Author: "MARSHALL, J. L." / Database: OpenAIRE - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"MARSHALL, J. L."' showing total 190 results

Start Over Author "MARSHALL, J. L." Database OpenAIRE

190 results on '"MARSHALL, J. L."'

1. Constraining the baryonic feedback with cosmic shear using the DES Year-3 small-scale measurements

Author: Chen, A., Aricò, G., Huterer, D., Angulo, R. E., Weaverdyck, N., Friedrich, O., Secco, L. F., Hernández-Monteagudo, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Brandao-Souza, A., Bridle, S. L., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Choi, A., Cordero, J., Crocce, M., Pereira, M. E. S., Davis, C., Derose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Ferté, A., Fosalba, P., Gatti, M., Gaztanaga, E., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Hoffmann, K., Huang, H., Huff, E. M., Jain, B., Jarvis, M., Jeffrey, N., Kacprzak, T., Krause, E., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Pandey, S., Park, Y., Porredon, A., Prat, J., Raveri, M., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchón, F., Pieres, A., Sanchez, E., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Des, Collaboration, Chen, A., Aricò, G., Huterer, D., Angulo, R. E., Weaverdyck, N., Friedrich, O., Secco, L. F., Hernández-Monteagudo, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Brandao-Souza, A., Bridle, S. L., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Choi, A., Cordero, J., Crocce, M., Pereira, M. E. S., Davis, C., Derose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Ferté, A., Fosalba, P., Gatti, M., Gaztanaga, E., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Hoffmann, K., Huang, H., Huff, E. M., Jain, B., Jarvis, M., Jeffrey, N., Kacprzak, T., Krause, E., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Pandey, S., Park, Y., Porredon, A., Prat, J., Raveri, M., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchón, F., Pieres, A., Sanchez, E., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Nuclear Theory, High Energy Physics::Phenomenology, cosmology observations, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics Cosmology and Nongalactic Astrophysics, Space and Planetary Science, gravitational lensing weak, large-scale structure of Universe, cosmology observation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use the small scales of the Dark Energy Survey (DES) Year-3 cosmic shear measurements, which are excluded from the DES Year-3 cosmological analysis, to constrain the baryonic feedback. To model the baryonic feedback, we adopt a baryonic correction model and use the numerical package \texttt{Baccoemu} to accelerate the evaluation of the baryonic nonlinear matter power spectrum. We design our analysis pipeline to focus on the constraints of the baryonic suppression effects, utilizing the implication given by a principal component analysis on the Fisher forecasts. Our constraint on the baryonic effects can then be used to better model and ameliorate the effects of baryons in producing cosmological constraints from the next generation large-scale structure surveys. We detect the baryonic suppression on the cosmic shear measurements with a $\sim 2 \sigma$ significance. The characteristic halo mass for which half of the gas is ejected by baryonic feedback is constrained to be $M_c > 10^{13.2} h^{-1} M_{\odot}$ (95\% C.L.). The best-fit baryonic suppression is $\sim 5\%$ at $k=1.0 {\rm Mpc}\ h^{-1}$ and $\sim 15\%$ at $k=5.0 {\rm Mpc} \ h^{-1}$. Our findings are robust with respect to the assumptions about the cosmological parameters, specifics of the baryonic model, and intrinsic alignments., Comment: 20 pages, 10 figures. DES Collaboration, Year-3 analysis
Published: 2022

2. Characterizing the intracluster light over the redshift range 0.2 < z < 0.8 in the DES-ACT overlap

Author: Golden-Marx, Jesse B., Zhang, Y., Ogando, R. L. C., Allam, S., Tucker, D. L., Miller, C. J., Hilton, M., Mutlu-Pakdil, B., Abbott, T. M. C., Aguena, M., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Bellido, J. García, Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Marshall, J. L., Melchior, P., Mena-Fernández, J., Miquel, R., Mohr, J. J., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Prat, J., Raveri, M., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Sifón, C., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Vincenzi, M., Weaverdyck, N., Yanny, B., and Collaboration, DES
Subjects: Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We characterise the properties and evolution of Bright Central Galaxies (BCGs) and the surrounding intracluster light (ICL) in galaxy clusters identified in overlapping regions of the Dark Energy Survey and Atacama Cosmology Telescope Survey (DES-ACT), covering the redshift range $0.20$14.4. We also measure the stellar mass - halo mass (SMHM) relation for the BCG+ICL system and find that the slope, $\beta$, which characterises the dependence of $M_{\rm 200m,SZ}$ on the BCG+ICL stellar mass, increases with radius. The outskirts are more strongly correlated with the halo than the core, which supports that the BCG+ICL system follows a two-phase growth, where recent growth ($z, Comment: 19 pages, 12 Figures, 3 Tables. Submitted to MNRAS on 9/7/2022 -- Metadata typo corrected
Published: 2023

3. The Dark Energy Survey supernova program: cosmological biases from supernova photometric classification

Author: Vincenzi, M., Sullivan, M., Möller, A., Armstrong, P., Bassett, B. A., Brout, D., Carollo, D., Carr, A., Davis, T. M., Frohmaier, C., Galbany, L., Glazebrook, K., Graur, O., Kelsey, L., Kessler, R., Kovacs, E., Lewis, G. F., Lidman, C., Malik, U., Nichol, R. C., Popovic, B., Sako, M., Scolnic, D., Smith, M., Taylor, G., Tucker, B. E., Wiseman, P., Aguena, M., Allam, S., Annis, J., Asorey, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., T. S., Li, Lima, M., Maia, M. A. G., Marshall, J. L., Miquel, R., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Varga, T. N., Weller, J., Wilkinson, R. D., Des, Collaboration, Vincenzi, M., Sullivan, M., Möller, A., Armstrong, P., Bassett, B. A., Brout, D., Carollo, D., Carr, A., Davis, T. M., Frohmaier, C., Galbany, L., Glazebrook, K., Graur, O., Kelsey, L., Kessler, R., Kovacs, E., Lewis, G. F., Lidman, C., Malik, U., Nichol, R. C., Popovic, B., Sako, M., Scolnic, D., Smith, M., Taylor, G., Tucker, B. E., Wiseman, P., Aguena, M., Allam, S., Annis, J., Asorey, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., T. S., Li, Lima, M., Maia, M. A. G., Marshall, J. L., Miquel, R., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Varga, T. N., Weller, J., Wilkinson, R. D., Des, Collaboration, UAM. Departamento de Física Teórica, Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), cosmology observations, FOS: Physical sciences, Física, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Astrophysics Cosmology and Nongalactic Astrophysics, Cosmology: Observations, Supernovae: General, surveys, supernovae general, Space and Planetary Science, survey, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmology observation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Artículo escrito por un elevado número de autores, solo se referencian el que aparece en primer lugar, los autores pertenecientes a la UAM y el nombre del grupo de colaboración, si lo hubiere, This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record Monthly Notices of the Royal Astronomical Society Volume 518.1 (2023): 1106-1127 is available online at: https://academic.oup.com/mnras/article-abstract/518/1/1106/6601453, Cosmological analyses of samples of photometrically identified type Ia supernovae (SNe Ia) depend on understanding the effects of ‘contamination’ from core-collapse and peculiar SN Ia events. We employ a rigorous analysis using the photometric classifier SuperNNova on state-of-the-art simulations of SN samples to determine cosmological biases due to such ‘non-Ia’ contamination in the Dark Energy Survey (DES) 5-yr SN sample. Depending on the non-Ia SN models used in the SuperNNova training and testing samples, contamination ranges from 0.8 to 3.5 per cent, with a classification efficiency of 97.7–99.5 per cent. Using the Bayesian Estimation Applied to Multiple Species (BEAMS) framework and its extension BBC (‘BEAMS with Bias Correction’), we produce a redshift-binned Hubble diagram marginalized over contamination and corrected for selection effects, and use it to constrain the dark energy equation-of-state, w. Assuming a flat universe with Gaussian ΩM prior of 0.311 ± 0.010, we show that biases on w are, This work was supported by the Science and Technology Facilities Council [grant number ST/P006760/1] through the DISCnet Cen¬tre for Doctoral Training. MS acknowledges support from EU/FP7¬ERC grant 615929, and PW acknowledges support from STFC grant ST/R000506/1. TMD acknowledges support from ARC grant FL180100168. LG acknowledges financial support from the Span¬ish Ministry of Science, Innovation and Universities (MICIU) un¬der the 2019 Ramón y Cajal program RYC2019-027683 and from the Spanish MICIU project PID2020-115253GA-I00. RH and MS were supported by DOE grant DE-FOA-0001781 and NASA grant NNH15ZDA001N-WFIRST. The material is based upon work sup¬ported by NASA under award number 80GSFC17M0002. LK thanks the UKRI Future Leaders Fellowship for support through the grant MR/T01881X/1. This paper has gone through internal review by the DES collab¬oration. 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 Uni¬versity of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fun¬damental Physics and Astronomy at Texas A&M University, Finan¬ciadora 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 Forschungsgemein¬schaft 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 Cam¬bridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University Col¬lege London, the DES-Brazil Consortium, the University of Edin¬burgh, 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, NFS’s NOIRLab, the University of Nottingham, The Ohio State Uni-versity, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the Uni¬versity of Sussex, Texas A&M University, and the OzDES Member¬ship 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 Na¬tional 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 re¬sults 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 Ciên¬cia e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014¬2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. De¬partment of Energy, Office of Science, Office of High Energy Physics. This work was completed in part with resources provided by the University of Chicago’s Research Computing Center. Finally, this work was based in part on data acquired at the Anglo-Australian Telescope, under program A/2013B/012. We acknowledge the traditional owners of the land on which the AAT stands, the Gamilaraay people, and pay our respects to elders past and present
Published: 2023

4. The DES view of the Eridanus supervoid and the CMB cold spot

Author: Kovács, A, Jeffrey, N, Gatti, M, Chang, C, Whiteway, L, Hamaus, N, Lahav, O, Pollina, G, Bacon, D, Kacprzak, T, Mawdsley, B, Nadathur, S, Zeurcher, D, García-Bellido, J, Alarcon, A, Amon, A, Bechtol, K, Bernstein, G M, Campos, A, Rosell, A Carnero, Kind, M Carrasco, Cawthon, R, Chen, R, Choi, A, Cordero, J, Davis, C, Derose, J, Doux, C, Drlica-Wagner, A, Eckert, K, Elsner, F, Elvin-Poole, J, Everett, S, Ferté, A, Giannini, G, Gruen, D, Gruendl, R A, Harrison, I, Hartley, W G, Herner, K, Huff, E M, Huterer, D, Kuropatkin, N, Jarvis, M, Leget, P F, Maccrann, N, Mccullough, J, Muir, J, Myles, J, Navarro-Alsina, A, Pandey, S, Prat, J, Raveri, M, Rollins, R P, Ross, A J, Rykoff, E S, Sánchez, C, Secco, L F, Sevilla-Noarbe, I, Sheldon, E, Shin, T, Troxel, M A, Tutusaus, I, Varga, T N, Yanny, B, Yin, B, Zhang, Y, Zuntz, J, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Bertin, E, Brooks, D, Burke, D, Carretero, J, Costanzi, M, da&nbsp, Costa, L N, Pereira, M E S, Davis, T, Deundefined, Vicente, J, Desai, S, Diehl, H T, Ferrero, I, Flaugher, B, Fosalba, P, Frieman, J, Gaztañaga, E, Gerdes, D, Giannantonio, T, Gschwend, J, Gutierrez, G, Hinton, S, Hollowood, D L, Honscheid, K, James, D, Kuehn, K, Lima, M, Maia, M A G, Marshall, J L, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, Ogando, R, Paz-Chinchon, F, Pieres, A, Plazas, A A, Monroy, M Rodriguez, Romer, K, Roodman, A, Sanchez, E, Schubnell, M, Serrano, S, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, M E C, Tarle, G, Thomas, D, C-H, To, Weller, J, UAM. Departamento de Física Teórica, Instituto de Astrofísica de Canarias (IAC), Tenerife, Univer Sité de Paris, University College London, The Barcelona Institute of Science and Technology, University of Pennsylvania, University of Chicago, Univer Sity of Chica Go, Ludwig-Maximilians Univer- Sität München, University of Portsmouth, ETH Zurich, Universidad Autonoma de Madrid, Argonne National Laboratory, Stanford University, University of Wisconsin- Madison, Carnegie Mellon University, Laboratório Interinstitucional de E-Astronomia - LIneA, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Duke University, The Ohio State Univer- Sity, University of Manchester, University of California, Santa Cruz Institute for Particle Physics, Fermi National Accelerator Laboratory, The Ohio State University, California Institute of Technology, SLAC National Accelerator Laboratory, University of Oxford, University of Gene Va, University of Michigan, University of Cambridge, Perimeter Institute for Theoretical Physics, Univer Sidade Estadual de Campinas, Medioambientales y Tecnológicas (CIEMAT), Brookhaven National Laboratory, Institut D'Estudis Espacials de Catalunya (IEEC), CSIC), Max Planck Institute for Extraterrestrial Physics, University of Edinb Urgh, Universidade de São Paulo (USP), Universidade Estadual Paulista (UNESP), Institut D'Astrophysique de Paris, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Queensland, IIT Hyderabad, University of Oslo, Univer Sity of Cambridge, Harvard and Smithsonian, Lowell Observatory, Macquarie University, Texas A&M Univer Sity, Princeton University, Institució Catalana de Recerca i Estudis Avan C Ats, Univer Sity of Sussex, University of Southampton, Oak Ridge National Labo- Ratory, Kovács, A, Jeffrey, N, Gatti, M, Chang, C, Whiteway, L, Hamaus, N, Lahav, O, Pollina, G, Bacon, D, Kacprzak, T, Mawdsley, B, Nadathur, S, Zeurcher, D, García-Bellido, J, Alarcon, A, Amon, A, Bechtol, K, Bernstein, G M, Campos, A, Rosell, A Carnero, Kind, M Carrasco, Cawthon, R, Chen, R, Choi, A, Cordero, J, Davis, C, Derose, J, Doux, C, Drlica-Wagner, A, Eckert, K, Elsner, F, Elvin-Poole, J, Everett, S, Ferté, A, Giannini, G, Gruen, D, Gruendl, R A, Harrison, I, Hartley, W G, Herner, K, Huff, E M, Huterer, D, Kuropatkin, N, Jarvis, M, Leget, P F, Maccrann, N, Mccullough, J, Muir, J, Myles, J, Navarro-Alsina, A, Pandey, S, Prat, J, Raveri, M, Rollins, R P, Ross, A J, Rykoff, E S, Sánchez, C, Secco, L F, Sevilla-Noarbe, I, Sheldon, E, Shin, T, Troxel, M A, Tutusaus, I, Varga, T N, Yanny, B, Yin, B, Zhang, Y, Zuntz, J, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Bertin, E, Brooks, D, Burke, D, Carretero, J, Costanzi, M, da&nbsp, Costa, L N, Pereira, M E S, Davis, T, De&nbsp, Vicente, J, Desai, S, Diehl, H T, Ferrero, I, Flaugher, B, Fosalba, P, Frieman, J, Gaztañaga, E, Gerdes, D, Giannantonio, T, Gschwend, J, Gutierrez, G, Hinton, S, Hollowood, D L, Honscheid, K, James, D, Kuehn, K, Lima, M, Maia, M A G, Marshall, J L, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, Ogando, R, Paz-Chinchon, F, Pieres, A, Plazas, A A, Monroy, M Rodriguez, Romer, K, Roodman, A, Sanchez, E, Schubnell, M, Serrano, S, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, M E C, Tarle, G, Thomas, D, C-H, To, Weller, J, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), European Research Council, National Science Foundation (US), European Commission, and Agenzia Spaziale Italiana
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic Background Radiation, FOS: Physical sciences, Física, Astronomy and Astrophysics, cosmic background radiation, Surveys, gravitational lensing: weak, surveys, Space and Planetary Science, Weak [Gravitational Lensing], survey, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: A. Kovács et al., The Cold Spot is a puzzling large-scale feature in the Cosmic Microwave Background temperature maps and its origin has been subject to active debate. As an important foreground structure at low redshift, the Eridanus supervoid was recently detected, but it was subsequently determined that, assuming the standard ΛCDM model, only about 10–20 per cent of the observed temperature depression can be accounted for via its Integrated Sachs–Wolfe imprint. However, R ≳ 100 h−1Mpc supervoids elsewhere in the sky have shown ISW imprints AISW ≈ 5.2 ± 1.6 times stronger than expected from ΛCDM (AISW = 1), which warrants further inspection. Using the Year-3 redMaGiC catalogue of luminous red galaxies from the Dark Energy Survey, here we confirm the detection of the Eridanus supervoid as a significant underdensity in the Cold Spot’s direction at z < 0.2. We also show, with S/N ≳ 5 significance, that the Eridanus supervoid appears as the most prominent large-scale underdensity in the dark matter mass maps that we reconstructed from DES Year-3 gravitational lensing data. While we report no significant anomalies, an interesting aspect is that the amplitude of the lensing signal from the Eridanus supervoid at the Cold Spot centre is about 30 per cent lower than expected from similar peaks found in N-body simulations based on the standard ΛCDM model with parameters Ωm = 0.279 and σ8 = 0.82. Overall, our results confirm the causal relation between these individually rare structures in the cosmic web and in the CMB, motivating more detailed future surveys in the Cold Spot region., AK has been supported by a Juan de la Cierva Incorporación fellowship with project number IJC2018-037730-I, and funding for this project was also available in part through SEV-2015-0548 and AYA2017-89891-P. 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 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).
Published: 2021

5. The Intrinsic Alignment of Red Galaxies in DES Y1 redMaPPer Galaxy Clusters

Author: Zhou, C., Tong, A., Troxel, M. A., Blazek, J., Lin, C., Bacon, D., Bleem, L., Rosell, A. Carnero, Chang, C., Costanzi, M., DeRose, J., Dietrich, J. P., Drlica-Wagner, A., Gruen, D., Gruendl, R. A., Hoyle, B., Jarvis, M., MacCrann, N., Mawdsley, B., McClintock, T., Melchior, P., Prat, J., Pujol, A., Rozo, E., Rykoff, E. S., Samuroff, S., Sánchez, C., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Tucker, D. L., Varga, T. N., Yanny, B., Zhang, Y., Zuntz, J., Alves, O., Amon, A., Bertin, E., Brooks, D., Burke, D. L., Kind, M. Carrasco, da Costa, L. N., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Gerdes, D. W., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Raveri, M., Romer, A. K., Sanchez, E., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Weaverdyck, N., Weller, J., and Wiseman, P.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Clusters of galaxies are sensitive to the most nonlinear peaks in the cosmic density field. The weak gravitational lensing of background galaxies by clusters can allow us to infer their masses. However, galaxies associated with the local environment of the cluster can also be intrinsically aligned due to the local tidal gradient, contaminating any cosmology derived from the lensing signal. We measure this intrinsic alignment in Dark Energy Survey (DES) Year 1 redMaPPer clusters. We find evidence of a non-zero mean radial alignment of galaxies within clusters between redshift 0.1-0.7. We find a significant systematic in the measured ellipticities of cluster satellite galaxies that we attribute to the central galaxy flux and other intracluster light. We attempt to correct this signal, and fit a simple model for intrinsic alignment amplitude ($A_{\textrm{IA}}$) to the measurement, finding $A_{\textrm{IA}}=0.15\pm 0.04$, when excluding data near the edge of the cluster. We find a significantly stronger alignment of the central galaxy with the cluster dark matter halo at low redshift and with higher richness and central galaxy absolute magnitude (proxies for cluster mass). This is an important demonstration of the ability of large photometric data sets like DES to provide direct constraints on the intrinsic alignment of galaxies within clusters. These measurements can inform improvements to small-scale modeling and simulation of the intrinsic alignment of galaxies to help improve the separation of the intrinsic alignment signal in weak lensing studies., 14 pages, 13 figures
Published: 2023

6. Mapping gas around massive galaxies: cross-correlation of DES Y3 galaxies and Compton-$y$-maps from SPT and Planck

Author: Sánchez, J., Omori, Y., Chang, C., Bleem, L. E., Crawford, T., Drlica-Wagner, A., Raghunathan, S., Zacharegkas, G., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Alves, O., Amon, A., Avila, S., Baxter, E., Bechtol, K., Benson, B. A., Bernstein, G. M., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Campos, A., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C. L., Chen, A., Choi, A., Chown, R., Costanzi, M., Crites, A. T., Crocce, M., da Costa, L. N., Pereira, M. E. S., de Haan, T., De Vicente, J., DeRose, J., Desai, S., Diehl, H. T., Dobbs, M. A., Dodelson, S., Doel, P., Elvin-Poole, J., Everett, W., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gatti, M., George, E. M., Gerdes, D. W., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Halverson, N. W., Hinton, S. R., Holder, G. P., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hrubes, J. D., James, D. J., Knox, L., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, A. T., Luong-Van, D., MacCrann, N., Marshall, J. L., McCullough, J., McMahon, J. J., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Mocanu, L., Mohr, J. J., Muir, J., Myles, J., Natoli, T., Padin, S., Palmese, A., Pandey, S., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Pryke, C., Raveri, M., Reichardt, C. L., Rodriguez-Monroy, M., Ross, A. J., Ruhl, J. E., Rykoff, E., Sánchez, C., Sanchez, E., Scarpine, V., Schaffer, K. K., Sevilla-Noarbe, I., Sheldon, E., Shirokoff, E., Smith, M., Soares-Santos, M., Staniszewski, Z., Stark, A. A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Vieira, J. D., Vincenzi, M., Weaverdyck, N., Williamson, R., Yanny, B., Yin, B., 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), CEA/DSM Centre de Saclay (CEA/DSM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), DES, and SPT
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), cosmology: observations, FOS: Physical sciences, galaxies: structure, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We cross-correlate positions of galaxies measured in data from the first three years of the Dark Energy Survey with Compton-$y$-maps generated using data from the South Pole Telescope (SPT) and the {\it Planck} mission. We model this cross-correlation measurement together with the galaxy auto-correlation to constrain the distribution of gas in the Universe. We measure the hydrostatic mass bias or, equivalently, the mean halo bias-weighted electron pressure $\langle b_{h}P_{e}\rangle$, using large-scale information. We find $\langle b_{h}P_{e}\rangle$ to be $[0.16^{+0.03}_{-0.04},0.28^{+0.04}_{-0.05},0.45^{+0.06}_{-0.10},0.54^{+0.08}_{-0.07},0.61^{+0.08}_{-0.06},0.63^{+0.07}_{-0.08}]$ meV cm$^{-3}$ at redshifts $z \sim [0.30, 0.46, 0.62,0.77, 0.89, 0.97]$. These values are consistent with previous work where measurements exist in the redshift range. We also constrain the mean gas profile using small-scale information, enabled by the high-resolution of the SPT data. We compare our measurements to different parametrized profiles based on the cosmo-OWLS hydrodynamical simulations. We find that our data are consistent with the simulation that assumes an AGN heating temperature of $10^{8.5}$K but are incompatible with the model that assumes an AGN heating temperature of $10^{8.0}$K. These comparisons indicate that the data prefer a higher value of electron pressure than the simulations within $r_{500c}$ of the galaxies' halos., Comment: 20 pages, 9 figures. Submitted to MNRAS
Published: 2023

7. The Dark Energy Survey Six-Year Calibration Star Catalog

Author: Rykoff, E. S., Tucker, D. L., Burke, D. L., Allam, S. S., Bechtol, K., Bernstein, G. M., Brout, D., Gruendl, R. A., Lasker, J., Smith, J. A., Wester, W. C., Yanny, B., Abbott, T. M. C., Aguena, M., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Rosell, A. Carnero, Carretero, J., Castander, F. J., Choi, A., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Giannini, G., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., James, D. J., Kuehn, K., Lahav, O., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Myles, J., Nord, B. D., Ogando, R. L. C., Palmese, A., Pieres, A., Malagón, A. A. Plazas, Raveri, M., Rodgríguez-Monroy, M., Sanchez, E., Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Varga, T. N., Vincenzi, M., Walker, A. R., Weaverdyck, N., and Wiseman, P.
Subjects: FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: This Technical Note presents a catalog of calibrated reference stars that was generated by the Forward Calibration Method (FGCM) pipeline (arXiv:1706.01542) as part of the FGCM photometric calibration of the full Dark Energy Survey (DES) 6-Year data set (Y6). This catalog provides DES grizY magnitudes for 17 million stars with i-band magnitudes mostly in the range 16 < i < 21 spread over the full DES footprint covering 5000 square degrees over the Southern Galactic Cap at galactic latitudes b < -20 degrees (plus a few outlying fields disconnected from the main survey footprint). These stars are calibrated to a uniformity of better than 1.8 milli-mag (0.18%) RMS over the survey area. The absolute calibration of the catalog is computed with reference to the STISNIC.007 spectrum of the Hubble Space Telescope CalSpec standard star C26202; including systematic errors, the absolute flux system is known at the approximately 1% level. As such, these stars provide a useful reference catalog for calibrating grizY-band or grizY-like band photometry in the Southern Hemisphere, particularly for observations within the DES footprint., 21 pages, 15 figures, Fermilab Technical Note. Official Data Access Site: https://des.ncsa.illinois.edu/releases/other ; Temporary Data Access Site: https://data.darkenergysurvey.org/public_calib/DES_6yr_CalibStarCat/index.html
Published: 2023
Full Text: View/download PDF

8. Cosmological constraints from the tomography of DES-Y3 galaxies with CMB lensing from ACT DR4

Author: Marques, G. A., Madhavacheril, M. S., Darwish, O., Shaikh, S., Aguena, M., Alves, O., Avila, S., Bacon, D., Baxter, E. J., Bechtol, K., Becker, M. R., Bertin, E., Blazek, J., Bond, J. Richard, Brooks, D., Cai, H., Calabrese, E., Rosell, A. Carnero, Carretero, M. Carrasco Kind J., Cawthon, R., Crocce, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Doux, C., Drlica-Wagner, A., Dunkley, J., Elvin-Poole, J., Everett, S., Ferraro, Simone, Ferrero, I., Flaugher, B., Fosalba, P., García-Bellido, J., Gatti, M., Giannini, G., Gluscevic, V., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hill, J. Colin, Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., Jeffrey, N., Kim, J., Kuehn, K., Lahav, O., Lemos, P., Lima, M., Huffenberger, K. M., MacCrann, N., Marshall, J. L., Mena-Fernández, J., Miquel, R., Mohr, J. J., Moodley, K., Muir, J., Naess, S., Nati, F., Page, L. A., Palmese, A., Malagón, A. A. Plazas, Porredon, A., Prat, J., Qu, F. J., Raveri, M., Ross, A. J., Rykoff, E. S., Farren, G. S., Samuroff, S., Sanchez, E., Schubnell, M., Sevilla-Noarbe, I., Sheldon, E., Sherwin, B. D., Sifón, C., Smith, M., Spergel, D. N., Staggs, S. T., Suchyta, E., Tarle, G., To, C., Van Engelen, A., Weaverdyck, N., Weller, J., Wenzl, L., Wiseman, P., Wollack, E. J., and Yanny, B.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a measurement of the cross-correlation between the MagLim galaxies selected from the Dark Energy Survey (DES) first three years of observations (Y3) and cosmic microwave background (CMB) lensing from the Atacama Cosmology Telescope (ACT) Data Release 4 (DR4), reconstructed over $\sim 436$ sq.deg. of the sky. Our galaxy sample, which covers $\sim 4143$ sq.deg., is divided into six redshift bins spanning the redshift range of $0.20, Comment: 42 pages, 17 figures
Published: 2023
Full Text: View/download PDF

