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1. 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

2. 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

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

Author: Chen, Angela, Huterer, Dragan, Lee, Sujeong, Ferté, Agnès, Weaverdyck, Noah, Alves, Otavio Alonso, Leonard, C. Danielle, MacCrann, Niall, Raveri, Marco, Porredon, Anna, Di Valentino, Eleonora, Muir, Jessica, Lemos, Pablo, Liddle, Andrew, Blazek, Jonathan, Campos, Andresa, Cawthon, Ross, Choi, Ami, Dodelson, Scott, Elvin-Poole, Jack, Gruen, Daniel, Ross, Ashley, Secco, Lucas F., Sevilla, Ignacio, Sheldon, Erin, Troxel, Michael A., Zuntz, Joe, Abbott, Tim, Aguena, Michel, Allam, Sahar, Annis, James, Avila, Santiago, Bertin, Emmanuel, Bhargava, Sunayana, Bridle, Sarah, Brooks, David, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, Costanzi, Matteo, Crocce, Martin, da Costa, Luiz, Pereira, Maria Elidaiana da Silva, Davis, Tamara, Doel, Peter, Eifler, Tim, Ferrero, Ismael, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Gerdes, David, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hinton, Samuel, Hollowood, Devon L., Honscheid, Klaus, Hoyle, Ben, James, David, Jarvis, Mike, Kuehn, Kyler, Lahav, Ofer, Maia, Marcio, Marshall, Jennifer, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Palmese, Antonella, Paz-Chinchon, Francisco, Malagón, Andrés Plazas, Roodman, Aaron, Sanchez, Eusebio, Scarpine, Vic, Schubnell, Michael, Serrano, Santiago, Smith, Mathew, Suchyta, Eric, Tarle, Gregory, Thomas, Daniel, To, Chun-Hao, Varga, Tamas Norbert, Weller, Jochen, Wilkinson, Reese, UAM. Departamento de Física Teórica, National Science Foundation (US), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, University of Michigan, Duke University, California Institute of Technology, Universidade Estadual Paulista (UNESP), Newcastle Unviersity, Ohio State University, University of Chicago, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), University of Manchester, Stanford University, University College London, Universidade de Lisboa, University of Edinburgh, Perimeter Institute for Theoretical Physics, Observatoire de Sauverny, Carnegie Mellon University, University of Wisconsin-Madison, 382 Via Pueblo Mall, Menlo Park, University of Pennsylvania, Medioambientales y Tecnológicas (CIEMAT), Brookhaven National Laboratory, NSF's National Optical-Infrared Astronomy Research Laboratory, Universidade de São Paulo (USP), LIneA, Fermi National Accelerator Laboratory, Universidad Autonoma de Madrid, Institut d'Astrophysique de Paris, University of Sussex, Instituto de Astrofisica de Canarias, Dpto. Astrofísica, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, Barcelona Institute of Science and Technology, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Queensland, University of Arizona, University of Oslo, Santa Cruz Institute for Particle Physics, Ludwig-Maximilians-Universität, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universität München, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Texas AandM University, Institució Catalana de Recerca i Estudis Avançats, University of Cambridge, Peyton Hall, University of Southampton, Oak Ridge National Laboratory, University of Portsmouth, Chen, Angela, Huterer, Dragan, Lee, Sujeong, Ferté, Agnè, Weaverdyck, Noah, Alonso Alves, Otavio, Leonard, C. Danielle, Maccrann, Niall, Raveri, Marco, Porredon, Anna, Di Valentino, Eleonora, Muir, Jessica, Lemos, Pablo, Liddle, Andrew, Blazek, Jonathan, Campos, Andresa, Cawthon, Ro, Choi, Ami, Dodelson, Scott, Elvin-Poole, Jack, Gruen, Daniel, Ross, Ashley, Secco, Lucas F., Sevilla, Ignacio, Sheldon, Erin, Troxel, Michael A., Zuntz, Joe, Abbott, Tim, Aguena, Michel, Allam, Sahar, Annis, Jame, Avila, Santiago, Bertin, Emmanuel, Bhargava, Sunayana, Bridle, Sarah, Brooks, David, Carnero Rosell, Aurelio, Carrasco Kind, Matia, Carretero, Jorge, Costanzi, Matteo, Crocce, Martin, da Costa, Luiz, Elidaiana da Silva Pereira, Maria, Davis, Tamara, Doel, Peter, Eifler, Tim, Ferrero, Ismael, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Gerdes, David, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hinton, Samuel, Hollowood, Devon L., Honscheid, Klau, Hoyle, Ben, James, David, Jarvis, Mike, Kuehn, Kyler, Lahav, Ofer, Maia, Marcio, Marshall, Jennifer, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Palmese, Antonella, Paz-Chinchon, Francisco, Plazas Malagón, André, Roodman, Aaron, Sanchez, Eusebio, Scarpine, Vic, Schubnell, Michael, Serrano, Santiago, Smith, Mathew, Suchyta, Eric, Tarle, Gregory, Thomas, Daniel, Chun-Hao, To, Varga, Tamas Norbert, Weller, Jochen, and Wilkinson, Reese
Subjects: matter: power spectrum, Cosmic microwave background, cosmic background radiation: polarization, Astrophysics, power spectrum, 01 natural sciences, Cosmology, hubble constant, High Energy Physics - Phenomenology (hep-ph), Scale Structure, cosmological model: parameter space, Power Spectrum, Dark energy, Astrophysics - Cosmology and Nongalactic Astrophysic, Large-scale structure of the Universe, 010303 astronomy & astrophysics, media_common, Physics, Energy, massive neutrinos, Hubble Constant, tension, Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology, halo-model, statistics, dark energy: density, Dark radiation, symbols, Halo-Model, energy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Dark matter, Cosmological parameters, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter: density, galaxy formation, Evolution of the Universe, symbols.namesake, scale structure, 0103 physical sciences, supernova, Galaxy formation and evolution, Self-Interactions, Massive Neutrinos, STFC, Sdss, 010308 nuclear & particles physics, RCUK, resolution, Física, self-interactions, inconsistent, Universe, cosmic background radiation: temperature, 13. Climate action, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Galaxy Formation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], sdss, Hubble's law
Abstract: Chen, A., et al. DES Collaboration, We study a phenomenological class of models where dark matter converts to dark radiation in the low redshift epoch. This class of models, dubbed DMDR, characterizes the evolution of comoving dark-matter density with two extra parameters, and may be able to help alleviate the observed discrepancies between early and late-time probes of the Universe. We investigate how the conversion affects key cosmological observables such as the cosmic microwave background (CMB) temperature and matter power spectra. Combining 3x2pt data from Year 1 of the Dark Energy Survey, Planck-2018 CMB temperature and polarization data, supernovae (SN) Type Ia data from Pantheon, and baryon acoustic oscillation (BAO) data from BOSS DR12, MGS and 6dFGS, we place new constraints on the amount of dark matter that has converted to dark radiation and the rate of this conversion. The fraction of the dark matter that has converted since the beginning of the Universe in units of the current amount of dark matter, ζ, is constrained at 68% confidence level to be, he DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (Grant No. FP7/2007-2013) including ERC Grants Agreement No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2).
Published: 2021
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4. 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
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5. Lensing Without Borders. I. A Blind Comparison of the Amplitude of Galaxy-Galaxy Lensing Between Independent Imaging Surveys

