%0 Generic %1 secco2021energy %A Secco, L. F. %A Samuroff, S. %A Krause, E. %A Jain, B. %A Blazek, J. %A Raveri, M. %A Campos, A. %A Amon, A. %A Chen, A. %A Doux, C. %A Choi, A. %A Gruen, D. %A Bernstein, G. M. %A Chang, C. %A DeRose, J. %A Myles, J. %A Ferté, A. %A Lemos, P. %A Huterer, D. %A Prat, J. %A Troxel, M. A. %A MacCrann, N. %A Liddle, A. R. %A Kacprzak, T. %A Fang, X. %A Sánchez, C. %A Pandey, S. %A Dodelson, S. %A Chintalapati, P. %A Hoffmann, K. %A Alarcon, A. %A Alves, O. %A Andrade-Oliveira, F. %A Baxter, E. J. %A Bechtol, K. %A Becker, M. R. %A Brandao-Souza, A. %A Camacho, H. %A Rosell, A. Carnero %A Kind, M. Carrasco %A Cawthon, R. %A Cordero, J. P. %A Crocce, M. %A Davis, C. %A Di Valentino, E. %A Drlica-Wagner, A. %A Eckert, K. %A Eifler, T. F. %A Elidaiana, M. %A Elsner, F. %A Elvin-Poole, J. %A Everett, S. %A Fosalba, P. %A Friedrich, O. %A Gatti, M. %A Giannini, G. %A Gruendl, R. A. %A Harrison, I. %A Hartley, W. G. %A Herner, K. %A Huang, H. %A Huff, E. M. %A Jarvis, M. %A Jeffrey, N. %A Kuropatkin, N. %A Leget, P. F. %A Muir, J. %A Mccullough, J. %A Alsina, A. Navarro %A Omori, Y. %A Park, Y. %A Porredon, A. %A Rollins, R. %A Roodman, A. %A Rosenfeld, R. %A Ross, A. J. %A Rykoff, E. S. %A Sanchez, J. %A Sevilla-Noarbe, I. %A Sheldon, E. S. %A Shin, T. %A Tutusaus, I. %A Varga, T. N. %A Weaverdyck, N. %A Wechsler, R. H. %A Yanny, B. %A Yin, B. %A Zhang, Y. %A Zuntz, J. %A Abbott, T. M. C. %A Aguena, M. %A Allam, S. %A Annis, J. %A Bacon, D. %A Bertin, E. %A Bhargava, S. %A Bridle, S. L. %A Brooks, D. %A Buckley-Geer, E. %A Burke, D. L. %A Carretero, J. %A Costanzi, M. %A da Costa, L. N. %A De Vicente, J. %A Diehl, H. T. %A Dietrich, J. P. %A Doel, P. %A Ferrero, I. %A Flaugher, B. %A Frieman, J. %A García-Bellido, J. %A Gaztanaga, E. %A Gerdes, D. W. %A Giannantonio, T. %A Gschwend, J. %A Gutierrez, G. %A Hinton, S. R. %A Hollowood, D. L. %A Honscheid, K. %A Hoyle, B. %A James, D. J. %A Jeltema, T. %A Kuehn, K. %A Lahav, O. %A Lima, M. %A Lin, H. %A Maia, M. A. G. %A Marshall, J. L. %A Martini, P. %A Melchior, P. %A Menanteau, F. %A Miquel, R. %A Mohr, J. J. %A Morgan, R. %A Ogando, R. L. C. %A Palmese, A. %A Paz-Chinchón, F. %A Petravick, D. %A Pieres, A. %A Malagón, A. A. Plazas %A Rodriguez-Monroy, M. %A Romer, A. K. %A Sanchez, E. %A Scarpine, V. %A Schubnell, M. %A Scolnic, D. %A Serrano, S. %A Smith, M. %A Soares-Santos, M. %A Suchyta, E. %A Swanson, M. E. C. %A Tarle, G. %A Thomas, D. %A To, C. %D 2021 %K library %T Dark Energy Survey Year 3 Results: Cosmology from Cosmic Shear and Robustness to Modeling Uncertainty %U http://arxiv.org/abs/2105.13544 %X This work and its companion paper, Amon et al. (2021), present cosmic shear measurements and cosmological constraints from over 100 million source galaxies in the Dark Energy Survey (DES) Year 3 data. We constrain the lensing amplitude parameter $S_8\equiv\sigma_8Ømega_\textrmm/0.3$ at the 3% level in $Łambda$CDM: $S_8=0.759^+0.025_-0.023$ (68% CL). Our constraint is at the 2% level when using angular scale cuts that are optimized for the $Łambda$CDM analysis: $S_8=0.772^+0.018_-0.017$ (68% CL). With cosmic shear alone, we find no statistically significant constraint on the dark energy equation-of-state parameter at our present statistical power. We carry out our analysis blind, and compare our measurement with constraints from two other contemporary weak-lensing experiments: the Kilo-Degree Survey (KiDS) and Hyper-Suprime Camera Subaru Strategic Program (HSC). We additionally quantify the agreement between our data and external constraints from the Cosmic Microwave Background (CMB). Our DES Y3 result under the assumption of $Łambda$CDM is found to be in statistical agreement with Planck 2018, although favors a lower $S_8$ than the CMB-inferred value by $2.3\sigma$ (a $p$-value of 0.02). This paper explores the robustness of these cosmic shear results to modeling of intrinsic alignments, the matter power spectrum and baryonic physics. We additionally explore the statistical preference of our data for intrinsic alignment models of different complexity. The fiducial cosmic shear model is tested using synthetic data, and we report no biases greater than 0.3$\sigma$ in the plane of $S_8\timesØmega_m$ caused by uncertainties in the theoretical models.

@misc{secco2021energy, abstract = {This work and its companion paper, Amon et al. (2021), present cosmic shear measurements and cosmological constraints from over 100 million source galaxies in the Dark Energy Survey (DES) Year 3 data. We constrain the lensing amplitude parameter $S_8\equiv\sigma_8\sqrt{\Omega_\textrm{m}/0.3}$ at the 3% level in $\Lambda$CDM: $S_8=0.759^{+0.025}_{-0.023}$ (68% CL). Our constraint is at the 2% level when using angular scale cuts that are optimized for the $\Lambda$CDM analysis: $S_8=0.772^{+0.018}_{-0.017}$ (68% CL). With cosmic shear alone, we find no statistically significant constraint on the dark energy equation-of-state parameter at our present statistical power. We carry out our analysis blind, and compare our measurement with constraints from two other contemporary weak-lensing experiments: the Kilo-Degree Survey (KiDS) and Hyper-Suprime Camera Subaru Strategic Program (HSC). We additionally quantify the agreement between our data and external constraints from the Cosmic Microwave Background (CMB). Our DES Y3 result under the assumption of $\Lambda$CDM is found to be in statistical agreement with Planck 2018, although favors a lower $S_8$ than the CMB-inferred value by $2.3\sigma$ (a $p$-value of 0.02). This paper explores the robustness of these cosmic shear results to modeling of intrinsic alignments, the matter power spectrum and baryonic physics. We additionally explore the statistical preference of our data for intrinsic alignment models of different complexity. The fiducial cosmic shear model is tested using synthetic data, and we report no biases greater than 0.3$\sigma$ in the plane of $S_8\times\Omega_\textrm{m}$ caused by uncertainties in the theoretical models.