9. Ultracool dwarfs candidates based on six years of the Dark Energy Survey data

Author: Ponte, M. dal, Santiago, B., Rosell, A. Carnero, De Paris, L., Pace, A. B., Bechtol, K., Abbott, T. M. C., Aguena, M., Allam, S., Alves, O., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Kind, M. Carrasco, Carretero, J., Conselice, C., Costanzi, M., Desai, S., De Vicente, J., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., James, D. J., Kuehn, K., Kuropatkin, N., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Malagón, A. A. Plazas, Pieres, A., Raveri, M., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Weaverdyck, N.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We present a sample of 19,583 ultracool dwarf candidates brighter than z $\leq 23$ selected from the Dark Energy Survey DR2 coadd data matched to VHS DR6, VIKING DR5 and AllWISE covering $\sim$ 4,800 $deg^2$. The ultracool candidates were first pre-selected based on their (i-z), (z-Y), and (Y-J) colours. They were further classified using a method that compares their optical, near-infrared and mid-infrared colours against templates of M, L and T dwarfs. 14,099 objects are presented as new L and T candidates and the remaining objects are from the literature, including 5,342 candidates from our previous work. Using this new and deeper sample of ultracool dwarf candidates we also present: 20 new candidate members to nearby young moving groups (YMG) and associations, variable candidate sources and four new wide binary systems composed of two ultracool dwarfs. Finally, we also show the spectra of twelve new ultracool dwarfs discovered by our group and presented here for the first time. These spectroscopically confirmed objects are a sanity check of our selection of ultracool dwarfs and photometric classification method., Comment: 18 pages, 10 figures, 7 tables. Accepted for publication in MNRAS
Published: 2023
Full Text: View/download PDF

10. Synchronous rotation in the (136199) Eris-Dysnomia system

Author: Bernstein, G. M., Holler, B. J., Navarro-Escamilla, R., Bernardinelli, P. H., Abbott, T. M. C., Aguena, M., Allam, S., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Brooks, D., Burke, D. L., Rosell, A. Carnero, Carretero, J., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Doel, P., Drlica-Wagner, A., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gutierrez, G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Marshall, J. L., Mena-Fernández, J., Miquel, R., Ogando, R. L. C., Pieres, A., Malagón, A. A. Plazas, Raveri, M., Reil, K., Sanchez, E., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., and Wiseman, P.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We combine photometry of Eris from a 6-month campaign on the Palomar 60-inch telescope in 2015, a 1-month Hubble Space Telescope WFC3 campaign in 2018, and Dark Energy Survey data spanning 2013--2018 to determine a light curve of definitive period $15.771\pm 0.008$~days (1-$\sigma$ formal uncertainties), with nearly sinusoidal shape and peak-to-peak flux variation of 3\%. This is consistent at part-per-thousand precision with the $P=15.78590\pm0.00005$~day period of Dysnomia's orbit around Eris, strengthening the recent detection of synchronous rotation of Eris by Szakats et al (2022) with independent data. Photometry from Gaia is consistent with the same light curve. We detect a slope of $0.05\pm0.01$~mag per degree of Eris' brightness with respect to illumination phase, intermediate between Pluto's and Charon's values. Variations of $0.3$~mag are detected in Dysnomia's brightness, plausibly consistent with a double-peaked light curve at the synchronous period. The synchronous rotation of Eris is consistent with simple tidal models initiated with a giant-impact origin of the binary, but is difficult to reconcile with gravitational capture of Dysnomia by Eris., Comment: Submitted to Planetary Science Journal
Published: 2023
Full Text: View/download PDF

11. Dark Energy Survey Year 3 results: Constraints on extensions to Λ CDM with weak lensing and galaxy clustering

Author: Abbott, T. M. C., Aguena, M., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Annis, J., Avila, S., Bacon, D., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Birrer, S., Blazek, J., Bocquet, S., Brandao-Souza, A., Bridle, S. L., Brooks, D., 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., Pereira, M. E. S., Davis, C., Davis, T. M., Derose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Farahi, A., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Friedel, D., Friedrich, O., Frieman, J., García-Bellido, J., Gatti, M., Giani, L., Giannantonio, T., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hamaus, N., Harrison, I., Hartley, W. G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huang, H., Huff, E. M., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeffrey, N., Jeltema, T., Kovacs, A., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, S., Leget, P. -F., Lemos, P., Leonard, C. D., Liddle, A. R., Lima, M., Lin, H., Maccrann, N., Marshall, J. L., Mccullough, J., Mena-Fernández, J., Menanteau, F., Miquel, R., Miranda, V., Mohr, J. J., Muir, J., Myles, J., Nadathur, S., Navarro-Alsina, A., Nichol, R. C., Ogando, R. L. C., Omori, Y., Palmese, A., Pandey, S., Park, Y., Paterno, M., Paz-Chinchón, F., Percival, W. J., Pieres, A., Plazas Malagón, A. A., Porredon, A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rogozenski, P., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Sanchez Cid, D., Scarpine, V., Scolnic, D., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Smith, M., Soares-Santos, M., Suchyta, E., Tabbutt, M., Tarle, G., Thomas, D., To, C., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Vincenzi, M., Walker, A. R., Weaverdyck, N., Wechsler, R. H., Weller, J., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., and Des, Collaboration
Published: 2023

12. Velocity dispersions of clusters in the Dark Energy Survey Y3 redMaPPer catalogue

Author: A Wetzell, V., Jeltema, T. E., Hegland, B., Everett, S., Giles, P. A., Wilkinson, R., Farahi, A., Costanzi, M., Hollowood, D. L., Upsdell, E., Saro, A., Myles, J., Bermeo, A., Bhargava, S., Collins, C. A., Cross, D., Eiger, O., Gardner, G., Hilton, M., Jobel, J., Kelly, P., Laubner, D., Liddle, A. R., Mann, R. G., Martinez, V., Mayers, J., Mcdaniel, A., Romer, A. K., Rooney, P., Sahlen, M., Stott, J., Swart, A., Turner, D. J., Viana, P. T. P., Abbott, T. M. C., Aguena, M., Allam, S., Andrade- Oliveira, F., Annis, J., Asorey, J., Bertin, E., Burke, D. L., Calcino, J., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Choi, A., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lewis, G. F., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, B. E., Tucker, D. L., Varga, T. N., Weller, J., Des, Collaboration, UAM. Departamento de Física Teórica, A Wetzell, V., Jeltema, T. E., Hegland, B., Everett, S., Giles, P. A., Wilkinson, R., Farahi, A., Costanzi, M., Hollowood, D. L., Upsdell, E., Saro, A., Myles, J., Bermeo, A., Bhargava, S., Collins, C. A., Cross, D., Eiger, O., Gardner, G., Hilton, M., Jobel, J., Kelly, P., Laubner, D., Liddle, A. R., Mann, R. G., Martinez, V., Mayers, J., Mcdaniel, A., Romer, A. K., Rooney, P., Sahlen, M., Stott, J., Swart, A., Turner, D. J., Viana, P. T. P., Abbott, T. M. C., Aguena, M., Allam, S., Andrade- Oliveira, F., Annis, J., Asorey, J., Bertin, E., Burke, D. L., Calcino, J., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Choi, A., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lewis, G. F., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, B. E., Tucker, D. L., Varga, T. N., Weller, J., Des, Collaboration, Department of Energy (US), European Commission, European Research Council, Ministero dell'Istruzione, dell'Università e della Ricerca, Ministerio de Ciencia, Innovación y Universidades (España), Fundação para a Ciência e a Tecnologia (Portugal), Agencia Estatal de Investigación (España), National Science Foundation (US), Generalitat de Catalunya, and Ministerio de Economía y Competitividad (España)
Subjects: X-Rays: Galaxies: Clusters, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Física, Astronomy and Astrophysics, galaxies: clusters: general, X-rays: galaxies: clusters, Astrophysics::Cosmology and Extragalactic Astrophysics, Space and Planetary Science, clusters: general [galaxies], galaxies: clusters [X-rays], CLUSTERS, QC, Astrophysics - Cosmology and Nongalactic Astrophysics, QB, Galaxies: Clusters: General
Abstract: DES Collaboration: V. Wetzell et al., We measure the velocity dispersions of clusters of galaxies selected by the red-sequence Matched-filter Probabilistic Percolation (redMaPPer) algorithm in the first three years of data from the Dark Energy Survey (DES), allowing us to probe cluster selection and richness estimation, λ, in light of cluster dynamics. Our sample consists of 126 clusters with sufficient spectroscopy for individual velocity dispersion estimates. We examine the correlations between cluster velocity dispersion, richness, X-ray temperature, and luminosity, as well as central galaxy velocity offsets. The velocity dispersion–richness relation exhibits a bimodal distribution. The majority of clusters follow scaling relations between velocity dispersion, richness, and X-ray properties similar to those found for previous samples; however, there is a significant population of clusters with velocity dispersions that are high for their richness. These clusters account for roughly 22 per cent of the λ < 70 systems in our sample, but more than half (55 per cent) of λ < 70 clusters at z > 0.5. A couple of these systems are hot and X-ray bright as expected for massive clusters with richnesses that appear to have been underestimated, but most appear to have high velocity dispersions for their X-ray properties likely due to line-of-sight structure. These results suggest that projection effects contribute significantly to redMaPPer selection, particularly at higher redshifts and lower richnesses. The redMaPPer determined richnesses for the velocity dispersion outliers are consistent with their X-ray properties, but several are X-ray undetected and deeper data are needed to understand their nature., This work was supported by the U.S. Department of Energy, Office of Science, Office of High Energy Physics, under Award Numbers DE-SC0010107 and A00-1465-001. AS is supported by the ERC-StG ‘ClustersXCosmo’ grant agreement 716762, by the FARE-MIUR grant ’ClustersXEuclid’ R165SBKTMA, and by INFN InDark Grant. PTPV was supported by Fundação para a Ciência e a Tecnologia (FCT) through research grants UIDB/04434/2020andUIDP/04434/2020. 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 University of Illinois at Urbana-Champaign - National Center for Supercomputing Applications, 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, 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 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, 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. This study is 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 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 EU Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This paper has been authored by Fermi Research Alliance, LLC under contract no. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2022

13. Dark Energy Survey Year 3 results: Cosmology from combined galaxy clustering and lensing validation on cosmological simulations

Author: DeRose, J., Wechsler, R. H., Becker, M. R., Rykoff, E. S., Pandey, S., MacCrann, N., Amon, A., Myles, J., Krause, E., Gruen, D., Jain, B., Troxel, M. A., Prat, J., Alarcon, A., Sanchez, C., Blazek, J., Crocce, M., Giannini, G., Gatti, M., Bernstein, G. M., Zuntz, J., Dodelson, S., Fang, X., Friedrich, O., Secco, L. F., Elvin-Poole, J., Porredon, A., Everett, S., Choi, A., Harrison, I., Cordero, J., Rodriguez-Monroy, M., McCullough, J., Cawthon, R., Chen, A., Alves, O., Andrade-Oliveira, F., Bechtol, K., Camacho, H., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Gruendl, R. A., Hartley, W. G., Huang, H., Huff, E. M., Kuropatkin, N., Raveri, M., Rosenfeld, R., Ross, A. J., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Yanny, B., Yin, B., Zhang, Y., Fosalba, P., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Castander, F. J., Chang, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Ferte, A., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchon, F., Petravick, D., Pieres, A., Malagon, A. A. Plazas, Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., UAM. Departamento de Física Teórica, A DeRose, J., Wechsler, R. H., Becker, M. R., Rykoff, E. S., Pandey, S., Maccrann, N., Amon, A., Myles, J., Krause, E., Gruen, D., Jain, B., Troxel, M. A., Prat, J., Alarcon, A., Sánchez, C., Blazek, J., Crocce, M., Giannini, G., Gatti, M., Bernstein, G. M., Zuntz, J., Dodelson, S., Fang, X., Friedrich, O., Secco, L. F., Elvin-Poole, J., Porredon, A., Everett, S., Choi, A., Harrison, I., Cordero, J., Rodriguez-Monroy, M., Mccullough, J., Cawthon, R., Chen, A., Alves, O., Andrade-Oliveira, F., Bechtol, K., Camacho, H., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Gruendl, R. A., Hartley, W. G., Huang, H., Huff, E. M., Kuropatkin, N., Raveri, M., Rosenfeld, R., Ross, A. J., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Yanny, B., Yin, B., Zhang, Y., Fosalba, P., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Castander, F. J., Chang, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Malagón, A. A. Plaza, Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., 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), European Commission, European Research Council, and Generalitat de Catalunya
Subjects: data release, Gravitational Lensing, model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), sky surveys, strophysics, FOS: Physical sciences, Física, Astrophysics::Cosmology and Extragalactic Astrophysics, oscillation spectroscopic survey, calibration, des, Dark Energy, Cosmology and Nongalactic Astrophysics, strophysic, challenge, impact, astro-ph.CO, Weak, redshift distributions, sdss, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: J. DeRose et al., We present a validation of the Dark Energy Survey Year 3 (DES Y3) 3×2-point analysis choices by testing them on Buzzard2.0, a new suite of cosmological simulations that is tailored for the testing and validation of combined galaxy clustering and weak-lensing analyses. We show that the buzzard2.0 simulations accurately reproduce many important aspects of the DES Y3 data, including photometric redshift and magnitude distributions, and the relevant set of two-point clustering and weak-lensing statistics. We then show that our model for the 3×2-point data vector is accurate enough to recover the true cosmology in simulated surveys assuming the true redshift distributions for our source and lens samples, demonstrating robustness to uncertainties in the modeling of the nonlinear matter power spectrum, nonlinear galaxy bias, and higher-order lensing corrections. Additionally, we demonstrate for the first time that our photometric redshift calibration methodology, including information from photometry, spectroscopy, clustering cross-correlations, and galaxy–galaxy lensing ratios, is accurate enough to recover the true cosmology in simulated surveys in the presence of realistic photometric redshift uncertainties., J. D. is supported by the Chamberlain fellowship at Lawrence Berkeley National Laboratory. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility located at Lawrence Berkeley National Laboratory, operated under Contract No. DE-AC02-05CH11231. We would like to thank Stanford University and the Stanford Research Computing Center for providing computational resources and support that contributed to these research results. 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 DESBrazil 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 LudwigMaximilians 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. This paper is 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. AST1138766andNo.AST-1536171.The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I.F. A.E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (Grant No. FP7/2007-2013) including ERC Grants No. 240672, No.291329,andNo.306478.Weacknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia(INCT)doe-Universo(CNPqGrantNo.465376/ 2014-2). This manuscript has been authored by Fermi Research Alliance, LLC, under Contract No. DE-AC0207CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2022

14. The Dark Energy Survey Year 3 and eBOSS: constraining galaxy intrinsic alignments across luminosity and colour space

Author: Samuroff, S., Mandelbaum, R., Blazek, J., Campos, A., MacCrann, N., Zacharegkas, G., Amon, A., Prat, J., Singh, S., Elvin-Poole, J., Ross, A. J., Alarcon, A., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Rosell, A. Carnero, Kind, M. Carrasco, Cawthon, R., Chang, C., Chen, R., Choi, A., Crocce, M., Davis, C., DeRose, J., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Everett, S., Ferté, A., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Herner, K., Huff, E. M., Jarvis, M., Kuropatkin, N., Leget, P. -F., Lemos, P., McCullough, J., Myles, J., Navarro-Alsina, A., Pandey, S., Porredon, A., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Roodman, A., Rossi, G., Rykoff, E. S., Sánchez, C., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troxel, M. A., Tutusaus, I., Weaverdyck, N., Yanny, B., Yin, B., Zhang, Y., Aguena, J. Zuntz M., Alves, O., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Marshall, J. L., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Newman, J., Palmese, A., Pieres, A., Malagón, A. A. Plazas, Sanchez, E., Scarpine, V., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., and To, C.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present direct constraints on galaxy intrinsic alignments using the Dark Energy Survey Year 3 (DES Y3), the Extended Baryon Oscillation Spectroscopic Survey (eBOSS) and its precursor, the Baryon Oscillation Spectroscopic Survey (BOSS). Our measurements incorporate photometric red sequence (redMaGiC) galaxies from DES with median redshift $z\sim0.2-1.0$, luminous red galaxies (LRGs) from eBOSS at $z\sim0.8$, and also a SDSS-III BOSS CMASS sample at $z\sim0.5$. We measure two point intrinsic alignment correlations, which we fit using a model that includes lensing, magnification and photometric redshift error. Fitting on scales $6, Comment: Submitted to MNRAS; 22 pages, 11 figures
Published: 2022

15. The Dark Energy Survey Year 3 high redshift sample: Selection, characterization and analysis of galaxy clustering

Author: Sánchez, C., Alarcon, A., Bernstein, G. M., Sanchez, J., Pandey, S., Raveri, M., Prat, J., Weaverdyck, N., Sevilla-Noarbe, I., Chang, C., Baxter, E., Omori, Y., Jain, B., Alves, O., Amon, A., Bechtol, K., Becker, M. R., Blazek, J., Choi, A., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Crocce, M., Cross, D., Derose, J., Diehl, H. T., Dodelson, S., Drlicawagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Everett, S., Xiao Fang, Fosalba, P., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Huang, H., Huff, E. M., Kuropatkin, N., Maccrann, N., Mccullough, J., Myles, J., Krause, E., Porredon, A., Rodriguezmonroy, M., Rykoff, E. S., Secco, L. F., Sheldon, E., Troxel, M. A., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Castander, F. J., Cawthon, R., Conselice, C., Costanzi, M., Pereira, M. E. S., Desai, S., Doel, P., Doux, C., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gutierrez, G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., and HEP, INSPIRE
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The fiducial cosmological analyses of imaging galaxy surveys like the Dark Energy Survey (DES) typically probe the Universe at redshifts $z < 1$. This is mainly because of the limited depth of these surveys, and also because such analyses rely heavily on galaxy lensing, which is more efficient at low redshifts. In this work we present the selection and characterization of high-redshift galaxy samples using DES Year 3 data, and the analysis of their galaxy clustering measurements. In particular, we use galaxies that are fainter than those used in the previous DES Year 3 analyses and a Bayesian redshift scheme to define three tomographic bins with mean redshifts around $z \sim 0.9$, $1.2$ and $1.5$, which significantly extend the redshift coverage of the fiducial DES Year 3 analysis. These samples contain a total of about 9 million galaxies, and their galaxy density is more than 2 times higher than those in the DES Year 3 fiducial case. We characterize the redshift uncertainties of the samples, including the usage of various spectroscopic and high-quality redshift samples, and we develop a machine-learning method to correct for correlations between galaxy density and survey observing conditions. The analysis of galaxy clustering measurements, with a total signal-to-noise $S/N \sim 70$ after scale cuts, yields robust cosmological constraints on a combination of the fraction of matter in the Universe $\Omega_m$ and the Hubble parameter $h$, $\Omega_m h = 0.195^{+0.023}_{-0.018}$, and 2-3% measurements of the amplitude of the galaxy clustering signals, probing galaxy bias and the amplitude of matter fluctuations, $b \sigma_8$. A companion paper $\textit{(in preparation)}$ will present the cross-correlations of these high-$z$ samples with CMB lensing from Planck and SPT, and the cosmological analysis of those measurements in combination with the galaxy clustering presented in this work., Comment: 28 pages, 25 figures. To be submitted to MNRAS. Comments welcome
Published: 2022

16. The Observed Evolution of the Stellar Mass-Halo Mass Relation for Brightest Central Galaxies

Author: Golden-Marx, Jesse B., Miller, C. J., Zhang, Y., Ogando, R. L. C., Palmese, A., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F. [UNESP], Annis, J., Bacon, D., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Costanzi, M., Crocce, M., Costa, L. N. da, Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Ferrero, I, Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchon, F., Petravick, D., Pieres, A., Malagon, A. A. Plazas, Prat, J., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V, Schubnell, M., Serrano, S., Sevilla-Noarbe, I, Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Varga, T. N., DES Collaboration, Golden-Marx, JB [0000-0002-6394-045X], Zhang, Y [0000-0001-5969-4631], Ogando, RLC [0000-0003-2120-1154], Palmese, A [0000-0002-6011-0530], Abbott, TMC [0000-0003-1587-3931], Aguena, M [0000-0001-5679-6747], Annis, J [0000-0002-0609-3987], Bacon, D [0000-0002-2562-8537], Bertin, E [0000-0002-3602-3664], Brooks, D [0000-0002-8458-5047], Carnero Rosell, A [0000-0003-3044-5150], Carrasco Kind, M [0000-0002-4802-3194], Castander, FJ [0000-0001-7316-4573], Costanzi, M [0000-0001-8158-1449], Crocce, M [0000-0002-9745-6228], Da Costa, LN [0000-0002-7731-277X], De Vicente, J [0000-0001-8318-6813], Desai, S [0000-0002-0466-3288], Diehl, HT [0000-0002-8357-7467], Drlica-Wagner, A [0000-0001-8251-933X], Evrard, AE [0000-0002-4876-956X], Ferrero, I [0000-0002-1295-1132], Fosalba, P [0000-0002-1510-5214], 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], Gruendl, RA [0000-0002-4588-6517], Gschwend, J [0000-0003-3023-8362], Hinton, SR [0000-0003-2071-9349], Hollowood, DL [0000-0002-9369-4157], Jeltema, T [0000-0001-6089-0365], Kuehn, K [0000-0003-0120-0808], Kuropatkin, N [0000-0003-2511-0946], 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], Paz-Chinchón, F [0000-0003-1339-2683], Pieres, A [0000-0001-9186-6042], Romer, AK [0000-0002-9328-879X], Sanchez, E [0000-0002-9646-8198], Serrano, S [0000-0002-0211-2861], Sevilla-Noarbe, I [0000-0002-1831-1953], Soares-Santos, M [0000-0001-6082-8529], Tarle, G [0000-0003-1704-0781], Apollo - University of Cambridge Repository, National Science Foundation (US), Ministerio de Ciencia e Innovación (España), European Commission, UAM. Departamento de Física Teórica, A Golden-Marx, Jesse B., Miller, C. J., Zhang, Y., Ogando, R. L. C., Palmese, A., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Buckley-Geer, E., Carnero Rosell, A., Carrasco Kind, M., Castander, F. J., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Prat, J., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares- Santos, M., Suchyta, E., Tarle, G., Varga, T. N., Shanghai Jiao Tong Univ, Univ Michigan, Fermilab Natl Accelerator Lab, Lab Interinst E Astron LIneA, Observ Nacl, Univ Chicago, NSFs Natl Opt Infrared Astron Res Lab, Universidade Estadual Paulista (UNESP), Univ Portsmouth, Inst Astrophys Paris, UPMC Univ Paris 06, UCL, Inst Astrofis Canarias, Univ La Laguna, Natl Ctr Supercomp Applicat, Univ Illinois, Inst Estudis Espacials Catalunya IEEC, CSIC, Univ Trieste, INAF Osservatorio Astron Trieste, Inst Fundamental Phys Universe, Ctr Invest Energet Medioambientales & Tecnol CIEM, IIT Hyderabad, Santa Cruz Inst Particle Phys, Univ Oslo, Univ Autonoma Madrid, Stanford Univ, SLAC Natl Accelerator Lab, Univ Geneva, Univ Queensland, Ohio State Univ, Ludwig Maximilians Univ Munchen, Ctr Astrophys Harvard & Smithsonian, Lawrence Berkeley Natl Lab, Univ Arizona, Macquarie Univ, Lowell Observ, Universidade de São Paulo (USP), Texas A&M Univ, Princeton Univ, Inst Catalana Recerca & Estudis Avancats, Barcelona Inst Sci & Technol, Max Planck Inst Extraterr Phys, Univ Wisconsin, Univ Cambridge, Univ Sussex, Univ Fed Rio Grande do Sul, Univ Southampton, and Oak Ridge Natl Lab
Subjects: Galaxy clusters, Galaxy evolution, Brightest cluster galaxies, astro-ph.GA, FOS: Physical sciences, Física, Galaxy cluster, Astronomy and Astrophysics, GALÁXIAS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Galaxy Astrophysics
Abstract: Golden-Marx; J. B. et al. (DES Collaboration), We quantify evolution in the cluster-scale stellar mass-halo mass (SMHM) relation's parameters using 2323 clusters and brightest central galaxies (BCGs) over the redshift range 0.03 ≤ z ≤ 0.60. The precision on the inferred SMHM parameters is improved by including the magnitude gap (m gap) between the BCG and fourth-brightest cluster member (M14) as a third parameter in the SMHM relation. At fixed halo mass, accounting for m gap, through a stretch parameter, reduces the SMHM relation's intrinsic scatter. To explore this redshift range, we use clusters, BCGs, and cluster members identified using the Sloan Digital Sky Survey C4 and redMaPPer cluster catalogs and the Dark Energy Survey redMaPPer catalog. Through this joint analysis, we detect no systematic differences in BCG stellar mass, m gap, and cluster mass (inferred from richness) between the data sets. We utilize the Pareto function to quantify each parameter's evolution. We confirm prior findings of negative evolution in the SMHM relation's slope (3.5σ), and detect negative evolution in the stretch parameter (4.0σ) and positive evolution in the offset parameter (5.8σ). This observed evolution, combined with the absence of BCG growth, when stellar mass is measured within 50 kpc, suggests that this evolution results from changes in the cluster's m gap. For this to occur, late-term growth must be in the intracluster light surrounding the BCG. We also compare the observed results to IllustrisTNG 300-1 cosmological hydrodynamic simulations and find modest qualitative agreement. However, the simulations lack the evolutionary features detected in the real data., 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 Ciênciae Tecnologia (INCT) do e-Universo (CNPq grant 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.
Published: 2022

17. 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

18. Dark Energy Survey Year 3 results: Measurement of the baryon acoustic oscillations with three-dimensional clustering

Author: Chan, K. C., Avila, S., Carnero Rosell, A., Ferrero, I., Elvin-Poole, J., Sanchez, E., Camacho, H., Porredon, A., Crocce, M., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Conselice, C., Costanzi, M., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Flaugher, B., Fosalba, P., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Lahav, O., Lidman, C., Lima, M., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Raveri, M., Rodriguez-Monroy, M., Roodman, A., Ross, A. J., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vincenzi, M., Weaverdyck, N., Des, Collaboration, Chan, K. C., Avila, S., Carnero Rosell, A., Ferrero, I., Elvin-Poole, J., Sanchez, E., Camacho, H., Porredon, A., Crocce, M., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Conselice, C., Costanzi, M., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Flaugher, B., Fosalba, P., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Lahav, O., Lidman, C., Lima, M., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Raveri, M., Rodriguez-Monroy, M., Roodman, A., Ross, A. J., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vincenzi, M., Weaverdyck, N., Des, Collaboration, National Science Foundation (US), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, European Commission, Comunidad de Madrid, Department of Energy (US), Ministerio de Educación y Ciencia (España), Science and Technology Facilities Council (UK), Generalitat de Catalunya, and HEP, INSPIRE
Subjects: Astrophysic, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics, Cosmology and Nongalactic Astrophysics, FOS: Physical sciences, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: K. C. Chan et al., The three-dimensional correlation function offers an effective way to summarize the correlation of the large-scale structure even for imaging galaxy surveys. We have applied the projected three-dimensional correlation function, ξp to measure the baryonic acoustic oscillations (BAO) scale on the first-three years Dark Energy Survey data. The sample consists of about 7 million galaxies in the redshift range 0.6, K. C.C. acknowledges the support from the National Science Foundation of China under the Grants No. 11873102 and No. 12273121, the science research grants from the China Manned Space Project with No. CMS-CSST-2021-B01, and the Science and Technology Program of Guangzhou, China (Grant No. 202002030360). S.A. is supported by the Spanish Agencia Estatal de Investigacion through the grant “IFT Centro de Excelencia Severo Ochoa by CEX2020-001007-S” and “EU-HORIZON-2020-776247 Enabling Weak Lensing Cosmology (EWC)”, and was also supported by Atraccion de Talento Program No. 2019-T1/TIC-12702 granted by the Comunidad de Madrid in Spain. 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 UrbanaChampaign, 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 Minist´erio 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 Energ´eticas, 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, 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. 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 (No. FP7/20072013) 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

19. Milky Way Satellite Census. IV. Constraints on Decaying Dark Matter from Observations of Milky Way Satellite Galaxies