Author: A Leauthaud, A Amon, S Singh, D Gruen, J U Lange, S Huang, N C Robertson, T N Varga, Y Luo, C Heymans, H Hildebrandt, C Blake, M Aguena, S Allam, F Andrade-Oliveira, J Annis, E Bertin, S Bhargava, J Blazek, S L Bridle, D Brooks, D L Burke, A Carnero Rosell, M Carrasco Kind, J Carretero, F J Castander, R Cawthon, A Choi, M Costanzi, L N da Costa, M E S Pereira, C Davis, J De Vicente, J DeRose, H T Diehl, J P Dietrich, P Doel, K Eckert, S Everett, A E Evrard, I Ferrero, B Flaugher, P Fosalba, J García-Bellido, M Gatti, E Gaztanaga, R A Gruendl, J Gschwend, W G Hartley, D L Hollowood, K Honscheid, B Jain, D J James, M Jarvis, B Joachimi, A Kannawadi, A G Kim, E Krause, K Kuehn, K Kuijken, N Kuropatkin, M Lima, N MacCrann, M A G Maia, M Makler, M March, J L Marshall, P Melchior, F Menanteau, R Miquel, H Miyatake, J J Mohr, B Moraes, S More, M Surhud, R Morgan, J Myles, R L C Ogando, A Palmese, F Paz-Chinchón, A A Plazas Malagón, J Prat, M M Rau, J Rhodes, M Rodriguez-Monroy, A Roodman, A J Ross, S Samuroff, C Sánchez, E Sanchez, V Scarpine, D J Schlegel, M Schubnell, S Serrano, I Sevilla-Noarbe, C Sifón, M Smith, J S Speagle, E Suchyta, G Tarle, D Thomas, J Tinker, C To, M A Troxel, L Van Waerbeke, P Vielzeuf, A H Wright, Santa Cruz, Stanford University, Carnegie Mellon University, Berkeley, Ludwig-Maximilians Universität München, Princeton University, University of Cambridge, Max Planck Institute for Extraterrestrial Physics, Royal Observatory, German Centre for Cosmolo gical Lensing, Swinburne University of Technology, Laboratoire d'Annecy De Physique Des Particules (LAPP), Laboratório Interinstitucional de e-Astronomia LIneA, Fermi National Accelerator Laboratory, Universidade Estadual Paulista (UNESP), Institut d'Astrophysique de Paris, CNRS, Northeastern University, Observatoire de Sauverny, University of Manchester, University College London, SLAC National Accelerator Laboratory, 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), CSIC), University of Wisconsin Madison, The Ohio State University, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, Univer sität Hamburg, Medioambientales y Tecnológicas (CIEMAT), Lawrence Berkeley National Laboratory, Santa Cruz Institute for Particle Physics, Ludwig-Maximilians-Universität, University of Pennsylvania, University of Michigan, University of Oslo, Universidad Autonoma de Madrid, University of Geneva, ASTRAVEO LLC, University of Arizona, Macquarie University, Lowell Observatory, Leiden University, Universidade de São Paulo (USP), ECyT UNSAM, Centro Brasileiro de Pesquisas Físicas, Texas A&M University, Institució Catalana de Recerca i Estudis Avancats, Nagoya University, University of Tokyo, Universidade Federal do Rio de Janeiro (UFRJ), The Inter-University Centre for Astronomy and Astrophysics, University of Chicago, University of British Columbia, California Institute of Technology, Pontificia Universidad Católica de Valparaíso, University of Southampton, University of Toronto, Oak Ridge National Laboratory, University of Portsmouth, New York University, Duke University, Leauthaud, A, Amon, A, Singh, S, Gruen, D, Lange, J U, Huang, S, Robertson, N C, Varga, T N, Luo, Y, Heymans, C, Hildebrandt, H, Blake, C, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Bertin, E, Bhargava, S, Blazek, J, Bridle, S L, Brooks, D, Burke, D L, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Castander, F J, Cawthon, R, Choi, A, Costanzi, M, da Costa, L N, Pereira, M E S, Davis, C, De Vicente, J, Derose, J, Diehl, H T, Dietrich, J P, Doel, P, Eckert, K, Everett, S, Evrard, A E, Ferrero, I, Flaugher, B, Fosalba, P, García-Bellido, J, Gatti, M, Gaztanaga, E, Gruendl, R A, Gschwend, J, Hartley, W G, Hollowood, D L, Honscheid, K, Jain, B, James, D J, Jarvis, M, Joachimi, B, Kannawadi, A, Kim, A G, Krause, E, Kuehn, K, Kuijken, K, Kuropatkin, N, Lima, M, Maccrann, N, Maia, M A G, Makler, M, March, M, Marshall, J L, Melchior, P, Menanteau, F, Miquel, R, Miyatake, H, Mohr, J J, Moraes, B, More, S, Surhud, M, Morgan, R, Myles, J, Ogando, R L C, Palmese, A, Paz-Chinchón, F, Malagón, A A Plaza, Prat, J, Rau, M M, Rhodes, J, Rodriguez-Monroy, M, Roodman, A, Ross, A J, Samuroff, S, Sánchez, C, Sanchez, E, Scarpine, V, Schlegel, D J, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Sifón, C, Smith, M, Speagle, J S, Suchyta, E, Tarle, G, Thomas, D, Tinker, J, To, C, Troxel, M A, Van Waerbeke, L, Vielzeuf, P, Wright, A H, UAM. Departamento de Física Teórica, National Science Foundation (US), Department of Energy (US), European Commission, European Research Council, Ministerio de Educación y Ciencia (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Laboratoire d'Annecy de Physique des Particules (LAPP), 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), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and DES
Subjects: photometric redshifts, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational lensing, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, bonn deep survey, 1st data, redshift distributions, shear calibration, Astrophysics::Galaxy Astrophysics, Observations, data release, Física, Astronomy and Astrophysics, observations [cosmology], Cosmology, Space and Planetary Science, cosmology: observations, cosmological constraints, cross-correlations, digital sky survey, iii. application, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cosmology and Nongalactic Astrophysics, observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: A. Leauthaud et al., Lensing without borders is a cross-survey collaboration created to assess the consistency of galaxy–galaxy lensing signals (ΔΣ) across different data sets and to carry out end-to-end tests of systematic errors. We perform a blind comparison of the amplitude of ΔΣ using lens samples from BOSS and six independent lensing surveys. We find good agreement between empirically estimated and reported systematic errors which agree to better than 2.3σ in four lens bins and three radial ranges. For lenses with zL > 0.43 and considering statistical errors, we detect a 3–4σ correlation between lensing amplitude and survey depth. This correlation could arise from the increasing impact at higher redshift of unrecognized galaxy blends on shear calibration and imperfections in photometric redshift calibration. At zL > 0.54, amplitudes may additionally correlate with foreground stellar density. The amplitude of these trends is within survey-defined systematic error budgets that are designed to include known shear and redshift calibration uncertainty. Using a fully empirical and conservative method, we do not find evidence for large unknown systematics. Systematic errors greater than 15 per cent (25 per cent) ruled out in three lens bins at 68 per cent (95 per cent) confidence at z < 0.54. Differences with respect to predictions based on clustering are observed to be at the 20–30 per cent level. Our results therefore suggest that lensing systematics alone are unlikely to fully explain the ‘lensing is low’ effect at z < 0.54. This analysis demonstrates the power of cross-survey comparisons and provides a promising path for identifying and reducing systematics in future lensing analyses., We acknowledge use of the lux supercomputer at UC Santa Cruz, funded by NSF MRI grant AST 1828315. This material is based on work supported by the U.D Department of Energy, Office of Science, Office of High Energy Physics under Award Number DE-SC0019301. AL acknowledges support from the David and Lucille Packard foundation, and from the Alfred.P Sloan foundation. CH acknowledges support from the European Research Council under grant number 647112, and support from the Max Planck Society and the Alexander von Humboldt Foundation in the framework of the Max Planck-Humboldt Research Award endowed by the Federal Ministry of Education and Research. KK acknowledges support from the Royal Society and Imperial College. HH is supported by a Heisenberg grant of the Deutsche Forschungsgemeinschaft (Hi 1495/5-1), as well as an ERC Consolidator Grant (no. 770935). AHW is supported by an European Research Council Consolidator Grant (no. 770935). 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; 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 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 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. The Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organisation (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from the Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science, and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. This paper makes use of software developed for the Large Synoptic Survey Telescope. We thank the LSST Project for making their code available as free software at http://dm.lsst.org This paper is based [in part] on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by Subaru Telescope and Astronomy Data Center (ADC) at NAOJ. Data analysis was in part carried out with the cooperation of Center for Computational Astrophysics (CfCA), NAOJ. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant no. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 177.A-3016, 177.A-3017, 177.A-3018, and 179.A-2004, and on data products produced by the KiDS consortium. The KiDS production team acknowledges support from: Deutsche Forschungsgemeinschaft, ERC, NOVA, and NWO-M grants; Target; the University of Padova, and the University Federico II (Naples). This work was supported by the Department of Energy, Laboratory Directed Research and Development program at SLAC National Accelerator Laboratory, under contract DE-AC02-76SF00515 and as a part of the Panofsky Fellowship awarded to DG. MM is partially funded by FAPERJ, CNPq, and CONICET. BM acknowledges support from the Brazilian funding agency FAPERJ.
Published: 2021
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6. Dark Energy Survey year 1 results: constraints on extended cosmological models from galaxy clustering and weak lensing

