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dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and weak lensing

Physical Review d 2022年第2期105卷 023520-023520页

作者： T. M. C. Abbott M. Aguena A. Alarcon S. Allam O. Alves A. Amon F. Andrade-Oliveira J. Annis S. Avila d. Bacon E. Baxter K. Bechtol M. R. Becker G. M. Bernstein S. Bhargava S. Birrer J. Blazek A. Brandao-Souza S. L. Bridle d. Brooks E. Buckley-Geer d. L. Burke H. Camacho A. Campos A. Carnero Rosell M. Carrasco Kind J. Carretero F. J. Castander R. Cawthon C. Chang A. Chen R. Chen A. Choi C. Conselice J. Cordero M. Costanzi M. Crocce L. N. da Costa M. E. da Silva Pereira C. davis T. M. davis J. de Vicente J. deRose S. desai E. di Valentino H. T. diehl J. P. dietrich S. dodelson P. doel C. doux A. drlica-Wagner K. Eckert T. F. Eifler F. Elsner J. Elvin-Poole S. Everett A. E. Evrard X. Fang A. Farahi E. Fernandez I. Ferrero A. Ferté P. Fosalba O. Friedrich J. Frieman J. García-Bellido M. Gatti E. Gaztanaga d. W. Gerdes T. Giannantonio G. Giannini d. Gruen R. A. Gruendl J. Gschwend G. Gutierrez I. Harrison W. G. Hartley K. Herner S. R. Hinton d. L. Hollowood K. Honscheid B. Hoyle E. M. Huff d. Huterer B. Jain d. J. James M. Jarvis N. Jeffrey T. Jeltema A. Kovacs E. Krause R. Kron K. Kuehn N. Kuropatkin O. Lahav P.-F. Leget P. Lemos A. R. Liddle C. Lidman M. Lima H. Lin N. MacCrann M. A. G. Maia J. L. Marshall P. Martini J. McCullough P. Melchior J. Mena-Fernández F. Menanteau R. Miquel J. J. Mohr R. Morgan J. Muir J. Myles S. Nadathur A. Navarro-Alsina R. C. Nichol R. L. C. Ogando Y. Omori A. Palmese S. Pandey Y. Park F. Paz-Chinchón d. Petravick A. Pieres A. A. Plazas Malagón A. Porredon J. Prat M. Raveri M. Rodriguez-Monroy R. P. Rollins A. K. Romer A. Roodman R. Rosenfeld A. J. Ross E. S. Rykoff S. Samuroff C. Sánchez E. Sanchez J. Sanchez d. Sanchez Cid V. Scarpine M. Schubnell d. Scolnic L. F. Secco S. Serrano I. Sevilla-Noarbe E. Sheldon T. Shin M. Smith M. Soares-Santos E. Suchyta M. E. C. Swanson M. Tabbutt G. Tarle d. Thomas C. To A. Troja M. A. Troxel d. L. Tucker I. Tutusaus T. N. Varga A. R. Walker N. Weaverdyck R. Wechsler J. Weller B. Yanny B. Yin Y. Zhang J. Zuntz Cerro Tololo Inter-American Observatory NSF’s National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile Laboratório Interinstitucional de e-Astronomia—LIneA Rua Gal. José Cristino 77 Rio de Janeiro RJ—20921-400 Brazil Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Fermi National Accelerator Laboratory P. O. Box 500 Batavia Illinois 60510 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Instituto de Física Teórica Universidade Estadual Paulista São Paulo 01140-070 Brazil Kavli Institute for Particle Astrophysics and Cosmology P. O. Box 2450 Stanford University Stanford California 94305 USA Instituto de Fisica Teorica UAM/CSIC Universidad Autonoma de Madrid 28049 Madrid Spain Institute of Cosmology and Gravitation University of Portsmouth Portsmouth PO1 3FX United Kingdom Institute for Astronomy University of Hawai’i 2680 Woodlawn Drive Honolulu Hawaii 96822 USA Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue Madison Wisconsin 53706-1390 USA Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA Department of Physics and Astronomy Pevensey Building University of Sussex Brighton BN1 9QH United Kingdom Graduate School of Education Stanford University 160 450 Serra Mall Stanford California 94305 USA Department of Physics Northeastern University Boston Massachusetts 02115 USA Laboratory of Astrophysics École Polytechnique Fédérale de Lausanne (EPFL) Observatoire de Sauverny 1290 Versoix Switzerland Instituto de Física Gleb Wataghin Universidade Estadual de Campinas 13083-859 Campinas SP Brazil Jodrell Bank Center for Astrophysics School of Physics and Astronomy University of Manchester Oxford Road Manchester M13 9PL United Kingdom Department of Physics and Astronomy University College London Gower Street London WC1E 6BT United Kingdom Department of Astronomy and Astroph

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=0.339−0.031+0.032 in ΛCdM, mean with 68% confidence limits; S8=0.775−0.024+0.026, Ωm=0.352−0.041+0.035, and dark energy equation-of-state parameter w=−0.98−0.20+0.32 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

关键词： Cosmological parameters Cosmology dark energy dark matter Large scale structure of the Universe