Author: A Mau, S., Nadler, E. O., Wechsler, R. H., Drlica-Wagner, A., Bechtol, K., Green, G., Huterer, D., Li, T. S., Mao, Y. -Y., Martínez-Vázquez, C. E., McNanna, M., Mutlu-Pakdil, B., Pace, A. B., Peter, A., Riley, A. H., Strigari, L., Wang, M. -Y., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., Crocce, M., Pereira, M. E. S., Davis, T. M., Vicente, J. De, Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Maia, M. A. G., Marshall, J. L., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Paz-Chinchón, F., Pieres, A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Tucker, D. L., Weller, J., DES Collaboration, Mau, S [0000-0003-3519-4004], Nadler, EO [0000-0002-1182-3825], Wechsler, RH [0000-0003-2229-011X], Drlica-Wagner, A [0000-0001-8251-933X], Bechtol, K [0000-0001-8156-0429], Green, G [0000-0001-5417-2260], Huterer, D [0000-0001-6558-0112], Li, TS [0000-0002-9110-6163], Mao, YY [0000-0002-1200-0820], Martínez-Vázquez, CE [0000-0002-9144-7726], McNanna, M [0000-0001-5435-7820], Mutlu-Pakdil, B [0000-0001-9649-4815], Pace, AB [0000-0002-6021-8760], Peter, A [0000-0002-8040-6785], Riley, AH [0000-0001-5805-5766], Strigari, L [0000-0001-5672-6079], Wang, MY [0000-0002-8226-6237], Aguena, M [0000-0001-5679-6747], Allam, S [0000-0002-7069-7857], Annis, J [0000-0002-0609-3987], Bacon, D [0000-0002-2562-8537], Bertin, E [0000-0002-3602-3664], Bocquet, S [0000-0002-4900-805X], Brooks, D [0000-0002-8458-5047], Burke, DL [0000-0003-1866-1950], Rosell, AC [0000-0003-3044-5150], Kind, MC [0000-0002-4802-3194], Carretero, J [0000-0002-3130-0204], Costanzi, M [0000-0001-8158-1449], Crocce, M [0000-0002-9745-6228], Davis, TM [0000-0002-4213-8783], Vicente, JD [0000-0001-8318-6813], Desai, S [0000-0002-0466-3288], Ferrero, I [0000-0002-1295-1132], Flaugher, B [0000-0002-2367-5049], Frieman, J [0000-0003-4079-3263], García-Bellido, J [0000-0002-9370-8360], Giannini, G [0000-0002-3730-1750], Gruen, D [0000-0003-3270-7644], Gruendl, RA [0000-0002-4588-6517], Gschwend, J [0000-0003-3023-8362], 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], Kuehn, K [0000-0003-0120-0808], Lahav, O [0000-0002-1134-9035], Maia, MAG [0000-0001-9856-9307], Marshall, JL [0000-0003-0710-9474], Miquel, R [0000-0002-6610-4836], Morgan, R [0000-0002-7016-5471], Ogando, RLC [0000-0003-2120-1154], Paz-Chinchón, F [0000-0003-1339-2683], Pieres, A [0000-0001-9186-6042], Sanchez, E [0000-0002-9646-8198], Serrano, S [0000-0002-0211-2861], Sevilla-Noarbe, I [0000-0002-1831-1953], Suchyta, E [0000-0002-7047-9358], Tarle, G [0000-0003-1704-0781], To, C [0000-0001-7836-2261], Tucker, DL [0000-0001-7211-5729], Weller, J [0000-0002-8282-2010], Apollo - University of Cambridge Repository, UAM. Departamento de Física Teórica, Department of Energy (US), National Science Foundation (US), Ministerio de Educación y Ciencia (España), Kavli Institute for Particle Astrophysics and Cosmology, Science and Technology Facilities Council (UK), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Ministerio de Economía y Competitividad (España), German Research Foundation, Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, European Research Council, A Mau, S., Nadler, E. O., Wechsler, R. H., Drlica-Wagner, A., Bechtol, K., Green, G., Huterer, D., T. S., Li, Mao, Y. -Y., Martínez-Vázquez, C. E., Mcnanna, M., Mutlu-Pakdil, B., Pace, A. B., Peter, A., Riley, A. H., Strigari, L., Wang, M. -Y., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., Crocce, M., Pereira, M. E. S., Davis, T. M., Vicente, J. De, Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Maia, M. A. G., Marshall, J. L., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Paz-Chinchón, F., Pieres, A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Tucker, D. L., Weller, J., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, FOS: Physical sciences, Física, Astronomy and Astrophysics, hep-ph, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy abundances, High Energy Physics - Phenomenology, Halo, High Energy Physics - Phenomenology (hep-ph), Dwarf Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark matter, astro-ph.CO, Dark Matter, Milky Way dark matter halo, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Mau et al., We use a recent census of the Milky Way (MW) satellite galaxy population to constrain the lifetime of particle dark matter (DM). We consider two-body decaying dark matter (DDM) in which a heavy DM particle decays with lifetime τ comparable to the age of the universe to a lighter DM particle (with mass splitting epsilon) and to a dark radiation species. These decays impart a characteristic "kick velocity," Vkick = epsilonc, on the DM daughter particles, significantly depleting the DM content of low-mass subhalos and making them more susceptible to tidal disruption. We fit the suppression of the present-day DDM subhalo mass function (SHMF) as a function of τ and Vkick using a suite of high-resolution zoom-in simulations of MW-mass halos, and we validate this model on new DDM simulations of systems specifically chosen to resemble the MW. We implement our DDM SHMF predictions in a forward model that incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk using an empirical model for the galaxy–halo connection. By comparing to the observed MW satellite population, we conservatively exclude DDM models with τ < 18 Gyr (29 Gyr) for Vkick = 20 kms−1 (40 kms−1) at 95% confidence. These constraints are among the most stringent and robust small-scale structure limits on the DM particle lifetime and strongly disfavor DDM models that have been proposed to alleviate the Hubble and S8 tensions., 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 No. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This 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.
Published: 2022

20. Dark Energy Survey Year 3 results: Cosmology with moments of weak lensing mass maps

Author: Gatti, M., Jain, B., Chang, C., Raveri, M., Zürcher, D., Secco, L., Whiteway, L., Jeffrey, N., Doux, C., Kacprzak, T., Bacon, D., Fosalba, P., Alarcon, A., Amon, A., Bechtol, K., Becker, M., Bernstein, G., Blazek, J., Campos, A., Choi, A., Davis, C., Derose, J., Dodelson, S., Elsner, F., Elvin-Poole, J., Everett, S., Ferte, A., Gruen, D., Harrison, I., Huterer, D., Jarvis, M., Krause, E., Leget, P. F., Lemos, P., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro, A., Pandey, S., Prat, J., Rollins, R. P., Roodman, A., Sanchez, C., Sheldon, E., Shin, T., Troxel, M., Tutusaus, I., Yin, B., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Ferrero, I., García-Bellido, J., Gaztanaga, E., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Rodriguez-Monroyv, M., Romer, A. K., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., DES Collaboration, Gatti, M., Jain, B., Chang, C., Raveri, M., Zürcher, D., Secco, L., Whiteway, L., Jeffrey, N., Doux, C., Kacprzak, T., Bacon, D., Fosalba, P., Alarcon, A., Amon, A., Bechtol, K., Becker, M., Bernstein, G., Blazek, J., Campos, A., Choi, A., Davis, C., Derose, J., Dodelson, S., Elsner, F., Elvin-Poole, J., Everett, S., Ferte, A., Gruen, D., Harrison, I., Huterer, D., Jarvis, M., Krause, E., Leget, P. F., Lemos, P., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro, A., Pandey, S., Prat, J., Rollins, R. P., Roodman, A., Sanchez, C., Sheldon, E., Shin, T., Troxel, M., Tutusaus, I., Yin, B., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Ferrero, I., García-Bellido, J., Gaztanaga, E., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Rodriguez-Monroyv, M., Romer, A. K., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Des, Collaboration, UAM. Departamento de Física Teórica, Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, European Commission, Agencia Estatal de Investigación (España), Generalitat de Catalunya, Ministerio de Economía y Competitividad (España), Department of Energy (US), National Aeronautics and Space Administration (US), and National Science Foundation (US)
Subjects: Gravitational Lensing, data-compression, inference, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Física, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, parameter-estimation, universe, Dark Energy, Astrophysic, cosmic shear 2-point, model predictions, galaxy, simulations, Weak, peak statistics, constraints, Cosmology and Nongalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: M. Gatti et al., We present a cosmological analysis using the second and third moments of the weak lensing mass (convergence) maps from the first three years of data (Y3) data of the Dark Energy Survey. The survey spans an effective area of 4139 square degrees and uses the images of over 100 million galaxies to reconstruct the convergence field. The second moment of the convergence as a function of smoothing scale contains information similar to standard shear 2-point statistics. The third moment, or the skewness, contains additional non-Gaussian information. The data is analyzed in the context of the ΛCDM model, varying five cosmological parameters and 19 nuisance parameters modeling astrophysical and measurement systematics. Our modeling of the observables is completely analytical, and has been tested with simulations in our previous methodology study. We obtain a 1.7% measurement of the amplitude of fluctuations parameter S8≡σ8(Ωm/0.3)0.5=0.784±0.013. The measurements are shown to be internally consistent across redshift bins, angular scales, and between second and third moments. In particular, the measured third moment is consistent with the expectation of gravitational clustering under the ΛCDM model. The addition of the third moment improves the constraints on S8 and Ωm by ∼15% and ∼25% compared to an analysis that only uses second moments. We compare our results with Planck constraints from the cosmic microwave background, finding a 2.2–2.8σ tension in the full parameter space, depending on the combination of moments considered. The third moment, independently, is in 2.8σ tension with Planck, and thus provides a cross-check on the analyses of 2-point correlations., 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. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grant agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). 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

21. 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

22. Dark energy survey year 3 results: High-precision measurement and modeling of galaxy-galaxy lensing

Author: Prat, J., Blazek, J., Sánchez, C., Tutusaus, I., Pandey, S., Elvin-Poole, J., Krause, E., Troxel, M. A., Secco, L. F., Amon, A., Derose, J., Zacharegkas, G., Chang, C., Jain, B., Maccrann, N., Park, Y., Sheldon, E., Giannini, G., Bocquet, S., To, C., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Choi, A., Cordero, J., Crocce, M., Davis, C., De Vicente, J., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Everett, S., Fang, X., Farahi, A., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Jarvis, M., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Porredon, A., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Shin, T., Troja, A., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., 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., James, D. J., Kuehn, K., Lahav, O., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Plazas Malagón, A. A., Sanchez, E., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Weller, J., Des, Collaboration, A Prat, J., Blazek, J., Sánchez, C., Tutusaus, I., Pandey, S., Elvin- Poole, J., Krause, E., Troxel, M. A., Secco, L. F., Amon, A., Derose, J., Zacharegkas, G., Chang, C., Jain, B., Maccrann, N., Park, Y., Sheldon, E., Giannini, G., Bocquet, S., To, C., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Choi, A., Cordero, J., Crocce, M., Davis, C., De Vicente, J., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Everett, S., Fang, X., Farahi, A., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Jarvis, M., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., Mccullough, J., Muir, J., Myles, J., Navarro- Alsina, A., Porredon, A., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Shin, T., Troja, A., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., 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., James, D. J., Kuehn, K., Lahav, O., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Plazas Malagón, A. A., Sanchez, E., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Weller, J., and UAM. Departamento de Física Teórica
Subjects: Gravitational Lensing, Cosmology and Nongalactic Astrophysics (astro-ph.CO), cosmological parameter constraints, FOS: Physical sciences, Física, marginalization, Astrophysics::Cosmology and Extragalactic Astrophysics, calibration, Astrophysics, Dark Energy, Astrophysic, Cosmology and Nongalactic Astrophysics, redshift distribution, mass, Weak, photometric data set, sdss, cosmic shear, Astrophysics - Cosmology and Nongalactic Astrophysics, intrinsic alignments
Abstract: DES Collaboration: J. Prat et al., We present and characterize the galaxy-galaxy lensing signal measured using the first three years of data from the Dark Energy Survey (DES Y3) covering 4132 deg2. These galaxy-galaxy measurements are used in the DES Y3 3×2pt cosmological analysis, which combines weak lensing and galaxy clustering information. We use two lens samples: a magnitude-limited sample and the redmagic sample, which span the redshift range ∼0.2–1 with 10.7 and 2.6 M galaxies, respectively. For the source catalog, we use the metacalibration shape sample, consisting of ≃100M galaxies separated into four tomographic bins. Our galaxy-galaxy lensing estimator is the mean tangential shear, for which we obtain a total SNR of ∼148 for maglim (∼120 for redmagic), and ∼67 (∼55) after applying the scale cuts of 6Mpc/h. Thus we reach percent-level statistical precision, which requires that our modeling and systematic-error control be of comparable accuracy. The tangential shear model used in the 3×2pt cosmological analysis includes lens magnification, a five-parameter intrinsic alignment model, marginalization over a point mass to remove information from small scales and a linear galaxy bias model validated with higher-order terms. We explore the impact of these choices on the tangential shear observable and study the significance of effects not included in our model, such as reduced shear, source magnification, and source clustering. We also test the robustness of our measurements to various observational and systematics effects, such as the impact of observing conditions, lens-source clustering, random-point subtraction, scale-dependent metacalibration responses, point spread function residuals, and B modes.
Published: 2022

23. Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and galaxy-galaxy lensing using the MagLim lens sample

Author: Porredon, A., Crocce, M., Elvin-Poole, J., Cawthon, R., Giannini, G., De Vicente, J., Carnero Rosell, A., Ferrero, I., Krause, E., Fang, X., Prat, J., Rodriguez-Monroy, M., Pandey, S., Pocino, A., Castander, F. J., Choi, A., Amon, A., Tutusaus, I., Dodelson, S., Sevilla-Noarbe, I., Fosalba, P., Gaztanaga, E., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Camacho, H., Campos, A., Carrasco Kind, M., Chintalapati, P., Cordero, J., Derose, J., Di Valentino, E., Doux, C., Eifler, T. F., Everett, S., Ferté, A., Friedrich, O., Gatti, M., Gruen, D., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jain, B., Jarvis, M., Lee, S., Lemos, P., Maccrann, N., Mena-Fernández, J., Muir, J., Myles, J., Park, Y., Raveri, M., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Sanchez Cid, D., Scolnic, D., Secco, L. F., Sheldon, E., Troja, A., Troxel, M. A., Weaverdyck, N., Yanny, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., 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., Romer, A. K., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Des, Collaboration, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Generalitat de Catalunya, European Research Council, Department of Energy (US), National Science Foundation (US), National Aeronautics and Space Administration (US), Porredon, A., Crocce, M., Elvin-Poole, J., Cawthon, R., Giannini, G., De Vicente, J., Carnero Rosell, A., Ferrero, I., Krause, E., Fang, X., Prat, J., Rodriguez-Monroy, M., Pandey, S., Pocino, A., Castander, F. J., Choi, A., Amon, A., Tutusaus, I., Dodelson, S., Sevilla-Noarbe, I., Fosalba, P., Gaztanaga, E., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Camacho, H., Campos, A., Carrasco Kind, M., Chintalapati, P., Cordero, J., Derose, J., Di Valentino, E., Doux, C., Eifler, T. F., Everett, S., Ferté, A., Friedrich, O., Gatti, M., Gruen, D., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jain, B., Jarvis, M., Lee, S., Lemos, P., Maccrann, N., Mena-Fernández, J., Muir, J., Myles, J., Park, Y., Raveri, M., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Sanchez Cid, D., Scolnic, D., Secco, L. F., Sheldon, E., Troja, A., Troxel, M. A., Weaverdyck, N., Yanny, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., 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., Romer, A. K., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Des, Collaboration, HEP, INSPIRE, 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), and DES
Subjects: luminous red galaxies, data release, pau survey, Cosmology and Nongalactic Astrophysics (astro-ph.CO), roman-space-telescope, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, oscillation spectroscopic survey, Astrophysic, Cosmology and Nongalactic Astrophysics, internal consistency, digital sky survey, redshift distributions, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], photometric data set, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], cosmic shear, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: A. Porredon et al., The cosmological information extracted from photometric surveys is most robust when multiple probes of the large scale structure of the Universe are used. Two of the most sensitive probes are the clustering of galaxies and the tangential shear of background galaxy shapes produced by those foreground galaxies, so-called galaxy-galaxy lensing. Combining the measurements of these two two-point functions leads to cosmological constraints that are independent of the way galaxies trace matter (the galaxy bias factor). The optimal choice of foreground, or lens, galaxies is governed by the joint, but conflicting requirements to obtain accurate redshift information and large statistics. We present cosmological results from the full 5000deg2 of the Dark Energy Survey’s first three years of observations (Y3) combining those two-point functions, using for the first time a magnitude-limited lens sample (MagLim) of 11 million galaxies, especially selected to optimize such combination, and 100 million background shapes. We consider two flat cosmological models, the Standard Model with dark energy and cold dark matter (ΛCDM ) a variation with a free parameter for the dark energy equation of state (wCDM). Both models are marginalized over 25 astrophysical and systematic nuisance parameters. In ΛCDM we obtain for the matter density Ωm=0.320+0.041−0.034 and for the clustering amplitude S8≡σ8(Ωm/0.3)0.5=0.778+0.037−0.031, at 68% C.L. The latter is only 1σ smaller than the prediction in this model informed by measurements of the cosmic microwave background by the Planck satellite. In wCDM we find Ωm=0.32+0.044−0.046, S8=0.777+0.049−0.051 and dark energy equation of state w=−1.031+0.218−0.379. We find that including smaller scales, while marginalizing over nonlinear galaxy bias, improves the constraining power in the Ωm−S8 plane by 31% and in the Ωm−w plane by 41% while yielding consistent cosmological parameters from those in the linear bias case. These results are combined with those from cosmic shear in a companion paper to present full DES-Y3 constraints from the three two-point functions (3×2pt)., 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, 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. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management systemis 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. ESP2015-66861, No. FPA2015-68048, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds fromthe 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 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 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. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a nonexclusive paid-up irrevocable world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. Computations were made on the supercomputer Guillimin from McGill University, managed by Calcul Quebec and Compute Canada. The operation of this supercomputer is funded by the Canada Foundation for Innovation (CFI), the ministere de l’Économie, de la science et de l’innovation du Quebec (MESI) and the Fonds de recherche du Quebec-Nature et technologies (FRQ-NT). This research is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (Grants No. OCI-0725070 and No. ACI-1238993) and the state of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. This research used resources of the Ohio Supercomputer Center (OSC) [117] and of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DE-AC02-05CH11231.
Published: 2022

24. Dark Energy Survey Year 3 Results: Constraints on extensions to $\Lambda$CDM with weak lensing and galaxy clustering

Author: DES Collaboration, Abbott, T. M. C., Aguena, M., Alarcon, A., Alves, O., Amon, A., Annis, J., Avila, S., Bacon, D., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Birrer, S., Blazek, J., Bocquet, S., Brandao-Souza, A., Bridle, S. L., Brooks, D., 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. S., Davis, C., Davis, T. M., DeRose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Farahi, A., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Friedel, D., Friedrich, O., Frieman, J., García-Bellido, J., Gatti, M., Giani, L., Giannantonio, T., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hamaus, N., Harrison, I., Hartley, W. G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huang, H., Huff, E. M., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeffrey, N., Jeltema, T., Kovacs, A., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, S., Leget, P. -F., Lemos, P., Leonard, C. D., Liddle, A. R., Lima, M., Lin, H., MacCrann, N., Marshall, J. L., McCullough, J., Mena-Fernández, J., Menanteau, F., Miquel, R., Miranda, V., Mohr, J. J., Muir, J., Myles, J., Nadathur, S., Navarro-Alsina, A., Nichol, R. C., Ogando, R. L. C., Omori, Y., Palmese, A., Pandey, S., Park, Y., Paterno, M., Paz-Chinchón, F., Percival, W. J., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rogozenski, P., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Cid, D. Sanchez, Scarpine, V., Scolnic, D., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Smith, M., Soares-Santos, M., Suchyta, E., Tabbutt, M., Tarle, G., Thomas, D., To, C., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Vincenzi, M., Walker, A. R., Weaverdyck, N., Wechsler, R. H., Weller, J., Yanny, B., Yin, B., Zhang, Y., and Zuntz, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We constrain extensions to the $\Lambda$CDM model using measurements from the Dark Energy Survey's first three years of observations and external data. The DES data are the two-point correlation functions of weak gravitational lensing, galaxy clustering, and their cross-correlation. We use simulated data and blind analyses of real data to validate the robustness of our results. In many cases, constraining power is limited by the absence of nonlinear predictions that are reliable at our required precision. The models are: dark energy with a time-dependent equation of state, non-zero spatial curvature, sterile neutrinos, modifications of gravitational physics, and a binned $\sigma_8(z)$ model which serves as a probe of structure growth. For the time-varying dark energy equation of state evaluated at the pivot redshift we find $(w_{\rm p}, w_a)= (-0.99^{+0.28}_{-0.17},-0.9\pm 1.2)$ at 68% confidence with $z_{\rm p}=0.24$ from the DES measurements alone, and $(w_{\rm p}, w_a)= (-1.03^{+0.04}_{-0.03},-0.4^{+0.4}_{-0.3})$ with $z_{\rm p}=0.21$ for the combination of all data considered. Curvature constraints of $\Omega_k=0.0009\pm 0.0017$ and effective relativistic species $N_{\rm eff}=3.10^{+0.15}_{-0.16}$ are dominated by external data. For massive sterile neutrinos, we improve the upper bound on the mass $m_{\rm eff}$ by a factor of three compared to previous analyses, giving 95% limits of $(\Delta N_{\rm eff},m_{\rm eff})\leq (0.28, 0.20\, {\rm eV})$. We also constrain changes to the lensing and Poisson equations controlled by functions $\Sigma(k,z) = \Sigma_0 \Omega_{\Lambda}(z)/\Omega_{\Lambda,0}$ and $\mu(k,z)=\mu_0 \Omega_{\Lambda}(z)/\Omega_{\Lambda,0}$ respectively to $\Sigma_0=0.6^{+0.4}_{-0.5}$ from DES alone and $(\Sigma_0,\mu_0)=(0.04\pm 0.05,0.08^{+0.21}_{-0.19})$ for the combination of all data. Overall, we find no significant evidence for physics beyond $\Lambda$CDM., Comment: Updated to match published version. 46 pages, 25 figures, data available at https://dev.des.ncsa.illinois.edu/releases/y3a2/Y3key-extensions
Published: 2022

25. C/2014 UN 271 (Bernardinelli-Bernstein): The Nearly Spherical Cow of Comets

Author: Bernardinelli, Pedro H., Bernstein, Gary M., Montet, Benjamin T., Weryk, Robert, Wainscoat, Richard, Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Kind, M. Carrasco, Carretero, J., Cawthon, R., Conselice, C., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Ogando, R. L. C., Paz-Chinch��n, F., Pieres, A., Malag��n, A. A. Plazas, Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Troxel, M. A., Varga, T. N., Walker, A. R., Zhang, Y., Bernardinelli, Pedro H. [0000-0003-0743-9422], Bernstein, Gary M. [0000-0002-8613-8259], Montet, Benjamin T. [0000-0001-7516-8308], Weryk, Robert [0000-0002-0439-9341], Wainscoat, Richard [0000-0002-1341-0952], Aguena, M. [0000-0001-5679-6747], Annis, J. [0000-0002-0609-3987], Bertin, E. [0000-0002-3602-3664], Brooks, D. [0000-0002-8458-5047], Carretero, J. [0000-0002-3130-0204], Cawthon, R. [0000-0003-2965-6786], Conselice, C. [0000-0003-1949-7638], Costanzi, M. [0000-0001-8158-1449], Diehl, H. T. [0000-0002-8357-7467], García-Bellido, J. [0000-0002-9370-8360], Gaztanaga, E. [0000-0001-9632-0815], Gerdes, D. W. [0000-0001-6942-2736], Gruendl, R. A. [0000-0002-4588-6517], Gschwend, J. [0000-0003-3023-8362], Hinton, S. R. [0000-0003-2071-9349], Hollowood, D. L. [0000-0002-9369-4157], Kuehn, K. [0000-0003-0120-0808], Marshall, J. L. [0000-0003-0710-9474], Menanteau, F. [0000-0002-1372-2534], Miquel, R. [0000-0002-6610-4836], Morgan, R. [0000-0002-7016-5471], Paz-Chinchón, F. [0000-0003-1339-2683], Pieres, A. [0000-0001-9186-6042], Roodman, A. [0000-0001-5326-3486], Sevilla-Noarbe, I. [0000-0002-1831-1953], Swanson, M. E. C. [0000-0002-1488-8552], Tarle, G. [0000-0003-1704-0781], To, C. [0000-0001-7836-2261], and Apollo - University of Cambridge Repository
Abstract: Comet C/2014 UN271 (Bernardinelli-Bernstein), incoming from the Oort cloud, is remarkable in having the brightest (and presumably largest) nucleus of any well-measured comet and having been discovered at the heliocentric distance r h �� 29 au, farther than any Oort cloud comet. In this work, we describe the discovery process and observations and the properties that can be inferred from images recorded until the first reports of activity in 2021 June. The orbit has i = 95��, with a perihelion of 10.97 au to be reached in 2031 and a previous aphelion at 40,400 �� 260 au. Backward integration of the orbit under a standard Galactic tidal model and known stellar encounters suggests a perihelion of q �� 18 au on its previous perihelion passage 3.5 Myr ago; hence, the current data could be the first ever obtained of a comet that has not been inside Uranus��s orbit in 4 Gyr. The photometric data show an unresolved nucleus with absolute magnitude H r = 8.0, colors that are typical of comet nuclei or Damocloids, and no secular trend as it traversed the range 34��23 au. For the r-band geometric albedo p r , this implies a diameter of 150(pr/0.04)��0.5 km. There is strong evidence of brightness fluctuations at the ��0.2 mag level, but no rotation period can be discerned. A coma, nominally consistent with a ��stationary�� 1/�� surface brightness distribution, grew in scattering cross section at an exponential rate from A f �� 1 to ��150 m as the comet approached from 28 to 20 au. The activity rate is consistent with a very simple model of sublimation of a surface species in radiative equilibrium with the Sun. The inferred enthalpy of sublimation matches those of CO2 and NH3. More volatile species, such as N2, CH4, and CO, must be far less abundant on the sublimating surfaces.
Published: 2021

