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

Chang, C.; 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.; FertÃ©, 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.; SÃ¡nchez, 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.; GarcÃ­a-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-ChinchÃ³n, F.; Pieres, A.; Plazas MalagÃ³n, A. A.; Pryke, C.; Reichardt, C. L.; RodrÃ­guez-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.; DES; SPT Collaborations

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

Chang, C.

•

Omori, Y.

•

Baxter, E. J.

altro

SPT Collaborations

2023

journal article

Periodico

PHYSICAL REVIEW D

Abstract

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. 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 omega m 1/4 0.272 thorn 0.032 pffiffiffiffiffiffiffiffiffiffiffiffiffiffi-0.052 and S8 equivalent to sigma 8 omega m=0.3 1/4 0.736 thorn 0.032 -0.028 (omega m 1/40.245 thorn 0.0-0.04426 and S8 1/40.734 thorn 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 omega m 1/4 0.270 thorn 0.043 -0.061 and S8 1/4 0.740 thorn 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.