg s -1 ) indicate that we are seeing the black hole in a phase of rapid growth, accreting at 30% of the Eddington limit. The rapid growth and high black-hole-to-galaxy mass ratio of Abell2744-QSO1 suggest that it may represent the missing link between black hole seeds 6 and one of the first luminous quasars 7 ., (© 2024. The Author(s), under exclusive licence to Springer Nature Limited.)
Published: 2024
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26. Methane emission from a cool brown dwarf.

Author: Faherty JK, Burningham B, Gagné J, Suárez G, Vos JM, Alejandro Merchan S, Morley CV, Rowland M, Lacy B, Kiman R, Caselden D, Kirkpatrick JD, Meisner A, Schneider AC, Kuchner MJ, Bardalez Gagliuffi DC, Beichman C, Eisenhardt P, Gelino CR, Gharib-Nezhad E, Gonzales E, Marocco F, Rothermich AJ, and Whiteford N
Abstract: Beyond our Solar System, aurorae have been inferred from radio observations of isolated brown dwarfs 1,2 . Within our Solar System, giant planets have auroral emission with signatures across the electromagnetic spectrum including infrared emission of H 3 and methane. Isolated brown dwarfs with auroral signatures in the radio have been searched for corresponding infrared features, but only null detections have been reported + and methane. Isolated brown dwarfs with auroral signatures in the radio have been searched for corresponding infrared features, but only null detections have been reported 3 . CWISEP J193518.59-154620.3. (W1935 for short) is an isolated brown dwarf with a temperature of approximately 482 K. Here we report James Webb Space Telescope observations of strong methane emission from W1935 at 3.326 μm. Atmospheric modelling leads us to conclude that a temperature inversion of approximately 300 K centred at 1-10 mbar replicates the feature. This represents an atmospheric temperature inversion for a Jupiter-like atmosphere without irradiation from a host star. A plausible explanation for the strong inversion is heating by auroral processes, although other internal and external dynamical processes cannot be ruled out. The best-fitting model rules out the contribution of H 3 + emission, which is prominent in Solar System gas giants. However, this is consistent with rapid destruction of H 3 + at the higher pressure where the W1935 emission originates 4 ., (© 2024. The Author(s).)
Published: 2024
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27. A small and vigorous black hole in the early Universe.

Author: Maiolino R, Scholtz J, Witstok J, Carniani S, D'Eugenio F, de Graaff A, Übler H, Tacchella S, Curtis-Lake E, Arribas S, Bunker A, Charlot S, Chevallard J, Curti M, Looser TJ, Maseda MV, Rawle TD, Rodríguez Del Pino B, Willott CJ, Egami E, Eisenstein DJ, Hainline KN, Robertson B, Williams CC, Willmer CNA, Baker WM, Boyett K, DeCoursey C, Fabian AC, Helton JM, Ji Z, Jones GC, Kumari N, Laporte N, Nelson EJ, Perna M, Sandles L, Shivaei I, and Sun F
Abstract: Several theories have been proposed to describe the formation of black hole seeds in the early Universe and to explain the emergence of very massive black holes observed in the first thousand million years after the Big Bang 1-3 . Models consider different seeding and accretion scenarios 4-7 , which require the detection and characterization of black holes in the first few hundred million years after the Big Bang to be validated. Here we present an extensive analysis of the JWST-NIRSpec spectrum of GN-z11, an exceptionally luminous galaxy at z = 10.6, revealing the detection of the [NeIV]λ2423 and CII*λ1335 transitions (typical of active galactic nuclei), as well as semi-forbidden nebular lines tracing gas densities higher than 10 9 cm -3 , typical of the broad line region of active galactic nuclei. These spectral features indicate that GN-z11 hosts an accreting black hole. The spectrum also reveals a deep and blueshifted CIVλ1549 absorption trough, tracing an outflow with velocity 800-1,000 km s -1 , probably driven by the active galactic nucleus. Assuming local virial relations, we derive a black hole mass of log ( M BH / M ⊙ ) = 6.2 ± 0.3 , accreting at about five times the Eddington rate. These properties are consistent with both heavy seeds scenarios and scenarios considering intermediate and light seeds experiencing episodic super-Eddington phases. Our finding explains the high luminosity of GN-z11 and can also provide an explanation for its exceptionally high nitrogen abundance., (© 2024. The Author(s).)
Published: 2024
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28. Most of the photons that reionized the Universe came from dwarf galaxies.