Author: DES Collaboration, Abbott, T. M. C., Abdalla, F. B., Avila, S., Banerji, M., Baxter, E., Bechtol, K., Becker, M. R., Bertin, E., Blazek, J., Bridle, S. L., Brooks, D., Brout, D., Burke, D. L., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, A., Crocce, M., Cunha, C. E., da Costa, L. N., Davis, C., De Vicente, J., DeRose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elvin-Poole, J., Evrard, A. E., Fernandez, E., Fert��, A., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., Hoyle, B., Huterer, D., Jain, B., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, S., Lemos, P., Leonard, C. D., Li, T. S., Liddle, A. R., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Miranda, V., Mohr, J. J., Muir, J., Nichol, R. C., Nord, B., Ogando, R. L. C., Plazas, A. A., Raveri, M., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Samuroff, S., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Vikram, V., Walker, A. R., Weaverdyck, N., Wechsler, R. H., Weller, J., Yanny, B., Zhang, Y., Zuntz, 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, UAM. Departamento de Física Teórica, Natl Opt Astron Observ, UCL, Rhodes Univ, Univ Portsmouth, Univ Cambridge, Univ Penn, LSST, Argonne Natl Lab, Inst Astrophys Paris, UPMC Univ Paris 06, Ohio State Univ, Ecole Polytech Fed Lausanne, Univ Manchester, Stanford Univ, SLAC Natl Accelerator Lab, Universidade Estadual Paulista (Unesp), Carnegie Mellon Univ, Lab Interinst & Astron LIneA, Observ Nacl, Univ Illinois, Natl Ctr Supercomp Applicat, Barcelona Inst Sci & Technol, CSIC, IEEC, Univ Chicago, Univ Michigan, Ctr Invest Energet Medioambientales & Tecnol CIEM, IIT Hyderabad, Fermilab Natl Accelerator Lab, Excellence Cluster Universe, Ludwig Maximilians Univ Munchen, CALTECH, Steward Observ, Univ Edinburgh, Univ Autonoma Madrid, Swiss Fed Inst Technol, Santa Cruz Inst Particle Phys, Max Planck Inst Extraterr Phys, Lawrence Berkeley Natl Lab, Australian Astron Observ, Universidade de São Paulo (USP), Texas A&M Univ, Inst Catalana Recerca & Estudis Avancats, Univ Sussex, Univ Southampton, Brandeis Univ, Universidade Estadual de Campinas (UNICAMP), Oak Ridge Natl Lab, National Optical Astronomy Observatory, University College London, Rhodes University, University of Portsmouth, University of Cambridge, University of Pennsylvania, Argonne National Laboratory, Institut d'Astrophysique de Paris, Ohio State University, Observatoire de Sauverny, University of Manchester, Stanford University, SLAC National Accelerator Laboratory, Universidade Estadual Paulista (UNESP), Carnegie Mellon University, Laboratório Interinstitucional de E-Astronomia - LIneA, Observatório Nacional, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, Barcelona Institute of Science and Technology, Institute of Space Sciences (ICE-CSIC), Institut d'Estudis Espacials de Catalunya (IEEC), University of Chicago, University of Michigan, Medioambientales y Tecnológicas (CIEMAT), 382 Via Pueblo Mall, Fermi National Accelerator Laboratory, Ludwig-Maximilians-Universität, California Institute of Technology, University of Edinburgh, Oak Ridge National Laboratory, Universidad Autonoma de Madrid, Ludwig-Maximilians Universität München, ETH Zurich, Santa Cruz Institute for Particle Physics, Max Planck Institute for Extraterrestrial Physics, Lawrence Berkeley National Laboratory, Australian Astronomical Observatory, Texas AandM University, Institució Catalana de Recerca i Estudis Avançats, University of Sussex, University of Southampton, and Physics Department
Subjects: luminous red galaxies, Planck, cosmological model, geometry, MATÉRIA ESCURA, gravitation: model, Cosmic microwave background, Astrophysics, cosmic background radiation, 4/3, des, 01 natural sciences, Cosmology, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), redshift distributions, Weak gravitational lensing, Physics, nucleosynthesis, neutrinos, hep-ph, High Energy Physics - Phenomenology, curvature, astro-ph.CO, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], lambda, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), General relativity, gr-qc, Dark matter, equation of state: time dependence, sloan digital sky survey, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), dark matter, efficient, symbols.namesake, gravitation: lens, 0103 physical sciences, 010306 general physics, STFC, 010308 nuclear & particles physics, Física, RCUK, redshift, Redshift, gravity, Automatic Keywords, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Dark energy, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], sdss, dark energy: equation of state
Abstract: We present constraints on extensions of the minimal cosmological models dominated by dark matter and dark energy, $\Lambda$CDM and $w$CDM, by using a combined analysis of galaxy clustering and weak gravitational lensing from the first-year data of the Dark Energy Survey (DES Y1) in combination with external data. We consider four extensions of the minimal dark energy-dominated scenarios: 1) nonzero curvature $\Omega_k$, 2) number of relativistic species $N_{\rm eff}$ different from the standard value of 3.046, 3) time-varying equation-of-state of dark energy described by the parameters $w_0$ and $w_a$ (alternatively quoted by the values at the pivot redshift, $w_p$, and $w_a$), and 4) modified gravity described by the parameters $\mu_0$ and $\Sigma_0$ that modify the metric potentials. We also consider external information from Planck CMB measurements; BAO measurements from SDSS, 6dF, and BOSS; RSD measurements from BOSS; and SNIa information from the Pantheon compilation. Constraints on curvature and the number of relativistic species are dominated by the external data; when these are combined with DES Y1, we find $\Omega_k=0.0020^{+0.0037}_{-0.0032}$ at the 68% confidence level, and $N_{\rm eff}, Comment: 22 pages, 7 figures, matches the published version
Published: 2019
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7. Cosmological Constraints from Multiple Probes in the Dark Energy Survey

