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Joint analysis of Dark Energy Survey Year 3 data and CMB lensing from SPT and Planck . 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., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruen, D., Gruendl, R.A., Harrison, Ian ORCID:, 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. and Williamson, R. 2023. Joint analysis of Dark Energy Survey Year 3 data and CMB lensing from SPT and Planck . II. Cross-correlation measurements and cosmological constraints. Physical Review D 107 (2) , 023530. 10.1103/PhysRevD.107.023530

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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     deg 2 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 Ω m = 0.272 + 0.032 − 0.052 and S 8 ≡ σ 8 √ Ω m / 0.3 = 0.736 + 0.032 − 0.028 ( Ω m = 0.245 + 0.026 − 0.044 and S 8 = 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 S 8 = 0.740 + 0.034 − 0.029 . Our constraints on S 8 are consistent with recent cosmic shear measurements, but lower than the values preferred by primary CMB measurements from Planck.

Item Type: Article
Date Type: Published Online
Status: Published
Schools: Physics and Astronomy
Publisher: American Physical Society
ISSN: 2470-0010
Date of First Compliant Deposit: 28 March 2023
Date of Acceptance: 30 September 2022
Last Modified: 06 May 2023 15:45

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