Author: Atek H, Labbé I, Furtak LJ, Chemerynska I, Fujimoto S, Setton DJ, Miller TB, Oesch P, Bezanson R, Price SH, Dayal P, Zitrin A, Kokorev V, Weaver JR, Brammer G, Dokkum PV, Williams CC, Cutler SE, Feldmann R, Fudamoto Y, Greene JE, Leja J, Maseda MV, Muzzin A, Pan R, Papovich C, Nelson EJ, Nanayakkara T, Stark DP, Stefanon M, Suess KA, Wang B, and Whitaker KE
Abstract: The identification of sources driving cosmic reionization, a major phase transition from neutral hydrogen to ionized plasma around 600-800 Myr after the Big Bang 1-3 , has been a matter of debate 4 . Some models suggest that high ionizing emissivity and escape fractions (f esc ) from quasars support their role in driving cosmic reionization 5,6 . Others propose that the high f esc values from bright galaxies generate sufficient ionizing radiation to drive this process 7 . Finally, a few studies suggest that the number density of faint galaxies, when combined with a stellar-mass-dependent model of ionizing efficiency and f esc , can effectively dominate cosmic reionization 8,9 . However, so far, comprehensive spectroscopic studies of low-mass galaxies have not been done because of their extreme faintness. Here we report an analysis of eight ultra-faint galaxies (in a very small field) during the epoch of reionization with absolute magnitudes between M UV ≈ -17 mag and -15 mag (down to 0.005L ⋆ (refs. 10,11 )). We find that faint galaxies during the first thousand million years of the Universe produce ionizing photons with log[ξ ion (Hz erg -1 )] = 25.80 ± 0.14, a factor of 4 higher than commonly assumed values 12 . If this field is representative of the large-scale distribution of faint galaxies, the rate of ionizing photons exceeds that needed for reionization, even for escape fractions of the order of 5%., (© 2024. The Author(s), under exclusive licence to Springer Nature Limited.)
Published: 2024
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29. A Milky Way-like barred spiral galaxy at a redshift of 3.

Author: Costantin L, Pérez-González PG, Guo Y, Buttitta C, Jogee S, Bagley MB, Barro G, Kartaltepe JS, Koekemoer AM, Cabello C, Corsini EM, Méndez-Abreu J, de la Vega A, Iyer KG, Bisigello L, Cheng Y, Morelli L, Arrabal Haro P, Buitrago F, Cooper MC, Dekel A, Dickinson M, Finkelstein SL, Giavalisco M, Holwerda BW, Huertas-Company M, Lucas RA, Papovich C, Pirzkal N, Seillé LM, Vega-Ferrero J, Wuyts S, and Yung LYA
Abstract: The majority of massive disk galaxies in the local Universe show a stellar barred structure in their central regions, including our Milky Way 1,2 . Bars are supposed to develop in dynamically cold stellar disks at low redshift, as the strong gas turbulence typical of disk galaxies at high redshift suppresses or delays bar formation 3,4 . Moreover, simulations predict bars to be almost absent beyond z = 1.5 in the progenitors of Milky Way-like galaxies 5,6 . Here we report observations of ceers-2112, a barred spiral galaxy at redshift z phot ≈ 3, which was already mature when the Universe was only 2 Gyr old. The stellar mass (M ★ = 3.9 × 10 9 M ⊙ ) and barred morphology mean that ceers-2112 can be considered a progenitor of the Milky Way 7-9 , in terms of both structure and mass-assembly history in the first 2 Gyr of the Universe, and was the closest in mass in the first 4 Gyr. We infer that baryons in galaxies could have already dominated over dark matter at z ≈ 3, that high-redshift bars could form in approximately 400 Myr and that dynamically cold stellar disks could have been in place by redshift z = 4-5 (more than 12 Gyrs ago) 10,11 ., (© 2023. The Author(s).)
Published: 2023
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30. Confirmation and refutation of very luminous galaxies in the early Universe.

