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To, C; Krause, E; Wu, H; Gruen, D; Wechsler, R H; Eifler, T F; Rykoff, E S; Costanzi, M; Becker, M R; Bernstein, G M; Blazek, J; Bocquet, S; Bridle, S L; Cawthon, R; Choi, A; Crocce, M; Davis, C; DeRose, J; Drlica-Wagner, A; Elvin-Poole, J; Fang, X; Farahi, A; Friedrich, O; Gatti, M; Gaztanaga, E; Giannantonio, T; Hartley, W G; Hoyle, B; Jarvis, M; MacCrann, N; McClintock, T; Miranda, V; Pereira, M E S; Park, Y; Porredon, A; Rau, M M; Ross, A J; Samuroff, S; Sánchez, C; Sevilla-Noarbe, I; Sheldon, E; Troxel, M A; Vielzeuf, P; Zhang, Y; Zuntz, J; Abbott, T M C; Aguena, M; Bhargava, S; Burke, D L; Carnero Rosell, A; Carrasco Kind, M; Carretero, J; Chang, C; Conselice, C; da Costa, L N; Davis, T M; Desai, S; Diehl, H T; Dietrich, J P; Everett, S; Evrard, A E; Ferrero, I; Flaugher, B; Fosalba, P; Frieman, J; García-Bellido, J; Gruendl, R A; Gutierrez, G; Hinton, S R; Hollowood, D L; Honscheid, K; Huterer, D; James, D J; Jeltema, T; Kron, R; Kuehn, K; Kuropatkin, N; Lima, M; Maia, M A G; Marshall, J L; Miquel, R; Morgan, R; Muir, J; Myles, J; Palmese, A; Paz-Chinchón, F; Plazas, A A; Romer, A K; Roodman, A; Santiago, B; Scarpine, V; Serrano, S; Suchyta, E; Swanson, M E C; Tarle, G; Thomas, D; Tucker, D L; Weller, J; Wester, W; Wilkinson, R D
Physical review letters, 04/2021, Volume: 126, Issue: 14Journal Article
We present the first joint analysis of cluster abundances and auto or cross-correlations of three cosmic tracer fields: galaxy density, weak gravitational lensing shear, and cluster density split by optical richness. From a joint analysis (4×2pt+N) of cluster abundances, three cluster cross-correlations, and the auto correlations of the galaxy density measured from the first year data of the Dark Energy Survey, we obtain Ω_{m}=0.305_{-0.038}^{+0.055} and σ_{8}=0.783_{-0.054}^{+0.064}. This result is consistent with constraints from the DES-Y1 galaxy clustering and weak lensing two-point correlation functions for the flat νΛCDM model. Consequently, we combine cluster abundances and all two-point correlations from across all three cosmic tracer fields (6×2pt+N) and find improved constraints on cosmological parameters as well as on the cluster observable-mass scaling relation. This analysis is an important advance in both optical cluster cosmology and multiprobe analyses of upcoming wide imaging surveys.