}, added-at = {2021-05-31T08:28:27.000+0200}, author = {Secco, L. F. and Samuroff, S. and Krause, E. and Jain, B. and Blazek, J. and Raveri, M. and Campos, A. and Amon, A. and Chen, A. and Doux, C. and Choi, A. and Gruen, D. and Bernstein, G. M. and Chang, C. and DeRose, J. and Myles, J. and Ferté, A. and Lemos, P. and Huterer, D. and Prat, J. and Troxel, M. A. and MacCrann, N. and Liddle, A. R. and Kacprzak, T. and Fang, X. and Sánchez, C. and Pandey, S. and Dodelson, S. and Chintalapati, P. and Hoffmann, K. and Alarcon, A. and Alves, O. and Andrade-Oliveira, F. and Baxter, E. J. and Bechtol, K. and Becker, M. R. and Brandao-Souza, A. and Camacho, H. and Rosell, A. Carnero and Kind, M. Carrasco and Cawthon, R. and Cordero, J. P. and Crocce, M. and Davis, C. and Di Valentino, E. and Drlica-Wagner, A. and Eckert, K. and Eifler, T. F. and Elidaiana, M. and Elsner, F. and Elvin-Poole, J. and Everett, S. and Fosalba, P. and Friedrich, O. and Gatti, M. and Giannini, G. and Gruendl, R. A. and Harrison, I. and Hartley, W. G. and Herner, K. and Huang, H. and Huff, E. M. and Jarvis, M. and Jeffrey, N. and Kuropatkin, N. and Leget, P. F. and Muir, J. and Mccullough, J. and Alsina, A. Navarro and Omori, Y. and Park, Y. and Porredon, A. and Rollins, R. and Roodman, A. and Rosenfeld, R. and Ross, A. J. and Rykoff, E. S. and Sanchez, J. and Sevilla-Noarbe, I. and Sheldon, E. S. and Shin, T. and Tutusaus, I. and Varga, T. N. and Weaverdyck, N. and Wechsler, R. H. and Yanny, B. and Yin, B. and Zhang, Y. and Zuntz, J. and Abbott, T. M. C. and Aguena, M. and Allam, S. and Annis, J. and Bacon, D. and Bertin, E. and Bhargava, S. and Bridle, S. L. and Brooks, D. and Buckley-Geer, E. and Burke, D. L. and Carretero, J. and Costanzi, M. and da Costa, L. N. and De Vicente, J. and Diehl, H. T. and Dietrich, J. P. and Doel, P. and Ferrero, I. and Flaugher, B. and Frieman, J. and García-Bellido, J. and Gaztanaga, E. and Gerdes, D. W. and Giannantonio, T. and Gschwend, J. and Gutierrez, G. and Hinton, S. R. and Hollowood, D. L. and Honscheid, K. and Hoyle, B. and James, D. J. and Jeltema, T. and Kuehn, K. and Lahav, O. and Lima, M. and Lin, H. and Maia, M. A. G. and Marshall, J. L. and Martini, P. and Melchior, P. and Menanteau, F. and Miquel, R. and Mohr, J. J. and Morgan, R. and Ogando, R. L. C. and Palmese, A. and Paz-Chinchón, F. and Petravick, D. and Pieres, A. and Malagón, A. A. Plazas and Rodriguez-Monroy, M. and Romer, A. K. and Sanchez, E. and Scarpine, V. and Schubnell, M. and Scolnic, D. and Serrano, S. and Smith, M. and Soares-Santos, M. and Suchyta, E. and Swanson, M. E. C. and Tarle, G. and Thomas, D. and To, C.}, biburl = {https://www.bibsonomy.org/bibtex/2ad81df31cc06bd593986f62290997251/gpkulkarni}, description = {Dark Energy Survey Year 3 Results: Cosmology from Cosmic Shear and Robustness to Modeling Uncertainty}, interhash = {ef11e16fc1e7ec201137010e09c74ed5}, intrahash = {ad81df31cc06bd593986f62290997251}, keywords = {library}, note = {cite arxiv:2105.13544Comment: 32+9 pages, 13+4 figures, see https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 cosmology release}, timestamp = {2021-05-31T08:28:27.000+0200}, title = {Dark Energy Survey Year 3 Results: Cosmology from Cosmic Shear and Robustness to Modeling Uncertainty}, url = {http://arxiv.org/abs/2105.13544}, year = 2021 }