Author: Arrabal Haro P, Dickinson M, Finkelstein SL, Kartaltepe JS, Donnan CT, Burgarella D, Carnall AC, Cullen F, Dunlop JS, Fernández V, Fujimoto S, Jung I, Krips M, Larson RL, Papovich C, Pérez-González PG, Amorín RO, Bagley MB, Buat V, Casey CM, Chworowsky K, Cohen SH, Ferguson HC, Giavalisco M, Huertas-Company M, Hutchison TA, Kocevski DD, Koekemoer AM, Lucas RA, McLeod DJ, McLure RJ, Pirzkal N, Seillé LM, Trump JR, Weiner BJ, Wilkins SM, and Zavala JA
Abstract: During the first 500 million years of cosmic history, the first stars and galaxies formed, seeding the Universe with heavy elements and eventually reionizing the intergalactic medium 1-3 . Observations with the James Webb Space Telescope (JWST) have uncovered a surprisingly high abundance of candidates for early star-forming galaxies, with distances (redshifts, z), estimated from multiband photometry, as large as z ≈ 16, far beyond pre-JWST limits 4-9 . Although such photometric redshifts are generally robust, they can suffer from degeneracies and occasionally catastrophic errors. Spectroscopic measurements are required to validate these sources and to reliably quantify physical properties that can constrain galaxy formation models and cosmology 10 . Here we present JWST spectroscopy that confirms redshifts for two very luminous galaxies with z > 11, and also demonstrates that another candidate with suggested z ≈ 16 instead has z = 4.9, with an unusual combination of nebular line emission and dust reddening that mimics the colours expected for much more distant objects. These results reinforce evidence for the early, rapid formation of remarkably luminous galaxies while also highlighting the necessity of spectroscopic verification. The large abundance of bright, early galaxies may indicate shortcomings in current galaxy formation models or deviations from physical properties (such as the stellar initial mass function) that are generally believed to hold at later times., (© 2023. The Author(s), under exclusive licence to Springer Nature Limited.)
Published: 2023
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31. Carbonaceous dust grains seen in the first billion years of cosmic time.

Author: Witstok J, Shivaei I, Smit R, Maiolino R, Carniani S, Curtis-Lake E, Ferruit P, Arribas S, Bunker AJ, Cameron AJ, Charlot S, Chevallard J, Curti M, de Graaff A, D'Eugenio F, Giardino G, Looser TJ, Rawle T, Rodríguez Del Pino B, Willott C, Alberts S, Baker WM, Boyett K, Egami E, Eisenstein DJ, Endsley R, Hainline KN, Ji Z, Johnson BD, Kumari N, Lyu J, Nelson E, Perna M, Rieke M, Robertson BE, Sandles L, Saxena A, Scholtz J, Sun F, Tacchella S, Williams CC, and Willmer CNA
Abstract: Large dust reservoirs (up to approximately 10 8 M ⊙ ) have been detected 1-3 in galaxies out to redshift z ≃ 8, when the age of the Universe was only about 600 Myr. Generating substantial amounts of dust within such a short timescale has proven challenging for theories of dust formation 4,5 and has prompted the revision of the modelling of potential sites of dust production 6-8 , such as the atmospheres of asymptotic giant branch stars in low-metallicity environments, supernova ejecta and the accelerated growth of grains in the interstellar medium. However, degeneracies between different evolutionary pathways remain when the total dust mass of galaxies is the only available observable. Here we report observations of the 2,175 Å dust attenuation feature, which is well known in the Milky Way and galaxies at z ≲ 3 (refs. 9-11 ), in the near-infrared spectra of galaxies up to z ≃ 7, corresponding to the first billion years of cosmic time. The relatively short timescale implied for the formation of carbonaceous grains giving rise to this feature 12 suggests a rapid production process, possibly in Wolf-Rayet stars or supernova ejecta., (© 2023. The Author(s).)
Published: 2023
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32. An infrared transient from a star engulfing a planet.

Author: De K, MacLeod M, Karambelkar V, Jencson JE, Chakrabarty D, Conroy C, Dekany R, Eilers AC, Graham MJ, Hillenbrand LA, Kara E, Kasliwal MM, Kulkarni SR, Lau RM, Loeb A, Masci F, Medford MS, Meisner AM, Patel N, Quiroga-Nuñez LH, Riddle RL, Rusholme B, Simcoe R, Sjouwerman LO, Teague R, and Vanderburg A
Abstract: Planets with short orbital periods (roughly under 10 days) are common around stars like the Sun 1,2 . Stars expand as they evolve and thus we expect their close planetary companions to be engulfed, possibly powering luminous mass ejections from the host star 3-5 . However, this phase has never been directly observed. Here we report observations of ZTF SLRN-2020, a short-lived optical outburst in the Galactic disk accompanied by bright and long-lived infrared emission. The resulting light curve and spectra share striking similarities with those of red novae 6,7 -a class of eruptions now confirmed 8 to arise from mergers of binary stars. Its exceptionally low optical luminosity (approximately 10 35 erg s -1 ) and radiated energy (approximately 6.5 × 10 41 erg) point to the engulfment of a planet of fewer than roughly ten Jupiter masses by its Sun-like host star. We estimate the Galactic rate of such subluminous red novae to be roughly between 0.1 and several per year. Future Galactic plane surveys should routinely identify these, showing the demographics of planetary engulfment and the ultimate fate of planets in the inner Solar System., (© 2023. The Author(s), under exclusive licence to Springer Nature Limited.)
Published: 2023
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33. Ten simple rules to cultivate transdisciplinary collaboration in data science.