26. The DECam Local Volume Exploration Survey Data Release 2

Author: Drlica-Wagner, A., Ferguson, P. S., Adamów, M., Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bechtol, K., Bell, E. F., Bertin, E., Bilaji, P., Bocquet, S., Bom, C. R., Brooks, D., Burke, D. L., Carballo-Bello, J. A., Carlin, J. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cerny, W., Chang, C., Choi, Y., Conselice, C., Costanzi, M., Crnojević, D., da Costa, L. N., de Vicente, J., Desai, S., Esteves, J., Everett, S., Ferrero, I., Fitzpatrick, M., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hartley, W. G., Hernandez-Lang, D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, A. K., Jacques, A., James, D. J., Johnson, M. D., Kuehn, K., Kuropatkin, N., Lahav, O., T. S., Li, Lidman, C., Lin, H., March, M., Marshall, J. L., Martínez-Delgado, D., Martínez-Vázquez, C. E., Massana, P., Mau, S., Mcnanna, M., Melchior, P., Menanteau, F., Miller, A. E., Miquel, R., Mohr, J. J., Morgan, R., Mutlu-Pakdil, B., Muñoz, R. R., Neilsen, E. H., Nidever, D. L., Nikutta, R., Nilo Castellon, J. L., Noël, N. E. D., Ogando, R. L. C., Olsen, K. A. G., Pace, A. B., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Plazas Malagón, A. A., Prat, J., Riley, A. H., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sako, M., Sakowska, J. D., Sanchez, E., Sánchez, F. J., Sand, D. J., Santana-Silva, L., Santiago, B., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Simon, J. D., Smith, M., Soares-Santos, M., Stringfellow, G. S., Suchyta, E., Suson, D. J., Tan, C. Y., Tarle, G., Tavangar, K., Thomas, D., To, C., Tollerud, E. J., Troxel, M. A., Tucker, D. L., Varga, T. N., Vivas, A. K., Walker, A. R., Weller, J., Wilkinson, R. D., J. F., Wu, Yanny, B., Zaborowski, E., Zenteno, A., Delve, Collaboration, Des, Collaboration, Astro Data Lab, Drlica-Wagner, A., Ferguson, P. S., Adamów, M., Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bechtol, K., Bell, E. F., Bertin, E., Bilaji, P., Bocquet, S., Bom, C. R., Brooks, D., Burke, D. L., Carballo-Bello, J. A., Carlin, J. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cerny, W., Chang, C., Choi, Y., Conselice, C., Costanzi, M., Crnojević, D., da Costa, L. N., de Vicente, J., Desai, S., Esteves, J., Everett, S., Ferrero, I., Fitzpatrick, M., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hartley, W. G., Hernandez-Lang, D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, A. K., Jacques, A., James, D. J., Johnson, M. D., Kuehn, K., Kuropatkin, N., Lahav, O., T. S., Li, Lidman, C., Lin, H., March, M., Marshall, J. L., Martínez-Delgado, D., Martínez-Vázquez, C. E., Massana, P., Mau, S., Mcnanna, M., Melchior, P., Menanteau, F., Miller, A. E., Miquel, R., Mohr, J. J., Morgan, R., Mutlu-Pakdil, B., Muñoz, R. R., Neilsen, E. H., Nidever, D. L., Nikutta, R., Nilo Castellon, J. L., Noël, N. E. D., Ogando, R. L. C., Olsen, K. A. G., Pace, A. B., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Plazas Malagón, A. A., Prat, J., Riley, A. H., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sako, M., Sakowska, J. D., Sanchez, E., Sánchez, F. J., Sand, D. J., Santana-Silva, L., Santiago, B., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Simon, J. D., Smith, M., Soares-Santos, M., Stringfellow, G. S., Suchyta, E., Suson, D. J., Tan, C. Y., Tarle, G., Tavangar, K., Thomas, D., To, C., Tollerud, E. J., Troxel, M. A., Tucker, D. L., Varga, T. N., Vivas, A. K., Walker, A. R., Weller, J., Wilkinson, R. D., J. F., Wu, Yanny, B., Zaborowski, E., Zenteno, A., Delve, Collaboration, Des, Collaboration, Astro Data Lab, Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, and Fundação de Amparo à Pesquisa do Estado de São Paulo
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astronomy and Astrophysics, Surveys, Astrophysics - Astrophysics of Galaxies, Catalogs, Local Group, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Catalog, Survey, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Full list of authors: Drlica-Wagner, A.; Ferguson, P. S.; Adamow, M.; Aguena, M.; Allam, S.; Andrade-Oliveira, F.; Bacon, D.; Bechtol, K.; Bell, E. F.; Bertin, E.; Bilaji, P.; Bocquet, S.; Bom, C. R.; Brooks, D.; Burke, D. L.; Carballo-Bello, J. A.; Carlin, J. L.; Carnero Rosell, A.; Kind, M. Carrasco; Carretero, J.; Castander, F. J.; Cerny, W.; Chang, C.; Choi, Y.; Conselice, C.; Costanzi, M.; Crnojevic, D.; da Costa, L. N.; De Vicente, J.; Desai, S.; Esteves, J.; Everett, S.; Ferrero, I; Fitzpatrick, M.; Flaugher, B.; Friedel, D.; Frieman, J.; Garcia-Bellido, J.; Gatti, M.; Gaztanaga, E.; Gerdes, D. W.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Hartley, W. G.; Hernandez-Lang, D.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; Hughes, A. K.; Jacques, A.; James, D. J.; Johnson, M. D.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Li, T. S.; Lidman, C.; Lin, H.; March, M.; Marshall, J. L.; Martinez-Delgado, D.; Martinez-Vazquez, C. E.; Massana, P.; Mau, S.; McNanna, M.; Melchior, P.; Menanteau, F.; Miller, A. E.; Miquel, R.; Mohr, J. J.; Morgan, R.; Mutlu-Pakdil, B.; Munoz, R. R.; Neilsen, E. H.; Nidever, D. L.; Nikutta, R.; Nilo Castellon, J. L.; Noel, N. E. D.; Ogando, R. L. C.; Olsen, K. A. G.; Pace, A. B.; Palmese, A.; Paz-Chinchon, F.; Pereira, M. E. S.; Pieres, A.; Malagon, A. A. Plazas; Prat, J.; Riley, A. H.; Rodriguez-Monroy, M.; Romer, A. K.; Roodman, A.; Sako, M.; Sakowska, J. D.; Sanchez, E.; Sanchez, F. J.; Sand, D. J.; Santana-Silva, L.; Santiago, B.; Schubnell, M.; Serrano, S.; Sevilla-Noarbe, I; Simon, J. D.; Smith, M.; Soares-Santos, M.; Stringfellow, G. S.; Suchyta, E.; Suson, D. J.; Tan, C. Y.; Tarle, G.; Tavangar, K.; Thomas, D.; To, C.; Tollerud, E. J.; Troxel, M. A.; Tucker, D. L.; Varga, T. N.; Vivas, A. K.; Walker, A. R.; Weller, J.; Wilkinson, R. D.; Wu, J. F.; Yanny, B.; Zaborowski, E.; Zenteno, A.; DELVE Collaboration; DES Collaboration; Astro Data Lab.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., We present the second public data release (DR2) from the DECam Local Volume Exploration survey (DELVE). DELVE DR2 combines new DECam observations with archival DECam data from the Dark Energy Survey, the DECam Legacy Survey, and other DECam community programs. DELVE DR2 consists of ∼160,000 exposures that cover >21,000 deg2 of the high-Galactic-latitude (∣b∣ > 10°) sky in four broadband optical/near-infrared filters (g, r, i, z). DELVE DR2 provides point-source and automatic aperture photometry for ∼2.5 billion astronomical sources with a median 5σ point-source depth of g = 24.3, r = 23.9, i = 23.5, and z = 22.8 mag. A region of ∼17,000 deg2 has been imaged in all four filters, providing four-band photometric measurements for ∼618 million astronomical sources. DELVE DR2 covers more than 4 times the area of the previous DELVE data release and contains roughly 5 times as many astronomical objects. DELVE DR2 is publicly available via the NOIRLab Astro Data Lab science platform. © 2022. The Author(s). Published by the American Astronomical Society., The DELVE project is partially supported by Fermilab LDRD project L2019-011, the NASA Fermi Guest Investigator Program Cycle 9 grant 91201, and the National Science Foundation (NSF) under grant AST-2108168. This work is supported by the Fermilab Visiting Scholars Award Program from the Universities Research Association. A.B.P. acknowledges support from NSF grant AST-1813881. J.L.C. acknowledges support from NSF grant AST-1816196. J.D.S. acknowledges support from NSF grant AST-1714873. S.R.M. acknowledges support from NSF grant AST-1909497. D.J.S. acknowledges support from NSF grants AST-1821967 and AST-1813708. D.C. acknowledges support from NSF grant AST-1814208. B.M.P. acknowledges support from the NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-2001663. S.M. acknowledges support from the NSF Graduate Research Fellowship under grant DGE-1656518. D.M.D. acknowledges financial support from the State Agency for Research of the Spanish MCIU through the "Centre of Excellence Severo Ochoa" award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709). C.P.M.B. and M.R.L.C. acknowledge support from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement no. 682115). L.S.S. acknowledges the financial support from FAPESP through the grant #2020/03301-5. J.A.C.B. acknowledges support from ANID FONDECYT Regular 1220083. 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 á 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. 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

27. OzDES Reverberation Mapping Program: H$β$ lags from the 6-year survey

Author: Malik, Umang, Sharp, Rob, Penton, A., Yu, Z., Martini, P., Lidman, C., Tucker, B. E., Davis, T. M., Lewis, G. F., Aguena, M., Allam, S., Alves, O., Andrade-Oliveira, F., Asorey, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Raveri, M., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Taylor, G., Tucker, D. L., Weaverdyck, N., and Wilkinson, R. D.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract: Reverberation mapping measurements have been used to constrain the relationship between the size of the broad-line region and luminosity of active galactic nuclei (AGN). This $R-L$ relation is used to estimate single-epoch virial black hole masses, and has been proposed for use to standardise AGN to determine cosmological distances. We present reverberation measurements made with H$β$ from the six-year Australian Dark Energy Survey (OzDES) Reverberation Mapping Program. We successfully recover reverberation lags for eight AGN at $0.12, Published in MNRAS
Published: 2022
Full Text: View/download PDF

28. Dark Energy Survey Year 3 Results: Constraints on extensions to $Λ$CDM with weak lensing and galaxy clustering

Author: DES Collaboration, Abbott, T. M. C., Aguena, M., Alarcon, A., Alves, O., Amon, A., Annis, J., Avila, S., Bacon, D., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Birrer, S., Blazek, J., Bocquet, S., Brandao-Souza, A., Bridle, S. L., Brooks, D., 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. S., Davis, C., Davis, T. M., DeRose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Farahi, A., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Friedel, D., Friedrich, O., Frieman, J., García-Bellido, J., Gatti, M., Giani, L., Giannantonio, T., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hamaus, N., Harrison, I., Hartley, W. G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huang, H., Huff, E. M., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeffrey, N., Jeltema, T., Kovacs, A., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, S., Leget, P. -F., Lemos, P., Leonard, C. D., Liddle, A. R., Lima, M., Lin, H., MacCrann, N., Marshall, J. L., McCullough, J., Mena-Fernández, J., Menanteau, F., Miquel, R., Miranda, V., Mohr, J. J., Muir, J., Myles, J., Nadathur, S., Navarro-Alsina, A., Nichol, R. C., Ogando, R. L. C., Omori, Y., Palmese, A., Pandey, S., Park, Y., Paterno, M., Paz-Chinchón, F., Percival, W. J., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rogozenski, P., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Cid, D. Sanchez, Scarpine, V., Scolnic, D., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Smith, M., Soares-Santos, M., Suchyta, E., Tabbutt, M., Tarle, G., Thomas, D., To, C., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Vincenzi, M., Walker, A. R., Weaverdyck, N., Wechsler, R. H., Weller, J., Yanny, B., Yin, B., Zhang, Y., and Zuntz, J.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences
Abstract: We constrain extensions to the $Λ$CDM model using measurements from the Dark Energy Survey's first three years of observations and external data. The DES data are the two-point correlation functions of weak gravitational lensing, galaxy clustering, and their cross-correlation. We use simulated data and blind analyses of real data to validate the robustness of our results. In many cases, constraining power is limited by the absence of nonlinear predictions that are reliable at our required precision. The models are: dark energy with a time-dependent equation of state, non-zero spatial curvature, sterile neutrinos, modifications of gravitational physics, and a binned $σ_8(z)$ model which serves as a probe of structure growth. For the time-varying dark energy equation of state evaluated at the pivot redshift we find $(w_{\rm p}, w_a)= (-0.99^{+0.28}_{-0.17},-0.9\pm 1.2)$ at 68% confidence with $z_{\rm p}=0.24$ from the DES measurements alone, and $(w_{\rm p}, w_a)= (-1.03^{+0.04}_{-0.03},-0.4^{+0.4}_{-0.3})$ with $z_{\rm p}=0.21$ for the combination of all data considered. Curvature constraints of $Ω_k=0.0009\pm 0.0017$ and effective relativistic species $N_{\rm eff}=3.10^{+0.15}_{-0.16}$ are dominated by external data. For massive sterile neutrinos, we improve the upper bound on the mass $m_{\rm eff}$ by a factor of three compared to previous analyses, giving 95% limits of $(ΔN_{\rm eff},m_{\rm eff})\leq (0.28, 0.20\, {\rm eV})$. We also constrain changes to the lensing and Poisson equations controlled by functions $Σ(k,z) = Σ_0 Ω_Λ(z)/Ω_{Λ,0}$ and $μ(k,z)=μ_0 Ω_Λ(z)/Ω_{Λ,0}$ respectively to $Σ_0=0.6^{+0.4}_{-0.5}$ from DES alone and $(Σ_0,μ_0)=(0.04\pm 0.05,0.08^{+0.21}_{-0.19})$ for the combination of all data. Overall, we find no significant evidence for physics beyond $Λ$CDM., Updated to match published version. 46 pages, 25 figures, data available at https://dev.des.ncsa.illinois.edu/releases/y3a2/Y3key-extensions
Published: 2022
Full Text: View/download PDF

29. Identification of Galaxy-Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning

Author: Zaborowski, E., Drlica-Wagner, A., Ashmead, F., Wu, J. F., Morgan, R., Bom, C. R., Shajib, A. J., Birrer, S., Cerny, W., Buckley-Geer, L., Mutlu-Pakdil, B., Ferguson, P. S., Glazebrook, K., Lozano, S. J. Gonzalez, Gordon, Y., Martinez, M., Manwadkar, V., O'Donnell, J., Poh, J., Riley, A., Sakowska, J. D., Santana-Silva, L., Santiago, B. X., Sluse, D., Tan, C. Y., Tollerud, E. J., Verma, A., Carballo-Bello, J. A., Choi, Y., James, D. J., Kuropatkin, N., Martínez-Vázquez, C. E., Nidever, D. L., Castellon, J. L. Nilo, Noël, N. E. D., Olsen, K. A. G., Pace, A. B., Mau, S., Yanny, B., Zenteno, A., Abbott, T. M. C., Aguena, M., Alves, O., Andrade-Oliveira, F., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Conselice, C. J., Costanzi, M., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Kuehn, K., Lin, H., Marshall, J. L., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Prat, J., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., To, C., and Weaverdyck, N.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: We perform a search for galaxy-galaxy strong lens systems using a convolutional neural network (CNN) applied to imaging data from the first public data release of the DECam Local Volume Exploration Survey (DELVE), which contains $\sim 520$ million astronomical sources covering $\sim 4,000$ $\mathrm{deg}^2$ of the southern sky to a $5σ$ point-source depth of $g=24.3$, $r=23.9$, $i=23.3$, and $z=22.8$ mag. Following the methodology of similar searches using DECam data, we apply color and magnitude cuts to select a catalog of $\sim 11$ million extended astronomical sources. After scoring with our CNN, the highest scoring 50,000 images were visually inspected and assigned a score on a scale from 0 (definitely not a lens) to 3 (very probable lens). We present a list of 617 strong lens candidates, 599 of which are previously unreported. We categorize our candidates using their human-assigned scores, resulting in 60 Grade A candidates, 160 Grade B candidates, and 397 Grade C candidates. We additionally highlight 8 potential quadruply lensed quasars from this sample. Due to the location of our search footprint in the northern Galactic cap ($b > 10$ deg) and southern celestial hemisphere (${\rm Dec.}, 27 pages; added machine-readable table
Published: 2022
Full Text: View/download PDF

30. Dark Energy Survey Year 3 Results: Cosmology from Cosmic Shear and Robustness to Data Calibration

Author: Amon, A., Gruen, D., Troxel, M. A., MacCrann, N., Dodelson, S., Choi, A., Doux, C., Secco, L. F., Samuroff, S., Krause, E., Cordero, J., Myles, J., DeRose, J., Wechsler, R. H., Gatti, M., Navarro-Alsina, A., Bernstein, G. M., Jain, B., Blazek, J., Alarcon, A., Ferté, A., Raveri, M., Lemos, P., Campos, A., Prat, J., Sánchez, C., Jarvis, M., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bridle, S. L., Camacho, H., Rosell, A. Carnero, Kind, M. Carrasco, Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Crocce, M., Davis, C., Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Everett, S., Fang, X., Fosalba, P., Friedrich, O., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Kuropatkin, N., Leget, P. -F., Liddle, A. R., McCullough, J., Muir, J., Pandey, S., Park, Y., Porredon, A., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Weaverdyck, N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., 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., Kron, R., 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., Malagón, A. A. Plazas, Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Weller, J., 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, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, European Research Council, Generalitat de Catalunya, Department of Energy (US), National Science Foundation (US), National Aeronautics and Space Administration (US), Ministerio de Economía y Competitividad (España), Amon, A., Gruen, D., Troxel, M. A., Maccrann, N., Dodelson, S., Choi, A., Doux, C., Secco, L. F., Samuroff, S., Krause, E., Cordero, J., Myles, J., Derose, J., Wechsler, R. H., Gatti, M., Navarro-Alsina, A., Bernstein, G. M., Jain, B., Blazek, J., Alarcon, A., Ferte, A., Lemos, P., Raveri, M., Campos, A., Prat, J., Sanchez, C., Jarvis, M., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bridle, S. L., Camacho, H., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Crocce, M., Davis, C., Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Everett, S., Fang, X., Fosalba, P., Friedrich, O., Gaztanaga, E., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Kuropatkin, N., Leget, P., Liddle, A. R., Mccullough, J., Muir, J., Pandey, S., Park, Y., Porredon, A., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Weaverdyck, N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kron, R., 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., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Tarle, G., Thomas, D., To, C., Weller, J., Stanford University, 382 Via Pueblo Mall, SLAC National Accelerator Laboratory, Duke University, University of Cambridge, Carnegie Mellon University, The Ohio State University, University of Pennsylvania, University of Chicago, University of Arizona, University of Manchester, Lawrence Berkeley National Laboratory, Universidade Estadual de Campinas (UNICAMP), Laboratório Interinstitucional de E-Astronomia, Observatoire de Sauverny, Argonne National Laboratory, California Institute of Technology, University College London, University of Sussex, University of Michigan, Universidade Estadual Paulista (UNESP), University of Wisconsin-Madison, Instituto de Astrofisica de Canarias, Universidad de la Laguna, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Fermi National Accelerator Laboratory, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Santa Cruz Institute for Particle Physics, The Barcelona Institute of Science and Technology, Denys Wilkinson Building, University of Geneva, University of Edinburgh, Universidade de Lisboa, Perimeter Institute for Theoretical Physics, The University of Tokyo, ETH Zurich, Medioambientales y Tecnológicas (CIEMAT), Brookhaven National Laboratory, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universität München, University of Portsmouth, Institut d'Astrophysique de Paris, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, IIT Hyderabad, Ludwig-Maximilians-Universität, University of Oslo, Universidad Autonoma de Madrid, University of Queensland, Center for Astrophysics|Harvard and Smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas AandM University, Harvard University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Southampton, and UAM. Departamento de Física Teórica
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), microwave background anisotropies, systematic-errors, FOS: Physical sciences, parameter constraints, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, large-scale structure, Astrophysic, weak-lensing surveys, Cosmology and Nongalactic Astrophysics, 0103 physical sciences, internal consistency, Weak, redshift distributions, 010303 astronomy & astrophysics, Gravitational Lensing, 010308 nuclear & particles physics, Física, Dark Energy, intrinsic correlation, matter power spectrum, 2-point correlation-functions, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: A. Amon et al., This work, together with its companion paper, Secco, Samuroff et al. [Phys. Rev. D 105, 023515 (2022)], present the Dark Energy Survey Year 3 cosmic-shear measurements and cosmological constraints based on an analysis of over 100 million source galaxies. With the data spanning 4143 deg2 on the sky, divided into four redshift bins, we produce a measurement with a signal-to-noise of 40. We conduct a blind analysis in the context of the Lambda-Cold Dark Matter (ΛCDM) model and find a 3% constraint of the clustering amplitude, S8≡σ8(Ωm/0.3)0.5=0.759+0.025−0.023. A ΛCDM-Optimized analysis, which safely includes smaller scale information, yields a 2% precision measurement of S8=0.772+0.018−0.017 that is consistent with the fiducial case. The two low-redshift measurements are statistically consistent with the Planck Cosmic Microwave Background result, however, both recovered S8 values are lower than the high-redshift prediction by 2.3σ and 2.1σ (p-values of 0.02 and 0.05), respectively. The measurements are shown to be internally consistent across redshift bins, angular scales and correlation functions. The analysis is demonstrated to be robust to calibration systematics, with the S8 posterior consistent when varying the choice of redshift calibration sample, the modeling of redshift uncertainty and methodology. Similarly, we find that the corrections included to account for the blending of galaxies shifts our best-fit S8 by 0.5σ without incurring a substantial increase in uncertainty. We examine the limiting factors for the precision of the cosmological constraints and find observational systematics to be subdominant to the modeling of astrophysics. Specifically, we identify the uncertainties in modeling baryonic effects and intrinsic alignments as the limiting systematics., This research manuscript made use of Astropy [204,205], GetDist [206], ChainConsumer10 [207] and Matplotlib [208], and has been prepared using NASA’s Astrophysics Data System Bibliographic Services. 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, 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. 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, and Office of High Energy Physics.
Published: 2021

31. Dark Energy Survey Year 3 Results: Constraints on cosmological parameters and galaxy bias models from galaxy clustering and galaxy-galaxy lensing using the redMaGiC sample

Author: Pandey, S., Krause, E., DeRose, J., MacCrann, N., Jain, B., Crocce, M., Blazek, J., Choi, A., Huang, H., To, C., Fang, X., Elvin-Poole, J., Prat, J., Porredon, A., Secco, L. F., Rodriguez-Monroy, M., Weaverdyck, N., Park, Y., Raveri, M., Rozo, E., Rykoff, E. S., Bernstein, G. M., Sánchez, C., Jarvis, M., Troxel, M. A., Zacharegkas, G., Chang, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Chintalapati, P., Davis, C., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Everett, S., Farahi, A., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Huff, E. M., Huterer, D., Kovacs, A., Leget, P. F., McCullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Rollins, R. P., Roodman, A., Rosenfeld, R., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. 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., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Dietrich, J. P., Doel, P., Evrard, A. E., 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., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Weller, J., DES Collaboration, 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, Department of Energy (US), National Science Foundation (US), Ministerio de Educación y Ciencia (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Australian Research Council, European Commission, European Research Council, Pandey, S., Krause, E., Derose, J., Maccrann, N., Jain, B., Crocce, M., Blazek, J., Choi, A., Huang, H., To, C., Fang, X., Elvin-Poole, J., Prat, J., Porredon, A., Secco, L. F., Rodriguez-Monroy, M., Weaverdyck, N., Park, Y., Raveri, M., Rozo, E., Rykoff, E. S., Bernstein, G. M., Sánchez, C., Jarvis, M., Troxel, M. A., Zacharegkas, G., Chang, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Chintalapati, P., Davis, C., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Everett, S., Farahi, A., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Huff, E. M., Huterer, D., Kovacs, A., Leget, P. F., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Rollins, R. P., Roodman, A., Rosenfeld, R., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. 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., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Dietrich, J. P., Doel, P., Evrard, A. E., 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., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Weller, J., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysic, combination, Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, Astrophysics of Galaxies, FOS: Physical sciences, marginalization, Astrophysics, Cosmology and Nongalactic Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, calibration, Astrophysics - Astrophysics of Galaxies, efficient, Astrophysic, scale dependence, Astrophysics of Galaxies (astro-ph.GA), halo-mass, evolution, impact, redshift distributions, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: S. Pandey et al., We constrain cosmological parameters and galaxy-bias parameters using the combination of galaxy clustering and galaxy-galaxy lensing measurements from the Dark Energy Survey (DES) year-3 data. We describe our modeling framework and choice of scales analyzed, validating their robustness to theoretical uncertainties in small-scale clustering by analyzing simulated data. Using a linear galaxy-bias model and redMaGiC galaxy sample, we obtain 10% constraints on the matter density of the Universe. We also implement a nonlinear galaxy-bias model to probe smaller scales that includes parametrization based on hybrid perturbation theory and find that it leads to a 17% gain in cosmological constraining power. We perform robustness tests of our methodology pipeline and demonstrate stability of the constraints to changes in the theory model. Using the redMaGiC galaxy sample as foreground lens galaxies and adopting the best-fitting cosmological parameters from DES year-1 data, we find the galaxy clustering and galaxy-galaxy lensing measurements to exhibit significant signals akin to decorrelation between galaxies and mass on large scales, which is not expected in any current models. This likely systematic measurement error biases our constraints on galaxy bias and the S8 parameter. We find that a scale-, redshift- and sky-area-independent phenomenological decorrelation parameter can effectively capture this inconsistency between the galaxy clustering and galaxy-galaxy lensing. We trace the source of this correlation to a color-dependent photometric issue and minimize its impact on our result by changing the selection criteria of redMaGiC galaxies. Using this new sample, our constraints on the S8 parameter are consistent with previous studies and we find a small shift in the Ωm constraints compared to the fiducial redMaGiC sample. We infer the constraints on the mean host-halo mass of the redMaGiC galaxies in this new sample from the large-scale bias constraints, finding the galaxies occupy halos of mass approximately 1.6×1013M⊙/h., E. K. is supported by the Department of Energy Grant No. DE-SC0020247 and the David and Lucile Packard Foundation. S. P. and B.J. are supported in part by the U.S. Department of Energy Grant No. DE-SC0007901 and NASA ATP Grant No. NNH17ZDA001N. 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 OhioStateUniversity, theMitchell 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 Energ´eticas, 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 UrbanaChampaign, 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 MünchenandtheassociatedExcellenceCluster 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 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-20160597, and No. MDM-2015-0509, some of which include ERDFfundsfromtheEuropean 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,andNo.306478.Weacknowledgesupportfrom the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through Project No. CE110001020. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DEAC02-07CH11359 with the U.S. Department of Energy, Office ofScience,OfficeofHighEnergyPhysics.
Published: 2021

32. Dwarf AGNs from Optical Variability for the Origins of Seeds (DAVOS): Insights from the Dark Energy Survey Deep Fields

Author: Burke, Colin J., Liu, Xin, Shen, Yue, Phadke, Kedar A., Yang, Qian, Hartley, Will G., Harrison, Ian, Palmese, Antonella, Guo, Hengxiao, Zhang, Kaiwen, Kron, Richard, Turner, David J., Giles, Paul A., Lidman, Christopher, Chen, Yu-Ching, Gruendl, Robert A., Choi, Ami, Amon, Alexandra, Sheldon, Erin, Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bertin, E., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., García-Bellido, J., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Reil, K., Romer, A. K., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Wilkinson, R. D., Collaboration, DES, Burke, Colin J., Liu, Xin, Shen, Yue, Phadke, Kedar A., Yang, Qian, Hartley, Will G., Harrison, Ian, Palmese, Antonella, Guo, Hengxiao, Zhang, Kaiwen, Kron, Richard, Turner, David J., Giles, Paul A., Lidman, Christopher, Chen, Yu-Ching, Gruendl, Robert A., Choi, Ami, Amon, Alexandra, Sheldon, Erin, Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bertin, E., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., García-Bellido, J., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Romer, A. K., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Wilkinson, R. D., and Des, Collaboration
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, black hole physics, galaxies active, galaxies dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, black hole physic, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: We present a sample of 706, $z < 1.5$ active galactic nuclei (AGNs) selected from optical photometric variability in three of the Dark Energy Survey (DES) deep fields (E2, C3, and X3) over an area of 4.64 deg$^2$. We construct light curves using difference imaging aperture photometry for resolved sources and non-difference imaging PSF photometry for unresolved sources, respectively, and characterize the variability significance. Our DES light curves have a mean cadence of 7 days, a 6 year baseline, and a single-epoch imaging depth of up to $g \sim 24.5$. Using spectral energy distribution (SED) fitting, we find 26 out of total 706 variable galaxies are consistent with dwarf galaxies with a reliable stellar mass estimate ($M_{\ast}, 21 pages, 22 figures incl. 3 appendices; accepted for publication in MNRAS
Published: 2021
Full Text: View/download PDF