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

arXiv

引用

arXiv 2021年

作者： Pandey, Shivam Krause, E. deRose, J. MacCrann, N. Jain, B. Crocce, M. Blazek, J. Choi, A. Huang, H. To, C. Fang, X. Elvin-Poole, J. Prat, J. Porredon, A. Secco, L.F. Rodriguez-Monroy, M. Weaverdyck, N. Park, Y. Raveri, M. Rozo, E. Rykoff, E.S. Bernstein, G.M. Sánchez, C. Jarvis, M. Troxel, M.A. Zacharegkas, G. Chang, C. Alarcon, A. Alves, O. Amon, A. Andrade-Oliveira, F. Baxter, E. Bechtol, K. Becker, M.R. Camacho, H. Campos, A. Carnero Rosell, A. Carrasco Kind, M. Cawthon, R. Chen, R. Chintalapati, P. davis, C. di Valentino, E. diehl, H.T. dodelson, S. doux, C. drlica-Wagner, A. Eckert, K. Eifler, T.F. Elsner, F. Everett, S. Farahi, A. Ferté, A. Fosalba, P. Friedrich, O. Gatti, M. Giannini, G. Gruen, d. Gruendl, R.A. Harrison, I. Hartley, W.G. Huff, E.M. Huterer, d. Kovacs, A. Leget, P.F. McCullough, J. Muir, J. Myles, J. Navarro-Alsina, A. Omori, Y. Rollins, R.P. Roodman, A. Rosenfeld, R. Sevilla-Noarbe, I. Sheldon, E. Shin, T. Troja, A. Tutusaus, I. Varga, T.N. Wechsler, R.H. Yanny, B. Yin, B. Zhang, Y. Zuntz, J. Abbott, T.M.C. Aguena, M. Allam, S. Annis, J. Bacon, d. Bertin, E. Brooks, d. Burke, d.L. Carretero, J. Conselice, C. Costanzi, M. da Costa, L.N. Pereira, M.E.S. de Vicente, J. dietrich, J.P. doel, P. Evrard, A.E. Ferrero, I. Flaugher, B. Frieman, J. García-Bellido, J. Gaztanaga, E. Gerdes, d.W. Giannantonio, T. Gschwend, J. Gutierrez, G. Hinton, S.R. Hollowood, d.L. Honscheid, K. James, d.J. Jeltema, T. Kuehn, K. Kuropatkin, N. Lahav, O. Lima, M. Lin, H. Maia, M.A.G. Marshall, J.L. Melchior, P. Menanteau, F. Miller, C.J. Miquel, R. Mohr, J.J. Morgan, R. Palmese, A. Paz-Chinchón, F. Petravick, d. Pieres, A. Plazas Malagón, A.A. Sanchez, E. Scarpine, V. Serrano, S. Smith, M. Soares-Santos, M. Suchyta, E. Tarle, G. Thomas, d. Weller, J. Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Department of Astronomy Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721-0065 United States Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States Department of Applied Mathematics and Theoretical Physics University of Cambridge CambridgeCB3 0WA United Kingdom Barcelona08034 Spain Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Department of Physics Northeastern University BostonMA02115 United States Observatoire de Sauverny Versoix1290 Switzerland Center for Cosmology and Astro-Particle Physics The Ohio State University ColumbusOH43210 United States Department of Physics University of Arizona TucsonAZ85721 United States Department of Physics Stanford University 382 Via Pueblo Mall StanfordCA94305 United States Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Department of Physics The Ohio State University ColumbusOH43210 United States Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Madrid Spain Department of Physics University of Michigan Ann ArborMI48109 United States UTIAS The University of Tokyo Chiba Kashiwa277-8583 Japan Department of Physics Duke University DurhamNC27708 United States Argonne National Laboratory 9700 South Cass Avenue LemontIL60439 United States Instituto de Física Teórica Universidade Estadual Paulista São Paulo Brazil Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 RJ Rio de Janeiro20921-400 Brazil Institute for Astronomy University of Hawai'i 2680 Woodlawn Drive HonoluluHI96822 United States Physics

We constrain cosmological parameters and galaxy-bias parameters using the combination of galaxy clustering and galaxy-galaxy lensing measurements from the dark Energy Survey (dES) Year-3 data. We describe our modeling framework and choice of scales analyzed, validating their robustness to theoretical uncertainties in small-scale clustering by analyzing simulated data. Using a linear galaxy bias model and redMaGiC galaxy sample, we obtain 10% constraints on the matter density of the universe. We also implement a non-linear galaxy bias model to probe smaller scales that includes parameterization based on hybrid perturbation theory, and find that it leads to a 17% gain in cosmological constraining power. We perform robustness tests of our methodology pipeline and demonstrate stability of the constraints to changes in the theory model. Using the redMaGiC galaxy sample as foreground lens galaxies, and adopting the best-fitting cosmological parameters from dES Year-1 data, we find the galaxy clustering and galaxy-galaxy lensing measurements to exhibit significant signals akin to de-correlation between galaxies and mass on large scales, which is not expected in any current models. This likely systematic measurement error biases our constraints on galaxy bias and the S8 parameter. We find that a scale-, redshift- and sky-area-independent phenomenological de-correlation parameter can effectively capture this inconsistency between the galaxy clustering and galaxy-galaxy lensing. We trace the source of this correlation to a color-dependent photometric issue and minimize its impact on our result by changing the selection criteria of redMaGiC galaxies. Using this new sample, our constraints on the S8 parameter are consistent with previous studies and we find a small shift in the Ωm constraints compared to the fiducial redMaGiC sample. We infer the constraints on the mean host halo mass of the redMaGiC galaxies in this new sample from the large-scale bias constraints, finding the