Author: Sahneh F, Balk MA, Kisley M, Chan CK, Fox M, Nord B, Lyons E, Swetnam T, Huppenkothen D, Sutherland W, Walls RL, Quinn DP, Tarin T, LeBauer D, Ribes D, Birnie DP 3rd, Lushbough C, Carr E, Nearing G, Fischer J, Tyle K, Carrasco L, Lang M, Rose PW, Rushforth RR, Roy S, Matheson T, Lee T, Brown CT, Teal TK, Papeș M, Kobourov S, and Merchant N
Subjects: Computational Biology, Humans, Intersectoral Collaboration, Cooperative Behavior, Data Science ethics, Data Science organization & administration, Data Science trends, Interdisciplinary Communication, Interprofessional Relations
Abstract: Competing Interests: The authors have declared that no competing interests exist.
Published: 2021
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34. Dark Energy Survey Year 1 Results: Cosmological Constraints from Cluster Abundances, Weak Lensing, and Galaxy Correlations.

Author: To C, Krause E, Rozo E, Wu H, Gruen D, Wechsler RH, Eifler TF, Rykoff ES, Costanzi M, Becker MR, Bernstein GM, Blazek J, Bocquet S, Bridle SL, Cawthon R, Choi A, Crocce M, Davis C, DeRose J, Drlica-Wagner A, Elvin-Poole J, Fang X, Farahi A, Friedrich O, Gatti M, Gaztanaga E, Giannantonio T, Hartley WG, Hoyle B, Jarvis M, MacCrann N, McClintock T, Miranda V, Pereira MES, Park Y, Porredon A, Prat J, Rau MM, Ross AJ, Samuroff S, Sánchez C, Sevilla-Noarbe I, Sheldon E, Troxel MA, Varga TN, Vielzeuf P, Zhang Y, Zuntz J, Abbott TMC, Aguena M, Amon A, Annis J, Avila S, Bertin E, Bhargava S, Brooks D, Burke DL, Carnero Rosell A, Carrasco Kind M, Carretero J, Chang C, Conselice C, da Costa LN, Davis TM, Desai S, Diehl HT, Dietrich JP, Everett S, Evrard AE, Ferrero I, Flaugher B, Fosalba P, Frieman J, García-Bellido J, Gruendl RA, Gutierrez G, Hinton SR, Hollowood DL, Honscheid K, Huterer D, James DJ, Jeltema T, Kron R, Kuehn K, Kuropatkin N, Lima M, Maia MAG, Marshall JL, Menanteau F, Miquel R, Morgan R, Muir J, Myles J, Palmese A, Paz-Chinchón F, Plazas AA, Romer AK, Roodman A, Sanchez E, Santiago B, Scarpine V, Serrano S, Smith M, Suchyta E, Swanson MEC, Tarle G, Thomas D, Tucker DL, Weller J, Wester W, and Wilkinson RD
Abstract: We present the first joint analysis of cluster abundances and auto or cross-correlations of three cosmic tracer fields: galaxy density, weak gravitational lensing shear, and cluster density split by optical richness. From a joint analysis (4×2pt+N) of cluster abundances, three cluster cross-correlations, and the auto correlations of the galaxy density measured from the first year data of the Dark Energy Survey, we obtain Ω_{m}=0.305_{-0.038}^{+0.055} and σ_{8}=0.783_{-0.054}^{+0.064}. This result is consistent with constraints from the DES-Y1 galaxy clustering and weak lensing two-point correlation functions for the flat νΛCDM model. Consequently, we combine cluster abundances and all two-point correlations from across all three cosmic tracer fields (6×2pt+N) and find improved constraints on cosmological parameters as well as on the cluster observable-mass scaling relation. This analysis is an important advance in both optical cluster cosmology and multiprobe analyses of upcoming wide imaging surveys.
Published: 2021
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35. Constraints on Dark Matter Properties from Observations of Milky Way Satellite Galaxies.