33. Dark Energy Survey Year 3 Results: Exploiting small-scale information with lensing shear ratios

Author: Sánchez, C., Prat, J., Zacharegkas, G., Pandey, S., Baxter, E., Bernstein, G. M., Blazek, J., Cawthon, R., Chang, C., Krause, E., Lemos, P., Park, Y., Raveri, M., Sanchez, J., Troxel, M. A., Amon, A., Fang, X., Friedrich, O., Gruen, D., Porredon, A., Secco, L. F., Samuroff, S., Alarcon, A., Alves, O., Andrade-Oliveira, F., Bechtol, K., Becker, M. R., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Chen, R., Choi, A., Crocce, M., Davis, C., De Vicente, J., Derose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Ferté, A., Fosalba, P., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jarvis, M., Jain, B., Kuropatkin, N., Leget, P. -F., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Rykoff, E. S., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., 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., 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., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Des, Collaboration, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), Department of Energy (US), Ministerio de Economía y Competitividad (España), European Research Council, Generalitat de Catalunya, European Commission, A Sánchez, C., Prat, J., Zacharegkas, G., Pandey, S., Baxter, E., Bernstein, G. M., Blazek, J., Cawthon, R., Chang, C., Krause, E., Lemos, P., Park, Y., Raveri, M., Sanchez, J., Troxel, M. A., Amon, A., Fang, X., Friedrich, O., Gruen, D., Porredon, A., Secco, L. F., Samuroff, S., Alarcon, A., Alves, O., Andrade-Oliveira, F., Bechtol, K., Becker, M. R., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Chen, R., Choi, A., Crocce, M., Davis, C., De Vicente, J., Derose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Ferté, A., Fosalba, P., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jarvis, M., Jain, B., Kuropatkin, N., Leget, P. -F., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Rykoff, E. S., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley- Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., 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., 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., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and UAM. Departamento de Física Teórica
Subjects: Gravitational Lensing, mice, Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, halo, Física, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, calibration, Astrophysics, Dark Energy, Astrophysic, Cosmology and Nongalactic Astrophysics, statistics, galaxies, luminosity, Weak, baryonic feedback, constraints, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], intrinsic alignments, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: C. Sánchez et al., Using the first three years of data from the Dark Energy Survey (DES), we use ratios of small-scale galaxy-galaxy lensing measurements around the same lens sample to constrain source redshift uncertainties, intrinsic alignments and other systematics or nuisance parameters of our model. Instead of using a simple geometric approach for the ratios as has been done in the past, we use the full modeling of the galaxy-galaxy lensing measurements, including the corresponding integration over the power spectrum and the contributions from intrinsic alignments and lens magnification. We perform extensive testing of the small-scale shear-ratio (SR) modeling by studying the impact of different effects such as the inclusion of baryonic physics, nonlinear biasing, halo occupation distribution descriptions and lens magnification, among others, and using realistic N-body simulations of the DES data. We validate the robustness of our constraints in the data by using two independent lens samples with different galaxy properties, and by deriving constraints using the corresponding large-scale ratios for which the modeling is simpler. The results applied to the DES Y3 data demonstrate how the ratios provide significant improvements in constraining power for several nuisance parameters in our model, especially on source redshift calibration and intrinsic alignments. For source redshifts, SR improves the constraints from the prior by up to 38% in some redshift bins. Such improvements, and especially the constraints it provides on intrinsic alignments, translate to tighter cosmological constraints when shear ratios are combined with cosmic shear and other 2pt functions. In particular, for the DES Y3 data, SR improves S8 constraints from cosmic shear by up to 31%, and for the full combination of probes (3×2pt) by up to 10%. The shear ratios presented in this work are used as an additional likelihood for cosmic shear, 2×2pt and the full 3×2pt in the fiducial DES Y3 cosmological analysis., C. S. is supported by Grant No. AST-1615555 from the U.S. National Science Foundation, and Grant No. DESC0007901 from the U.S. Department of Energy (DOE). J. P. is supported by DOE Grant No. DE-SC0021429. 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 UrbanaChampaign, 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 DESBrazil 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, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State UniverFIG. 16. Correlation matrix for the lensing ratios, on the left panel using the REDMAGIC lens sample and on the right panel using the MAGLIM sample. sity, 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 Grants No. AST1138766 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. SEV2012-0234, No. SEV-2016-0597, and No. MDM-20150509, 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 Grants Agreement No. 240672, No. 291329, and No. 306478.
Published: 2021
Full Text: View/download PDF

34. Dark Energy Survey Year 3 Results: Galaxy clustering and systematics treatment for lens galaxy samples

Author: Rodriguez-Monroy M., Weaverdyck N., Elvin-Poole J., Crocce M., Carnero Rosell A., Andrade-Oliveira F., Avila S., Bechtol K., Bernstein G. M., Blazek J., Camacho H., Cawthon R., De Vicente J., Derose J., Dodelson S., Everett S., Fang X., Ferrero I., Ferte A., Friedrich O., Gaztanaga E., Giannini G., Gruendl R. A., Hartley W. G., Herner K., Huff E. M., Jarvis M., Krause E., MacCrann N., Mena-Fernandez J., Muir J., Pandey S., Park Y., Porredon A., Prat J., Rosenfeld R., Ross A. J., Rozo E., Rykoff E. S., Sanchez E., Sanchez Cid D., Sevilla-Noarbe I., Tabbutt M., To C., Wagoner E. L., Wechsler R. H., Aguena M., Allam S., Amon A., Annis J., Bacon D., Baxter E., Bertin E., Bhargava S., Brooks D., Burke D. L., Carrasco Kind M., Carretero J., Castander F. J., Choi A., Conselice C., Costanzi M., Da Costa L. N., Pereira M. E. S., Desai S., Diehl H. T., Flaugher B., Fosalba P., Frieman J., Garcia-Bellido J., Giannantonio T., Gruen D., Gschwend J., Gutierrez G., Hinton S. R., Hollowood D. L., Honscheid K., Huterer D., Jain B., James D. J., Kuehn K., Kuropatkin N., Lima M., Maia M. A. G., March M., Marshall J. L., Melchior P., Menanteau F., Miller C. J., Miquel R., Mohr J. J., Morgan R., Palmese A., Paz-Chinchon F., Pieres A., Plazas Malagon A. A., Roodman A., Scarpine V., Serrano S., Smith M., Soares-Santos M., Suchyta E., Tarle G., Thomas D., Varga T. N., UAM. Departamento de Física Teórica, National Science Foundation (US), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Educación y Ciencia (España), National Aeronautics and Space Administration (US), Generalitat de Catalunya, Medioambientales y Tecnologicas (CIEMAT), University of Michigan, The Ohio State University, Institut d'Estudis Espacials de Catalunya (IEEC), S/n, Instituto de Astrofisica de Canarias, Laboratorio Interinstitucional de E-Astronomia-LIneA, Dpto. Astrofísica, Universidade Estadual Paulista (UNESP), Universidad Autonoma de Madrid, University of WisconsinMadison, University of Pennsylvania, Northeastern University, Observatoire de Sauverny, Lawrence Berkeley National Laboratory, Carnegie Mellon University, Santa Cruz Institute for Particle Physics, University of Arizona, University of Oslo, California Institute of Technology, University of Cambridge, The Barcelona Institute of Science and Technology, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, University of Geneva, Fermi National Accelerator Laboratory, Stanford University, The University of Tokyo, University of Chicago, Slac National Accelerator Laboratory, 382 Via Pueblo Mall, University of Portsmouth, University of Hawai'i, Institut d'Astrophysique de Paris, University of Sussex, University College London, University of Manchester, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatorio Nacional, Iit Hyderabad, University of Queensland, Center for Astrophysics | Harvard &smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas A &m University, Peyton Hall, Institucio Catalana de Recerca i Estudis Avancats, Ludwig-Maximilians-Universitat, Max Planck Institute for Extraterrestrial Physics, University of Southampton, Oak Ridge National Laboratory, Ludwig-Maximilians Universitat Munchen, 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, Rodriguez-Monroy, M., Weaverdyck, N., Elvin-Poole, J., Crocce, M., Carnero Rosell, A., Andrade-Oliveira, F., Avila, S., Bechtol, K., Bernstein, G. M., Blazek, J., Camacho, H., Cawthon, R., De Vicente, J., Derose, J., Dodelson, S., Everett, S., Fang, X., Ferrero, I., Ferte, A., Friedrich, O., Gaztanaga, E., Giannini, G., Gruendl, R. A., Hartley, W. G., Herner, K., Huff, E. M., Jarvis, M., Krause, E., Maccrann, N., Mena-Fernandez, J., Muir, J., Pandey, S., Park, Y., Porredon, A., Prat, J., Rosenfeld, R., Ross, A. J., Rozo, E., Rykoff, E. S., Sanchez, E., Sanchez Cid, D., Sevilla-Noarbe, I., Tabbutt, M., To, C., Wagoner, E. L., Wechsler, R. H., Aguena, M., Allam, S., Amon, A., Annis, J., Bacon, D., Baxter, E., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carrasco Kind, M., Carretero, J., Castander, F. J., Choi, A., Conselice, C., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., Desai, S., Diehl, H. T., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Giannantonio, T., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., Jain, B., James, D. J., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A. A., Roodman, A., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., and Varga, T. N.
Subjects: Cosmological parameter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, FOS: Physical sciences, observation [Cosmology], Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, 01 natural sciences, Observations [Cosmology], Cosmological parameters, Cosmology: observations, Dark energy, Large-scale structure of the Universe, mitigation, 0103 physical sciences, emission, scale structure catalogs, cosmological parameters, dark energy, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, 010308 nuclear & particles physics, Física, Astronomy and Astrophysics, redshift, uncertainties, Dark Energy, Space and Planetary Science, cosmology: observations, Cosmological Parameters, large-scale structure of the universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], constraints, Large-Scale Structure of the Universe, cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: M. Rodríguez-Monroy, N. Weaverdyck, J. Elvin-Poole et al., In this work, we present the galaxy clustering measurements of the two DES lens galaxy samples: a magnitude-limited sample optimized for the measurement of cosmological parameters, MAGLIM, and a sample of luminous red galaxies selected with the REDMAGIC algorithm. MAGLIM/REDMAGIC sample contains over 10 million/2.5 million galaxies and is divided into six/five photometric redshift bins spanning the range z ∈ [0.20, 1.05]/z ∈ [0.15, 0.90]. Both samples cover 4143 deg2 over which we perform our analysis blind, measuring the angular correlation function with an S/N ∼ 63 for both samples. In a companion paper, these measurements of galaxy clustering are combined with the correlation functions of cosmic shear and galaxy–galaxy lensing of each sample to place cosmological constraints with a 3 × 2pt analysis. We conduct a thorough study of the mitigation of systematic effects caused by the spatially varying survey properties and we correct the measurements to remove artificial clustering signals. We employ several decontamination methods with different configurations to ensure the robustness of our corrections and to determine the systematic uncertainty that needs to be considered for the final cosmology analyses. We validate our fiducial methodology using lognormal mocks, showing that our decontamination procedure induces biases no greater than 0.5σ in the (Ωm, b) plane, where b is the galaxy bias., Funding for the Dark Energy Survey Projects has been provided by the US Department of Energy, the US 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, 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. This paper is 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 Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This paper has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the US Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2021
Full Text: View/download PDF

35. The DES Bright Arcs Survey: Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey 5,000 Sq. Deg. Footprint

Author: O'Donnell, J. H., Wilkinson, R. D., Diehl, H. T., Aros-Bunster, C., Bechtol, K., Birrer, S., Buckley-Geer, E. J., Rosell, A. Carnero, Kind, M. Carrasco, da Costa, L. N., Lozano, S. J. Gonzalez, Gruendl, R. A., Hilton, M., Lin, H., Lindgren, K. A., Martin, J., Pieres, A., Rykoff, E. S., Sevilla-Noarbe, I., Sheldon, E., Sif��n, 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., Garc��a-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-Chinch��n, F., Pereira, M. E. S., Malag��n, A. A. Plazas, 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: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the combined results of eight searches for strong gravitational lens systems in the full 5,000 sq. deg. of Dark Energy Survey (DES) observations. The observations accumulated by the end of the third observing season fully covered the DES footprint in 5 filters (grizY), with an $i-$band limiting magnitude (at $10\sigma$) 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. 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., Comment: 38 pages, 17 figures, 4 tables, accepted by ApJS
Published: 2021

36. Validation of selection function, sample contamination and mass calibration in galaxy cluster samples

Author: Grandis, S., Klein, M., Mohr, J. J., Bocquet, S., Paulus, M., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Benson, B. A., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Capasso, R., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Eifler, T. F., Everett, S., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinch��n, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Saro, A., Scarpine, V., Schubnell, M., Serrano, S., Sheldon, E., Smith, M., Stark, A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., 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), DES, Grandis, S., Klein, M., Mohr, J. J., Bocquet, S., Paulus, M., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Benson, B. A., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Capasso, R., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Eifler, T. F., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Saro, A., Scarpine, V., Schubnell, M., Serrano, S., Sheldon, E., Smith, M., Stark, A. A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Varga, T. N., Weller, J., Wilkinson, R., National Science Foundation (US), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, and European Research Council
Subjects: Software_OPERATINGSYSTEMS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), ComputingMethodologies_SIMULATIONANDMODELING, Calibration (statistics), statistical [methods], RAIOS X, FOS: Physical sciences, Sample (statistics), Data_CODINGANDINFORMATIONTHEORY, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, methods: statistical, galaxies: clusters: general, large-scale structure of Universe, X-rays: galaxies: clusters, Astrophysics - Cosmology and Nongalactic Astrophysics, Hardware_INTEGRATEDCIRCUITS, clusters: general [galaxies], Limit (mathematics), Statistical physics, 010303 astronomy & astrophysics, Selection (genetic algorithm), Galaxy cluster, STFC, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, RCUK, Astronomy and Astrophysics, Function (mathematics), ComputerSystemsOrganization_PROCESSORARCHITECTURES, galaxies: cluster [X-rays], South Pole Telescope, Space and Planetary Science, Outlier, galaxies: clusters [X-rays], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: DES Collaboration: et al., We construct and validate the selection function of the MARD-Y3 galaxy cluster sample. This sample was selected through optical follow-up of the 2nd ROSAT faint source catalogue with Dark Energy Survey year 3 data. The selection function is modelled by combining an empirically constructed X-ray selection function with an incompleteness model for the optical follow-up. We validate the joint selection function by testing the consistency of the constraints on the X-ray flux–mass and richness–mass scaling relation parameters derived from different sources of mass information: (1) cross-calibration using South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) clusters, (2) calibration using number counts in X-ray, in optical and in both X-ray and optical while marginalizing over cosmological parameters, and (3) other published analyses. We find that the constraints on the scaling relation from the number counts and SPT-SZ cross-calibration agree, indicating that our modelling of the selection function is adequate. Furthermore, we apply a largely cosmology independent method to validate selection functions via the computation of the probability of finding each cluster in the SPT-SZ sample in the MARD-Y3 sample and vice versa. This test reveals no clear evidence for MARD-Y3 contamination, SPT-SZ incompleteness or outlier fraction. Finally, we discuss the prospects of the techniques presented here to limit systematic selection effects in future cluster cosmological studies., 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 MINECO under grants AYA2015- 71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, 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 7th Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).
Published: 2020

37. Noise from undetected sources in Dark Energy Survey images

Author: Eckert, K., Bernstein, G. M., Amara, A., Amon, A., Choi, A., Everett, S., Gruen, D., Gruendl, R. A., Huff, E. M., Kuropatkin, N., Roodman, A., Sheldon, E., Yanny, B., Zhang, Y., Abbott, T. M. C., Aguena, M., Avila, S., Bechtol, K., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Eifler, T. F., Evrard, A. E., Flaugher, B., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kron, R., Kuehn, K., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinch��n, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R., Wester, W., Wilkinson, R. D., Zuntz, J., Collaboration, the DES, Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), University of Illinois, Kavli Institute for Theoretical Physics, University of Chicago, The Ohio State University, Texas A&M University, Financiadora de Estudos e Projetos (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), German Research Foundation, Eckert, K., Bernstein, G. M., Amara, A., Amon, A., Choi, A., Everett, S., Gruen, D., Gruendl, R. A., Huff, E. M., Kuropatkin, N., Roodman, A., Sheldon, E., Yanny, B., Zhang, Y., Abbott, T. M. C., Aguena, M., Avila, S., Bechtol, K., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Eifler, T. F., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kron, R., Kuehn, K., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R., Wester, W., Wilkinson, R. D., Zuntz, J., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Diffuse radiation, weak, techniques: image processing, diffuse radiation [gravitational lensing], media_common.quotation_subject, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Poisson distribution, 7. Clean energy, 01 natural sciences, symbols.namesake, weak [gravitational lensing], 0103 physical sciences, Image noise, gravitational lensing: weak, techniques: image processing, diffuse radiation, education, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Weak gravitational lensing, STFC, media_common, Physics, education.field_of_study, image processing [techniques], 010308 nuclear & particles physics, Gravitational lensing: Weak, Shot noise, RCUK, Astronomy and Astrophysics, Techniques: Image processing, Galaxy, diffuse radiation, 13. Climate action, Space and Planetary Science, Sky, symbols, astro-ph.CO, Astrophysics - Instrumentation and Methods for Astrophysics, Noise (radio), Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract: For ground-based optical imaging with current CCD technology, the Poisson fluctuations in source and sky background photon arrivals dominate the noise budget and are readily estimated. Another component of noise, however, is the signal from the undetected population of stars and galaxies. Using injection of artifical galaxies into images, we demonstrate that the measured variance of galaxy moments (used for weak gravitational lensing measurements) in Dark Energy Survey (DES) images is significantly in excess of the Poisson predictions, by up to 30 per cent, and that the background sky levels are overestimated by current software. By cross-correlating distinct images of 'empty' sky regions, we establish that there is a significant image noise contribution from undetected static sources (US), which, on average, are mildly resolved at DES resolution. Treating these US as a stationary noise source, we compute a correction to the moment covariance matrix expected from Poisson noise. The corrected covariance matrix matches the moment variances measured on the injected DES images to within 5 per cent. Thus, we have an empirical method to statistically account for US in weak lensing measurements, rather than requiring extremely deep sky simulations. We also find that local sky determinations can remove most of the bias in flux measurements, at a small penalty in additional, but quantifiable, noise., KDE and GMB acknowledge support from NASA through a Research Support Agreement with grant 12-EUCLID11-0004, and grants AST-1615555 from the US National Science Foundation, and DE-SC0007901 from the US Department of Energy. Funding for the DES Projects has been provided by the US 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 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 MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, 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) e-Universe (CNPq grant 465376/2014-2).
Published: 2020

38. Machine Learning for Searching the Dark Energy Survey for Trans-Neptunian Objects

Author: Henghes, B., Lahav, O., Gerdes, D. W., Lin, H. W., Morgan, R., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sánchez, C., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., To, C., Wilkinson, R. D., DES Collaboration, UAM. Departamento de Física Teórica, 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, Henghes, B., Lahav, O., Gerdes, D. W., Lin, H. W., Morgan, R., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sánchez, C., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., To, C., Wilkinson, R. D., and Des, Collaboration
Subjects: Random Forests, FOS: Computer and information sciences, Solar System, Computer Science - Machine Learning, 010504 meteorology & atmospheric sciences, Computer science, FOS: Physical sciences, Machine learning, computer.software_genre, 01 natural sciences, Minor Planets, Machine Learning (cs.LG), Planet, 0103 physical sciences, Minor planet, Astrophysics - Earth and Planetary Astrophysic, [INFO]Computer Science [cs], Trans-Neptunian object, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Orbital elements, Earth and Planetary Astrophysics (astro-ph.EP), Random Forest, Receiver operating characteristic, business.industry, Trans-Neptunian objects, Minor planets, Computational methods, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Física, Astronomy and Astrophysics, Computational method, Trans-Neptunian Objects, Random forest, Space and Planetary Science, Asteroid, Artificial intelligence, business, Astrophysics - Instrumentation and Methods for Astrophysic, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], computer, Classifier (UML), Computational Methods
Abstract: In this paper we investigate how implementing machine learning could improve the efficiency of the search for Trans-Neptunian Objects (TNOs) within Dark Energy Survey (DES) data when used alongside orbit fitting. The discovery of multiple TNOs that appear to show a similarity in their orbital parameters has led to the suggestion that one or more undetected planets, an as yet undiscovered "Planet 9", may be present in the outer Solar System. DES is well placed to detect such a planet and has already been used to discover many other TNOs. Here, we perform tests on eight different supervised machine learning algorithms, using a dataset consisting of simulated TNOs buried within real DES noise data. We found that the best performing classifier was the Random Forest which, when optimised, performed well at detecting the rare objects. We achieve an area under the receiver operating characteristic (ROC) curve, (AUC) $= 0.996 \pm 0.001$. After optimizing the decision threshold of the Random Forest, we achieve a recall of 0.96 while maintaining a precision of 0.80. Finally, by using the optimized classifier to pre-select objects, we are able to run the orbit-fitting stage of our detection pipeline five times faster., Comment: Published in PASP, 16 pages, 6 figures
Published: 2020
Full Text: View/download PDF

39. Shadows in the Dark: Low-Surface-Brightness Galaxies Discovered in the Dark Energy Survey

Author: Tanoglidis, D., Drlica-Wagner, A., Wei, K., Li, T. S., Sánchez, F. J., Zhang, Y., Peter, A. H. G., Feldmeier-Krause, A., Prat, J., Casey, K., Palmese, A., Sánchez, C., DeRose, J., Conselice, C., Gagnon, L., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bechtol, K., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chang, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Huterer, D., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, D. L., Walker, A. R., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), UAM. Departamento de Física Teórica, Tanoglidis, D., Drlica-Wagner, A., Wei, K., T. S., Li, Sánchez, F. J., Zhang, Y., Peter, A. H. G., Feldmeier-Krause, A., Prat, J., Casey, K., Palmese, A., Sánchez, C., Derose, J., Conselice, C., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bechtol, K., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Chang, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Huterer, D., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, D. L., and Walker, A. R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, FOS: Physical sciences, Astrophysics, Sky surveys, 01 natural sciences, Imaging data, Luminosity, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Coma Cluster, Surface brightness, Sky survey, Global Air Sampling Program, education, 010303 astronomy & astrophysics, STFC, Low surface brightness galaxie, Physics, education.field_of_study, 010308 nuclear & particles physics, Física, RCUK, Astronomy and Astrophysics, Galaxies, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Star Formation, Dark energy, Low surface brightness galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present a catalog of 23,790 extended low-surface-brightness galaxies (LSBGs) identified in $\sim 5000 ��^2$ from the first three years of imaging data from the Dark Energy Survey (DES). Based on a single-component S��rsic model fit, we define extended LSBGs as galaxies with $g$-band effective radii $R_{eff}(g) > 2.5''$ and mean surface brightness $\bar��_{eff}(g) > 24.2 \,mag ��rcsec^{-2}$. We find that the distribution of LSBGs is strongly bimodal in $(g-r)$ vs.\ $(g-i$) color space. We divide our sample into red ($g-i \geq 0.60$) and blue ($g-i 1.5 \,kpc$ and central surface brighthness $��_0(g) > 24.0\, mag \,arcsec^{-2}$. The wide-area sample of LSBGs in DES can be used to test the role of environment on models of LSBG formation and evolution., 31 pages, 19 figures. Version accepted for publication in ApJS. Data products related to this work can be found in: https://des.ncsa.illinois.edu/releases/other/y3-lsbg
Published: 2020
Full Text: View/download PDF

40. A DESGW search for the electromagnetic counterpart to the LIGO/Virgo gravitational-wave binary neutron star merger candidate S190510g

Author: Garcia, A., Morgan, R., Herner, K., Palmese, A., Soares-Santos, M., Annis, J., Brout, D., Vivas, A. K., Drlica-Wagner, A., Santana-Silva, L., Tucker, D. L., Allam, S., Wiesner, M., García-Bellido, J., Gill, M. S. S., Sako, M., Kessler, R., Davis, T. M., Scolnic, D., Casares, J., Chen, H., Conselice, C., Cooke, J., Doctor, Z., Foley, R. J., Horvath, J., Howell, D. A., Kilpatrick, C. D., Lidman, C., E. , F. Olivares, Paz-Chinchón, F., Pineda-G. , J., Quirola-Vásquez, J., Rest, A., Sherman, N., Abbott, T. M. C., Aguena, M., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Everett, S., Flaugher, B., Fosalba, P., Friedel, D., 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., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R., Weller, J., Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), Higher Education Funding Council for England, University of Illinois, University of Chicago, Texas A&M University, Financiadora de Estudos e Projetos (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional das Fundaçôes Estaduais de Amparo à Pesquisa (Brasil), German Research Foundation, University of California, Argonne National Laboratory (US), University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (España), University College London, University of London, University of Edinburgh, Federal Institute of Technology Zurich, Consejo Superior de Investigaciones Científicas (España), University of Michigan, University of Pennsylvania, Stanford University, European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Garcia, A., Morgan, R., Herner, K., Palmese, A., Soares-Santos, M., Annis, J., Brout, D., Vivas, A. K., Drlica-Wagner, A., Santana-Silva, L., Tucker, D. L., Allam, S., Wiesner, M., García-Bellido, J., Gill, M. S. S., Sako, M., Kessler, R., Davis, T. M., Scolnic, D., Casares, J., Chen, H., Conselice, C., Cooke, J., Doctor, Z., Foley, R. J., Horvath, J., Howell, D. A., Kilpatrick, C. D., Lidman, C., F. Olivares, E., Paz-Chinchón, F., Pineda-G., J., Quirola-Vásquez, J., Rest, A., Sherman, N., Abbott, T. M. C., Aguena, M., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Everett, S., Flaugher, B., Fosalba, P., Friedel, D., 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., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R., and Weller, J.
Subjects: neutron star: binary, Software_OPERATINGSYSTEMS, 010504 meteorology & atmospheric sciences, Binary number, Astrophysics, Kilonova, 7. Clean energy, 01 natural sciences, optical, LIGO, dark energy, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), ComputerSystemsOrganization_PROCESSORARCHITECTURES, Supernova, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, data analysis method, ComputingMethodologies_SIMULATIONANDMODELING, FOS: Physical sciences, Data_CODINGANDINFORMATIONTHEORY, Gravitational-wave astronomy, electromagnetic field: production, Gravitational wave astronomy (675), binary: coalescence, 0103 physical sciences, Binary star, supernova, Hardware_INTEGRATEDCIRCUITS, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], detector: optical, Instrumentation and Methods for Astrophysics (astro-ph.IM), STFC, 0105 earth and related environmental sciences, Gravitational wave, gravitational radiation, RCUK, Astronomy and Astrophysics, Neutron star, VIRGO, 13. Climate action, Space and Planetary Science, gravitational radiation: emission, gravitational wave astronomy, Gravitational wave astronomy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: DES Collaboration: et al., We present the results from a search for the electromagnetic counterpart of the LIGO/Virgo event S190510g using the Dark Energy Camera (DECam). S190510g is a binary neutron star (BNS) merger candidate of moderate significance detected at a distance of 227 ± 92 Mpc and localized within an area of 31 (1166) square degrees at 50% (90%) confidence. While this event was later classified as likely nonastrophysical in nature within 30 hours of the event, our short latency search and discovery pipeline identified 11 counterpart candidates, all of which appear consistent with supernovae following offline analysis and spectroscopy by other instruments. Later reprocessing of the images enabled the recovery of six more candidates. Additionally, we implement our candidate selection procedure on simulated kilonovae and supernovae under DECam observing conditions (e.g., seeing and exposure time) with the intent of quantifying our search efficiency and making informed decisions on observing strategy for future similar events. This is the first BNS counterpart search to employ a comprehensive simulation-based efficiency study. We find that using the current follow-up strategy, there would need to be 19 events similar to S190510g for us to have a 99% chance of detecting an optical counterpart, assuming a GW170817-like kilonova. We further conclude that optimization of observing plans, which should include preference for deeper images over multiple color information, could result in up to a factor of 1.5 reduction in the total number of follow-ups needed for discovery., 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 UrbanaChampaign, 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, 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 InterAmerican Observatory at NSFs 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, SEV2016-0588, 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) e-Universe (CNPq grant 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 material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under grant No. 1744555. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation. R.M. thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining grant #1829740, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. F.O.E. acknowledges support from the FONDECYT grant No. 1201223.
Published: 2020