Author: Eric H. Neilsen, Martin Crocce, A. Carnero Rosell, J. Carretero, Tamara M. Davis, Martin Becker, J. P. Dietrich, J. Gschwend, Richard G. McMahon, J. DeRose, L. F. Secco, D. J. Brout, Darren L. DePoy, W. G. Hartley, F. J. Castander, Richard G. Kron, P. Andersen, Lluís Galbany, A. Roodman, Tommaso Giannantonio, C. Davis, Gary Bernstein, Daniel Gruen, S. A. Uddin, Ofer Lahav, J. Lasker, Elisabeth Krause, J. Muir, Enrique Gaztanaga, N. E. Sommer, Rob Sharp, D. L. Hollowood, Risa H. Wechsler, D. W. Gerdes, A. G. Kim, V. Scarpine, S. Serrano, Richard Kessler, A. Campos, Eli S. Rykoff, Erin Sheldon, David Brooks, D. L. Burke, Geraint F. Lewis, David Goldstein, Carlos Solans Sanchez, Bonnie Zhang, Alex Drlica-Wagner, Marcos Lima, I. Sevilla-Noarbe, H. T. Diehl, P. Martini, M. Gatti, David Bacon, J. Calcino, David J. James, Joseph J. Mohr, J. Prat, Samuel Hinton, Bruce A. Bassett, J. P. Marriner, M. Carrasco Kind, Eric J. Baxter, G. Gutierrez, Dragan Huterer, Niall MacCrann, M. H.L.S. Wang, Bhuvnesh Jain, B. Flaugher, F. Andrade-Oliveira, Alistair R. Walker, Robert C. Nichol, Joe Zuntz, S. Kent, Pablo Fosalba, S. Allam, Ryan J. Foley, Robert A. Gruendl, Anais Möller, N. Kokron, E. Bertin, R. Cawthon, Ramon Miquel, Ashley J. Ross, Juan Estrada, M. S. Schubnell, P. Doel, Marcelle Soares-Santos, J. Annis, H. Camacho, Will J. Percival, N. Weaverdyck, A. Porredon, Karl Glazebrook, Enrique Fernández, Juan Garcia-Bellido, P. Challis, Huan Lin, Daniela Carollo, Jennifer L. Marshall, Brad E. Tucker, K. Honscheid, Brian Yanny, Shantanu Desai, N. Kuropatkin, E. Kasai, Rafe Schindler, Mathew Smith, A. Alarcon, M. Childress, C. Lidman, Felipe Menanteau, Daniel Scolnic, Gregory Tarle, L. N. da Costa, Tesla E. Jeltema, August E. Evrard, E. Swann, K. C. Chan, J. De Vicente, P. Lemos, Daniel Thomas, Brian Nord, Flavia Sobreira, Michael Troxel, Joshua A. Frieman, M. March, M. E. C. Swanson, Matt J. Jarvis, Kyler Kuehn, P. Vielzeuf, Yanxi Zhang, Tim Eifler, Keith Bechtol, Antonella Palmese, Rogerio Rosenfeld, M. A. G. Maia, J. K. Hoormann, Ricardo L. C. Ogando, Ben Hoyle, A. A. Plazas, A. K. Romer, C. B. D'Andrea, Edward Macaulay, Jack Elvin-Poole, S. Samuroff, R. C. Thomas, Eric Morganson, Jacobo Asorey, Yen-Chen Pan, Peter Melchior, N. Banik, Jonathan Blazek, Tenglin Li, Sarah Bridle, Scott Dodelson, Santiago Avila, Chihway Chang, Carlos E. Cunha, Jochen Weller, T. M. C. Abbott, Hiranya V. Peiris, E. J. Sanchez, 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 Optical Astronomy Observatory, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Fermi National Accelerator Laboratory, University of Queensland, Dark Cosmology Centre, Universidade Estadual Paulista (UNESP), Laboratório Interinstitucional de E-Astronomia - LIneA, Korea Astronomy and Space Science Institute, University of Portsmouth, African Institute for Mathematical Sciences, South African Astronomical Observatory, University of Pennsylvania, LSST, University of Wisconsin-Madison, Argonne National Laboratory, Institut d'Astrophysique de Paris, Ohio State University, Observatoire de Sauverny, University of Manchester, University College London, Stanford University, SLAC National Accelerator Laboratory, Universidade de São Paulo (USP), Carnegie Mellon University, Medioambientales y Tecnológicas (CIEMAT), Astrophysical Observatory of Turin, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, Barcelona Institute of Science and Technology, Harvard-Smithsonian Center for Astrophysics, University of Chicago, University of Southampton, Observatório Nacional, Texas A and M University, 382 Via Pueblo Mall, IIT Hyderabad, Excellence Cluster Universe, Ludwig-Maximilians-Universität, Steward Observatory, California Institute of Technology, University of Michigan, Santa Cruz Institute for Particle Physics, University of Pittsburgh, Universidad Autonoma de Madrid, University of Cambridge, Ludwig-Maximilians Universität München, Swinburne University of Technology, ETH Zurich, Max Planck Institute for Extraterrestrial Physics, University of Namibia, Lawrence Berkeley National Laboratory, Macquarie University, University of Sydney, Australian National University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), National Astronomical Observatory of Japan, Academia Sinica, University of Waterloo, Perimeter Institute for Theoretical Physics, University of Sussex, Brookhaven National Laboratory, Physics Department, Universidade Estadual de Campinas (UNICAMP), Duke University, Observatories of the Carnegie Institution for Science, University of Edinburgh, Natl Opt Astron Observ, IEEC, CSIC, Fermilab Natl Accelerator Lab, Univ Queensland, Univ Copenhagen, Universidade Estadual Paulista (Unesp), Lab Interinst E Astron LIneA, Korea Astron & Space Sci Inst, Univ Portsmouth, African Inst Math Sci, South African Astron Observ, Univ Penn, Univ Wisconsin, Argonne Natl Lab, CNRS, UPMC Univ Paris 06, Ohio State Univ, Ecole Polytech Fed Lausanne, Univ Manchester, UCL, Stanford Univ, SLAC Natl Accelerator Lab, Carnegie Mellon Univ, Ctr Invest Energet Medioambientales & Tecnol CIEM, Astrophys Observ Turin, Univ Illinois, Natl Ctr Supercomp Applicat, Barcelona Inst Sci & Technol, Harvard Smithsonian Ctr Astrophys, Univ Chicago, Univ Southampton, Observ Nacl, Texas A&M Univ, Ludwig Maximilians Univ Munchen, Steward Observ, CALTECH, Univ Michigan, Santa Cruz Inst Particle Phys, Univ Pittsburgh, Univ Autonoma Madrid, Univ Cambridge, Swinburne Univ Technol, Swiss Fed Inst Technol, Max Planck Inst Extraterr Phys, Univ Namibia, Lawrence Berkeley Natl Lab, Macquarie Univ, Univ Sydney, Australian Natl Univ, Princeton Univ, Inst Catalana Recerca & Estudis Avancats, ARC Ctr Excellence All Sky Astrophys CAASTRO, Natl Astron Observ Japan, Acad Sinica, Univ Waterloo, Perimeter Inst Theoret Phys, Univ Sussex, Brookhaven Natl Lab, Brandeis Univ, Duke Univ, Observ Carnegie Inst Sci, and Univ Edinburgh
Subjects: bao, Cosmology and Nongalactic Astrophysics (astro-ph.CO), MATÉRIA ESCURA, media_common.quotation_subject, Cosmic microwave background, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, des, Gravitation and Astrophysics, 7. Clean energy, 01 natural sciences, Cosmology, supernova, galaxies, 0103 physical sciences, redshift distributions, 010306 general physics, QC, STFC, Weak gravitational lensing, media_common, Physics, Equation of state (cosmology), RCUK, Shape of the universe, Universe, 13. Climate action, astro-ph.CO, Dark energy, baryon acoustic-oscillations, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], sdss, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The combination of multiple observational probes has long been advocated as a powerful technique to constrain cosmological parameters, in particular dark energy. The Dark Energy Survey has measured 207 spectroscopically--confirmed Type Ia supernova lightcurves; the baryon acoustic oscillation feature; weak gravitational lensing; and galaxy clustering. Here we present combined results from these probes, deriving constraints on the equation of state, $w$, of dark energy and its energy density in the Universe. Independently of other experiments, such as those that measure the cosmic microwave background, the probes from this single photometric survey rule out a Universe with no dark energy, finding $w=-0.80^{+0.09}_{-0.11}$. The geometry is shown to be consistent with a spatially flat Universe, and we obtain a constraint on the baryon density of $\Omega_b=0.069^{+0.009}_{-0.012}$ that is independent of early Universe measurements. These results demonstrate the potential power of large multi-probe photometric surveys and pave the way for order of magnitude advances in our constraints on properties of dark energy and cosmology over the next decade., Comment: 8 pages, 2 figures; v3 matches version accepted by PRL
Published: 2019
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8. Magneto-hydrodynamical origin of eclipsing time variations in post-common-envelope binaries for solar mass secondaries

Author: M. Völschow, Felipe Navarrete, Jennifer Schober, Ronald E. Mennickent, Dominik R. G. Schleicher, Petri J. Käpylä, Universidad de Concepción, Centre of Excellence Research on Solar Long-Term Variability and Effects, ReSoLVE, Observatoire de Sauverny, University of Hamburg, Department of Computer Science, Aalto-yliopisto, and Aalto University
Subjects: MECHANISM, MHD, MODELS, FOS: Physical sciences, Astrophysics, Rotation, 01 natural sciences, Common envelope, eclipsing [binaries], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Solar mass, STAR, 010308 nuclear & particles physics, Astronomy and Astrophysics, numerical [methods], WHITE-DWARF, ACTIVITY CYCLES, dynamo, EVOLUTION, Magnetic field, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, ORBITAL PERIOD MODULATION, CONVECTION, Dynamo theory, rotation [stars], Solar rotation, Magnetohydrodynamics, Dynamo
Abstract: Eclipsing time variations have been observed for a wide range of binary systems, including post-common-envelope binaries. A frequently proposed explanation, apart from the possibility of having a third body, is the effect of magnetic activity, which may alter the internal structure of the secondary star, particularly its quadrupole moment, and thereby cause quasi-periodic oscillations. Here we present two compressible non-ideal magneto-hydrodynamical (MHD) simulations of the magnetic dynamo in a solar mass star, one of them with three times the solar rotation rate ("slow rotator"), the other one with twenty times the solar rotation rate ("rapid rotator"), to account for the high rotational velocities in close binary systems. For the slow rotator, we find that both the magnetic field and the stellar quadrupole moment change in a quasi-periodic manner, leading to O-C (observed - corrected times of the eclipse) variations of ~0.025 s. For the rapid rotator, the behavior of the magnetic field as well as the quadrupole moment changes become considerably more complex, due to the less coherent dynamo solution. The resulting O-C variations are of the order 0.13 s. The observed system V471~Tau shows two modes of eclipsing time variations, with amplitudes of 151 s and 20 s, respectively. However, the current simulations may not capture all relevant effects due to the neglect of the centrifugal force and self-gravity. Considering the model limitations and that the rotation of V471 Tau is still a factor of 2.5 faster than our rapid rotator, it may be conceivable to reach the observed magnitudes., Comment: 16 pages, 24 figures, accepted for publication with MNRAS
Published: 2019
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9. Dark Energy Survey Year 1 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing

Author: Abbott, T. M. C., Abdalla, F. B., Alarcon, A., Aleksic, J., Allam, S., Allen, S., Amara, A., Annis, J., Asorey, J., Avila, S., Bacon, D., Balbinot, E., Banerji, M., Banik, N., Barkhouse, W., Baumer, M., Baxter, E., Bechtol, K., Becker, M. R., Benoit-Levy, A., Benson, B. A., Bernstein, G. M., Bertin, E., Blazek, J., Bridle, S. L., Brooks, D., Brout, D., Buckley-Geer, E., Burke, D. L., Busha, M. T., Campos, A. [UNESP], Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, N., Childress, M., Choi, A., Conselice, C., Crittenden, R., Crocce, M., Cunha, C. E., D'Andrea, C. B., Costa, L. N. da, Das, R., Davis, T. M., Davis, C., De Vicente, J., DePoy, D. L., DeRose, J., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elliott, A. E., Elsner, F., Elvin-Poole, J., Estrada, J., Evrard, A. E., Fang, Y., Fernandez, E., Ferte, A., Finley, D. A., Flaugher, B., Fosalba, P., Friedrich, O., Frieman, J., Garcia-Bellido, J., Garcia-Fernandez, M., Gatti, M., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gill, M. S. S., Glazebrook, K., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hamilton, S., Hartley, W. G., Hinton, S. R., Honscheid, K., Hoyle, B., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. D., Johnson, M. W. G., Kacprzak, T., Kent, S., Kim, A. G., King, A., Kirk, D., Kokron, N., Kovacs, A., Krause, E., Krawiec, C., Kremin, A., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lacasa, F. [UNESP], Lahav, O., Li, T. S., Liddle, A. R., Lidman, C., Lima, M., Lin, H., MacCrann, N., Maia, M. A. G., Makler, M., Manera, M., March, M., Marshall, J. L., Martini, P., McMahon, R. G., Melchior, P., Menanteau, F., Miquel, R., Miranda, V., Mudd, D., Muir, J., Moller, A., Neilsen, E., Nichol, R. C., Nord, B., Nugent, P., Ogando, R. L. C., Palmese, A., Peacock, J., Peiris, H. V., Peoples, J., Percival, W. J., Petravick, D., Plazas, A. A., Porredon, A., Prat, J., Pujol, A., Rau, M. M., Refregier, A., Ricker, P. M., Roe, N., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R. [UNESP], Ross, A. J., Rozo, E., Rykoff, E. S., Sako, M., Salvador, A. I., Samuroff, S., Sanchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schindler, R., Scolnic, D., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, R. C., Smith, M., Smith, J., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Tucker, B. E., Uddin, S. A., Varga, T. N., Vielzeuf, P., Vikram, V., Vivas, A. K., Walker, A. R., Wang, M., Wechsler, R. H., Weller, J., Wester, W., Wolf, R. C., Yanny, B., Yuan, F., Zenteno, A., Zhang, B., Zhang, Y., Zuntz, J., Dark Energy Survey 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 Optical Astronomy Observatory, Rhodes University, University College London, IEEC-CSIC, Barcelona Institute of Science and Technology, Fermi National Accelerator Laboratory, Stanford University, ETH Zurich, University of Queensland, ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), University of Portsmouth, Universidad Autonoma de Madrid, University of Surrey, University of Cambridge, Witmer Hall, SLAC National Accelerator Laboratory, University of Pennsylvania, LSST, Institut d'Astrophysique de Paris, University of Chicago, Observatoire de Sauverny, Ohio State University, University of Manchester, Universidade Estadual Paulista (UNESP), Laboratório Interinstitucional de E-Astronomia - LIneA, Observatório Nacional, National Center for Supercomputing Applications, University of Illinois, University of Southampton, School of Physics and Astronomy, University of Michigan, Medioambientales y Tecnológicas (CIEMAT), Texas A and M University, IIT Hyderabad, Excellence Cluster Universe, Ludwig-Maximilians-Universität, California Institute of Technology, University of Edinburgh, Ludwig-Maximilians Universität München, Max Planck Institute for Extraterrestrial Physics, Swinburne University of Technology, 501 Campbell Hall, Lawrence Berkeley National Laboratory, University of Washington, Santa Cruz Institute for Particle Physics, Universidade de São Paulo (USP), Australian Astronomical Observatory, Argonne National Laboratory, Centro Brasileiro de Pesquisas Físicas, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, Australian National University, University of Sussex, University of Arizona, UFRGS, Brookhaven National Laboratory, Dept. Physics-Astronomy, Universidade Estadual de Campinas (UNICAMP), Oak Ridge National Laboratory, Chinese Academy of Sciences, Cerro Tololo Interamer Observ, Rhodes Univ, UCL, CSIC, Barcelona Inst Sci & Technol, Fermilab Natl Accelerator Lab, Stanford Univ, Swiss Fed Inst Technol, Univ Queensland, ARC Ctr Excellence All Sky Astrophys CAASTRO, Univ Portsmouth, UAM, Univ Surrey, Univ Cambridge, Univ North Dakota, SLAC Natl Accelerator Lab, Univ Penn, CNRS, UPMC Univ Paris 06, Univ Chicago, EPFL, Ohio State Univ, Univ Manchester, Universidade Estadual Paulista (Unesp), Lab Interinst Astron LIneA, Observ Nacl, Natl Ctr Supercomp Applicat, Univ Illinois, Univ Southampton, Univ Nottingham, Univ Michigan, Ctr Invest Energet Medioambient & Tecnol CIEMAT, Texas A&M Univ, Ludwig Maximilians Univ Munchen, CALTECH, Univ Edinburgh, Max Planck Inst Extraterr Phys, Swinburne Univ Technol, Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Univ Washington, Santa Cruz Inst Particle Phys, Australian Astron Observ, Argonne Natl Lab, Ctrt Brasileiro Pesquisas Fisicas, Princeton Univ, Inst Catalana Recerca & Estudis Avancats, Australian Natl Univ, Univ Sussex, Univ Arizona, Univ Fed Rio Grande do Sul, Brookhaven Natl Lab, Austin Peay State Univ, Oak Ridge Natl Lab, and Chinese Acad Sci
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, symbols.namesake, 0103 physical sciences, Planck, 010303 astronomy & astrophysics, Weak gravitational lensing, STFC, ResearchInstitutes_Networks_Beacons/MERI, QC, Physics, 010308 nuclear & particles physics, Astronomy, RCUK, Manchester Environmental Research Institute, Redshift, Galaxy, symbols, Dark energy, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present cosmological results from a combined analysis of galaxy clustering and weak gravitational lensing, using 1321 deg$^2$ of $griz$ imaging data from the first year of the Dark Energy Survey (DES Y1). We combine three two-point functions: (i) the cosmic shear correlation function of 26 million source galaxies in four redshift bins, (ii) the galaxy angular autocorrelation function of 650,000 luminous red galaxies in five redshift bins, and (iii) the galaxy-shear cross-correlation of luminous red galaxy positions and source galaxy shears. To demonstrate the robustness of these results, we use independent pairs of galaxy shape, photometric redshift estimation and validation, and likelihood analysis pipelines. To prevent confirmation bias, the bulk of the analysis was carried out while blind to the true results; we describe an extensive suite of systematics checks performed and passed during this blinded phase. The data are modeled in flat $\Lambda$CDM and $w$CDM cosmologies, marginalizing over 20 nuisance parameters, varying 6 (for $\Lambda$CDM) or 7 (for $w$CDM) cosmological parameters including the neutrino mass density and including the 457 $\times$ 457 element analytic covariance matrix. We find consistent cosmological results from these three two-point functions, and from their combination obtain $S_8 \equiv \sigma_8 (\Omega_m/0.3)^{0.5} = 0.783^{+0.021}_{-0.025}$ and $\Omega_m = 0.264^{+0.032}_{-0.019}$ for $\Lambda$CDM for $w$CDM, we find $S_8 = 0.794^{+0.029}_{-0.027}$, $\Omega_m = 0.279^{+0.043}_{-0.022}$, and $w=-0.80^{+0.20}_{-0.22}$ at 68% CL. The precision of these DES Y1 results rivals that from the Planck cosmic microwave background measurements, allowing a comparison of structure in the very early and late Universe on equal terms. Although the DES Y1 best-fit values for $S_8$ and $\Omega_m$ are lower than the central values from Planck ..., Comment: Matches published version. Results essentially unchanged, except updated covariance matrix leads to improved chi^2 (colored text removed)
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10. Dark Energy Survey Year 3 results: galaxy-halo connection from galaxy-galaxy lensing

Author: Martin Crocce, R. D. Wilkinson, Maria E. S. Pereira, Joe Zuntz, Alex Drlica-Wagner, K. Honscheid, J. Blazek, Elisabeth Krause, Scott Dodelson, Chihway Chang, Matthew R. Becker, S. Desai, F. J. Castander, T. M. C. Abbott, Marcos Lima, Antonella Palmese, C. Doux, Chun-Hao To, E. J. Sanchez, Stella Seitz, I. Tutusaus, E. Bertin, M. A. G. Maia, J. Annis, A. Alarcon, I. Ferrero, Matt J. Jarvis, Eli S. Rykoff, Peter Doel, Brian Yanny, Yanxi Zhang, P. F. Leget, Josh Frieman, David J. Brooks, W. G. Hartley, J. P. Dietrich, Juan Garcia-Bellido, Ramon Miquel, Bhuvnesh Jain, H. T. Diehl, David Bacon, A. Roodman, G. Zacharegkas, J. McCullough, M. Costanzi, E. M. Huff, R. Chen, M Gatti, Niall MacCrann, Jennifer L. Marshall, Carlos Solans Sanchez, Samuel Hinton, Michel Aguena, Adriano Pieres, C. Davis, G. Gutierrez, B. Yin, B. Flaugher, Alexandra Amon, R. P. Rollins, J. Myles, J. Gschwend, Gary Bernstein, K. Herner, A. Navarro-Alsina, Keith Bechtol, Enrique Gaztanaga, Ami Choi, Ben Hoyle, J. Carretero, G. Giannini, J. DeRose, E. Suchyta, August E. Evrard, Felipe Menanteau, David J. James, A. Carnero Rosell, S. Everett, Jack Elvin-Poole, A. Porredon, Youngsoo Park, Pablo Fosalba, Risa H. Wechsler, Daniel Thomas, Peter Melchior, R. Cawthon, Agnès Ferté, J. Cordero, D. L. Burke, D. L. Hollowood, R. L. C. Ogando, S. Serrano, A. Campos, F. Paz-Chinchón, I. Harrison, S. Allam, Robert A. Gruendl, M. Smith, Daniel Gruen, T. Shin, M. Carrasco Kind, F. Andrade-Oliveira, Marco Raveri, L. F. Secco, G. Tarle, Erin Sheldon, Ashley J. Ross, I. Sevilla-Noarbe, Kyler Kuehn, N. Kuropatkin, K. D. Eckert, T. N. Varga, L. N. da Costa, Michael Troxel, S. Pandey, J. Muir, J. Prat, 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, Zacharegkas, G., Chang, C., Prat, J., Pandey, S., Ferrero, I., Blazek, J., Jain, B., Crocce, M., Derose, J., Palmese, A., Seitz, S., Sheldon, E., Hartley, W. G., Wechsler, R. H., Dodelson, S., Fosalba, P., Krause, E., Park, Y., Sanchez, C., Alarcon, A., Amon, A., Bechtol, K., Becker, M. R., Bernstein, G. M., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Choi, A., Cordero, J., Davis, C., Diehl, H. T., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferte, A., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Herner, K., Huff, E. M., Jarvis, M., Kuropatkin, N., Leget, P. -F., Maccrann, N., Mccullough, J., Myles, J., Navarro-Alsina, A., Porredon, A., Raveri, M., Rollins, R. P., Roodman, A., Ross, A. J., Rykoff, E. S., Secco, L. F., Sevilla-Noarbe, I., Shin, T., Troxel, M. A., Tutusaus, I., Varga, T. N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carretero, J., Castander, F. J., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Muir, J., Ogando, R. L. C., Paz-Chinchon, F., Pieres, A., Sanchez, E., Serrano, S., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Wilkinson, R. D., Department of Energy (US), National Science Foundation (US), Ministerio de Educación y Ciencia (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, European Research Council, National Aeronautics and Space Administration (US), University of Chicago, University of Pennsylvania, University of Oslo, Northeastern University, Observatoire de Sauverny, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), Lawrence Berkeley National Laboratory, Fermi National Accelerator Laboratory, Giessenbachstrasse, Ludwig-Maximilians Universität München, Brookhaven National Laboratory, University of Geneva, Stanford University, Slac National Accelerator Laboratory, Carnegie Mellon University, University of Arizona, University of Tokyo, Argonne National Laboratory, University of Wisconsin-Madison, la Laguna, Laboratório Interinstitucional de E-Astronomia-LIneA, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Duke University, Ohio State University, University of Manchester, Santa Cruz Institute for Particle Physics, California Institute of Technology, Barcelona Institute of Science and Technology, Denys Wilkinson Building, University of Cambridge, Universidade Estadual de Campinas (UNICAMP), Medioambientales y Tecnológicas (CIEMAT), University of Edinburgh, Casilla, Universidade Estadual Paulista (UNESP), University of Portsmouth, Institut d'Astrophysique de Paris, University College London, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, Iit Hyderabad, Ludwig-Maximilians-Universität, 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, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Southampton, Oak Ridge National Laboratory, University of Sussex, and UAM. Departamento de Física Teórica
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Halo occupation distribution, Cosmology, matter haloes, Galactic halo, gravitational lensing: weak, dark matter [cosmology], weak [gravitational lensing], 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, large-scale structure of universe, occupation distribution, massive galaxies, model, 010308 nuclear & particles physics, 100 square degrees, Física, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, cosmology: dark matter, large-scale structure of Universe, Galaxy, Redshift, radial-distribution, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, cosmological constraints, cfhtlens, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], sdss, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: G. Zacharegkas et al., Galaxy–galaxy lensing is a powerful probe of the connection between galaxies and their host dark matter haloes, which is important both for galaxy evolution and cosmology. We extend the measurement and modelling of the galaxy–galaxy lensing signal in the recent Dark Energy Survey Year 3 cosmology analysis to the highly non-linear scales (∼100 kpc). This extension enables us to study the galaxy–halo connection via a Halo Occupation Distribution (HOD) framework for the two lens samples used in the cosmology analysis: a luminous red galaxy sample (REDMAGIC) and a magnitude-limited galaxy sample (MAGLIM). We find that REDMAGIC (MAGLIM) galaxies typically live in dark matter haloes of mass log10(Mh/M⊙) ≈ 13.7 which is roughly constant over redshift (13.3−13.5 depending on redshift). We constrain these masses to ∼15 per cent ⁠, approximately 1.5 times improvement over the previous work. We also constrain the linear galaxy bias more than five times better than what is inferred by the cosmological scales only. We find the satellite fraction for REDMAGIC (MAGLIM) to be ∼0.1−0.2 (0.1−0.3) with no clear trend in redshift. Our constraints on these halo properties are broadly consistent with other available estimates from previous work, large-scale constraints, and simulations. The framework built in this paper will be used for future HOD studies with other galaxy samples and extensions for cosmological analyses., CC is supported by the Henry Luce Foundation. JP is supported by DOE grant 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 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. 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 programme 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.

11. Strong Lensing by Galaxies.

Author: Shajib AJ, Vernardos G, Collett TE, Motta V, Sluse D, Williams LLR, Saha P, Birrer S, Spiniello C, and Treu T
Abstract: Strong gravitational lensing at the galaxy scale is a valuable tool for various applications in astrophysics and cosmology. Some of the primary uses of galaxy-scale lensing are to study elliptical galaxies' mass structure and evolution, constrain the stellar initial mass function, and measure cosmological parameters. Since the discovery of the first galaxy-scale lens in the 1980s, this field has made significant advancements in data quality and modeling techniques. In this review, we describe the most common methods for modeling lensing observables, especially imaging data, as they are the most accessible and informative source of lensing observables. We then summarize the primary findings from the literature on the astrophysical and cosmological applications of galaxy-scale lenses. We also discuss the current limitations of the data and methodologies and provide an outlook on the expected improvements in both areas in the near future., Competing Interests: Competing InterestsThe authors have no conflicts of interest to report., (© The Author(s) 2024.)
Published: 2024
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12. Strong Gravitational Lensing and Microlensing of Supernovae.

