Joint analysis of Dark Energy Survey Year 3 data and CMB lensing from SPT and P l a n c k . II. Cross-correlation measurements and cosmological constraints

Journal Article · 31 January 2023 · Physical Review. D.

DOI: https://doi.org/10.1103/physrevd.107.023530 · OSTI ID:1995666

Chang, C.  ^[1]; Omori, Y.; Baxter, E.  J.; Doux, C.; Choi, A.; Pandey, S.; Alarcon, A.; Alves, O.; Amon, A.; Andrade-Oliveira, F.; Bechtol, K.; Becker, M.  R.; Bernstein, G.  M.; Bianchini, F.; Blazek, J.; Bleem, L.  E.; Camacho, H.; Campos, A.; Carnero Rosell, A.; Carrasco Kind, M. ; Cawthon, R.; Chen, R.; Cordero, J.; Crawford, T.  M.; Crocce, M.; Davis, C.; DeRose, J.; Dodelson, S.; Drlica-Wagner, A.; Eckert, K.; Eifler, T.  F.; Elsner, F.; Elvin-Poole, J.; Everett, S.; Fang, X.; Ferté, A.; Fosalba, P.; Friedrich, O.; Gatti, M.; Giannini, G.; Gruen, D.; Gruendl, R.  A.; Harrison, I.; Herner, K.; Huang, H.; Huff, E.  M.; Huterer, D.; Jarvis, M.; Kovacs, A.; Krause, E.; Kuropatkin, N.; Leget, P. -F.; Lemos, P.; Liddle, A.  R.; MacCrann, N.; McCullough, J.; Muir, J.; Myles, J.; Navarro-Alsina, A.; Park, Y.; Porredon, A.; Prat, J.; Raveri, M.; Rollins, R.  P.; Roodman, A.; Rosenfeld, R.; Ross, A.  J.; Rykoff, E.  S.; Sánchez, C.; Sanchez, J.; Secco, L.  F.; Sevilla-Noarbe, I.; Sheldon, E.; Shin, T.; Troxel, M.  A.; Tutusaus, I.; Varga, T.  N.; Weaverdyck, N.; Wechsler, R.  H.; Wu, W.  L. K.; Yanny, B.; Yin, B.; Zhang, Y.; Zuntz, J.; Abbott, T.  M. C.; Aguena, M.; Allam, S.; Annis, J.; Bacon, D.; Benson, B.  A.; Bertin, E.; Bocquet, S.; Brooks, D.; Burke, D.  L.; Carlstrom, J.  E.; Carretero, J.; Chang, C.  L.; Chown, R.; Costanzi, M.; da Costa, L.  N.; Crites, A.  T.; Pereira, M.  E. S.; de Haan, T.; De Vicente, J.; Desai, S.; Diehl, H.  T.; Dobbs, M.  A.; Doel, P.; Everett, W.; Ferrero, I.; Flaugher, B.; Friedel, D.; Frieman, J.; García-Bellido, J.; Gaztanaga, E.; George, E.  M.; Giannantonio, T.; Halverson, N.  W.; Hinton, S.  R.; Holder, G.  P.; Hollowood, D.  L.; Holzapfel, W.  L.; Honscheid, K.; Hrubes, J.  D.; James, D.  J.; Knox, L.; Kuehn, K.; Lahav, O.; Lee, A.  T.; Lima, M.; Luong-Van, D.; March, M.; McMahon, J.  J.; Melchior, P.; Menanteau, F.; Meyer, S.  S.; Miquel, R.; Mocanu, L.; Mohr, J.  J.; Morgan, R.; Natoli, T.; Padin, S.; Palmese, A.; Paz-Chinchón, F.; Pieres, A.; Plazas Malagón, A.  A.; Pryke, C.; Reichardt, C.  L.; Rodríguez-Monroy, M.; Romer, A.  K.; Ruhl, J.  E.; Sanchez, E.; Schaffer, K.  K.; Schubnell, M.; Serrano, S.; Shirokoff, E.; Smith, M.; Staniszewski, Z.; Stark, A.  A.; Suchyta, E.; Tarle, G.; Thomas, D.; To, C.; Vieira, J.  D.; Weller, J.; Williamson, R.

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1. University of Chicago, IL (United States). Kavli Institute for Cosmological Physics (KICP). DES Collaboration et al.; SPT Collaboration et al.

Cross-correlations of galaxy positions and galaxy shears with maps of gravitational lensing of the cosmic microwave background (CMB) are sensitive to the distribution of large-scale structure in the Universe. Such cross-correlations are also expected to be immune to some of the systematic effects that complicate correlation measurements internal to galaxy surveys. We present measurements and modeling of the cross-correlations between galaxy positions and galaxy lensing measured in the first three years of data from the Dark Energy Survey with CMB lensing maps derived from a combination of data from the 2500 deg² SPT-SZ survey conducted with the South Pole Telescope and full-sky data from the Planck satellite. The CMB lensing maps used in this analysis have been constructed in a way that minimizes biases from the thermal Sunyaev Zel’dovich effect, making them well suited for cross-correlation studies. The total signal-to-noise of the cross-correlation measurements is 23.9 (25.7) when using a choice of angular scales optimized for a linear (nonlinear) galaxy bias model. Here we use the cross-correlation measurements to obtain constraints on cosmological parameters. For our fiducial galaxy sample, which consist of four bins of magnitude-selected galaxies, we find constraints of Ω_m=0.272$$^{+0.032}_{-0.052}$$ and S₈≡σ8$$\sqrt{Ω_m/0.3}$$=0.736$$^{+0.032}_{-0.028}$$ (Ω_m=0.245$$^{+0.026}_{-0.044}$$ and S₈=0.734$$^{+0.035}_{-0.028}$$) when assuming linear (nonlinear) galaxy bias in our modeling. Considering only the cross-correlation of galaxy shear with CMB lensing, we find Ω_m=0.270$$^{+0.043}_{-0.061}$$ and S₈=0.740$$^{+0.034}_{-0.029}$$. Our constraints on S8 are consistent with recent cosmic shear measurements, but lower than the values preferred by primary CMB measurements from Planck.

• Research Organization: Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States); Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Univ. of Michigan, Ann Arbor, MI (United States)
• Sponsoring Organization: USDOE Office of Science (SC), High Energy Physics (HEP)
• Contributing Organization: DES Collaboration; SPT Collaboration
• Grant/Contract Number: AC05-00OR22725; AC02-07CH11359; SC0012704; SC0021949; AC02-06CH11357; SC0019193
• OSTI ID: 1995666
• Alternate ID(s): OSTI ID: 1861823; OSTI ID: 1922878; OSTI ID: 2350562; OSTI ID: 2352221
• Report Number(s): FERMILAB-PUB-22-098-PPD; arXiv:2203.12440; DES-2021-0648; TRN: US2405075
• Journal Information: Physical Review. D., Vol. 107, Issue 2; ISSN 2470-0010
• Publisher: American Physical Society (APS)Copyright Statement
• Country of Publication: United States
• Language: English