A measurement of the mean central optical depth of galaxy clusters via the pairwise kinematic Sunyaev-Zel'dovich effect with SPT-3G and DES
Creators: name: Schiappucci, E.
name: Bianchini, F.
name: Aguena, M.
name: Archipley, M.
name: Balkenhol, L.
name: Bleem, L. E.
name: Chaubal, P.
name: Crawford, T. M.
name: Grandis, S.
name: Omori, Y.
name: Reichardt, C. L.
name: Rozo, E.
name: Rykoff, E. S.
name: To, C.
name: Abbott, T. M. C.
name: Ade, P. A. R.
name: Alves, O.
name: Anderson, A. J.
name: Andrade-Oliveira, F.
name: Annis, J.
name: Avva, J. S.
name: Bacon, D.
name: Benabed, K.
name: Bender, A. N.
name: Benson, B. A.
name: Bernstein, G. M.
name: Bertin, E.
name: Bocquet, S.
name: Bouchet, F. R.
name: Brooks, D.
name: Burke, D. L.
name: Carlstrom, J. E.
name: Rosell, A. Carnero
name: Kind, M. Carrasco
name: Carretero, J.
name: Cecil, T. W.
name: Chang, C. L.
name: Chichura, P. M.
name: Chou, T. -L.
name: Costanzi, M.
name: Cukierman, A.
name: da Costa, L. N.
name: Daley, C.
name: de Haan, T.
name: Desai, S.
name: Dibert, K. R.
name: Diehl, H. T.
name: Dobbs, M. A.
name: Doel, P.
name: Doux, C.
name: Dutcher, D.
name: Everett, S.
name: Everett, W.
name: Feng, C.
name: Ferguson, K. R.
name: Ferrero, I.
name: Ferté, A.
name: Flaugher, B.
name: Foster, A.
name: Frieman, J.
name: Galli, S.
name: Gambrel, A. E.
name: García-Bellido, J.
name: Gardner, R. W.
name: Gatti, M.
name: Giannantonio, T.
name: Goeckner-Wald, N.
name: Gruen, D.
name: Gualtieri, R.
name: Guns, S.
name: Gutierrez, G.
name: Halverson, N. W.
name: Hinton, S. R.
name: Hivon, E.
name: Holder, G. P.
name: Hollowood, D. L.
name: Holzapfel, W. L.
name: Honscheid, K.
name: Hood, J. C.
name: Huang, N.
name: James, D. J.
name: Knox, L.
name: Korman, M.
name: Kuehn, K.
name: Kuo, C. -L.
name: Lahav, O.
name: Lee, A. T.
name: Lidman, C.
name: Lima, M.
name: Lowitz, A. E.
name: Lu, C.
name: March, M.
name: Mena-Fernández, J.
name: Menanteau, F.
name: Millea, M.
name: Miquel, R.
name: Mohr, J. J.
name: Montgomery, J.
name: Muir, J.
name: Natoli, T.
name: Noble, G. I.
name: Novosad, V.
name: Ogando, R. L. C.
name: Padin, S.
name: Pan, Z.
name: Paz-Chinchón, F.
name: Pereira, M. E. S.
name: Pieres, A.
name: Malagón, A. A. Plazas
name: Prabhu, K.
name: Prat, J.
name: Quan, W.
name: Rahlin, A.
name: Raveri, M.
name: Rodriguez-Monroy, M.
name: Romer, A. K.
name: Rouble, M.
name: Ruhl, J. E.
name: Sanchez, E.
name: Scarpine, V.
name: Schubnell, M.
name: Smecher, G.
name: Smith, M.
name: Soares-Santos, M.
name: Sobrin, J. A.
name: Suchyta, E.
name: Suzuki, A.
name: Tarle, G.
name: Thomas, D.
name: Thompson, K. L.
name: Thorne, B.
name: Tucker, C.
name: Umilta, C.
name: Vieira, J. D.
name: Vincenzi, M.
name: Wang, G.
name: Weaverdyck, N.
name: Weller, J.
name: Whitehorn, N.
name: Wu, W. L. K.
name: Yefremenko, V.
name: Young, M. R.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We infer the mean optical depth of a sample of optically-selected galaxy clusters from the Dark Energy Survey (DES) via the pairwise kinematic Sunyaev-Zel'dovich (kSZ) effect. The pairwise kSZ signal between pairs of clusters drawn from the DES Year-3 cluster catalog is detected at $4.1 σ$ in cosmic microwave background (CMB) temperature maps from two years of observations with the SPT-3G camera on the South Pole Telescope. After cuts, there are 24,580 clusters in the $\sim 1,400$ deg$^2$ of the southern sky observed by both experiments. We infer the mean optical depth of the cluster sample with two techniques. The optical depth inferred from the pairwise kSZ signal is $\barτ_e = (2.97 \pm 0.73) \times 10^{-3}$, while that inferred from the thermal SZ signal is $\barτ_e = (2.51 \pm 0.55^{\text{stat}} \pm 0.15^{\rm syst}) \times 10^{-3}$. The two measures agree at $0.6 σ$. We perform a suite of systematic checks to test the robustness of the analysis.