Dark Energy Survey Year 1 Results: Cosmological Constraints from Cluster Abundances and Weak Lensing
Creators: name: DES Collaboration
name: Abbott, Tim
name: Aguena, Michel
name: Alarcon, Alex
name: Allam, Sahar
name: Allen, Steve
name: Annis, James
name: Avila, Santiago
name: Bacon, David
name: Bermeo, Alberto
name: Bernstein, Gary
name: Bertin, Emmanuel
name: Bhargava, Sunayana
name: Bocquet, Sebastian
name: Brooks, David
name: Brout, Dillon
name: Buckley-Geer, Elizabeth
name: Burke, David
name: Rosell, Aurelio Carnero
name: Kind, Matias Carrasco
name: Carretero, Jorge
name: Castander, Francisco Javier
name: Cawthon, Ross
name: Chang, Chihway
name: Chen, Xinyi
name: Choi, Ami
name: Costanzi, Matteo
name: Crocce, Martin
name: da Costa, Luiz
name: Davis, Tamara
name: De Vicente, Juan
name: DeRose, Joseph
name: Desai, Shantanu
name: Diehl, H. Thomas
name: Dietrich, Jörg
name: Dodelson, Scott
name: Doel, Peter
name: Drlica-Wagner, Alex
name: Eckert, Kathleen
name: Eifler, Tim
name: Elvin-Poole, Jack
name: Estrada, Juan
name: Everett, Spencer
name: Evrard, August
name: Farahi, Arya
name: Ferrero, Ismael
name: Flaugher, Brenna
name: Fosalba, Pablo
name: Frieman, Josh
name: Garcia-Bellido, Juan
name: Gatti, Marco
name: Gaztanaga, Enrique
name: Gerdes, David
name: Giannantonio, Tommaso
name: Giles, Paul
name: Grandis, Sebastian
name: Gruen, Daniel
name: Gruendl, Robert
name: Gschwend, Julia
name: Gutierrez, Gaston
name: Hartley, Will
name: Hinton, Samuel
name: Hollowood, Devon L.
name: Honscheid, Klaus
name: Hoyle, Ben
name: Huterer, Dragan
name: James, David
name: Jarvis, Mike
name: Jeltema, Tesla
name: Johnson, Margaret
name: Kent, Stephen
name: Krause, Elisabeth
name: Kron, Richard
name: Kuehn, Kyler
name: Kuropatkin, Nikolay
name: Lahav, Ofer
name: Li, Ting
name: Lidman, Christopher
name: Lima, Marcos
name: Lin, Huan
name: MacCrann, Niall
name: Maia, Marcio
name: Mantz, Adam
name: Marshall, Jennifer
name: Martini, Paul
name: Mayers, Julian
name: Melchior, Peter
name: Mena, Juan
name: Menanteau, Felipe
name: Miquel, Ramon
name: Mohr, Joe
name: Nichol, Robert
name: Nord, Brian
name: Ogando, Ricardo
name: Palmese, Antonella
name: Paz-Chinchon, Francisco
name: Malagón, Andrés Plazas
name: Prat, Judit
name: Rau, Markus Michael
name: Romer, Kathy
name: Roodman, Aaron
name: Rooney, Philip
name: Rozo, Eduardo
name: Rykoff, Eli
name: Sako, Masao
name: Samuroff, Simon
name: Sanchez, Carles
name: Saro, Alexandro
name: Scarpine, Vic
name: Schubnell, Michael
name: Scolnic, Daniel
name: Serrano, Santiago
name: Sevilla, Ignacio
name: Sheldon, Erin
name: Smith, J. Allyn
name: Suchyta, Eric
name: Swanson, Molly
name: Tarle, Gregory
name: Thomas, Daniel
name: To, Chun-Hao
name: Troxel, Michael A.
name: Tucker, Douglas
name: Varga, Tamas Norbert
name: von der Linden, Anja
name: Walker, Alistair
name: Wechsler, Risa
name: Weller, Jochen
name: Wilkinson, Reese
name: Wu, Hao-Yi
name: Yanny, Brian
name: Zhang, Zhuowen
name: Zuntz, Joe
Publisher: name: arXiv
Year: 2020
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We perform a joint analysis of the counts and weak lensing signal of redMaPPer clusters selected from the Dark Energy Survey (DES) Year 1 dataset. Our analysis uses the same shear and source photometric redshifts estimates as were used in the DES combined probes analysis. Our analysis results in surprisingly low values for $S_8 =σ_8(Ω_{\rm m}/0.3)^{0.5}= 0.65\pm 0.04$, driven by a low matter density parameter, $Ω_{\rm m}=0.179^{+0.031}_{-0.038}$, with $σ_8-Ω_{\rm m}$ posteriors in $2.4σ$ tension with the DES Y1 3x2pt results, and in $5.6σ$ with the Planck CMB analysis. These results include the impact of post-unblinding changes to the analysis, which did not improve the level of consistency with other data sets compared to the results obtained at the unblinding. The fact that multiple cosmological probes (supernovae, baryon acoustic oscillations, cosmic shear, galaxy clustering and CMB anisotropies), and other galaxy cluster analyses all favor significantly higher matter densities suggests the presence of systematic errors in the data or an incomplete modeling of the relevant physics. Cross checks with X-ray and microwave data, as well as independent constraints on the observable--mass relation from SZ selected clusters, suggest that the discrepancy resides in our modeling of the weak lensing signal rather than the cluster abundance. Repeating our analysis using a higher richness threshold ($λ\ge 30$) significantly reduces the tension with other probes, and points to one or more richness-dependent effects not captured by our model.
description: 35 pages, 20 figures, submitted to Physical Review D