A. Chen, G. Aricò, D. Huterer, R. E. Angulo, N. Weaverdyck, O. Friedrich, L. F. Secco, C. Hernández-Monteagudo, A. Alarcon, O. Alves, A. Amon, F. Andrade-Oliveira, E. J. Baxter, K. Bechtol, M. R. Becker, G. M. Bernstein, J. Blazek, A. Brandao-Souza, S. L. Bridle, H. Camacho, A. Campos, A. Carnero Rosell, M. Carrasco Kind, R. Cawthon, C. Chang, R. Chen, P. Chintalapati, A. Choi, J. P. Cordero, M. Crocce, M. E. S. Pereira, C. Davis, J. DeRose, E. Di Valentino, H. T. Diehl, S. Dodelson, C. Doux, A. Drlica-Wagner, K. Eckert, T. F. Eifler, F. Elsner, J. Elvin-Poole, S. Everett, X. Fang, A. Ferté, P. Fosalba, M. Gatti, E. Gaztanaga, G. Giannini, D. Gruen, R. A. Gruendl, I. Harrison, W. G. Hartley, K. Herner, K. Hoffmann, H. Huang, E. M. Huff, B. Jain, M. Jarvis, N. Jeffrey, T. Kacprzak, E. Krause, N. Kuropatkin, P. -F. Leget, P. Lemos, A. R. Liddle, N. MacCrann, J. Mccullough, J. Muir, J. Myles, A. Navarro-Alsina, Y. Omori, S. Pandey, Y. Park, A. Porredon, J. Prat, M. Raveri, A. Refregier, R. P. Rollins, A. Roodman, R. Rosenfeld, A. J. Ross, E. S. Rykoff, S. Samuroff, C. Sánchez, J. Sanchez, I. Sevilla-Noarbe, E. Sheldon, T. Shin, A. Troja, M. A. Troxel, I. Tutusaus, T. N. Varga, R. H. Wechsler, B. Yanny, B. Yin, Y. Zhang, J. Zuntz, M. Aguena, J. Annis, D. Bacon, E. Bertin, S. Bocquet, D. Brooks, D. L. Burke, J. Carretero, C. J. Conselice, M. Costanzi, L. N. da Costa, J. De Vicente, S. Desai, P. Doel, I. Ferrero, B. Flaugher, J. A. Frieman, J. García-Bellido, D. Gerdes, T. Giannantonio, J. Gschwend, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, O. Lahav, M. March, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, F. Paz-Chinchón, A. Pieres, E. Sanchez, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, D. Thomas, C. To, DES Collaboration
Abstract
We use the small scales of the Dark Energy Survey (DES) Year-3 cosmic shear measurements, which are excluded from the DES Year-3 cosmological analysis, to constrain the baryonic feedback. To model the baryonic feedback, we adopt a baryonic correction model and use the numerical package baccoemu to accelerate the evaluation of the baryonic non-linear 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>1013.2 h−1 M⊙ (95 per cent C.L.). The best-fitting baryonic suppression is ∼5 per cent at k=1.0Mpc h−1 and ∼15 per cent 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.
Keywords
gravitational lensing: weak, large-scale structure of Universe, cosmology: observations
Monthly Notices of the Royal Astronomical Society
Volume 518, Issue 4, Page 5340
2023 February
