Mass calibration of DES Year-3 clusters via SPT-3G CMB cluster lensing

• Main Authors: Ansarinejad, B, Raghunathan, S, Abbott, T.M.C, Ade, P.A.R, Aguena, M, Alves, O, Anderson, A.J, Andrade-Oliveira, F, Archipley, M, Balkenhol, L, Benabed, K, Bender, A.N, Benson, B.A, Bertin, E, Bianchini, F, Bleem, L.E, Bocquet, S, Bouchet, F.R, Brooks, D, Bryant, L, Burke, D.L, Camphuis, E, Carlstrom, J.E, Carnero Rosell, A, Carretero, J, Castander, F.J, Cecil, T.W, Chang, C.L, Chaubal, P, Chichura, P.M, Chou, T.-L, Coerver, A, Costanzi, M, Crawford, T.M, Cukierman, A, da Costa, L.N, Daley, C, Davis, T.M, de Haan, T, Desai, S, de Vicente, J, Dibert, K.R, Dobbs, M.A, Doel, P, Doussot, A, Doux, C, Dutcher, D, Everett, W, Feng, C, Ferguson, K.R, Ferrero, I, Fichman, K, Foster, A, Frieman, J, Galli, S, Gambrel, A.E, García-Bellido, J, Gardner, R.W, Gaztanaga, E, Ge, F, Giannini, G, Goeckner-Wald, N, Grandis, S, Gruendl, R.A, Gualtieri, R, Guidi, F, Guns, S, Gutierrez, G, Halverson, N.W, Hinton, S.R, Hivon, E, Holder, G.P, Hollowood, D.L, Holzapfel, W.L, Honscheid, K, Hood, J.C, Huang, N, James, D.J, Kéruzoré, F, Knox, L, Korman, M, Kuo, C.-L, Lee, A.T, Lee, S, Levy, K, Lowitz, A.E, Lu, C, Maniyar, A, Marshall, J.L, Mena-Fernández, J, Menanteau, F, Miquel, R, Millea, M, Mohr, J.J, Montgomery, J, Nakato, Y, Natoli, T, Noble, G.I, Novosad, V, Ogando, R.L.C, Omori, Y, Padin, S, Palmese, A, Pan, Z, Paschos, P, Pereira, M.E.S, Pieres, A, Plazas Malagón, A.A, Prabhu, K, Quan, W, Rahlin, A, Rahimi, M, Reichardt, C.L, Reil, K, Romer, A.K, Rouble, M, Ruhl, J.E, Sanchez, E, Sanchez Cid, D, Schiappucci, E, Sevilla-Noarbe, I, Smecher, G, Smith, M, Sobrin, J.A, Stark, A.A, Stephen, J, Suchyta, E, Suzuki, A, Swanson, M.E.C, Tandoi, C, Tarle, G, Thompson, K.L, Thorne, B, Trendafilova, C, Tucker, C, Umilta, C, Vieira, J.D, Wang, G, Weaverdyck, N, Whitehorn, N, Wiseman., P, Wu, W.L.K, Yefremenko, V, Young, M.R, Zebrowski., J.A
• Other Authors: Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), DES, SPT
• Format: Report
• Language: English
• Published: HAL CCSD 2024
• Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]; South Pole; South pole
• Online Access: https://hal.science/hal-04531940

International audience We measure the stacked lensing signal in the direction of galaxy clusters in the Dark Energy Survey Year 3 (DES Y3) redMaPPer sample, using cosmic microwave background (CMB) temperature data from SPT-3G, the third-generation CMB camera on the South Pole Telescope (SPT). We estimate the lensing signal using temperature maps constructed from the initial 2 years of data from the SPT-3G 'Main' survey, covering 1500 deg$^2$ of the Southern sky. We then use this signal as a proxy for the mean cluster mass of the DES sample. In this work, we employ three versions of the redMaPPer catalogue: a Flux-Limited sample containing 8865 clusters, a Volume-Limited sample with 5391 clusters, and a Volume&Redshift-Limited sample with 4450 clusters. For the three samples, we find the mean cluster masses to be ${M}_{200{\rm{m}}}=1.66\pm0.13$ [stat.]$\pm0.03$ [sys.], $1.97\pm0.18$ [stat.]$\pm0.05$ [sys.], and $2.11\pm0.20$ [stat.]$\pm0.05$ [sys.]$\times{10}^{14}\ {\rm{M}}_{\odot }$, respectively. This is a factor of $\sim2$ improvement relative to the precision of measurements with previous generations of SPT surveys and the most constraining cluster mass measurements using CMB cluster lensing to date. Overall, we find no significant tensions between our results and masses given by redMaPPer mass-richness scaling relations of previous works, which were calibrated using CMB cluster lensing, optical weak lensing, and velocity dispersion measurements from various combinations of DES, SDSS and Planck data. We then divide our sample into 3 redshift and 3 richness bins, finding no significant tensions with optical weak-lensing calibrated masses in these bins. We forecast a $5.8\%$ constraint on the mean cluster mass of the DES Y3 sample with the complete SPT-3G surveys when using both temperature and polarization data and including an additional $\sim1400$ deg$^2$ of observations from the 'Extended' SPT-3G survey.