关键词： Galaxies

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dark Energy Survey Year 3 Results: Redshift Calibration of the MagLim Lens Sample from the combination of SOMPZ and clustering and its impact on Cosmology

arXiv

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arXiv 2022年

作者： Giannini, Giulia Alarcon, A. Gatti, M. Porredon, A. Crocce, M. Bernstein, G.M. Cawthon, R. Sánchez, C. doux, C. Elvin-Poole, J. Raveri, M. Myles, J. Lin, H. Amon, A. Allam, S. Alves, O. Andrade-Oliveira, F. Baxter, E. Bechtol, K. Becker, M.R. Blazek, J. Camacho, H. Campos, A. Carnero Rosell, A. Carrasco Kind, M. Choi, A. Cordero, J. de Vicente, J. deRose, J. diehl, H.T. dodelson, S. drlica-Wagner, A. Eckert, K. Fang, X. Farahi, A. Fosalba, P. Friedrich, O. Gruen, d. Gruendl, R.A. Gschwend, J. Harrison, I. Hartley, W.G. Huff, E.M. Jarvis, M. Krause, E. Kuropatkin, N. Lemos, P. MacCrann, N. McCullough, J. Muir, J. Pandey, S. Prat, J. Rodriguez-Monroy, M. Ross, A.J. Rykoff, E.S. Samuroff, S. Secco, L.F. Sevilla-Noarbe, I. Sheldon, E. Troxel, M.A. Tucker, d.L. Weaverdyck, N. Yanny, B. Yin, B. Zhang, Y. Abbott, T.M.C. Aguena, M. Bacon, d. Bertin, E. Bocquet, S. Brooks, d. Burke, d.L. Carretero, J. Castander, F.J. Costanzi, M. da Costa, L.N. Pereira, M.E.S. desai, S. doel, P. Ferrero, I. Flaugher, B. Friedel, d. Frieman, J. García-Bellido, J. Gerdes, d.W. Gutierrez, G. Hinton, S.R. Hollowood, d.L. Honscheid, K. James, d.J. Kent, S. Kuehn, K. Lahav, O. Lidman, C. Lima, M. Melchior, P. Mena-Fernández, J. Menanteau, F. Miquel, R. Ogando, R.L.C. Paterno, M. Paz-Chinchón, F. Pieres, A. Plazas Malagón, A.A. Roodman, A. Sanchez, E. Scarpine, V. Smith, M. Suchyta, E. Swanson, M.E.C. Tarle, G. Thomas, d. To, C. Vincenzi, M. Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States The Barcelona Institute of Science and Technology Campus UAB Bellaterra Barcelona08193 Spain Argonne National Laboratory 9700 South Cass Avenue LemontIL60439 United States Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Center for Cosmology and Astro-Particle Physics The Ohio State University ColumbusOH43210 United States Department of Physics The Ohio State University ColumbusOH43210 United States Barcelona08034 Spain Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Physics Department William Jewell College LibertyMO64068 United States Department of Physics Stanford University 382 Via Pueblo Mall StanfordCA94305 United States Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Department of Physics University of Michigan Ann ArborMI48109 United States Institute for Astronomy University of Hawai’i 2680 Woodlawn Drive HonoluluHI96822 United States Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue MadisonWI53706-1390 United States Department of Physics Northeastern University BostonMA02115 United States Instituto de Física Teórica Universidade Estadual Paulista São Paulo Brazil Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 RJ Rio de Janeiro20921-400 Brazil Department of Physics Car

We present an alternative calibration of the MagLim lens sample redshift distributions from the dark Energy Survey (dES) first three years of data (Y3). The new calibration is based on a combination of a Self-Organising Maps based scheme and clustering redshifts to estimate redshift distributions and inherent uncertainties, which is expected to be more accurate than the original dES Y3 redshift calibration of the lens sample. We describe in detail the methodology, we validate it on simulations and discuss the main effects dominating our error budget. The new calibration is in fair agreement with the fiducial dES Y3 n(z) calibration, with only mild differences (m = 0.30 ± 0.04, σ8 = 0.81 ± 0.07 and S8 = 0.81 ± 0.04, which implies a ∼ 0.4σshift in the Ω − S8 plane compared to the fiducial dES Y3 results, highlighting the importance of the redshift calibration of the lens sample in multi-probe cosmological analyses. Copyright © 2022, The Authors. All rights reserved.

