Abstract: | 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 $5 leq
lambda leq 180$ 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, $mathcal{M}(lambda,z) varpropto M_0 lambda^{F}
(1+z)^{G}$. We find $M_0 equiv langle
M_{200mathrm{m}},|,lambda=30,z=0.5
angle=left[ 2.35 pm 0.22
m{(stat)}
pm 0.12
m{(sys)}
ight] cdot 10^{14} M_odot$, with $F =
1.12,pm,0.20
m{(stat)}, pm, 0.06
m{(sys)}$ and $G = 0.18,pm,
0.75
m{(stat)}, pm, 0.24
m{(sys)}$. 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 $zleq 0.3$ to
$zleq0.8$. Calibration uncertainties of shear measurements and photometric
redshift estimates dominate our systematic error budget and require substantial
improvements for forthcoming studies. |