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

Journal Article · Mon Nov 28 00:00:00 EST 2022 · Physical Review. D.

DOI:https://doi.org/10.1103/physrevd.106.103530· OSTI ID:1906914

Porredon, A.  ^[1]; Crocce, M.; Elvin-Poole, J.; Cawthon, R.; Giannini, G.; De Vicente, J.; Carnero Rosell, A.; Ferrero, I.; Krause, E.; Fang, X.; Prat, J.; Rodriguez-Monroy, M.; Pandey, S.; Pocino, A.; Castander, F.  J.; Choi, A.; Amon, A.; Tutusaus, I.; Dodelson, S.; Sevilla-Noarbe, I. ; Fosalba, P.; Gaztanaga, E.; Alarcon, A.; Alves, O.; Andrade-Oliveira, F.; Baxter, E.; Bechtol, K.; Becker, M.  R.; Bernstein, G.  M.; Blazek, J.; Camacho, H.; Campos, A.; Carrasco Kind, M.; Chintalapati, P.; Cordero, J.; DeRose, J.; Di Valentino, E.; Doux, C.; Eifler, T.  F.; Everett, S.; Ferté, A.; Friedrich, O.; Gatti, M.; Gruen, D.; Harrison, I.; Hartley, W.  G.; Herner, K.; Huff, E.  M.; Huterer, D.; Jain, B.; Jarvis, M.; Lee, S.; Lemos, P.; MacCrann, N.; Mena-Fernández, J.; Muir, J.; Myles, J.; Park, Y.; Raveri, M.; Rosenfeld, R.; Ross, A.  J.; Rykoff, E.  S.; Samuroff, S.; Sánchez, C.; Sanchez, E.; Sanchez, J.; Sanchez Cid, D.; Scolnic, D.; Secco, L.  F.; Sheldon, E.; Troja, A.; Troxel, M.  A.; Weaverdyck, N.; Yanny, B.; Zuntz, J.; Abbott, T.  M. C.; Aguena, M.; Allam, S.; Annis, J.; Avila, S.; Bacon, D.; Bertin, E.; Bhargava, S.; Brooks, D.; Buckley-Geer, E.; Burke, D.  L.; Carretero, J.; Costanzi, M.; da Costa, L.  N.; Pereira, M.  E. S.; Davis, T.  M.; Desai, S.; Diehl, H.  T.; Dietrich, J.  P.; Doel, P.; Drlica-Wagner, A.; Eckert, K.; Evrard, A.  E.; Flaugher, B.; Frieman, J.; García-Bellido, J.; Gerdes, D.  W.; Giannantonio, T.; Gruendl, R.  A.; Gschwend, J.; Gutierrez, G.; Hinton, S.  R.; Hollowood, D.  L.; Honscheid, K.; Hoyle, B.; James, D.  J.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Lidman, C.; Lima, M.; Lin, H.; Maia, M.  A. G.; Marshall, J.  L.; Martini, P.; Melchior, P.; Menanteau, F.; Miquel, R.; Mohr, J.  J.; Morgan, R.; Ogando, R.  L. C.; Palmese, A.; Paz-Chinchón, F.; Petravick, D.; Pieres, A.; Plazas Malagón, A.  A.; Romer, A.  K.; Santiago, B.; Scarpine, V.; Schubnell, M.; Serrano, S.; Smith, M.; Soares-Santos, M.; Suchyta, E.; Tarle, G.; Thomas, D.; To, C.; Varga, T.  N.; Weller, J.

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1. The Ohio State University, Columbus, OH (United States); Institute of Space Sciences (ICE, CSIC), Barcelona (Spain); Institut d’Estudis Espacials de Catalunya (IEEC), Barcelona (Spain). DES Collaboration. et al.

Two of the most sensitive probes of the large scale structure of the universe are the clustering of galaxies and the tangential shear of background galaxy shapes produced by those foreground galaxies, so-called galaxy-galaxy lensing. Combining the measurements of these two two-point functions leads to cosmological constraints that are independent of the galaxy bias factor. The optimal choice of foreground, or lens, galaxies is governed by the joint, but conflicting requirements to obtain accurate redshift information and large statistics. We present cosmological results from the full 5000 sq. deg² of the Dark Energy Survey first three years of observations (Y3) combining those two-point functions, using for the first time a magnitude-limited lens sample (MagLim) of 11 million galaxies especially selected to optimize such combination, and 100 million background shapes. We consider two cosmological models, flat ΛCDM and wCDM. In ΛCDM we obtain for the matter density Ω_m = 0.320$$^{+0.041}_{–0.034}$$ and for the clustering amplitude S₈ = σ₈(Ω_m/0.3)^0.5 = 0.778$$^{+0.037}_{–0.031}$$, at 68% C.L. The latter is only 1σ smaller than the prediction in this model informed by measurements of the cosmic microwave background by the Planck satellite. In wCDM we find Ω_m = 0.32$$^{+0.044}_{–0.046}$$, S₈ = 0.777$$^{+0.049}_{–0.051}$$, and dark energy equation of state w = –1.031$$^{+0.218}_{–0.379}$$. We find that including smaller scales while marginalizing over non-linear galaxy bias improves the constraining power in the Ω_m – S₈ plane by 31% and in the Ω_m – w plane by 41% while yielding consistent cosmological parameters from those in the linear bias case. Furthermore, these results are combined with those from cosmic shear in a companion paper to present full DES-Y3 constraints from the three two-point functions (3 x 2pt).

• Research Organization: Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States); SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States); Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States); Brookhaven National Laboratory (BNL), Upton, NY (United States)
• Sponsoring Organization: USDOE Office of Science (SC), High Energy Physics (HEP)
• Contributing Organization: DES Collaboration
• Grant/Contract Number: SC0010118; AC02-07CH11359; AC05-00OR22725
• OSTI ID: 1906914
• Alternate ID(s): OSTI ID: 1823528; OSTI ID: 1992717
• Report Number(s): FERMILAB-PUB-21-251-AE; arXiv:2105.13546; TRN: US2311772
• Journal Information: Physical Review. D., Vol. 106, Issue 10; ISSN 2470-0010
• Publisher: American Physical Society (APS)
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
cosmological parameters
cosmology
dark energy
dark matter
gravitational lenses
large scale structure of the universe
sky surveys