41. Dark Energy Survey Year 3 Results: Galaxy mock catalogs for BAO analysis

Author: Ferrero, I., Crocce, M., Tutusaus, I., Porredon, A., Blot, L., Fosalba, P., Rosell, A. Carnero, Avila, S., Izard, A., Elvin-Poole, J., Chan, K. C., Camacho, H., Rosenfeld, R., Sanchez, E., Tallada-Crespí, P., Carretero, J., Sevilla-Noarbe, I., Gaztanaga, E., Andrade-Oliveira, F., De Vicente, J., Mena-Fernández, J., Ross, A. J., Cid, D. Sanchez, Ferté, A., Brandao-Souza, A., Fang, X., Krause, E., Gomes, D., Aguena, M., Allam, S., Annis, J., Bertin, E., Brooks, D., Kind, M. Carrasco, Castander, F. J., Cawthon, R., Choi, A., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huterer, D., James, D. J., Kuehn, K., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Muir, J., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Percival, W. J., Malagón, A. A. Plazas, Rodriguez-Monroy, M., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Ferrero, I., Crocce, M., Tutusaus, I., Porredon, A., Blot, L., Fosalba, P., Carnero Rosell, A., Avila, S., Izard, A., Elvin-Poole, J., Chan, K. C., Camacho, H., Rosenfeld, R., Sanchez, E., Tallada-Crespi, P., Carretero, J., Sevilla-Noarbe, I., Gaztanaga, E., Andrade-Oliveira, F., De Vicente, J., Mena-Fernandez, J., Ross, A. J., Sanchez Cid, D., Ferte, A., Brandao-Souza, A., Fang, X., Krause, E., Gomes, D., Aguena, M., Allam, S., Annis, J., Bertin, E., Brooks, D., Carrasco Kind, M., Castander, F. J., Cawthon, R., Choi, A., Conselice, C., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huterer, D., James, D. J., Kuehn, K., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Muir, J., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Percival, W. J., Plazas Malagon, A. A., Rodriguez-Monroy, M., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., University of Oslo, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), The Ohio State University, Max-Planck-Institut für Astrophysik, Instituto de Astrofisica de Canarias, Laboratório Interinstitucional de e-Astronomia - LIneA, Dpto. Astrofísica, Universidad Autonoma de Madrid, University of Portsmouth, Sun Yat-sen University, Universidade Estadual Paulista (UNESP), ICTP South American Institute for Fundamental Research, Medioambientales y Tecnológicas (CIEMAT), Port d'Informació Científica (PIC), The Barcelona Institute of Science and Technology, California Institute of Technology, Universidade Estadual de Campinas (UNICAMP), University of Arizona, Universidade de São Paulo (USP), Rua General José Cristino, Fermi National Accelerator Laboratory, Institut d'Astrophysique de Paris, University College London, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, University of Wisconsin-Madison, University of Manchester, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, University of Chicago, Santa Cruz Institute for Particle Physics, Stanford University, SLAC National Accelerator Laboratory, University of Queensland, Ludwig-Maximilians-Universität, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Texas AandM University, Institució Catalana de Recerca i Estudis Avançats, University of Cambridge, University of Waterloo, Perimeter Institute for Theoretical Physics, Princeton University, University of Southampton, Oak Ridge National Laboratory, Giessenbachstrasse, and Ludwig-Maximilians Universität München
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Halo occupation distribution, Galaxies: distances and redshifts, Observational cosmology, distances and redshifts [Galaxies], halo [Galaxy], Catalogs, Galaxy: halo, Methods: numerical, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, numerical [Methods], Computer Science::Information Retrieval, distances and redshift [Galaxies], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Redshift survey, Redshift, Galaxy, Space and Planetary Science, Dark energy, Catalog, Baryon acoustic oscillations, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Ferrero, I., et al. (DES Collaboration), The calibration and validation of scientific analysis in simulations is a fundamental tool to ensure unbiased and robust results in observational cosmology. In particular, mock galaxy catalogs are a crucial resource to achieve these goals in the measurement of baryon acoustic oscillation (BAO) in the clustering of galaxies. Here we present a set of 1952 galaxy mock catalogs designed to mimic the Dark Energy Survey Year 3 BAO sample over its full photometric redshift range 0:6 < zphoto < 1:1. The mocks are based upon 488 ICE-COLA fast N-body simulations of full-sky light cones and were created by populating halos with galaxies, using a hybrid halo occupation distribution halo abundance matching model. This model has ten free parameters, which were determined, for the first time, using an automatic likelihood minimization procedure.We also introduced a novel technique to assign photometric redshift for simulated galaxies, following a two-dimensional probability distribution with VIMOS Public Extragalactic Redshift Survey data. The calibration was designed to match the observed abundance of galaxies as a function of photometric redshift, the distribution of photometric redshift errors, and the clustering amplitude on scales smaller than those used for BAO measurements. An exhaustive analysis was done to ensure that the mocks reproduce the input properties. Finally, mocks were tested by comparing the angular correlation function w(θ), angular power spectrum ζp(rΓ) and projected clustering p(r?) to theoretical predictions and data. The impact of volume replication in the estimate of the covariance is also investigated. The success in accurately reproducing the photometric redshift uncertainties and the galaxy clustering as a function of redshift render this mock creation pipeline as a benchmark for future analyses of photometric galaxy surveys.
Published: 2021

42. DES Y3 results: Blending shear and redshift biases in image simulations

Author: MacCrann, N., Becker, M. R., McCullough, J., Amon, A., Gruen, D., Jarvis, M., Choi, A., Troxel, M. A., Sheldon, E., Yanny, B., Herner, K., Dodelson, S., Zuntz, J., Eckert, K., Rollins, R. P., Varga, T. N., Bernstein, G. M., Gruendl, R. A., Harrison, I., Hartley, W. G., Sevilla-Noarbe, I., Pieres, A., Bridle, S. L., Myles, J., Alarcon, A., Everett, S., S��nchez, C., Huff, E. M., Tarsitano, F., Gatti, M., Secco, L. F., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., Crocce, M., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Ferrero, I., Fert��, A., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Muir, J., Ogando, R. L. C., Palmese, A., Paz-Chinch��n, F., Plazas, A. A., Rodriguez-Monroy, M., Roodman, A., Samuroff, S., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., 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), and DES
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: As the statistical power of galaxy weak lensing reaches percent level precision, large, realistic and robust simulations are required to calibrate observational systematics, especially given the increased importance of object blending as survey depths increase. To capture the coupled effects of blending in both shear and photometric redshift calibration, we define the effective redshift distribution for lensing, $n_{\gamma}(z)$, and describe how to estimate it using image simulations. We use an extensive suite of tailored image simulations to characterize the performance of the shear estimation pipeline applied to the Dark Energy Survey (DES) Year 3 dataset. We describe the multi-band, multi-epoch simulations, and demonstrate their high level of realism through comparisons to the real DES data. We isolate the effects that generate shear calibration biases by running variations on our fiducial simulation, and find that blending-related effects are the dominant contribution to the mean multiplicative bias of approximately $-2\%$. By generating simulations with input shear signals that vary with redshift, we calibrate biases in our estimation of the effective redshfit distribution, and demonstrate the importance of this approach when blending is present. We provide corrected effective redshift distributions that incorporate statistical and systematic uncertainties, ready for use in DES Year 3 weak lensing analyses., Comment: Submitted to MNRAS. See https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 cosmology release. Version accepted by mnras
Published: 2021

43. Cross-correlation of DES Y3 lensing and ACT/${\it Planck}$ thermal Sunyaev Zel'dovich Effect I: Measurements, systematics tests, and feedback model constraints

Author: Gatti, M., Pandey, S., Baxter, E., Hill, J. C., Moser, E., Raveri, M., Fang, X., DeRose, J., Giannini, G., Doux, C., Huang, H., Battaglia, N., Alarcon, A., Amon, A., Becker, M., Campos, A., Chang, C., Chen, R., Choi, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferte, A., Harrison, I., Maccrann, N., Mccullough, J., Myles, J., Alsina, A. Navarro, Prat, J., Rollins, R. P., Sanchez, C., Shin, T., Troxel, M., Tutusaus, I., Yin, B., Abbott, T., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bernstein, G., Bertin, E., Bolliet, B., Bond, J. R., Brooks, D., Burke, D. L., Calabrese, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cawthon, R., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. da Silva, DeVicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Dunkley, J., Evrard, A. E., Ferraro, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcıa-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Herner, K., Hincks, A. D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, J. P., Huterer, D., Jain, B., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Lima, M., Lokken, M., Madhavacheril, M. S., Maia, M. A. G., Marshall, J. L., Mcmahon, J. J., Melchior, P., Moodley, K., Mohr, J. J., Morgan, R., Nati, F., Niemack, M. D., Page, L., Palmese, A., Paz-Chinchon, F., Pieres, A., Malagon, A. A. Plazas, Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Schaan, E., Secco, L. F., Serrano, S., Sheldon, E., Sherwin, B. D., Sifon, C., Smith, M., Soares-Santos, M., Spergel, D., Suchyta, E., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Weller, J., Wilkinson, R. D., Wollack, E. J., and Xu, Z.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a tomographic measurement of the cross-correlation between thermal Sunyaev-Zeldovich (tSZ) maps from ${\it Planck}$ and the Atacama Cosmology Telescope (ACT) and weak galaxy lensing shears measured during the first three years of observations of the Dark Energy Survey (DES Y3). This correlation is sensitive to the thermal energy in baryons over a wide redshift range, and is therefore a powerful probe of astrophysical feedback. We detect the correlation at a statistical significance of $21\sigma$, the highest significance to date. We examine the tSZ maps for potential contaminants, including cosmic infrared background (CIB) and radio sources, finding that CIB has a substantial impact on our measurements and must be taken into account in our analysis. We use the cross-correlation measurements to test different feedback models. In particular, we model the tSZ using several different pressure profile models calibrated against hydrodynamical simulations. Our analysis marginalises over redshift uncertainties, shear calibration biases, and intrinsic alignment effects. We also marginalise over $\Omega_{\rm m}$ and $\sigma_8$ using ${\it Planck}$ or DES priors. We find that the data prefers the model with a low amplitude of the pressure profile at small scales, compatible with a scenario with strong AGN feedback and ejection of gas from the inner part of the halos. When using a more flexible model for the shear profile, constraints are weaker, and the data cannot discriminate between different baryonic prescriptions., Comment: submitted to PRD
Published: 2021
Full Text: View/download PDF

44. OzDES Reverberation Mapping Program: The first Mg II lags from five years of monitoring

Author: Yu, Zhefu, Martini, Paul, Penton, A., Davis, T. M., Malik, U., Lidman, C., Tucker, B. E., Sharp, R., Kochanek, C. S., Peterson, B. M., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Asorey, J., Bertin, E., Brooks, D., Burke, D. L., Calcino, J., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Costanzi, M., da Costa, L. N., Pereira, M. E. S., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., James, D. J., Kim, A. G., Kron, R., Kuehn, K., Kuropatkin, N., Lewis, G. F., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Möller, A., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., and Tucker, D. L.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: Reverberation mapping is a robust method to measure the masses of supermassive black holes (SMBHs) outside of the local Universe. Measurements of the radius -- luminosity ($R-L$) relation using the Mg II emission line are critical for determining these masses near the peak of quasar activity at $z \approx 1 - 2$, and for calibrating secondary mass estimators based on Mg II that can be applied to large samples with only single-epoch spectroscopy. We present the first nine Mg II lags from our five-year Australian Dark Energy Survey (OzDES) reverberation mapping program, which substantially improves the number and quality of Mg II lag measurements. As the Mg II feature is somewhat blended with iron emission, we model and subtract both the continuum and iron contamination from the multi-epoch spectra before analyzing the Mg II line. We also develop a new method of quantifying correlated spectroscopic calibration errors based on our numerous, contemporaneous observations of F-stars. The lag measurements for seven of our nine sources are consistent with both the H$\beta$ and Mg II $R-L$ relations reported by previous studies. Our simulations verify the lag reliability of our nine measurements, and we estimate that the median false positive rate of the lag measurements is $4\%$., Comment: 18 pages, 12 figures. MNRAS, Volume 507, Issue 3, November 2021, Pages 3771-3788
Published: 2021
Full Text: View/download PDF

45. First Measurement of the Hubble Constant from a Dark Standard Siren using the Dark Energy Survey Galaxies and the LIGO/Virgo Binary-Black-hole Merger GW170814