关键词： Calibration

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Constraining the Baryonic Feedback with Cosmic Shear Using the dES Year-3 Small-Scale Measurements

arXiv

引用

arXiv 2022年

作者： Chen, Angela Aricò, G. Huterer, d. Angulo, R. Weaverdyck, N. Friedrich, O. Secco, L.F. Hernández-Monteagudo, C. Alarcon, A. Alves, O. Amon, A. Andrade-Oliveira, F. Baxter, E. Bechtol, K. Becker, M.R. Bernstein, G.M. Blazek, J. Brandao-Souza, A. Bridle, S.L. Camacho, H. Campos, A. Carnero Rosell, A. Carrasco Kind, M. Cawthon, R. Chang, C. Chen, R. Chintalapati, P. Choi, A. Cordero, J. Crocce, M. Pereira, M.E.S. davis, C. deRose, J. di Valentino, E. diehl, H.T. dodelson, S. doux, C. drlica-Wagner, A. Eckert, K. Eifler, T.F. Elsner, F. Elvin-Poole, J. Everett, S. Fang, X. Ferté, A. Fosalba, P. Gatti, M. Gaztanaga, E. Giannini, G. Gruen, d. Gruendl, R.A. Harrison, I. Hartley, W.G. Herner, K. Hoffmann, K. Huang, H. Huff, E.M. Jain, B. Jarvis, M. Jeffrey, N. Kacprzak, T. Krause, E. Kuropatkin, N. Leget, P.-F. Lemos, P. Liddle, A.R. MacCrann, N. McCullough, J. Muir, J. Myles, J. Navarro-Alsina, A. Omori, Y. Pandey, S. Park, Y. Porredon, A. Prat, J. Raveri, M. Refregier, A. Rollins, R.P. Roodman, A. Rosenfeld, R. Ross, A.J. Rykoff, E.S. Samuroff, S. Sánchez, C. Sanchez, J. Sevilla-Noarbe, I. Sheldon, E. Shin, T. Troja, A. Troxel, M.A. Tutusaus, I. Varga, T.N. Wechsler, R.H. Yanny, B. Yin, B. Zhang, Y. Zuntz, J. Aguena, M. Annis, J. Bacon, d. Bertin, E. Bocquet, S. Brooks, d. Burke, d.L. Carretero, J. Conselice, C. Costanzi, M. da Costa, L.N. de Vicente, J. desai, S. doel, P. Ferrero, I. Flaugher, B. Frieman, J. García-Bellido, J. Gerdes, d.W. Giannantonio, T. Gschwend, J. Gutierrez, G. Hinton, S.R. Hollowood, d.L. Honscheid, K. James, d.J. Kuehn, K. Lahav, O. March, M. Marshall, J.L. Melchior, P. Menanteau, F. Miquel, R. Mohr, J.J. Morgan, R. Paz-Chinchón, F. Pieres, A. Sanchez, E. Smith, M. Suchyta, E. Tarle, G. Thomas, d. To, C. Department of Physics University of Michigan Ann ArborMI48109 United States UTIAS The University of Tokyo Chiba Kashiwa277-8583 Japan Institute for Computational Science University of Zurich Winterthurerstrasse 190 Zurich8057 Switzerland Paseo Manuel de Lardizabal 4 Guipuzkoa Donostia-San Sebastián20018 Spain Departamento de Física Universidad de Zaragoza Pedro Cerbuna 12 Zaragoza50009 Spain IKERBASQUE Basque Foundation for Science Bilbao48013 Spain Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Department of Astrophysics Research Instituto de Astrofísica de Canarias CVía Láctea sn Tenerife La LagunaE-38205 Spain Departamento de Astrofísica Universidad de La Laguna Avenida Francisco Sánchez sn Tenerife La LagunaE-38205 Spain Argonne National Laboratory 9700 South Cass Avenue Lemont IL60439 United States Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 RJ Rio de Janeiro20921-400 Brazil Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States Institute for Astronomy University of Hawai’i 2680 Woodlawn Drive HonoluluHI96822 United States Physics Department University of Wisconsin-Madison 2320 Chamberlin Hall 1150 University Avenue MadisonWI53706-1390 United States Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Department of Physics Northeastern University BostonMA02115 United States Observatoire de Sauverny Versoix 1290 Switzerland Instituto de Física Gleb Wataghin Universidade Estadual de Campinas Campinas SP 13083-859 Brazil Jodrell Bank Center for Astrophysics School of Physics and Astronomy University of Manchester Oxford Road Manc

We use the small scales of the dark Energy Survey (dES) Year-3 cosmic shear measurements, which are excluded from the dES Year-3 cosmological analysis, to constrain the baryonic feedback. To model the baryonic feedback, we adopt a baryonic correction model and use the numerical package Baccoemu to accelerate the evaluation of the baryonic nonlinear matter power spectrum. We design our analysis pipeline to focus on the constraints of the baryonic suppression effects, utilizing the implication given by a principal component analysis on the Fisher forecasts. Our constraint on the baryonic effects can then be used to better model and ameliorate the effects of baryons in producing cosmological constraints from the next generation large-scale structure surveys. We detect the baryonic suppression on the cosmic shear measurements with a ∼ 2σ significance. The characteristic halo mass for which half of the gas is ejected by baryonic feedback is constrained to be Mc > 1013.2h−1Mo (95% C.L.). The best-fit baryonic suppression is ∼ 5% at k = 1.0Mpc h−1 and ∼ 15% at k = 5.0Mpc h−1. Our findings are robust with respect to the assumptions about the cosmological parameters, specifics of the baryonic model, and intrinsic alignments. Copyright © 2022, The Authors. All rights reserved.

关键词： Principal component analysis

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dark Energy Survey Year 3 Results: High-precision measurement and modeling of galaxy-galaxy lensing

arXiv

引用

arXiv 2021年

作者： Prat, Judit Blazek, J. Sánchez, C. Tutusaus, I. Pandey, S. Elvin-Poole, J. Krause, E. Troxel, M.A. Secco, L.F. Amon, A. deRose, J. Zacharegkas, G. Chang, C. Jain, B. MacCrann, N. Park, Y. Sheldon, E. Giannini, G. Bocquet, S. To, C. Alarcon, A. Alves, O. Andrade-Oliveira, F. Baxter, E. Bechtol, K. Becker, M.R. Bernstein, G.M. Camacho, H. Campos, A. Carnero Rosell, A. Carrasco Kind, M. Cawthon, R. Chen, R. Choi, A. Cordero, J. Crocce, M. davis, C. de Vicente, J. diehl, H.T. dodelson, S. doux, C. drlica-Wagner, A. Eckert, K. Eifler, T.F. Elsner, F. Everett, S. Fang, X. Farahi, A. Ferté, A. Fosalba, P. Friedrich, O. Gatti, M. Gruen, d. Gruendl, R.A. Harrison, I. Hartley, W.G. Herner, K. Huang, H. Huff, E.M. Huterer, d. Jarvis, M. Kuropatkin, N. Leget, P.-F. Lemos, P. Liddle, A.R. McCullough, J. Muir, J. Myles, J. Navarro-Alsina, A. Porredon, A. Raveri, M. Rodriguez-Monroy, M. Rollins, R.P. Roodman, A. Rosenfeld, R. Ross, A.J. Rykoff, E.S. Sanchez, J. Sevilla-Noarbe, I. Shin, T. Troja, A. Varga, T.N. Weaverdyck, N. Wechsler, R.H. Yanny, B. Yin, B. Zuntz, J. Abbott, T.M.C. Aguena, M. Allam, S. Annis, J. Bacon, d. Brooks, d. Burke, d.L. Carretero, J. Conselice, C. Costanzi, M. da Costa, L.N. Pereira, M.E.S. desai, S. dietrich, J.P. doel, P. Evrard, A.E. Ferrero, I. Flaugher, B. Frieman, J. García-Bellido, J. Gaztanaga, E. Gerdes, d.W. Giannantonio, T. Gschwend, J. Gutierrez, G. Hinton, S.R. Hollowood, d.L. Honscheid, K. James, d.J. Kuehn, K. Lahav, O. Lin, H. Maia, M.A.G. Marshall, J.L. Martini, P. Melchior, P. Menanteau, F. Miller, C.J. Miquel, R. Mohr, J.J. Morgan, R. Ogando, R.L.C. Palmese, A. Paz-Chinchón, F. Petravick, d. Plazas Malagón, A.A. Sanchez, E. Serrano, S. Smith, M. Soares-Santos, M. Suchyta, E. Tarle, G. Thomas, d. Weller, J. Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Department of Physics Northeastern University BostonMA02115 United States Observatoire de Sauverny Versoix1290 Switzerland Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Barcelona08034 Spain Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Center for Cosmology and Astro-Particle Physics The Ohio State University ColumbusOH43210 United States Department of Physics The Ohio State University ColumbusOH43210 United States Department of Astronomy Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721-0065 United States Department of Physics Duke University DurhamNC27708 United States Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States Department of Applied Mathematics and Theoretical Physics University of Cambridge CambridgeCB3 0WA United Kingdom UTIAS The University of Tokyo Chiba Kashiwa277-8583 Japan Brookhaven National Laboratory Bldg 510 UptonNY11973 United States The Barcelona Institute of Science and Technology Campus UAB Bellaterra Barcelona08193 Spain Faculty of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 Munich81679 Germany Department of Physics Stanford University 382 Via Pueblo Mall StanfordCA94305 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Argonne National Laboratory 9700 South Cass Avenue LemontIL60439 United States Department of Physics University of Michigan Ann ArborMI48109 United States Instituto de Física Teórica Universidade Estadual Paulista São Paulo Brazil Laboratório Interinstitucional de e-Astronomia - LIneA Rua G

We present and characterize the galaxy-galaxy lensing signal measured using the first three years of data from the dark Energy Survey (dES Y3) covering 4132 deg2. These galaxy-galaxy measurements are used in the dES Y3 3×2pt cosmological analysis, which combines weak lensing and galaxy clustering information. We use two lens samples: a magnitude-limited sample and the redMaGic sample, which span the redshift range ∼ 0.2 − 1 with 10.7 M and 2.6 M galaxies respectively. For the source catalog, we use the Metacalibration shape sample, consisting of '100 M galaxies separated into 4 tomographic bins. Our galaxy-galaxy lensing estimator is the mean tangential shear, for which we obtain a total S/N of ∼148 for MagLim (∼120 for redMaGic), and ∼67 (∼55) after applying the scale cuts of 6 Mpc/ℎ. Thus we reach percent-level statistical precision, which requires that our modeling and systematic-error control be of comparable accuracy. The tangential shear model used in the 3×2pt cosmological analysis includes lens magnification, a five-parameter intrinsic alignment model (TATT), marginalization over a point-mass to remove information from small scales and a linear galaxy bias model validated with higher-order terms. We explore the impact of these choices on the tangential shear observable and study the significance of effects not included in our model, such as reduced shear, source magnification and source clustering. We also test the robustness of our measurements to various observational and systematics effects, such as the impact of observing conditions, lens-source clustering, random-point subtraction, scale-dependent Metacalibration responses, PSF residuals, and B-modes. Copyright © 2021, The Authors. All rights reserved.

关键词： Galaxies

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dark Energy Survey Year 3 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing

arXiv

引用

arXiv 2021年

作者： 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. Ferté, A. Fosalba, P. Friedrich, O. Frieman, J. García-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-Fernández, 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-Chinchón, F. Petravick, d. Pieres, A. Plazas Malagón, 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. Sánchez, 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. Cerro Tololo Inter-American Observatory NSF's National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 RJ Rio de Janeiro20921-400 Brazil Argonne National Laboratory 9700 South Cass Avenue LemontIL60439 United States Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Department of Physics University of Michigan Ann ArborMI48109 United States Instituto de Física Teórica Universidade Estadual Paulista São Paulo Brazil Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States Instituto de Fisica Teorica UAM CSIC Universidad Autonoma de Madrid Madrid28049 Spain Institute of Cosmology and Gravitation University of Portsmouth PortsmouthPO1 3FX United Kingdom Institute for Astronomy University of Hawai'i 2680 Woodlawn Drive HonoluluHI96822 United States Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue MadisonWI53706-1390 United States Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Department of Physics and Astronomy University of Sussex Pevensey Building BrightonBN1 9QH United Kingdom Graduate School of Education Stanford University 160 450 Serra Mall StanfordCA94305 United States Department of Physics Northeastern University BostonMA02115 United States Observatoire de Sauverny Versoix1290 Switzerland Instituto de Física Gleb Wataghin Universidade Estadual de Campinas SP Campinas13083-859 Brazil Jodrell Bank Center for Astrophysics School of Physics and Astronomy University of Manchester Oxford Road ManchesterM13 9PL United Kingdom Department of Physics & Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States SLAC Na

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+0.032−0.024 in ΛCdM, mean with 68% confidence limits;S8 = 0.775+0.26−0.24, 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 to 0.48. We find better agreement between dES 3×2pt and Planck than

关键词： Galaxies

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SPT clusters with dES and HST weak lensing. II. Cosmological constraints from the abundance of massive halos

引用

Physical Review d 2024年第8期110卷 083510页

作者： S. Bocquet S. Grandis L. E. Bleem M. Klein J. J. Mohr T. Schrabback T. M. C. Abbott P. A. R. Ade M. Aguena A. Alarcon S. Allam S. W. Allen O. Alves A. Amon A. J. Anderson J. Annis B. Ansarinejad J. E. Austermann S. Avila d. Bacon M. Bayliss J. A. Beall K. Bechtol M. R. Becker A. N. Bender B. A. Benson G. M. Bernstein S. Bhargava F. Bianchini M. Brodwin d. Brooks L. Bryant A. Campos R. E. A. Canning J. E. Carlstrom A. Carnero Rosell M. Carrasco Kind J. Carretero F. J. Castander R. Cawthon C. L. Chang C. Chang P. Chaubal R. Chen H. C. Chiang A. Choi T-L. Chou R. Citron C. Corbett Moran J. Cordero M. Costanzi T. M. Crawford A. T. Crites L. N. da Costa M. E. S. Pereira C. davis T. M. davis J. deRose S. desai T. de Haan H. T. diehl M. A. dobbs S. dodelson C. doux A. drlica-Wagner K. Eckert J. Elvin-Poole S. Everett W. Everett I. Ferrero A. Ferté A. M. Flores J. Frieman J. Gallicchio J. García-Bellido M. Gatti E. M. George G. Giannini M. d. Gladders d. Gruen R. A. Gruendl N. Gupta G. Gutierrez N. W. Halverson I. Harrison W. G. Hartley K. Herner S. R. Hinton G. P. Holder d. L. Hollowood W. L. Holzapfel K. Honscheid J. d. Hrubes N. Huang J. Hubmayr E. M. Huff d. Huterer K. d. Irwin d. J. James M. Jarvis G. Khullar K. Kim L. Knox R. Kraft E. Krause K. Kuehn N. Kuropatkin F. Kéruzoré O. Lahav A. T. Lee P.-F. Leget d. Li H. Lin A. Lowitz N. MacCrann G. Mahler A. Mantz J. L. Marshall J. McCullough M. Mcdonald J. J. McMahon J. Mena-Fernández F. Menanteau S. S. Meyer R. Miquel J. Montgomery J. Myles T. Natoli A. Navarro-Alsina J. P. Nibarger G. I. Noble V. Novosad R. L. C. Ogando Y. Omori S. Padin S. Pandey P. Paschos S. Patil A. Pieres A. A. Plazas Malagón A. Porredon J. Prat C. Pryke M. Raveri C. L. Reichardt J. Roberson R. P. Rollins C. Romero A. Roodman J. E. Ruhl E. S. Rykoff B. R. Saliwanchik L. Salvati C. Sánchez E. Sanchez d. Sanchez Cid A. Saro K. K. Schaffer L. F. Secco I. Sevilla-Noarbe K. Sharon E. Sheldon T. Shin C. Sievers G. Smecher M. Smith T. Somboonpanyakul M. Sommer B. Stalder A. A. Stark J. Stephen V. Straz University Observatory Faculty of Physics Universität Innsbruck Institut für Astro- und Teilchenphysik Technikerstraße 25/8 6020 Innsbruck Austria High-Energy Physics Division Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA Max Planck Institute for Extraterrestrial Physics Gießenbachstraße 1 85748 Garching Germany Argelander-Institut für Astronomie Auf dem Hügel 71 53121 Bonn Germany Cerro Tololo Inter-American Observatory NSF’s National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile School of Physics and Astronomy Cardiff University Cardiff CF24 3YB United Kingdom Laboratório Interinstitucional de e-Astronomia—LIneA Rua Gal. José Cristino 77 Rio de Janeiro Rio de Janeiro—20921-400 Brazil Fermi National Accelerator Laboratory P. O. Box 500 Batavia Illinois 60510 USA Kavli Institute for Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall Stanford California 94305 USA Department of Physics Stanford University 382 Via Pueblo Mall Stanford California 94305 USA SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo Park California 94025 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Institute of Astronomy University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom School of Physics University of Melbourne Parkville Victoria 3010 Australia NIST Quantum Devices Group 325 Broadway Mailcode 817.03 Boulder Colorado 80305 USA Department of Physics University of Colorado Boulder Colorado 80309 USA Institut de Física d’Altes Energies (IFAE) The Barcelona Institute of Science and Technology Campus UAB 08193 Bellaterra (Barcelona) Spain Institute of Cosmology and Gravitation University of Portsmouth Portsmouth

We present cosmological constraints from the abundance of galaxy clusters selected via the thermal Sunyaev-Zel’dovich (SZ) effect in South Pole Telescope (SPT) data with a simultaneous mass calibration using weak gravitational lensing data from the dark Energy Survey (dES) and the Hubble Space Telescope (HST). The cluster sample is constructed from the combined SPT-SZ, SPTpol ECS, and SPTpol 500d surveys, and comprises 1,005 confirmed clusters in the redshift range 0.25–1.78 over a total sky area of 5200 deg2. We use dES Year 3 weak-lensing data for 688 clusters with redshifts z<0.95 and HST weak-lensing data for 39 clusters with 0.6d allow us to empirically constrain the SZ observable-mass relation without having to make strong assumptions about, e.g., the hydrodynamical state of the clusters. For a flat ΛCdM cosmology, and marginalizing over the sum of massive neutrinos, we measure Ωm=0.286±0.032, σ8=0.817±0.026, and the parameter combination σ8(Ωm/0.3)0.25=0.805±0.016. Our measurement of S8≡σ8Ωm/0.3=0.795±0.029 and the constraint from Planck CMB anisotropies (2018 TT, TE, EE+lowE) differ by 1.1σ. In combination with that Planck dataset, we place a 95% upper limit on the sum of neutrino masses ∑mν<0.18 eV. When additionally allowing the dark energy equation of state parameter w to vary, we obtain w=−1.45±0.31 from our cluster-based analysis. In combination with Planck data, we measure w=−1.34−0.15+0.22, or a 2.2σ difference with a cosmological constant. We use the cluster abundance to measure σ8 in five redshift bins between 0.25 and 1.8, and we find the results to be consistent with structure growth as predicted by the ΛCdM model fit to Planck primary CMB data.

关键词： Cosmological parameters dark energy Large scale structure of the Universe Galaxy clusters

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dark Energy Survey Year 3 Results: Constraints on extensions to ΛCdM with weak lensing and galaxy clustering