Author: Suyu SH, Goobar A, Collett T, More A, and Vernardos G
Abstract: Strong gravitational lensing and microlensing of supernovae (SNe) are emerging as a new probe of cosmology and astrophysics in recent years. We provide an overview of this nascent research field, starting with a summary of the first discoveries of strongly lensed SNe. We describe the use of the time delays between multiple SN images as a way to measure cosmological distances and thus constrain cosmological parameters, particularly the Hubble constant, whose value is currently under heated debates. New methods for measuring the time delays in lensed SNe have been developed, and the sample of lensed SNe from the upcoming Rubin Observatory Legacy Survey of Space and Time (LSST) is expected to provide competitive cosmological constraints. Lensed SNe are also powerful astrophysical probes. We review the usage of lensed SNe to constrain SN progenitors, acquire high-z SN spectra through lensing magnifications, infer SN sizes via microlensing, and measure properties of dust in galaxies. The current challenge in the field is the rarity and difficulty in finding lensed SNe. We describe various methods and ongoing efforts to find these spectacular explosions, forecast the properties of the expected sample of lensed SNe from upcoming surveys particularly the LSST, and summarize the observational follow-up requirements to enable the various scientific studies. We anticipate the upcoming years to be exciting with a boom in lensed SN discoveries., Competing Interests: Competing InterestsThe authors declare that they have no competing interests. SHS is a guest editor of the Space Science Reviews topical collection “Strong Gravitational Lensing”, which includes this review article., (© The Author(s) 2024.)
Published: 2024
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13. Time-Delay Cosmography: Measuring the Hubble Constant and Other Cosmological Parameters with Strong Gravitational Lensing.

Author: Birrer S, Millon M, Sluse D, Shajib AJ, Courbin F, Erickson S, Koopmans LVE, Suyu SH, and Treu T
Abstract: Multiply lensed images of a same source experience a relative time delay in the arrival of photons due to the path length difference and the different gravitational potentials the photons travel through. This effect can be used to measure absolute distances and the Hubble constant ( H 0 ) and is known as time-delay cosmography. The method is independent of the local distance ladder and early-universe physics and provides a precise and competitive measurement of H 0 . With upcoming observatories, time-delay cosmography can provide a 1% precision measurement of H 0 and can decisively shed light on the current reported 'Hubble tension'. This manuscript details the general methodology developed over the past decades in time-delay cosmography, discusses recent advances and results, and, foremost, provides a foundation and outlook for the next decade in providing accurate and ever more precise measurements with increased sample size and improved observational techniques., Competing Interests: Competing InterestsThe authors declare no competing interests., (© The Author(s) 2024.)
Published: 2024
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14. FLAMINGO: calibrating large cosmological hydrodynamical simulations with machine learning.

Author: Kugel R, Schaye J, Schaller M, Helly JC, Braspenning J, Elbers W, Frenk CS, McCarthy IG, Kwan J, Salcido J, van Daalen MP, Vandenbroucke B, Bahé YM, Borrow J, Chaikin E, Huško F, Jenkins A, Lacey CG, Nobels FSJ, and Vernon I
Abstract: To fully take advantage of the data provided by large-scale structure surveys, we need to quantify the potential impact of baryonic effects, such as feedback from active galactic nuclei (AGN) and star formation, on cosmological observables. In simulations, feedback processes originate on scales that remain unresolved. Therefore, they need to be sourced via subgrid models that contain free parameters. We use machine learning to calibrate the AGN and stellar feedback models for the FLAMINGO (Fullhydro Large-scale structure simulations with All-sky Mapping for the Interpretation of Next Generation Observations) cosmological hydrodynamical simulations. Using Gaussian process emulators trained on Latin hypercubes of 32 smaller volume simulations, we model how the galaxy stellar mass function (SMF) and cluster gas fractions change as a function of the subgrid parameters. The emulators are then fit to observational data, allowing for the inclusion of potential observational biases. We apply our method to the three different FLAMINGO resolutions, spanning a factor of 64 in particle mass, recovering the observed relations within the respective resolved mass ranges. We also use the emulators, which link changes in subgrid parameters to changes in observables, to find models that skirt or exceed the observationally allowed range for cluster gas fractions and the SMF. Our method enables us to define model variations in terms of the data that they are calibrated to rather than the values of specific subgrid parameters. This approach is useful, because subgrid parameters are typically not directly linked to particular observables, and predictions for a specific observable are influenced by multiple subgrid parameters., (© 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.)
Published: 2023
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15. Constraints on the Hubble constant from supernova Refsdal's reappearance.

Author: Kelly PL, Rodney S, Treu T, Oguri M, Chen W, Zitrin A, Birrer S, Bonvin V, Dessart L, Diego JM, Filippenko AV, Foley RJ, Gilman D, Hjorth J, Jauzac M, Mandel K, Millon M, Pierel J, Sharon K, Thorp S, Williams L, Broadhurst T, Dressler A, Graur O, Jha S, McCully C, Postman M, Schmidt KB, Tucker BE, and von der Linden A
Abstract: The gravitationally lensed supernova Refsdal appeared in multiple images produced through gravitational lensing by a massive foreground galaxy cluster. After the supernova appeared in 2014, lens models of the galaxy cluster predicted that an additional image of the supernova would appear in 2015, which was subsequently observed. We use the time delays between the images to perform a blinded measurement of the expansion rate of the Universe, quantified by the Hubble constant ( H 0 ). Using eight cluster lens models, we infer [Formula: see text]. Using the two models most consistent with the observations, we find [Formula: see text]. The observations are best reproduced by models that assign dark-matter halos to individual galaxies and the overall cluster.
Published: 2023
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16. Solar Wind Protons in the Diamagnetic Cavity at Comet 67P/Churyumov-Gerasimenko.

Author: Goetz C, Scharré L, Wedlund CS, Moeslinger A, Nilsson H, Odelstad E, Taylor MGGT, and Volwerk M
Abstract: The plasma environment at a comet can be divided into different regions with distinct plasma characteristics. Two such regions are the solar wind ion cavity, which refers to the part of the outer coma that does not contain any solar wind ions anymore; and the diamagnetic cavity, which is the region of unmagnetized plasma in the innermost coma. From theory and previous observations, it was thought that under usual circumstances no solar wind ion should be observable near or inside of the diamagnetic cavity. For the first time, we report on five observations that show that protons near solar wind energies can also be found inside the diamagnetic cavity. We characterize these proton signatures, where and when they occur, and discuss possible mechanisms that could lead to protons penetrating the inner coma and traversing the diamagnetic cavity boundary. By understanding these observations, we hope to better understand the interaction region of the comet with the solar wind under nonstandard conditions. The protons detected inside the diamagnetic cavity have directions and energies consistent with protons of solar wind origin. The five events occur only at intermediate gas production rates and low cometocentric distances. Charge transfer reactions, high solar wind dynamic pressure and a neutral gas outburst can be ruled out as causes. We suggest that the anomalous appearance of protons in the diamagnetic cavity is due to a specific solar wind configuration where the solar wind velocity is parallel to the interplanetary magnetic field, thus inhibiting mass-loading and deflection., (© 2023. The Authors.)
Published: 2023
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17. Uncovering a population of gravitational lens galaxies with magnified standard candle SN Zwicky.

Author: Goobar A, Johansson J, Schulze S, Arendse N, Carracedo AS, Dhawan S, Mörtsell E, Fremling C, Yan L, Perley D, Sollerman J, Joseph R, Hinds KR, Meynardie W, Andreoni I, Bellm E, Bloom J, Collett TE, Drake A, Graham M, Kasliwal M, Kulkarni SR, Lemon C, Miller AA, Neill JD, Nordin J, Pierel J, Richard J, Riddle R, Rigault M, Rusholme B, Sharma Y, Stein R, Stewart G, Townsend A, Vinko J, Wheeler JC, and Wold A
Abstract: Detecting gravitationally lensed supernovae is among the biggest challenges in astronomy. It involves a combination of two very rare phenomena: catching the transient signal of a stellar explosion in a distant galaxy and observing it through a nearly perfectly aligned foreground galaxy that deflects light towards the observer. Here we describe how high-cadence optical observations with the Zwicky Transient Facility, with its unparalleled large field of view, led to the detection of a multiply imaged type Ia supernova, SN Zwicky, also known as SN 2022qmx. Magnified nearly 25-fold, the system was found thanks to the standard candle nature of type Ia supernovae. High-spatial-resolution imaging with the Keck telescope resolved four images of the supernova with very small angular separation, corresponding to an Einstein radius of only θ E = 0.167″ and almost identical arrival times. The small θ E and faintness of the lensing galaxy are very unusual, highlighting the importance of supernovae to fully characterize the properties of galaxy-scale gravitational lenses, including the impact of galaxy substructures., Competing Interests: Competing interestsThe authors declare no competing interests., (© The Author(s) 2023, corrected publication 2023.)
Published: 2023
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18. Dark Energy Survey Year 1 Results: Cosmological Constraints from Cluster Abundances, Weak Lensing, and Galaxy Correlations.