Author: Soares-Santos, M, Palmese, A, Hartley, W, Annis, J, Garcia-Bellido, J, Lahav, O, Doctor, Z, Fishbach, M, Holz, D. E, Lin, H, Pereira, M. E. S, Garcia, A, Herner, K, Kessler, R, Peiris, V, H, Sako, M, Allam, S, Brout, D, Carnero Rosell, A, Chen, H. Y, Conselice, C, Derose, J, Devicente, J, Diehl, H. T, Gill, M. S. S, Gschwend, J, Sevilla-Noarbe, I and Tucker, D. L., Wechsler, R, Berger, E, Cowperthwaite, P. S, Metzger, B. D, Williams, P. K. G, Abbott, T. M. C, Abdalla, F. B, Avila, S, Bechtol, K, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, D. L, Kind, Carrasco and Carretero, M., J, Castander, F. J, Crocce, M, Cunha, C. E, D'Andrea, C. B, da Costa, L. N, Davis, C, Desai, S, Doel, P, Drlica-Wagner, A, Eifler, T. F, Evrard, A. E, Flaugher, B, Fosalba, P, Frieman, J, Gaztanaga, E, Gerdes, D. W, Gruen, D, Gruendl, R. A, Gutierrez, G, Hollowood, D. L, Hoyle, B, James, D. J, Jeltema, T, Kuehn, K, Kuropatkin, N, T. S, Li, Lima, M, Maia, M. A. G, Marshall, J. L, Menanteau, F, Miquel, R, Neilsen, E, Ogando, R. L. C, Plazas, A. A, Romer, A. K, Roodman, A, Sanchez, E, Scarpine, V and Schindler, R, Schubnell, M, Serrano, S, Smith, M, Smith, R. C, Sobreira, F, Suchyta, E, Swanson, M. E. C, Tarle, G, Thomas, R. C, Walker, A. R, Wester, W, Zuntz, J, Abbott, B. P, Abbott, R, Abbott, T. D, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, R. X, Adya, V. B, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O. D, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, M. A, Altin, P. A, Amato, A, Ananyeva, A, Anderson, S. B, Anderson, W. G, Angelova, S, Appert, S, Arai, K, Araya, M. C, Areeda, J. S, Arene, M, Ascenzi, S, Ashton, G, Aston, S. M, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Avendano, V and Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, M. K. M, Bae, S, Baker, P. T, Baldaccini, F, Ballardin, G, Ballmer, S. W, Banagiri, S, Barayoga, J. C, Barclay, S. E, Barish, B. C, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I and Bassiri, Basti, A, Bawaj, M, Bayley, J. C, Bazzan, M, Becsy, B, Bejger, M, Bell, A. S, Beniwal, D, Bergmann, G, Bernuzzi, S, Bero, J. J, Berry, C. P. L, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Bilenko, I. A, Bilgili, S. A, Billingsley, G, Birch, J, Birney, R, Birnholtz, O, Biscans, S, Biscoveanu, S, Bisht, A, Bitossi, M, Blackburn, J. K, Blair, C. D, Blair, D. G, Blair, R. M, Bloemen, S, Bode, N, Boer, M, Boetzel, Y, Bogaert, G, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B. A, Booth, C. D, Bork, R, Boschi, V and Bose, Bossie, K, Bossilkov, V and Bosveld, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P. R, Bramley, A, Branchesi, M, Brau, J. E, Briant, T, Briggs, J. H, Brighenti, F, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A. F, Brown, D. D, Brunett, S, Buikema, A, Bulik, T, Bulten, H. J, Buonanno, A, Buskulic, D, Buy, C, Byer, R. L, Cabero, M, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, Calderon and Callister, J., T. A., Calloni, E, Camp, J. B, Campbell, W. A, Cannon, K. C, Cao, H, Cao, J, Capocasa, E, Carbognani, F, Caride, S, Carney, M. F, Carullo, G, Diaz, Casanueva and Casentini, J., C, Caudill, S, Cavaglia, M, Cavalieri, R, Cella, G, Cerda-Duran, P, Cerretani, G, Cesarini, E, Chaibi, O, Chakravarti, K, Chamberlin, S. J, Chan, M, Chao, S, Charlton, P, Chase, E. A, Chassande-Mottin, E, Chatterjee, D, Chaturvedi, M, Chatziioannou, K, Cheeseboro, B. D, Chen, X, Chen, Y, Cheng, H-P and Cheong, C. K., Chia, H. Y, Chincarini, A, Chiummo, A, Cho, G, Cho, H. S, Cho, M, Christensen, N, Chu, Q, Chua, S, Chung, K. W, Chung, S, Ciani, G, Ciobanu, A. A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, J. A, Clearwater, P, Cleva, F, Cocchieri, C, Coccia, E, Colgan, R, Colleoni, M, Collette, C. G, Collins, C, Cominsky, L. R, Constancio Jr, M, Conti, L, Cooper, S. J, Corban, P, Corbitt, T. R, Cordero-Carrion, I and Corley, K. R., Cornish, N, Corsi, A, Cortese, S, Costa, C. A, Cotesta, R, Coughlin, M. W, Coughlin, S. B, Coulon, J-P and Countryman, S. T., Couvares, P, Covas, P. B, Cowan, E. E, Coward, D. M, Cowart, M. J, Coyne, D. C, Coyne, R, Creighton, J. D. E, Creighton, T. D, Cripe, J, Croquette, M, Crowder, S. G, Cullen, T. J, Cumming, A, Cunningham, L, Cuoco, E, Dal Canton, T, Dalya, G, D'Antonio, S, Danilishin, S. L, Danzmann, K, Dasgupta, A, Costa, Da Silva and Datrier, C. F., L. E. H., Dattilo, V and Dave, I and Davis, D, Daw, E. J, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Deleglise, S, Del Pozzo, W, Demarchi, L. M, Demos, N, Dent, T, De Pietri, R, Derby, J, De Rosa, R, De Rossi, C, Desalvo, R, de Varona, O, Dhurandhar, S, Diaz, M. C, Dietrich, T, Di Fiore, L, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Palma, Di, I and Di Renzo, F, Dmitriev, A, Donovan, F, Dooley, K. L, Doravari, S, Dorrington, I and Downes, T. P., Drago, M, Driggers, J. C, Du, Z, Dupej, P, Dwyer, S. E, Easter, P. J, Edo, T. B, Edwards, M. C, Effler, A, Ehrens, P, Eichholz, J, Eikenberry, S. S, Eisenmann, M, Eisenstein, R. A, Estelles, H, Estevez, D, Etienne, Z. B, Etzel, T, Evans, M, Evans, T. M, Fafone, V and Fair, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, W. M, Fauchon-Jones, E. J, Favata, M, Fays, M, Fazio, M, Fee, C, Feicht, J, Fejer, M. M, Feng, F, Fernandez-Galiana, A, Ferrante, I and Ferreira, E. C., Ferreira, T. A, Ferrini, F, Fidecaro, F, Fiori, I and Fiorucci, Fisher, R. P, Fishner, J. M, Fitz-Axen, M, Flaminio, R, Fletcher, M, Flynn, E, Fong, H, Fournier, J-D and Font, J. A., Forsyth, P. W. F, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Fritschel, P, Frolov, V. V, Fulda, P, Fyffe, M, Gabbard, H. A, Gadre, B. U, Gaebel, S. M, Gair, J. R, Gammaitoni, L, Ganija, M. R, Gaonkar, S. G, Garcia-Quiros, C, Garufi, F, Gateley, B, Gaudio, S, Gaur, G, Gayathri, V and Gemme, G, Genin, E, Gennai, A, George, D, George, J, Gergely, L, Germain, V and Ghonge, Ghosh, Abhirup and Ghosh, Archisman and Ghosh, Giacomazzo, B, Giaime, J. A, Giardina, K. D, Giazotto, A, Gill, K, Giordano, G, Glover, L, Godwin, P, Goetz, E, Goetz, R, Goncharov, B, Gonzalez, G, Castro, Gonzalez and Gopakumar, J. M., Gorodetsky, M. L, Gossan, S. E, Gosselin, M, Gouaty, R, Grado, A, Graef, C, Granata, M, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, A. C, Green, R, Gretarsson, E. M, Groot, P, Grote, H, Grunewald, S, Guidi, G. M, Gulati, H. K, Guo, Y, Gupta, A, Gupta, M. K, Gustafson, E. K, Gustafson, R, Haegel, L, Halim, O, Hall, B. R, Hall, E. D, Hamilton, E. Z, Hammond, G, Haney, M, Hanke, M. M, Hanks, J, Hanna, C, Hannuksela, O. A, Hanson, J, Hardwick, T, Haris, K, Harms, J, Harry, G. M, Harry, I. W, Haster, C-J and Haughian, K, Hayes, F. J, Healy, J, Heidmann, A, Heintze, M. C, Heitmann, H, Hemming, G, Hendry, M, Heng, I. S, Hennig, J, Heptonstall, A. W, Vivanco, Francisco Hernandez and Heurs, M, Hild, S, Hinderer, T, Hoak, D, Hochheim, S, Hofman, D, Holgado, A. M, Holland, N. A, Holt, K, Hopkins, P, Horst, C, Hough, J, Howell, E. J, Hoy, C. G, Hreibi, A, Huerta, E. A, Hughey, B, Hulko, M, Husa, S, Huttner, S. H, Huynh-Dinh, T, Idzkowski, B, Iess, A, Ingram, C, Inta, R, Intini, G, Irwin, B, Isac, J-M and Isa, H. N., Isi, M, Iyer, B. R, Izumi, K, Jacqmin, T, Jadhav, S. J, Jani, K, Janthalur, N. N, Jaranowski, P, Jenkins, A. C, Jiang, J, Johnson, D. S, Jones, A. W, Jones, I, Jones, R, Jonker, R. J. G, Ju, L, Junker, J, Kalaghatgi, Kalogera, V and Kamai, B, Kandhasamy, S, Kang, G, Kanner, J. B, Kapadia, S. J, Karki, S, Karvinen, K. S, Kashyap, R, Kasprzack, M, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaufer, S, Kawabe, K, Keerthana, N, Kefelian, F, Keitel, D, Kennedy, R, Key, J. S, Khalili, F. Y, Khan, H, Khan, I and Khan, Khan, Z, Khazanov, E. A, Khursheed, M, Kijbunchoo, N, Kim, Chunglee and Kim, J. C., Kim, K, Y-M and Kim, W, Kim, W. S, Kimball, C, King, E. J, King, P. J, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J. S, Kleybolte, L, Klika, J. H, Klimenko, S, Knowles, T. D, Koch, P, Koehlenbeck, S. M, Koekoek, G, Koley, S, Kondrashov, V and Kontos, Koper, N, Korobko, M, Korth, W. Z, Kowalska, I and Kozak, D. B., Kringel, V and Krishnendu, Krolak, A, Kuehn, G, Kumar, A, Kumar, P, Kumar, R, Kumar, S, Kuo, L, Kutynia, A, Kwang, S, Lackey, B. D, Lai, K. H, Lam, T. L, Landry, M, Lane, B. B, Lang, R. N, Lange, J, Lantz, B, Lanza, R. K, Lasky, P. D, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y. K, Lee, C. H, Lee, H. K, Lee, H. M, Lee, H. W, Lee, J, Lee, K, Lehmann, J, Lenon, A, Letendre, N, Levin, Y, Li, J, K. J. L, Li, T. G. F, Li, Li, X, Lin, F, Linde, F, Linker, S. D, Littenberg, T. B, Liu, J, Liu, X, R. K. L, Lo, Lockerbie, N. A, London, L. T, Longo, A, Lorenzini, M, Loriette, V and Lormand, Losurdo, G, Lough, J. D, Lousto, C. O, Lovelace, G, Lower, M. E, Lueck, H, Lumaca, D, Lundgren, A. P, Lynch, R, Ma, Y, Macas, R, Macfoy, S, Macinnis, M, Macleod, D. M, Macquet, A, Hernandez, Magana and Magana-Sandoval, I., Zertuche, Magana and Magee, L., R. M., Majorana, E, Maksimovic, I and Malik, Man, N, Mandic, V and Mangano, V and Mansell, G. L., Manske, M, Mantovani, M, Marchesoni, F, Marion, F, Marka, S, Marka, Z, Markakis, C, Markosyan, A. S, Markowitz, A, Maros, E, Marquina, A, Marsat, S, Martelli, F, Martin, I. W, Martin, R. M, Martynov, Mason, K, Massera, E, Masserot, A, Massinger, T. J, Masso-Reid, M, Mastrogiovanni, S, Matas, A, Matichard, F, Matone, L, Mavalvala, N, Mazumder, N, Mccann, J. J, Mccarthy, R, Mcclelland, D. E, Mccormick, S, Mcculler, L, Mcguire, S. C, Mciver, J, Mcmanus, D. J, Mcrae, T, Mcwilliams, S. T, Meacher, D, Meadors, G. D, Mehmet, M, Mehta, A. K, Meidam, J, Melatos, A, Mendell, G, Mercer, R. A, Mereni, L, Merilh, E. L, Merzougui, M, Meshkov, S, Messenger, C, Messick, C, Metzdorff, R, Meyers, P. M, Miao, H, Michel, C, Middleton, H, Mikhailov, E. E, Milano, L, Miller, A. L, Miller, A, Millhouse, M, Mills, J. C, Milovich-Goff, M. C, Minazzoli, O, Minenkov, Y, Mishkin, A, Mishra, C, Mistry, T, Mitra, S, Mitrofanov, V. P, Mitselmakher, G, Mittleman, R, Mo, G, Moffa, D, Mogushi, K, Mohapatra, S. R. P, Montani, M, Moore, C. J, Moraru, D, Moreno, G, Morisaki, S, Mours, B, Mow-Lowry, C. M, Mukherjee, Arunava and Mukherjee, Mukherjee, S, Mukund, N, Mullavey, A, Munch, J, Muniz, E. A, Muratore, M, Murray, P. G, Nardecchia, I and Naticchioni, L, Nayak, R. K, Neilson, J, Nelemans, G, Nelson, T. J. N, Nery, M, Neunzert, A, K. Y, Ng, Ng, S, Nguyen, P, Nichols, D, Nissanke, S, Nocera, F, North, C, Nuttall, L. K, Obergaulinger, M, Oberling, J, O'Brien, B. D, O'Dea, G. D, Ogin, G. H, J. J, Oh, S. H, Oh, Ohme, F, Ohta, H, Okada, M. A, Oliver, M, O'Reilly, B, Oppermann, P, O'Shaughnessy, R, Oram, Richard J, Ormiston, R. G, Ortega, L. F, Ossokine, S, Ottaway, D. J, Overmier, H, Owen, B. J, Pace, A. E, Pagano, G, Page, M. A, Pai, A, Pai, S. A, Palamos, J. R, Palashov, O, Palomba, C, Pal-Singh, A, Pan, Huang-Wei and Pang, Pang, P. T. H, Pankow, C, Pannarale, F, Pant, B. C, Paoletti, F, Paoli, A, Parida, A, Parker, W, Pascucci, D, Pasqualetti, A, Passaquieti, R, Passuello, D, Patil, M, Patricelli, B, Pearlstone, B. L, Pedersen, C, Pedraza, M, Pedurand, R, Pele, A, Penn, S, Perez, C. J, Perreca, A, Pfeiffer, H. P, Phelps, M, Phukon, K. S, Piccinni, O. J, Pichot, M, Piergiovanni, F, Pillant, G, Pinard, L, Pirello, M, Pitkin, M, Poggiani, R, Pong, D. Y. T, Ponrathnam, S, Popolizio, P, Porter, E. K, Powell, J, Prajapati, A. K, Prasad, J, Prasai, K, Prasanna, R, Pratten, G, Prestegard, T, Privitera, S, Prodi, G. A, Prokhorov, L. G, Puncken, O, Punturo, M, Puppo, P, Puerrer, M, Qi, H, Quetschke, V and Quinonez, P. J., Quintero, E. A, Quitzow-James, R, Radkins, H, Radulescu, N, Raffai, P, Raja, S, Rajan, C, Rajbhandari, B, Rakhmanov, M, Ramirez, K. E, Ramos-Buades, A, Rana, Javed and Rao, Rapagnani, P, Raymond, V and Razzano, Read, J, Regimbau, T, Rei, L, Reid, S, Reitze, D. H, Ren, W, Ricci, F, Richardson, C. J, Richardson, J. W, Ricker, P. M, Riles, K, Rizzo, M, Robertson, N. A, Robie, R, Rocchi, A, Rolland, L, Rollins, J. G, Roma, V. J, Romanelli, M, Romano, R, Romel, C. L, Romie, J. H, Rose, K, Rosinska, D, Rosofsky, S. G, Ross, M. P, Rowan, S, Ruediger, A, Ruggi, P, Rutins, G, Ryan, K, Sachdev, S, Sadecki, T, Sakellariadou, M, Salconi, L, Saleem, M, Samajdar, A, Sammut, L, Sanchez, E. J, Sanchez, L. E, Sanchis-Gual, N, Sandberg, V and Sanders, J. R., Santiago, K. A, Sarin, N, Sassolas, B, Saulson, P. R, Sauter, O, Savage, R. L, Schale, P, Scheel, M, Scheuer, J, Schmidt, P, Schnabel, R, Schofield, R. M. S, Schoenbeck, A, Schreiber, E, Schulte, B. W, Schutz, B. F, Schwalbe, S. G, Scott, J, Scott, S. M, Seidel, E, Sellers, D, Sengupta, A. S, Sennett, N, Sentenac, D, Sequino, V and Sergeev, Shaddock, D. A, Shaffer, T, Shahriar, M. S, Shaner, M. B, Shao, L, Sharma, P, Shawhan, P, Shen, H, Shink, R, Shoemaker, D. H, Shoemaker, D. M, Shyamsundar, S, Siellez, K, Sieniawska, M, Sigg, D, Silva, A. D, Singer, L. P, Singh, N, Singhal, A, Sintes, A. M, Sitmukhambetov, S, Skliris, V and Slagmolen, B. J. J., Slaven-Blair, T. J, Smith, J. R, Smith, R. J. E, Somala, S, Son, E. J, Sorazu, B, Sorrentino, F, Souradeep, T, Sowell, E, Spencer, A. P, Srivastava, A. K, Srivastava, V and Staats, Stachie, C, Standke, M, Steer, D. A, Steinke, M, Steinlechner, J, Steinlechner, S, Steinmeyer, D, Stevenson, S. P, Stocks, D, Stone, R, Stops, D. J, Strain, K. A, Stratta, G, Strigin, S. E, Strunk, A, Sturani, R, Stuver, A. L, Sudhir, V and Summerscales, T. Z., Sun, L, Sunil, S, Sur, A, Suresh, J, Sutton, P. J, Swinkels, B. L, Szczepanczyk, M. J, Tacca, M, Tait, S. C, Talbot, C, Talukder, D, Tanner, D. B, Tapai, M, Taracchini, A, Tasson, J. D, Taylor, R, Thies, F, Thomas, M, Thomas, P, Thondapu, S. R, Thorne, K. A, Thrane, E, Tiwari, Shubhanshu and Tiwari, Srishti and Tiwari, V and Toland, Tonelli, M, Tornasi, Z, Torres-Forne, A, Torrie, Toyra, D, Travasso, F, Traylor, G, Tringali, M. C, Trovato, A, Trozzo, L, Trudeau, R, Tsang, K. W, Tse, M, Tso, R, Tsukada, L, Tsuna, D, Tuyenbayev, D, Ueno, K, Ugolini, D, Unnikrishnan, C. S, Urban, A. L, Usman, S. A, Vahlbruch, H, Vajente, G, Valdes, G, van Bakel, N, van Beuzekom, M, van den Brand, J. F. J, van den Broeck, C, Vander-Hyde, D. C, Van, Heijningen, van der Schaaf, L, van Veggel, A. A, Vardaro, M, Varma, V, Vass, S, Vasuth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P. J, Venkateswara, K, Venugopalan, G, Verkindt, D, Vetrano, F, Vicere, A, Viets, A. D, Vine, D. J, Vinet, J-Y and Vitale, Vo, T, Vocca, H, Vorvick, C, Vyatchanin, S. P, Wade, A. R, Wade, L. E, Wade, M, Walet, R, Walker, M, Wallace, L, Walsh, S, Wang, G, Wang, H, Wang, J. Z, Wang, W. H, Wang, Y. F, Ward, R. L, Warden, Z. A, Warner, J, Was, M, Watchi, J, Wei, L-W and Weaver, Weinert, M, Weinstein, A. J, Weiss, R, Wellmann, F, Wen, L, Wessel, E. K, Wessels, P, Westhouse, J. W, Wette, K, Whelan, J. T, Whiting, B. F, Whittle, C, Wilken, D. M, Williams, D, Williamson, A. R, Willis, J. L, Willke, B, Wimmer, M. H, Winkler, W, Wipf, C. C, Wittel, H, Woan, G, Woehler, J, Wofford, J. K, Worden, J, Wright, J. L, D. S, Wu, Wysocki, D. M, Xiao, L, Yamamoto, H, Yancey, C. C, Yang, L, Yap, M. J, Yazback, M, Yeeles, D. W, Hang and Yu, Haocun and Yuen, S. H. R., Yvert, M, Zadrozny, A. K, Zendri, J-P and Zanolin, Zelenova, T, Zevin, M, Zhang, J, Zhang, L, Zhang, T, Zhao, C, Zhou, M, Zhou, Z, Zhu, X. J, Zimmerman, A, Zucker, M. E, Zweizig, J, DES Collaboration and LIGO Sci Collaboration and Virgo Collaboration, 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 des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut des Fonctions Optiques pour les Technologies de l'informatiON (Institut FOTON), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS)-Université Bretagne Loire (UBL)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Laboratoire Kastler Brossel (LKB [Collège de France]), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Collège de France (CdF)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon, ESPCI ParisTech, DES, LIGO Scientific, Virgo, Van Swinderen Institute for Particle Physics and G, Soares-Santos, M, Palmese, A, Hartley, W, Annis, J, Garcia-Bellido, J, Lahav, O, Doctor, Z, Fishbach, M, Holz, D, Lin, H, Pereira, M, Garcia, A, Herner, K, Kessler, R, Peiris, H, Sako, M, Allam, S, Brout, D, Rosell, A, Chen, H, Conselice, C, Derose, J, Devicente, J, Diehl, H, Gill, M, Gschwend, J, Sevilla-Noarbe, I, Tucker, D, Wechsler, R, Berger, E, Cowperthwaite, P, Metzger, B, Williams, P, Abbott, T, Abdalla, F, Avila, S, Bechtol, K, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, D, Kind, M, Carretero, J, Castander, F, Crocce, M, Cunha, C, D’Andrea, C, Costa, L, Davis, C, Desai, S, Doel, P, Drlica-Wagner, A, Eifler, T, Evrard, A, Flaugher, B, Fosalba, P, Frieman, J, Gaztanaga, E, Gerdes, D, Gruen, D, Gruendl, R, Gutierrez, G, Hollowood, D, Hoyle, B, James, D, Jeltema, T, Kuehn, K, Kuropatkin, N, Li, T, Lima, M, Maia, M, Marshall, J, Menanteau, F, Miquel, R, Neilsen, E, Ogando, R, Plazas, A, Romer, A, Roodman, A, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Serrano, S, Smith, M, Smith, R, Sobreira, F, Suchyta, E, Swanson, M, Tarle, G, Thomas, R, Walker, A, Wester, W, Zuntz, J, Abbott, B, Abbott, R, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, R, Adya, V, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, M, Altin, P, Amato, A, Ananyeva, A, Anderson, S, Anderson, W, Angelova, S, Appert, S, Arai, K, Araya, M, Areeda, J, Arène, M, Ascenzi, S, Ashton, G, Aston, S, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Avendano, V, Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, M, Bae, S, Baker, P, Baldaccini, F, Ballardin, G, Ballmer, S, Banagiri, S, Barayoga, J, Barclay, S, Barish, B, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, J, Bazzan, M, Bécsy, B, Bejger, M, Bell, A, Beniwal, D, Bergmann, G, Bernuzzi, S, Bero, J, Berry, C, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Bilenko, I, Bilgili, S, Billingsley, G, Birch, J, Birney, R, Birnholtz, O, Biscans, S, Biscoveanu, S, Bisht, A, Bitossi, M, Blackburn, J, Blair, C, Blair, D, Blair, R, Bloemen, S, Bode, N, Boer, M, Boetzel, Y, Bogaert, G, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B, Booth, C, Bork, R, Boschi, V, Bose, S, Bossie, K, Bossilkov, V, Bosveld, J, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P, Bramley, A, Branchesi, M, Brau, J, Briant, T, Briggs, J, Brighenti, F, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A, Brown, D, Brunett, S, Buikema, A, Bulik, T, Bulten, H, Buonanno, A, Buskulic, D, Buy, C, Byer, R, Cabero, M, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, J, Callister, T, Calloni, E, Camp, J, Campbell, W, Cannon, K, Cao, H, Cao, J, Capocasa, E, Carbognani, F, Caride, S, Carney, M, Carullo, G, Diaz, J, Casentini, C, Caudill, S, Cavaglià, M, Cavalieri, R, Cella, G, Cerdá-Durán, P, Cerretani, G, Cesarini, E, Chaibi, O, Chakravarti, K, Chamberlin, S, Chan, M, Chao, S, Charlton, P, Chase, E, Chassande-Mottin, E, Chatterjee, D, Chaturvedi, M, Chatziioannou, K, Cheeseboro, B, Chen, X, Chen, Y, Cheng, H, Cheong, C, Chia, H, Chincarini, A, Chiummo, A, Cho, G, Cho, H, Cho, M, Christensen, N, Chu, Q, Chua, S, Chung, K, Chung, S, Ciani, G, Ciobanu, A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, J, Clearwater, P, Cleva, F, Cocchieri, C, Coccia, E, Cohadon, P, Colgan, R, Colleoni, M, Collette, C, Collins, C, Cominsky, L, Constancio, M, Conti, L, Cooper, S, Corban, P, Corbitt, T, Cordero-Carrión, I, Corley, K, Cornish, N, Corsi, A, Cortese, S, Costa, C, Cotesta, R, Coughlin, M, Coughlin, S, Coulon, J, Countryman, S, Couvares, P, Covas, P, Cowan, E, Coward, D, Cowart, M, Coyne, D, Coyne, R, Creighton, J, Creighton, T, Cripe, J, Croquette, M, Crowder, S, Cullen, T, Cumming, A, Cunningham, L, Cuoco, E, Canton, T, Dálya, G, Danilishin, S, D’Antonio, S, Danzmann, K, Dasgupta, A, Datrier, L, Dattilo, V, Dave, I, Davis, D, Daw, E, Debra, D, Deenadayalan, M, Degallaix, J, Laurentis, M, Deléglise, S, Pozzo, W, Demarchi, L, Demos, N, Dent, T, Pietri, R, Derby, J, Rosa, R, Rossi, C, Desalvo, R, Varona, O, Dhurandhar, S, Díaz, M, Dietrich, T, Fiore, L, Giovanni, M, Girolamo, T, Lieto, A, Ding, B, Pace, S, Palma, I, Renzo, F, Dmitriev, A, Donovan, F, Dooley, K, Doravari, S, Dorrington, I, Downes, T, Drago, M, Driggers, J, Du, Z, Dupej, P, Dwyer, S, Easter, P, Edo, T, Edwards, M, Effler, A, Ehrens, P, Eichholz, J, Eikenberry, S, Eisenmann, M, Eisenstein, R, Estelles, H, Estevez, D, Etienne, Z, Etzel, T, Evans, M, Evans, T, Fafone, V, Fair, H, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, W, Fauchon-Jones, E, Favata, M, Fays, M, Fazio, M, Fee, C, Feicht, J, Fejer, M, Feng, F, Fernandez-Galiana, A, Ferrante, I, Ferreira, E, Ferreira, T, Ferrini, F, Fidecaro, F, Fiori, I, Fiorucci, D, Fisher, R, Fishner, J, Fitz-Axen, M, Flaminio, R, Fletcher, M, Flynn, E, Fong, H, Font, J, Forsyth, P, Fournier, J, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Fritschel, P, Frolov, V, Fulda, P, Fyffe, M, Gabbard, H, Gadre, B, Gaebel, S, Gair, J, Gammaitoni, L, Ganija, M, Gaonkar, S, García-Quirós, C, Garufi, F, Gateley, B, Gaudio, S, Gaur, G, Gayathri, V, Gemme, G, Genin, E, Gennai, A, George, D, George, J, Gergely, L, Germain, V, Ghonge, S, Ghosh, A, Ghosh, S, Giacomazzo, B, Giaime, J, Giardina, K, Giazotto, A, Gill, K, Giordano, G, Glover, L, Godwin, P, Goetz, E, Goetz, R, Goncharov, B, González, G, Castro, J, Gopakumar, A, Gorodetsky, M, Gossan, S, Gosselin, M, Gouaty, R, Grado, A, Graef, C, Granata, M, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, A, Green, R, Gretarsson, E, Groot, P, Grote, H, Grunewald, S, Guidi, G, Gulati, H, Guo, Y, Gupta, A, Gupta, M, Gustafson, E, Gustafson, R, Haegel, L, Halim, O, Hall, B, Hall, E, Hamilton, E, Hammond, G, Haney, M, Hanke, M, Hanks, J, Hanna, C, Hannuksela, O, Hanson, J, Hardwick, T, Haris, K, Harms, J, Harry, G, Harry, I, Haster, C, Haughian, K, Hayes, F, Healy, J, Heidmann, A, Heintze, M, Heitmann, H, Hemming, G, Hendry, M, Heng, I, Hennig, J, Heptonstall, A, Vivanco, F, Heurs, M, Hild, S, Hinderer, T, Hoak, D, Hochheim, S, Hofman, D, Holgado, A, Holland, N, Holt, K, Hopkins, P, Horst, C, Hough, J, Howell, E, Hoy, C, Hreibi, A, Huerta, E, Hughey, B, Hulko, M, Husa, S, Huttner, S, Huynh-Dinh, T, Idzkowski, B, Iess, A, Ingram, C, Inta, R, Intini, G, Irwin, B, Isa, H, Isac, J, Isi, M, Iyer, B, Izumi, K, Jacqmin, T, Jadhav, S, Jani, K, Janthalur, N, Jaranowski, P, Jenkins, A, Jiang, J, Johnson, D, Jones, A, Jones, D, Jones, R, Jonker, R, Ju, L, Junker, J, Kalaghatgi, C, Kalogera, V, Kamai, B, Kandhasamy, S, Kang, G, Kanner, J, Kapadia, S, Karki, S, Karvinen, K, Kashyap, R, Kasprzack, M, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaufer, S, Kawabe, K, Keerthana, N, Kéfélian, F, Keitel, D, Kennedy, R, Key, J, Khalili, F, Khan, H, Khan, I, Khan, S, Khan, Z, Khazanov, E, Khursheed, M, Kijbunchoo, N, Kim, C, Kim, J, Kim, K, Kim, W, Kim, Y, Kimball, C, King, E, King, P, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J, Kleybolte, L, Klika, J, Klimenko, S, Knowles, T, Koch, P, Koehlenbeck, S, Koekoek, G, Koley, S, Kondrashov, V, Kontos, A, Koper, N, Korobko, M, Korth, W, Kowalska, I, Kozak, D, Kringel, V, Krishnendu, N, Królak, A, Kuehn, G, Kumar, A, Kumar, P, Kumar, R, Kumar, S, Kuo, L, Kutynia, A, Kwang, S, Lackey, B, Lai, K, Lam, T, Landry, M, Lane, B, Lang, R, Lange, J, Lantz, B, Lanza, R, Lasky, P, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y, Lee, C, Lee, H, Lee, J, Lee, K, Lehmann, J, Lenon, A, Letendre, N, Levin, Y, Li, J, Li, K, Li, X, Lin, F, Linde, F, Linker, S, Littenberg, T, Liu, J, Liu, X, Lo, R, Lockerbie, N, London, L, Longo, A, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lough, J, Lousto, C, Lovelace, G, Lower, M, Lück, H, Lumaca, D, Lundgren, A, Lynch, R, Ma, Y, Macas, R, Macfoy, S, Macinnis, M, Macleod, D, Macquet, A, Hernandez, I, Magaña-Sandoval, F, Zertuche, L, Magee, R, Majorana, E, Maksimovic, I, Malik, A, Man, N, Mandic, V, Mangano, V, Mansell, G, Manske, M, Mantovani, M, Marchesoni, F, Marion, F, Márka, S, Márka, Z, Markakis, C, Markosyan, A, Markowitz, A, Maros, E, Marquina, A, Marsat, S, Martelli, F, Martin, I, Martin, R, Martynov, D, Mason, K, Massera, E, Masserot, A, Massinger, T, Masso-Reid, M, Mastrogiovanni, S, Matas, A, Matichard, F, Matone, L, Mavalvala, N, Mazumder, N, Mccann, J, Mccarthy, R, Mcclelland, D, Mccormick, S, Mcculler, L, Mcguire, S, Mciver, J, Mcmanus, D, Mcrae, T, Mcwilliams, S, Meacher, D, Meadors, G, Mehmet, M, Mehta, A, Meidam, J, Melatos, A, Mendell, G, Mercer, R, Mereni, L, Merilh, E, Merzougui, M, Meshkov, S, Messenger, C, Messick, C, Metzdorff, R, Meyers, P, Miao, H, Michel, C, Middleton, H, Mikhailov, E, Milano, L, Miller, A, Millhouse, M, Mills, J, Milovich-Goff, M, Minazzoli, O, Minenkov, Y, Mishkin, A, Mishra, C, Mistry, T, Mitra, S, Mitrofanov, V, Mitselmakher, G, Mittleman, R, Mo, G, Moffa, D, Mogushi, K, Mohapatra, S, Montani, M, Moore, C, Moraru, D, Moreno, G, Morisaki, S, Mours, B, Mow-Lowry, C, Mukherjee, A, Mukherjee, D, Mukherjee, S, Mukund, N, Mullavey, A, Munch, J, Muñiz, E, Muratore, M, Murray, P, Nardecchia, I, Naticchioni, L, Nayak, R, Neilson, J, Nelemans, G, Nelson, T, Nery, M, Neunzert, A, Ng, K, Ng, S, Nguyen, P, Nichols, D, Nissanke, S, Nocera, F, North, C, Nuttall, L, Obergaulinger, M, Oberling, J, O’Brien, B, O’Dea, G, Ogin, G, Oh, J, Oh, S, Ohme, F, Ohta, H, Okada, M, Oliver, M, Oppermann, P, Oram, R, O’Reilly, B, Ormiston, R, Ortega, L, O’Shaughnessy, R, Ossokine, S, Ottaway, D, Overmier, H, Owen, B, Pace, A, Pagano, G, Page, M, Pai, A, Pai, S, Palamos, J, Palashov, O, Palomba, C, Pal-Singh, A, Pan, H, Pang, B, Pang, P, Pankow, C, Pannarale, F, Pant, B, Paoletti, F, Paoli, A, Parida, A, Parker, W, Pascucci, D, Pasqualetti, A, Passaquieti, R, Passuello, D, Patil, M, Patricelli, B, Pearlstone, B, Pedersen, C, Pedraza, M, Pedurand, R, Pele, A, Penn, S, Perez, C, Perreca, A, Pfeiffer, H, Phelps, M, Phukon, K, Piccinni, O, Pichot, M, Piergiovanni, F, Pillant, G, Pinard, L, Pirello, M, Pitkin, M, Poggiani, R, Pong, D, Ponrathnam, S, Popolizio, P, Porter, E, Powell, J, Prajapati, A, Prasad, J, Prasai, K, Prasanna, R, Pratten, G, Prestegard, T, Privitera, S, Prodi, G, Prokhorov, L, Puncken, O, Punturo, M, Puppo, P, Pürrer, M, Qi, H, Quetschke, V, Quinonez, P, Quintero, E, Quitzow-James, R, Radkins, H, Radulescu, N, Raffai, P, Raja, S, Rajan, C, Rajbhandari, B, Rakhmanov, M, Ramirez, K, Ramos-Buades, A, Rana, J, Rao, K, Rapagnani, P, Raymond, V, Razzano, M, Read, J, Regimbau, T, Rei, L, Reid, S, Reitze, D, Ren, W, Ricci, F, Richardson, C, Richardson, J, Ricker, P, Riles, K, Rizzo, M, Robertson, N, Robie, R, Rocchi, A, Rolland, L, Rollins, J, Roma, V, Romanelli, M, Romano, R, Romel, C, Romie, J, Rose, K, Rosińska, D, Rosofsky, S, Ross, M, Rowan, S, Rüdiger, A, Ruggi, P, Rutins, G, Ryan, K, Sachdev, S, Sadecki, T, Sakellariadou, M, Salconi, L, Saleem, M, Samajdar, A, Sammut, L, Sanchez, L, Sanchis-Gual, N, Sandberg, V, Sanders, J, Santiago, K, Sarin, N, Sassolas, B, Saulson, P, Sauter, O, Savage, R, Schale, P, Scheel, M, Scheuer, J, Schmidt, P, Schnabel, R, Schofield, R, Schönbeck, A, Schreiber, E, Schulte, B, Schutz, B, Schwalbe, S, Scott, J, Scott, S, Seidel, E, Sellers, D, Sengupta, A, Sennett, N, Sentenac, D, Sequino, V, Sergeev, A, Shaddock, D, Shaffer, T, Shahriar, M, Shaner, M, Shao, L, Sharma, P, Shawhan, P, Shen, H, Shink, R, Shoemaker, D, Shyamsundar, S, Siellez, K, Sieniawska, M, Sigg, D, Silva, A, Singer, L, Singh, N, Singhal, A, Sintes, A, Sitmukhambetov, S, Skliris, V, Slagmolen, B, Slaven-Blair, T, Smith, J, Somala, S, Son, E, Sorazu, B, Sorrentino, F, Souradeep, T, Sowell, E, Spencer, A, Srivastava, A, Srivastava, V, Staats, K, Stachie, C, Standke, M, Steer, D, Steinke, M, Steinlechner, J, Steinlechner, S, Steinmeyer, D, Stevenson, S, Stocks, D, Stone, R, Stops, D, Strain, K, Stratta, G, Strigin, S, Strunk, A, Sturani, R, Stuver, A, Sudhir, V, Summerscales, T, Sun, L, Sunil, S, Sur, A, Suresh, J, Sutton, P, Swinkels, B, Szczepańczyk, M, Tacca, M, Tait, S, Talbot, C, Talukder, D, Tanner, D, Tápai, M, Taracchini, A, Tasson, J, Taylor, R, Thies, F, Thomas, M, Thomas, P, Thondapu, S, Thorne, K, Thrane, E, Tiwari, S, Tiwari, V, Toland, K, Tonelli, M, Tornasi, Z, Torres-Forné, A, Torrie, C, Töyrä, D, Travasso, F, Traylor, G, Tringali, M, Trovato, A, Trozzo, L, Trudeau, R, Tsang, K, Tse, M, Tso, R, Tsukada, L, Tsuna, D, Tuyenbayev, D, Ueno, K, Ugolini, D, Unnikrishnan, C, Urban, A, Usman, S, Vahlbruch, H, Vajente, G, Valdes, G, van Bakel, N, van Beuzekom, M, van den Brand, J, Broeck, C, Vander-Hyde, D, van Heijningen, J, van der Schaaf, L, van Veggel, A, Vardaro, M, Varma, V, Vass, S, Vasúth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P, Venkateswara, K, Venugopalan, G, Verkindt, D, Vetrano, F, Viceré, A, Viets, A, Vine, D, Vinet, J, Vitale, S, Vo, T, Vocca, H, Vorvick, C, Vyatchanin, S, Wade, A, Wade, L, Wade, M, Walet, R, Walker, M, Wallace, L, Walsh, S, Wang, G, Wang, H, Wang, J, Wang, W, Wang, Y, Ward, R, Warden, Z, Warner, J, Was, M, Watchi, J, Weaver, B, Wei, L, Weinert, M, Weinstein, A, Weiss, R, Wellmann, F, Wen, L, Wessel, E, Weßels, P, Westhouse, J, Wette, K, Whelan, J, Whiting, B, Whittle, C, Wilken, D, Williams, D, Williamson, A, Willis, J, Willke, B, Wimmer, M, Winkler, W, Wipf, C, Wittel, H, Woan, G, Woehler, J, Wofford, J, Worden, J, Wright, J, Wu, D, Wysocki, D, Xiao, L, Yamamoto, H, Yancey, C, Yang, L, Yap, M, Yazback, M, Yeeles, D, Yu, H, Yuen, S, Yvert, M, Zadrożny, A, Zanolin, M, Zelenova, T, Zendri, J, Zevin, M, Zhang, J, Zhang, L, Zhang, T, Zhao, C, Zhou, M, Zhou, Z, Zhu, X, Zimmerman, A, Zucker, M, Zweizig, J, IoP (FNWI), Astroparticle Physics (IHEF, IoP, FNWI), (Astro)-Particles Physics, The DES Collaboration, The LIGO Scientific Collaboration, The Virgo Collaboration, Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Annecy de Physique des Particules (LAPP), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF (institution))-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), Holz, De, Pereira, Me, Peiris, Hv, Rosell, Ac, Chen, Hy, Diehl, Ht, Tucker, Dl, Metzger, Bd, Williams, Pkg, Abbott, Tmc, Abdalla, Fb, Burke, Dl, Kind, Mc, Castander, Fj, Cunha, Ce, D'Andrea, Cb, da Costa, Ln, Eifler, Tf, Evrard, Ae, Gerdes, Dw, Gruendl, Ra, Hollowood, Dl, James, Dj, Maia, Mag, Marshall, Jl, Ogando, Rlc, Plazas, Aa, Romer, Ak, Smith, Rc, Swanson, Mec, Thomas, Rc, Walker, Ar, Abbott, Bp, Abbott, Td, Adhikari, Rx, Adya, Vb, Aguiar, Od, Aloy, Ma, Altin, Pa, Anderson, Sb, Anderson, Wg, Angelova, Sv, Araya, Mc, Arene, M, Aston, Sm, Bader, Mkm, Baker, Pt, Ballmer, Sw, Barayoga, Jc, Barclay, Se, Barish, Bc, Bayley, Jc, Becsy, B, Bero, Jj, Berry, Cpl, Bilenko, Ia, Bilgili, Sa, Blackburn, Jk, Blair, Cd, Blair, Dg, Blair, Rm, Boom, Ba, Booth, Cd, Brady, Pr, Brau, Je, Briggs, Jh, Brooks, Af, Brown, Dd, Bulten, Hj, Byer, Rl, Bustillo, Jc, Callister, Ta, Camp, Jb, Campbell, Wa, Cannon, Kc, Carney, Mf, Diaz, Jc, Cavaglia, M, Cerda-Duran, P, Chamberlin, Sj, Chase, Ea, Cheeseboro, Bd, Cheng, Hp, Cheong, Ck, Chia, Hy, Chung, Kw, Ciobanu, Aa, Clark, Ja, Collette, Cg, Cominsky, Lr, Cooper, Sj, Corbitt, Tr, Cordero-Carrion, I, Corley, Kr, Costa, Ca, Coughlin, Mw, Coughlin, Sb, Coulon, Jp, Countryman, St, Covas, Pb, Cowan, Ee, Coward, Dm, Cowart, Mj, Coyne, Dc, Creighton, Jde, Creighton, Td, Crowder, Sg, Cullen, Tj, Dal Canton, T, Dalya, G, D'Antonio, S, Danilishin, Sl, Costa, Cfd, Datrier, Leh, Daw, Ej, De Laurentis, M, Deleglise, S, Del Pozzo, W, Demarchi, Lm, De Pietri, R, De Rosa, R, De Rossi, C, de Varona, O, Diaz, Mc, Di Fiore, L, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Di Pace, S, Di Palma, I, Di Renzo, F, Dooley, Kl, Downes, Tp, Driggers, Jc, Dwyer, Se, Easter, Pj, Edo, Tb, Edwards, Mc, Eisenstein, Ra, Etienne, Zb, Evans, Tm, Farr, Wm, Fauchon-Jones, Ej, Fejer, Mm, Ferreira, Ec, Ferreira, Ta, Fisher, Rp, Fishner, Jm, Fournier, Jd, Font, Ja, Forsyth, Pwf, Frolov, Vv, Gabbard, Ha, Gadre, Bu, Gaebel, Sm, Gair, Jr, Ganija, Mr, Gaonkar, Sg, Garcia-Quiros, C, Giaime, Ja, Giardina, Kd, Gonzalez, G, Castro, Jmg, Gorodetsky, Ml, Gossan, Se, Green, Ac, Gretarsson, Em, Guidi, Gm, Gulati, Hk, Gupta, Mk, Gustafson, Ek, Hall, Br, Hall, Ed, Hamilton, Ez, Hanke, Mm, Hannuksela, Oa, Harry, Gm, Harry, Iw, Haster, Cj, Hayes, Fj, Heintze, Mc, Heptonstall, Aw, Vivanco, Fh, Holgado, Am, Holland, Na, Howell, Ej, Hoy, Cg, Huerta, Ea, Huttner, Sh, Isac, Jm, Isa, Hn, Iyer, Br, Jadhav, Sj, Janthalur, Nn, Jenkins, Ac, Jones, Aw, Jones, Di, Jonker, Rjg, Kalaghatgi, Cv, Kanner, Jb, Kapadia, Sj, Keerthana, Nv, Kefelian, F, Khalili, Fy, Khazanov, Ea, Kim, Jc, Kim, Ym, King, Ej, King, Pj, Klika, Jh, Knowles, Td, Koehlenbeck, Sm, Korth, Wz, Kozak, Db, Krolak, A, Lackey, Bd, Lai, Kh, Lam, Tl, Lane, Bb, Lang, Rn, Lanza, Rk, Lasky, Pd, Lecoeuche, Yk, Lee, Ch, Lee, Hk, Lee, Hm, Lee, Hw, Li, Kjl, Li, Tgf, Linker, Sd, Littenberg, Tb, Lo, Rkl, Lockerbie, Na, London, Lt, Lough, Jd, Lousto, Co, Lower, Me, Luck, H, Lundgren, Ap, Macleod, Dm, Hernandez, Im, Magana-Sandoval, F, Zertuche, Lm, Magee, Rm, Mansell, Gl, Marka, S, Marka, Z, Martin, Iw, Martin, Rm, Martynov, Dv, Massinger, Tj, Mccann, Jj, Mcclelland, De, Mcguire, Sc, Mcmanus, Dj, Mcwilliams, St, Meadors, Gd, Mehta, Ak, Mercer, Ra, Merilh, El, Meyers, Pm, Mikhailov, Ee, Miller, Al, Mills, Jc, Milovich-Goff, Mc, Mitrofanov, Vp, Mohapatra, Srp, Moore, Cj, Mow-Lowry, Cm, Muniz, Ea, Murray, Pg, Nayak, Rk, Nelson, Tjn, Ng, Ky, Nuttall, Lk, O'Brien, Bd, O'Dea, Gd, Ogin, Gh, Oh, Jj, Oh, Sh, Okada, Ma, O'Reilly, B, O'Shaughnessy, R, Oram, Rj, Ormiston, Rg, Ortega, Lf, Ottaway, Dj, Owen, Bj, Pace, Ae, Page, Ma, Pai, Sa, Palamos, Jr, Pan, Hw, Pang, Pth, Pant, Bc, Pearlstone, Bl, Perez, Cj, Pfeiffer, Hp, Piccinni, Oj, Pong, Dyt, Porter, Ek, Prajapati, Ak, Prodi, Ga, Prokhorov, Lg, Purrer, M, Quinonez, Pj, Quintero, Ea, Ramirez, Ke, Reitze, Dh, Richardson, Cj, Richardson, Jw, Ricker, Pm, Robertson, Na, Rollins, Jg, Roma, Vj, Romel, Cl, Romie, Jh, Rosinska, D, Rosofsky, Sg, Ross, Mp, Rudiger, A, Sanchez, Ej, Sanchez, Le, Sanders, Jr, Santiago, Ka, Saulson, Pr, Savage, Rl, Schofield, Rm, Schonbeck, A, Schulte, Bw, Schutz, Bf, Schwalbe, Sg, Scott, Sm, Shaddock, Da, Shaner, Mb, Shoemaker, Dh, Shoemaker, Dm, Silva, Ad, Singer, Lp, Sintes, Am, Slagmolen, Bjj, Slaven-Blair, Tj, Smith, Jr, Smith, Rje, Son, Ej, Spencer, Ap, Srivastava, Ak, Steer, Da, Stevenson, Sp, Stops, Dj, Strain, Ka, Strigin, Se, Stuver, Al, Summerscales, Tz, Sutton, Pj, Swinkels, Bl, Szczepanczyk, Mj, Tait, Sc, Tanner, Db, Tapai, M, Tasson, Jd, Thondapu, Sr, Thorne, Ka, Torres-Forne, A, Torrie, Ci, Toyra, D, Tringali, Mc, Tsang, Kw, Urban, Al, Usman, Sa, van den Brand, Jfj, van den Broeck, C, Vander-Hyde, Dc, van Heijningen, Jv, van Veggel, Aa, Vasuth, M, Veitch, Pj, Vicere, A, Viets, Ad, Vine, Dj, Vinet, Jy, Vyatchanin, Sp, Wade, Ar, Wade, Le, Wang, Jz, Wang, Wh, Wang, Yf, Ward, Rl, Warden, Za, Wei, Lw, Weinstein, Aj, Wessel, Ek, Wessels, P, Westhouse, Jw, Whelan, Jt, Whiting, Bf, Wilken, Dm, Williamson, Ar, Willis, Jl, Wimmer, Mh, Wipf, Cc, Wofford, Jk, Wright, Jl, Wysocki, Dm, Yancey, Cc, Yap, Mj, Yeeles, Dw, Yu, Hc, Yuen, Shr, Zadrozny, Ak, Zendri, Jp, Zhu, Xj, Zucker, Me, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), ITA, USA, GBR, FRA, DEU, ESP, RS: FSE Grav. waves and fundamental physics, Grav. waves and fundamental physics, RS: FSE MSP, Soares-Santos, M., Palmese, A., Hartley, W., Annis, J., Garcia-Bellido, J., Lahav, O., Doctor, Z., Fishbach, M., Holz, D. E., Lin, H., Pereira, M. E. S., Garcia, A., Herner, K., Kessler, R., Peiris, H. V., Sako, M., Allam, S., Brout, D., Rosell, A. Carnero, Chen, H. Y., Conselice, C., Derose, J., Devicente, J., Diehl, H. T., Gill, M. S. S., Gschwend, J., Sevilla-Noarbe, I., Tucker, D. L., Wechsler, R., Berger, E., Cowperthwaite, P. S., Metzger, B. D., Williams, P. K. G., Abbott, T. M. C., Abdalla, F. B., Avila, S., Bechtol, K., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D’Andrea, C. B., Costa, L. N. da, Davis, C., Desai, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hollowood, D. L., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Li, T. S., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Neilsen, E., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, R. C., Walker, A. R., Wester, W., Zuntz, J., Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arène, M., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., Aultoneal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Bejger, M., Bell, A. S., Beniwal, D., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Briggs, J. H., Brighenti, F., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brown, D. D., Brunett, S., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderón, Callister, T. A., Calloni, E., Camp, J. B., Campbell, W. A., Cannon, K. C., Cao, H., Cao, J., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglià, M., Cavalieri, R., Cella, G., Cerdá-Durán, P., Cerretani, G., Cesarini, E., Chaibi, O., Chakravarti, K., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Chatziioannou, K., Cheeseboro, B. D., Chen, X., Chen, Y., Cheng, H. -P., Cheong, C. K., Chia, H. Y., Chincarini, A., Chiummo, A., Cho, G., Cho, H. S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Chung, S., Ciani, G., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. -F., Colgan, R., Colleoni, M., Collette, C. G., Collins, C., Cominsky, L. R., Constancio, M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Croquette, M., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Dálya, G., Danilishin, S. L., D’Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. Da Silva, Datrier, L. E. H., Dattilo, V., Dave, I., Davis, D., Daw, E. J., Debra, D., Deenadayalan, M., Degallaix, J., Laurentis, M. De, Deléglise, S., Pozzo, W. Del, Demarchi, L. M., Demos, N., Dent, T., Pietri, R. De, Derby, J., De Rosa, Rosario, Rossi, C. De, Desalvo, R., Varona, O. de, Dhurandhar, S., Díaz, M. C., Dietrich, T., Fiore, L. Di, Giovanni, M. Di, Di Girolamo, T., Lieto, A. Di, Ding, B., Pace, S. Di, Palma, I. Di, Renzo, F. Di, Dmitriev, A., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Dupej, P., Dwyer, S. E., Easter, P. J., Edo, T. B., Edwards, M. C., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Fee, C., Feicht, J., Fejer, M. M., Feng, F., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. A., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Fishner, J. M., Fitz-Axen, M., Flaminio, R., Fletcher, M., Flynn, E., Fong, H., Font, J. A., Forsyth, P. W. F., Fournier, J. -D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Ganija, M. R., Gaonkar, S. G., García-Quirós, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giacomazzo, B., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Giordano, G., Glover, L., Godwin, P., Goetz, E., Goetz, R., Goncharov, B., González, G., Castro, J. M. Gonzalez, Gopakumar, A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Granata, M., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, E. M., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Gulati, H. K., Guo, Y., Gupta, A., Gupta, M. K., Gustafson, E. K., Gustafson, R., Haegel, L., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannuksela, O. A., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Haster, C. -J., Haughian, K., Hayes, F. J., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Vivanco, Francisco Hernandez, Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hochheim, S., Hofman, D., Holgado, A. M., Holland, N. A., Holt, K., Hopkins, P., Horst, C., Hough, J., Howell, E. J., Hoy, C. G., Hreibi, A., Huerta, E. A., Hughey, B., Hulko, M., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idzkowski, B., Iess, A., Ingram, C., Inta, R., Intini, G., Irwin, B., Isa, H. N., Isac, J. -M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jadhav, S. J., Jani, K., Janthalur, N. N., Jaranowski, P., Jenkins, A. C., Jiang, J., Johnson, D. S., Jones, A. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kashyap, R., Kasprzack, M., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Keerthana, N. V., Kéfélian, F., Keitel, D., Kennedy, R., Key, J. S., Khalili, F. Y., Khan, H., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Khursheed, M., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. -M., Kimball, C., King, E. J., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klika, J. H., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koekoek, G., Koley, S., Kondrashov, V., Kontos, A., Koper, N., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Krishnendu, N., Królak, A., Kuehn, G., Kumar, A., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Lai, K. H., Lam, T. L., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lehmann, J., Lenon, A., Letendre, N., Levin, Y., Li, J., Li, K. J. L., Li, T. G. F., Li, X., Lin, F., Linde, F., Linker, S. D., Littenberg, T. B., Liu, J., Liu, X., Lo, R. K. L., Lockerbie, N. A., London, L. T., Longo, A., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lower, M. E., Lück, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., Macinnis, M., Macleod, D. M., Macquet, A., Hernandez, I. Magaña, Magaña-Sandoval, F., Zertuche, L. Magaña, Magee, R. M., Majorana, E., Maksimovic, I., Malik, A., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martynov, D. V., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mccann, J. J., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcculler, L., Mcguire, S. C., Mciver, J., Mcmanus, D. J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Mehta, A. K., Meidam, J., Melatos, A., Mendell, G., Mercer, R. A., Mereni, L., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, A., Millhouse, M., Mills, J. C., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Mishkin, A., Mishra, C., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Mo, G., Moffa, D., Mogushi, K., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morisaki, S., Mours, B., Mow-Lowry, C. M., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Muratore, M., Murray, P. G., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Ng, K. Y., Ng, S., Nguyen, P., Nichols, D., Nissanke, S., Nocera, F., North, C., Nuttall, L. K., Obergaulinger, M., Oberling, J., O’Brien, B. D., O’Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Ohta, H., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard J., O’Reilly, B., Ormiston, R. G., Ortega, L. F., O’Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Pagano, G., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, Huang-Wei, Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. L., Pedersen, C., Pedraza, M., Pedurand, R., Pele, A., Penn, S., Perez, C. J., Perreca, A., Pfeiffer, H. P., Phelps, M., Phukon, K. S., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pillant, G., Pinard, L., Pirello, M., Pitkin, M., Poggiani, R., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Powell, J., Prajapati, A. K., Prasad, J., Prasai, K., Prasanna, R., Pratten, G., Prestegard, T., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quinonez, P. J., Quintero, E. A., Quitzow-James, R., Radkins, H., Radulescu, N., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rana, Javed, Rao, K., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Ren, W., Ricci, F., Richardson, C. J., Richardson, J. W., Ricker, P. M., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romanelli, M., Romano, R., Romel, C. L., Romie, J. H., Rose, K., Rosińska, D., Rosofsky, S. G., Ross, M. P., Rowan, S., Rüdiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sakellariadou, M., Salconi, L., Saleem, M., Samajdar, A., Sammut, L., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sandberg, V., Sanders, J. R., Santiago, K. A., Sarin, N., Sassolas, B., Saulson, P. R., Sauter, O., Savage, R. L., Schale, P., Scheel, M., Scheuer, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schulte, B. W., Schutz, B. F., Schwalbe, S. G., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sennett, N., Sentenac, D., Sequino, V., Sergeev, A., Shaddock, D. A., Shaffer, T., Shahriar, M. S., Shaner, M. B., Shao, L., Sharma, P., Shawhan, P., Shen, H., Shink, R., Shoemaker, D. H., Shoemaker, D. M., Shyamsundar, S., Siellez, K., Sieniawska, M., Sigg, D., Silva, A. D., Singer, L. P., Singh, N., Singhal, A., Sintes, A. M., Sitmukhambetov, S., Skliris, V., Slagmolen, B. J. J., Slaven-Blair, T. J., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Sowell, E., Spencer, A. P., Srivastava, A. K., Srivastava, V., Staats, K., Stachie, C., Standke, M., Steer, D. A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S. P., Stocks, D., Stone, R., Stops, D. J., Strain, K. A., Stratta, G., Strigin, S. E., Strunk, A., Sturani, R., Stuver, A. L., Sudhir, V., Summerscales, T. Z., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Talukder, D., Tanner, D. B., Tápai, M., Taracchini, A., Tasson, J. D., Taylor, R., Thies, F., Thomas, M., Thomas, P., Thondapu, S. R., Thorne, K. A., Thrane, E., Tiwari, Shubhanshu, Tiwari, Srishti, Tiwari, V., Toland, K., Tonelli, M., Tornasi, Z., Torres-Forné, A., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Tringali, M. C., Trovato, A., Trozzo, L., Trudeau, R., Tsang, K. W., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tuyenbayev, D., Ueno, K., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., van Bakel, N., van Beuzekom, M., van den Brand, J. F. J., Broeck, C. Van Den, Vander-Hyde, D. C., van Heijningen, J. V., van der Schaaf, L., van Veggel, A. A., Vardaro, M., Varma, V., Vass, S., Vasúth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., Viceré, A., Viets, A. D., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, J. Z., Wang, W. H., Wang, Y. F., Ward, R. L., Warden, Z. A., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Wellmann, F., Wen, L., Wessel, E. K., Weßels, P., Westhouse, J. W., Wette, K., Whelan, J. T., Whiting, B. F., Whittle, C., Wilken, D. M., Williams, D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Wofford, J. K., Worden, J., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, L., Yamamoto, H., Yancey, C. C., Yang, L., Yap, M. J., Yazback, M., Yeeles, D. W., Yu, Hang, Yu, Haocun, Yuen, S. H. R., Yvert, M., Zadrożny, A. K., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, T., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zimmerman, A., Zucker, M. E., Zweizig, J., Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution))
Subjects: 010504 meteorology & atmospheric sciences, Astronomy, Astrophysics, cosmic background radiation, 01 natural sciences, black hole, LIGO, dark energy, 010303 astronomy & astrophysics, gravitational wave, QC, Photometric redshift, QB, Physics, Settore FIS/01, Hubble constant, CATALOG, observations [cosmology], gravitational waves, Physical Sciences, symbols, astro-ph.CO, STELLAR MASS, Astrophysics - Cosmology and Nongalactic Astrophysics, observation [cosmology], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, AST-1138766, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, gravitational radiation: direct detection, electromagnetic field: production, symbols.namesake, SDG 17 - Partnerships for the Goals, Binary black hole, statistical analysis, surveys, 0103 physical sciences, supernova, AST-1536171, Luminosity distance, STFC, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, ONDAS GRAVITACIONAIS, Science & Technology, catalogs, cosmology: observations, gravitational radiation, RCUK, Astronomy and Astrophysics, redshift, Galaxy, Redshift, gravitational radiation detector, VIRGO, Physics and Astronomy, black hole: binary, RESOLUTION, Space and Planetary Science, gravitational radiation: emission, Dark energy, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law
Abstract: We present a multi-messenger measurement of the Hubble constant H_0 using the binary-black-hole merger GW170814 as a standard siren, combined with a photometric redshift catalog from the Dark Energy Survey (DES). The luminosity distance is obtained from the gravitational wave signal detected by the LIGO/Virgo Collaboration (LVC) on 2017 August 14, and the redshift information is provided by the DES Year 3 data. Black-hole mergers such as GW170814 are expected to lack bright electromagnetic emission to uniquely identify their host galaxies and build an object-by-object Hubble diagram. However, they are suitable for a statistical measurement, provided that a galaxy catalog of adequate depth and redshift completion is available. Here we present the first Hubble parameter measurement using a black-hole merger. Our analysis results in $H_0 = 75.2^{+39.5}_{-32.4}~{\rm km~s^{-1}~Mpc^{-1}}$, which is consistent with both SN Ia and CMB measurements of the Hubble constant. The quoted 68% credible region comprises 60% of the uniform prior range [20,140] ${\rm km~s^{-1}~Mpc^{-1}}$, and it depends on the assumed prior range. If we take a broader prior of [10,220] ${\rm km~s^{-1}~Mpc^{-1}}$, we find $H_0 = 78^{+ 96}_{-24}~{\rm km~s^{-1}~Mpc^{-1}}$ ($57\%$ of the prior range). Although a weak constraint on the Hubble constant from a single event is expected using the dark siren method, a multifold increase in the LVC event rate is anticipated in the coming years and combinations of many sirens will lead to improved constraints on $H_0$., Comment: 18 pages, 2 Figures, submitted to ApJL
Published: 2019