arXiv

引用

arXiv 2022年

作者： Abbott, T.M.C. Aguena, M. Alarcon, A. Alves, O. Amon, A. Andrade-Oliveira, F. Annis, J. Avila, S. Bacon, d. Baxter, E. Bechtol, K. Becker, M.R. Bernstein, G.M. Birrer, S. Blazek, J. Bocquet, S. Brandao-Souza, A. Bridle, S.L. Brooks, d. Burke, d.L. Camacho, H. Campos, A. Carnero Rosell, A. Carrasco Kind, M. Carretero, J. Castander, F.J. Cawthon, R. Chang, C. Chen, A. Chen, R. Choi, A. Conselice, C. Cordero, J. Costanzi, M. Crocce, M. da Costa, L.N. Pereira, M.E.S. davis, C. davis, T.M. deRose, J. desai, S. di Valentino, E. diehl, H.T. dodelson, S. doel, P. doux, C. drlica-Wagner, A. Eckert, K. Eifler, T.F. Elsner, F. Elvin-Poole, J. Everett, S. Fang, X. Farahi, A. Ferrero, I. Ferté, A. Flaugher, B. Fosalba, P. Friedel, d. Friedrich, O. Frieman, J. García-Bellido, J. Gatti, M. Giani, L. Giannantonio, T. Giannini, G. Gruen, d. Gruendl, R.A. Gschwend, J. Gutierrez, G. Hamaus, N. Harrison, I. Hartley, W.G. Herner, K. Hinton, S.R. Hollowood, d.L. Honscheid, K. Huang, H. Huff, E.M. Huterer, d. Jain, B. James, d.J. Jarvis, M. Jeffrey, N. Jeltema, T. Kovacs, A. Krause, E. Kuehn, K. Kuropatkin, N. Lahav, O. Lee, S. Leget, P.-F. Lemos, P. Leonard, C.d. Liddle, A.R. Lima, M. Lin, H. MacCrann, N. Marshall, J.L. McCullough, J. Mena-Fernández, J. Menanteau, F. Miquel, R. Miranda, V. Mohr, J.J. Muir, Jessica Myles, J. Nadathur, S. Navarro-Alsina, A. Nichol, R.C. Ogando, R.L.C. Omori, Y. Palmese, A. Pandey, S. Park, Y. Paterno, M. Paz-Chinchón, F. Percival, W.J. Pieres, A. Plazas Malagón, A.A. Porredon, A. Prat, J. Raveri, M. Rodriguez-Monroy, M. Rogozenski, P. Rollins, R.P. Romer, A.K. Roodman, A. Rosenfeld, R. Ross, A.J. Rykoff, E.S. Samuroff, S. Sánchez, C. Sanchez, E. Sanchez, J. Sanchez Cid, d. Scarpine, V. Scolnic, d. Secco, L.F. Sevilla-Noarbe, I. Sheldon, E. Shin, T. Smith, M. Soares-Santos, M. Suchyta, E. Tabbutt, M. Tarle, G. Thomas, d. To, C. Troja, A. Troxel, M.A. Tutusaus, I. Varga, T.N. Vincenzi, M. Walker, A.R. Weaverdyck, N. Wechsler, R.H. Weller, J. Yanny, B. Yin, B. Zhang, Y. Zuntz, J. Cerro Tololo Inter-American Observatory NSF’s National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 RJ Rio de Janeiro20921-400 Brazil Argonne National Laboratory 9700 South Cass Avenue LemontIL60439 United States Department of Physics University of Michigan Ann ArborMI48109 United States Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Instituto de Fisica Teorica UAM CSIC Universidad Autonoma de Madrid Madrid28049 Spain Institute of Cosmology and Gravitation University of Portsmouth PortsmouthPO1 3FX United Kingdom Institute for Astronomy University of Hawai’i 2680 Woodlawn Drive HonoluluHI96822 United States Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue MadisonWI53706-1390 United States Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Department of Physics Northeastern University BostonMA02115 United States University Observatory Faculty of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 Munich81679 Germany Instituto de Física Gleb Wataghin Universidade Estadual de Campinas SP Campinas13083-859 Brazil Jodrell Bank Center for Astrophysics School of Physics and Astronomy University of Manchester Oxford Road ManchesterM13 9PL United Kingdom Department of Physics & Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Instituto de Física Teórica Universidade Estadual Paulista

We constrain six possible extensions to the ΛCdM model using measurements from the dark Energy Survey’s first three years of observations, alone and in combination with external cosmological probes. The dES data are the two-point correlation functions of weak gravitational lensing, galaxy clustering, and their cross-correlation. We use simulated data vectors and blind analyses of real data to validate the robustness of our results to astrophysical and modeling systematic errors. In many cases, constraining power is limited by the absence of theoretical predictions beyond the linear regime that are reliable at our required precision. The ΛCdM extensions are: dark energy with a time-dependent equation of state, non-zero spatial curvature, additional relativistic degrees of freedom, sterile neutrinos with eV-scale mass, modifications of gravitational physics, and a binned σ8(z) model which serves as a phenomenological probe of structure growth. For the time-varying dark energy equation of state evaluated at the pivot redshift we find (wp, wa) = (−0.99+0−0.2817, −0.9 ± 1.2) at 68% confidence with zp = 0.24 from the dES measurements alone, and (wp, wa) = (−1.03+0−0.0403, −0.4+0−0.43) with zp = 0.21 for the combination of all data considered. Curvature constraints of Ωk = 0.0009 ± 0.0017 and effective relativistic species Neff = 3.10+0−0.1516 are dominated by external data, though adding dES information to external low redshift probes tightens the Ωk constraints that can be made without CMB observables by 20%. For massive sterile neutrinos, dES combined with external data improves the upper bound on the mass meff by a factor of three compared to previous analyses, giving 95% limits of (∆Neff , meff ) ≤ (0.28, 0.20 eV) when using priors matching a comparable Planck analysis. For modified gravity, we constrain changes to the lensing and Poisson equations controlled by functions Σ(k, z) = Σ0ΩΛ(z)/ΩΛ,0 and µ(k, z) = µ0ΩΛ(z)/ΩΛ,0 respectively to Σ0 = 0.6+0−0.45 from dES alone

关键词： Probes

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