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

Author: Chan JHH, Schive HY, Wong SK, Chiueh T, and Broadhurst T
Abstract: Extremely light bosonic wave dark matter (ψDM) is an emerging dark matter candidate contesting the conventional cold dark matter paradigm and a model subject to intense scrutiny of late. This work for the first time reports testable salient features pertinent to gravitational lenses of ψDM halos. ψDM halos are distinctly filled with large-amplitude, small-scale density fluctuations with δρ/ρ_{halo}∼1 in form of density granules. This halo yields ubiquitous flux ratio anomalies of a few tens of percent, as is typically found for lensed quasars, and may also produce rare hexad and octad images for sources located in well-defined caustic zones. We have found new critical features appearing in the highly demagnified lens center when the halo has sufficiently high surface density near a very compact massive core.
Published: 2020
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20. Cosmological Constraints from Multiple Probes in the Dark Energy Survey.

Author: Abbott TMC, Alarcon A, Allam S, Andersen P, Andrade-Oliveira F, Annis J, Asorey J, Avila S, Bacon D, Banik N, Bassett BA, Baxter E, Bechtol K, Becker MR, Bernstein GM, Bertin E, Blazek J, Bridle SL, Brooks D, Brout D, Burke DL, Calcino J, Camacho H, Campos A, Carnero Rosell A, Carollo D, Carrasco Kind M, Carretero J, Castander FJ, Cawthon R, Challis P, Chan KC, Chang C, Childress M, Crocce M, Cunha CE, D'Andrea CB, da Costa LN, Davis C, Davis TM, De Vicente J, DePoy DL, DeRose J, Desai S, Diehl HT, Dietrich JP, Dodelson S, Doel P, Drlica-Wagner A, Eifler TF, Elvin-Poole J, Estrada J, Evrard AE, Fernandez E, Flaugher B, Foley RJ, Fosalba P, Frieman J, Galbany L, García-Bellido J, Gatti M, Gaztanaga E, Gerdes DW, Giannantonio T, Glazebrook K, Goldstein DA, Gruen D, Gruendl RA, Gschwend J, Gutierrez G, Hartley WG, Hinton SR, Hollowood DL, Honscheid K, Hoormann JK, Hoyle B, Huterer D, Jain B, James DJ, Jarvis M, Jeltema T, Kasai E, Kent S, Kessler R, Kim AG, Kokron N, Krause E, Kron R, Kuehn K, Kuropatkin N, Lahav O, Lasker J, Lemos P, Lewis GF, Li TS, Lidman C, Lima M, Lin H, Macaulay E, MacCrann N, Maia MAG, March M, Marriner J, Marshall JL, Martini P, McMahon RG, Melchior P, Menanteau F, Miquel R, Mohr JJ, Morganson E, Muir J, Möller A, Neilsen E, Nichol RC, Nord B, Ogando RLC, Palmese A, Pan YC, Peiris HV, Percival WJ, Plazas AA, Porredon A, Prat J, Romer AK, Roodman A, Rosenfeld R, Ross AJ, Rykoff ES, Samuroff S, Sánchez C, Sanchez E, Scarpine V, Schindler R, Schubnell M, Scolnic D, Secco LF, Serrano S, Sevilla-Noarbe I, Sharp R, Sheldon E, Smith M, Soares-Santos M, Sobreira F, Sommer NE, Swann E, Swanson MEC, Tarle G, Thomas D, Thomas RC, Troxel MA, Tucker BE, Uddin SA, Vielzeuf P, Walker AR, Wang M, Weaverdyck N, Wechsler RH, Weller J, Yanny B, Zhang B, Zhang Y, and Zuntz J
Abstract: The combination of multiple observational probes has long been advocated as a powerful technique to constrain cosmological parameters, in particular dark energy. The Dark Energy Survey has measured 207 spectroscopically confirmed type Ia supernova light curves, the baryon acoustic oscillation feature, weak gravitational lensing, and galaxy clustering. Here we present combined results from these probes, deriving constraints on the equation of state, w, of dark energy and its energy density in the Universe. Independently of other experiments, such as those that measure the cosmic microwave background, the probes from this single photometric survey rule out a Universe with no dark energy, finding w=-0.80_{-0.11}^{+0.09}. The geometry is shown to be consistent with a spatially flat Universe, and we obtain a constraint on the baryon density of Ω_{b}=0.069_{-0.012}^{+0.009} that is independent of early Universe measurements. These results demonstrate the potential power of large multiprobe photometric surveys and pave the way for order of magnitude advances in our constraints on properties of dark energy and cosmology over the next decade.
Published: 2019
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21. Warm-hot baryons comprise 5-10 per cent of filaments in the cosmic web.

Author: Eckert D, Jauzac M, Shan H, Kneib JP, Erben T, Israel H, Jullo E, Klein M, Massey R, Richard J, and Tchernin C
Abstract: Observations of the cosmic microwave background indicate that baryons account for 5 per cent of the Universe's total energy content. In the local Universe, the census of all observed baryons falls short of this estimate by a factor of two. Cosmological simulations indicate that the missing baryons have not condensed into virialized haloes, but reside throughout the filaments of the cosmic web (where matter density is larger than average) as a low-density plasma at temperatures of 10(5)-10(7) kelvin, known as the warm-hot intergalactic medium. There have been previous claims of the detection of warm-hot baryons along the line of sight to distant blazars and of hot gas between interacting clusters. These observations were, however, unable to trace the large-scale filamentary structure, or to estimate the total amount of warm-hot baryons in a representative volume of the Universe. Here we report X-ray observations of filamentary structures of gas at 10(7) kelvin associated with the galaxy cluster Abell 2744. Previous observations of this cluster were unable to resolve and remove coincidental X-ray point sources. After subtracting these, we find hot gas structures that are coherent over scales of 8 megaparsecs. The filaments coincide with over-densities of galaxies and dark matter, with 5-10 per cent of their mass in baryonic gas. This gas has been heated up by the cluster's gravitational pull and is now feeding its core. Our findings strengthen evidence for a picture of the Universe in which a large fraction of the missing baryons reside in the filaments of the cosmic web.
Published: 2015
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22. The nongravitational interactions of dark matter in colliding galaxy clusters.

Author: Harvey D, Massey R, Kitching T, Taylor A, and Tittley E
Abstract: Collisions between galaxy clusters provide a test of the nongravitational forces acting on dark matter. Dark matter's lack of deceleration in the "bullet cluster" collision constrained its self-interaction cross section σ(DM)/m < 1.25 square centimeters per gram (cm(2)/g) [68% confidence limit (CL)] (σ(DM), self-interaction cross section; m, unit mass of dark matter) for long-ranged forces. Using the Chandra and Hubble Space Telescopes, we have now observed 72 collisions, including both major and minor mergers. Combining these measurements statistically, we detect the existence of dark mass at 7.6σ significance. The position of the dark mass has remained closely aligned within 5.8 ± 8.2 kiloparsecs of associated stars, implying a self-interaction cross section σ(DM)/m < 0.47 cm(2)/g (95% CL) and disfavoring some proposed extensions to the standard model., (Copyright © 2015, American Association for the Advancement of Science.)
Published: 2015
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22 results on '"Observatoire de Sauverny"'

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

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

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

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

5. Lensing Without Borders. I. A Blind Comparison of the Amplitude of Galaxy-Galaxy Lensing Between Independent Imaging Surveys

6. Dark Energy Survey year 1 results: constraints on extended cosmological models from galaxy clustering and weak lensing

7. Cosmological Constraints from Multiple Probes in the Dark Energy Survey

8. Magneto-hydrodynamical origin of eclipsing time variations in post-common-envelope binaries for solar mass secondaries

9. Dark Energy Survey Year 1 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing

10. Dark Energy Survey Year 3 results: galaxy-halo connection from galaxy-galaxy lensing

11. Strong Lensing by Galaxies.

12. Strong Gravitational Lensing and Microlensing of Supernovae.

13. Time-Delay Cosmography: Measuring the Hubble Constant and Other Cosmological Parameters with Strong Gravitational Lensing.

14. FLAMINGO: calibrating large cosmological hydrodynamical simulations with machine learning.

15. Constraints on the Hubble constant from supernova Refsdal's reappearance.

16. Solar Wind Protons in the Diamagnetic Cavity at Comet 67P/Churyumov-Gerasimenko.

17. Uncovering a population of gravitational lens galaxies with magnified standard candle SN Zwicky.

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

19. Multiple Images and Flux Ratio Anomaly of Fuzzy Gravitational Lenses.

20. Cosmological Constraints from Multiple Probes in the Dark Energy Survey.

21. Warm-hot baryons comprise 5-10 per cent of filaments in the cosmic web.

22. The nongravitational interactions of dark matter in colliding galaxy clusters.

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