46. Milky Way Satellite Census. III. Constraints on Dark Matter Properties from Observations of Milky Way Satellite Galaxies

Author: Nadler, E. O., Drlica-Wagner, A., Bechtol, K., Mau, S., Wechsler, R. H., Gluscevic, V., Boddy, K., Pace, A. B., Li, T. S., McNanna, M., Riley, A. H., Garc��a-Bellido, J., Mao, Y. -Y., Green, G., Burke, D. L., Peter, A., Jain, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Brooks, D., Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Honscheid, K., Huterer, D., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinch��n, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Walker, A. R., and Wester, W.
Subjects: High Energy Physics - Phenomenology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Phenomenology (hep-ph), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a comprehensive study of Milky Way (MW) satellite galaxies to constrain the fundamental properties of dark matter (DM). This analysis fully incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and marginalizes over uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk. Our results are consistent with the cold, collisionless DM paradigm and yield the strongest cosmological constraints to date on particle models of warm, interacting, and fuzzy dark matter. At $95\%$ confidence, we report limits on (i) the mass of thermal relic warm DM, $m_{\rm WDM} > 6.5\ \mathrm{keV}$ (free-streaming length, $\lambda_{\rm{fs}} \lesssim 10\,h^{-1}\ \mathrm{kpc}$), (ii) the velocity-independent DM-proton scattering cross section, $\sigma_{0} < 8.8\times 10^{-29}\ \mathrm{cm}^{2}$ for a $100\ \mathrm{MeV}$ DM particle mass (DM-proton coupling, $c_p \lesssim (0.3\ \mathrm{GeV})^{-2}$), and (iii) the mass of fuzzy DM, $m_{\phi}> 2.9 \times 10^{-21}\ \mathrm{eV}$ (de Broglie wavelength, $\lambda_{\rm{dB}} \lesssim 0.5\ \mathrm{kpc}$). These constraints are complementary to other observational and laboratory constraints on DM properties., Comment: 15 pages, 5 figures, 2 tables. Updated to published version
Published: 2020

47. Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z similar to 1

Author: Gupta, N., Pannella, M., Mohr, J. J., Klein, M., Rykoff, E. S., Annis, J., Avila, S., Bianchini, F., Brooks, D., Buckley-Geer, E., Bulbul, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chiu, L, Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Evrard, A. E., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., McDonald, M., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Reichardt, C. L., Sanchez, E., Santiago, B., Saro, A., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Shao, X., Smith, M., Stott, J. P., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Vikram, V., and Zenteno, A.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We study the properties of the Sydney University Molonglo Sky Survey (SUMSS) 843 MHz radio active galactic nuclei (AGNs) population in galaxy clusters from two large catalogues created using the Dark Energy Survey (DES): similar to 11 800 optically selected RM-Y3 and similar to 1000 X-ray selected MARD-Y3 clusters. We show that cluster radio loud AGNs are highly concentrated around cluster centres to z similar to 1. We measure the halo occupation number for cluster radio AGNs above a threshold luminosity, finding that the number of radio AGNs per cluster increases with cluster halo mass as N proportional to M-1(.2 +/- 0.1) (N proportional to M-0.(68 +/- 0.34)) for the RM-Y3 (MARD-Y3) sample. Together, these results indicate that radio mode feedback is favoured in more massive galaxy clusters. Using optical counterparts for these sources, we demonstrate weak redshift evolution in the host broad-band colours and the radio luminosity at fixed host galaxy stellar mass. We use the redshift evolution in radio luminosity to break the degeneracy between density and luminosity evolution scenarios in the redshift trend of the radio AGNs luminosity function (LF). The LF exhibits a redshift trend of the form (1 + z)(gamma) in density and luminosity, respectively, of gamma(D) = 3.0 +/- 0.4 and gamma(P) = 0.21 +/- 0.15 in the RM-Y3 sample, and gamma(D) = 2.6 +/- 0.7 and gamma(P) = 0.31 +/- 0.15 in MARD-Y3. We discuss the physical drivers of radio mode feedback in cluster AGNs, and we use the cluster radio galaxy LF to estimate the average radio-mode feedback energy as a function of cluster mass and redshift and compare it to the core (
Published: 2020

48. A chemo-dynamical link between the Gj��ll stream and NGC 3201

Author: Hansen, T. T., Riley, A. H., Strigari, L. E., Marshall, J. L., Ferguson, P. S., Zepeda, J., and Sneden, C.
Subjects: Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Recent analysis of the second data release of Gaia has revealed a number of new stellar streams surrounding the Milky Way. It has been suggested that one of these streams, Gj��ll, is associated with the globular cluster NGC 3201, but thus far the association has only been based on kinematics of the stream stars. In this work we identify five likely stream members in the Gaia data that are bright enough for high-resolution spectroscopic follow-up with the Harlan J. Smith telescope at McDonald Observatory. One star is ruled out as a member based on its radial velocity. Abundance analysis of the remaining four kinematic members reveals a good chemical match to NGC 3201 for two of the stars, driven by their similar Al and $��$-element abundances. Of the remaining two, one shows no chemical similarity to NGC 3201 and is likely an unassociated Milky Way halo field star, while the other exhibits a similar Al abundance but has somewhat lower $��$-element abundances. The chemical tagging of stars in the Gj��ll stream to NGC 3201 confirms this association and provides direct proof of the hierarchical formation of the Milky Way., 12 pages, 10 Tables and 4 Figures, Accepted for publication in ApJ
Published: 2020
Full Text: View/download PDF

49. $��_{\star}$ Masses: Weak Lensing Calibration of the Dark Energy Survey Year 1 redMaPPer Clusters using Stellar Masses

Author: Pereira, M. E. S., Palmese, A., Varga, T. N., McClintock, T., Soares-Santos, M., Burgad, J., Annis, J., Farahi, A., Lin, H., Choi, A., DeRose, J., Esteves, J., Gatti, M., Gruen, D., Hartley, W. G., Hoyle, B., Jeltema, T., MacCrann, N., Roodman, A., S��nchez, C., Shin, T., von der Linden, A., Zuntz, J., Abbott, T. M. C., Aguena, M., Avila, S., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Estrada, J., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinch��n, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Wechsler, R. H., Weller, J., and Zhang, Y.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present the weak lensing mass calibration of the stellar mass based $��_{\star}$ mass proxy for redMaPPer galaxy clusters in the Dark Energy Survey Year 1. For the first time we are able to perform a calibration of $��_{\star}$ at high redshifts, $z>0.33$. In a blinded analysis, we use $\sim 6,000$ clusters split into 12 subsets spanning the ranges $0.1 \leqslant z, 20 pages, 10 figures, submitted to MNRAS
Published: 2020
Full Text: View/download PDF

50. The Host Galaxies of Rapidly Evolving Transients in the Dark Energy Survey

Author: Wiseman, P., Pursiainen, M., Childress, M., Swann, E., Smith, M., Galbany, L., Lidman, C., Davis, T. M., Gutiérrez, C. P., Möller, A., Thomas, B. P., Frohmaier, C., Foley, R. J., Hinton, S. R., Kelsey, L., Kessler, R., Lewis, G. F., Sako, M., Scolnic, D., Sullivan, M., Vincenzi, M., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., Diehl, H. T., Doel, P., Everett, S., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sommer, N. E., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, B. E., Tucker, D. L., Varga, T. N., Walker, A. R., Wiseman, P, Pursiainen, M, Childress, M, Swann, E, Smith, M, Galbany, L, Lidman, C, M Davis, T, P Gutiérrez, C, Möller, A, P Thomas, B, Frohmaier, C, J Foley, R, R Hinton, S, Kelsey, L, Kessler, R, F Lewis, G, Sako, M, Scolnic, D, Sullivan, M, Vincenzi, M, T M, C Abbott, Aguena, M, Allam, S, Annis, J, Bertin, E, Bhargava, S, Brooks, D, L Burke, D, A Carnero Rosell, Carollo, D, M Carrasco Kind, Carretero, J, Costanzi, M, N da Costa, L, T Diehl, H, Doel, P, Everett, S, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Glazebrook, K, Gruen, D, A Gruendl, R, Gschwend, J, Gutierrez, G, L Hollowood, D, Honscheid, K, J James, D, Kuehn, K, Kuropatkin, N, Lima, M, M A, G Maia, L Marshall, J, Martini, P, Menanteau, F, Miquel, R, Palmese, A, Paz-Chinchón, F, A Plazas, A, K Romer, A, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, E Sommer, N, Suchyta, E, M E, C Swanson, Tarle, G, E Tucker, B, L Tucker, D, N Varga, T, and R Walker, A
Subjects: abundances – galaxies: photometry – galaxies: star formation – transients: supernovae [galaxies], endocrine system, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), galaxies: abundances – galaxies: photometry – galaxies: star formation – transients: supernovae, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: Rapidly evolving transients (RETs), also termed fast blue optical transients (FBOTs), are a distinct class of astrophysical event. They are characterised by lightcurves that decline much faster than common classes supernovae (SNe), span vast ranges in peak luminosity and can be seen to redshifts greater than 1. Their evolution on fast timescales has hindered high quality follow-up observations, and thus their origin and explosion/emission mechanism remains unexplained. In this paper we define the largest sample of RETs to date, comprising 106 objects from the Dark Energy Survey, and perform the most comprehensive analysis of RET host galaxies. Using deep-stacked photometry and emission-lines from OzDES spectroscopy, we derive stellar masses and star-formation rates (SFRs) for 49 host galaxies, and metallicities for 37. We find that RETs explode exclusively in star-forming galaxies and are thus likely associated with massive stars. Comparing RET hosts to samples of host galaxies of other explosive transients as well as field galaxies, we find that RETs prefer galaxies with high specific SFRs, indicating a link to young stellar populations, similar to stripped-envelope SNe. RET hosts appear to show a lack of chemical enrichment, their metallicities akin to long duration gamma-ray bursts and superluminous SN host galaxies. There are no clear relationships between properties of the host galaxies and the peak magnitudes or decline rates of the transients themselves., Comment: 16 pages, 15 figures, submitted to MNRAS
Published: 2020

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Language

Journal

Database

Publisher

190 results on '"MARSHALL, J. L."'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources