Weak-lensing mass calibration of redMaPPer galaxy clusters in Dark Energy Survey Science Verification data
Creators: name: Melchior, P.
name: Gruen, D.
name: McClintock, T.
name: Varga, T. N.
name: Sheldon, E.
name: Rozo, E.
name: Amara, A.
name: Becker, M. R.
name: Benson, B. A.
name: Bermeo, A.
name: Bridle, S. L.
name: Clampitt, J.
name: Dietrich, J. P.
name: Hartley, W. G.
name: Hollowood, D.
name: Jain, B.
name: Jarvis, M.
name: Jeltema, T.
name: Kacprzak, T.
name: MacCrann, N.
name: Rykoff, E. S.
name: Saro, A.
name: Suchyta, E.
name: Troxel, M. A.
name: Zuntz, J.
name: Bonnett, C.
name: Plazas, A. A.
name: Abbott, T. M. C.
name: Abdalla, F. B.
name: Annis, J.
name: Benoit-Lévy, A.
name: Bernstein, G. M.
name: Bertin, E.
name: Brooks, D.
name: Buckley-Geer, E.
name: Rosell, A. Carnero
name: Kind, M. Carrasco
name: Carretero, J.
name: Cunha, C. E.
name: D'Andrea, C. B.
name: da Costa, L. N.
name: Desai, S.
name: Eifler, T. F.
name: Flaugher, B.
name: Fosalba, P.
name: García-Bellido, J.
name: Gaztanaga, E.
name: Gerdes, D. W.
name: Gruendl, R. A.
name: Gschwend, J.
name: Gutierrez, G.
name: Honscheid, K.
name: James, D. J.
name: Kirk, D.
name: Krause, E.
name: Kuehn, K.
name: Kuropatkin, N.
name: Lahav, O.
name: Lima, M.
name: Maia, M. A. G.
name: March, M.
name: Martini, P.
name: Menanteau, F.
name: Miller, C. J.
name: Miquel, R.
name: Mohr, J. J.
name: Nichol, R. C.
name: Ogando, R.
name: Romer, A. K.
name: Sanchez, E.
name: Scarpine, V.
name: Sevilla-Noarbe, I.
name: Smith, R. C.
name: Soares-Santos, M.
name: Sobreira, F.
name: Swanson, M. E. C.
name: Tarle, G.
name: Thomas, D.
name: Walker, A. R.
name: Weller, J.
name: Zhang, Y.
Publisher: name: arXiv
Year: 2016
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We use weak-lensing shear measurements to determine the mean mass of optically selected galaxy clusters in Dark Energy Survey Science Verification data. In a blinded analysis, we split the sample of more than 8,000 redMaPPer clusters into 15 subsets, spanning ranges in the richness parameter $5 \leq λ\leq 180$ and redshift $0.2 \leq z \leq 0.8$, and fit the averaged mass density contrast profiles with a model that accounts for seven distinct sources of systematic uncertainty: shear measurement and photometric redshift errors; cluster-member contamination; miscentering; deviations from the NFW halo profile; halo triaxiality; and line-of-sight projections. We combine the inferred cluster masses to estimate the joint scaling relation between mass, richness and redshift, $\mathcal{M}(λ,z) \varpropto M_0 λ^{F} (1+z)^{G}$. We find $M_0 \equiv \langle M_{200\mathrm{m}}\,|\,λ=30,z=0.5\rangle=\left[ 2.35 \pm 0.22\ \rm{(stat)} \pm 0.12\ \rm{(sys)} \right] \cdot 10^{14}\ M_\odot$, with $F = 1.12\,\pm\,0.20\ \rm{(stat)}\, \pm\, 0.06\ \rm{(sys)}$ and $G = 0.18\,\pm\, 0.75\ \rm{(stat)}\, \pm\, 0.24\ \rm{(sys)}$. The amplitude of the mass-richness relation is in excellent agreement with the weak-lensing calibration of redMaPPer clusters in SDSS by Simet et al. (2016) and with the Saro et al. (2015) calibration based on abundance matching of SPT-detected clusters. Our results extend the redshift range over which the mass-richness relation of redMaPPer clusters has been calibrated with weak lensing from $z\leq 0.3$ to $z\leq0.8$. Calibration uncertainties of shear measurements and photometric redshift estimates dominate our systematic error budget and require substantial improvements for forthcoming studies.
description: 22 pages, 14 figures, accepted by MNRAS