Author: Nadler EO, Drlica-Wagner A, Bechtol K, Mau S, Wechsler RH, Gluscevic V, Boddy K, Pace AB, Li TS, McNanna M, Riley AH, García-Bellido J, Mao YY, Green G, Burke DL, Peter A, Jain B, Abbott TMC, Aguena M, Allam S, Annis J, Avila S, Brooks D, Carrasco Kind M, Carretero J, Costanzi M, da Costa LN, De Vicente J, Desai S, Diehl HT, Doel P, Everett S, Evrard AE, Flaugher B, Frieman J, Gerdes DW, Gruen D, Gruendl RA, Gschwend J, Gutierrez G, Hinton SR, Honscheid K, Huterer D, James DJ, Krause E, Kuehn K, Kuropatkin N, Lahav O, Maia MAG, Marshall JL, Menanteau F, Miquel R, Palmese A, Paz-Chinchón F, Plazas AA, Romer AK, Sanchez E, Scarpine V, Serrano S, Sevilla-Noarbe I, Smith M, Soares-Santos M, Suchyta E, Swanson MEC, Tarle G, Tucker DL, Walker AR, and Wester W
Abstract: We perform a comprehensive study of Milky Way (MW) satellite galaxies to constrain the fundamental properties of dark matter (DM). This analysis fully incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and marginalizes over uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk. Our results are consistent with the cold, collisionless DM paradigm and yield the strongest cosmological constraints to date on particle models of warm, interacting, and fuzzy dark matter. At 95% confidence, we report limits on (i) the mass of thermal relic warm DM, m_{WDM}>6.5 keV (free-streaming length, λ_{fs}≲10h^{-1} kpc), (ii) the velocity-independent DM-proton scattering cross section, σ_{0}<8.8×10^{-29} cm^{2} for a 100 MeV DM particle mass [DM-proton coupling, c_{p}≲(0.3 GeV)^{-2}], and (iii) the mass of fuzzy DM, m_{ϕ}>2.9×10^{-21} eV (de Broglie wavelength, λ_{dB}≲0.5 kpc). These constraints are complementary to other observational and laboratory constraints on DM properties.
Published: 2021
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35 results on '"NSF's National Optical-Infrared Astronomy Research Laboratory"'

1. A dusty veil shading Betelgeuse during its Great Dimming

2. Dark energy survey year 3 results: Galaxy sample for BAO measurement

3. The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters

4. The Dark Energy Survey Bright Arcs Survey: Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey 5000 Square Degree Footprint

5. GOODS-ALMA 2.0: Source catalog, number counts, and prevailing compact sizes in 1.1 mm galaxies

6. From the fire: a deeper look at the Phoenix stream

7. Dark Energy Survey Year 3 results: A 2.7% measurement of baryon acoustic oscillation distance scale at redshift 0.835

8. Dark Energy Survey Year 3 results: Cosmology from cosmic shear and robustness to modeling uncertainty

9. Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and weak lensing

10. The mass and galaxy distribution around SZ-selected clusters

11. C/2014 UN271(Bernardinelli-Bernstein): The Nearly Spherical Cow of Comets

12. DES Y1 results: Splitting growth and geometry to test $\Lambda$CDM

13. Constraints on dark matter to dark radiation conversion in the late universe with DES-Y1 and external data

14. Dark Energy Survey Year 3 results: Curved-sky weak lensing mass map reconstruction

15. CHARA array adaptive optics: complex operational software and performance

16. COLDz: A High Space Density of Massive Dusty Starburst Galaxies ~1 Billion Years after the Big Bang

17. The Dark Side of Pluto

18. A dormant overmassive black hole in the early Universe.

19. Accelerated formation of ultra-massive galaxies in the first billion years.

20. Using JADES NIRCam photometry to investigate the dependence of stellar mass inferences on the IMF in the early universe.

21. Spectroscopic confirmation of two luminous galaxies at a redshift of 14.

22. Author Correction: A small and vigorous black hole in the early Universe.

23. A recently quenched galaxy 700 million years after the Big Bang.

24. A contact binary satellite of the asteroid (152830) Dinkinesh.

25. A high black-hole-to-host mass ratio in a lensed AGN in the early Universe.

26. Methane emission from a cool brown dwarf.

27. A small and vigorous black hole in the early Universe.

28. Most of the photons that reionized the Universe came from dwarf galaxies.

29. A Milky Way-like barred spiral galaxy at a redshift of 3.

30. Confirmation and refutation of very luminous galaxies in the early Universe.

31. Carbonaceous dust grains seen in the first billion years of cosmic time.

32. An infrared transient from a star engulfing a planet.

33. Ten simple rules to cultivate transdisciplinary collaboration in data science.

34. Dark Energy Survey Year 1 Results: Cosmological Constraints from Cluster Abundances, Weak Lensing, and Galaxy Correlations.

35. Constraints on Dark Matter Properties from Observations of Milky Way Satellite Galaxies.

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35 results on '"NSF's National Optical-Infrared Astronomy Research Laboratory"'

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