Author: "NSF's National Optical-Infrared Astronomy Research Laboratory" / Publication Year Range: Last 3 years - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"NSF's National Optical-Infrared Astronomy Research Laboratory"' showing total 23 results

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

1. 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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2. 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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3. 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

4. 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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5. 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
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6. 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

7. 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
Full Text: View/download PDF

8. 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

9. 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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10. 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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11. 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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12. 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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13. 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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14. 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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15. 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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16. 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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17. 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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18. 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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19. 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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20. 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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21. 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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22. 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
Full Text: View/download PDF

23. 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
Full Text: View/download PDF

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

17. Methane emission from a cool brown dwarf.

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

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

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

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

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

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

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

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