$μ_{\star}$ Masses: Weak Lensing Calibration of the Dark Energy Survey Year 1 redMaPPer Clusters using Stellar Masses
Creators: name: Pereira, M. E. S.
name: Palmese, A.
name: Varga, T. N.
name: McClintock, T.
name: Soares-Santos, M.
name: Burgad, J.
name: Annis, J.
name: Farahi, A.
name: Lin, H.
name: Choi, A.
name: DeRose, J.
name: Esteves, J.
name: Gatti, M.
name: Gruen, D.
name: Hartley, W. G.
name: Hoyle, B.
name: Jeltema, T.
name: MacCrann, N.
name: Roodman, A.
name: Sánchez, C.
name: Shin, T.
name: von der Linden, A.
name: Zuntz, J.
name: Abbott, T. M. C.
name: Aguena, M.
name: Avila, S.
name: Bertin, E.
name: Bhargava, S.
name: Bridle, S. L.
name: Brooks, D.
name: Burke, D. L.
name: Rosell, A. Carnero
name: Kind, M. Carrasco
name: Carretero, J.
name: Costanzi, M.
name: da Costa, L. N.
name: Desai, S.
name: Diehl, H. T.
name: Dietrich, J. P.
name: Doel, P.
name: Estrada, J.
name: Everett, S.
name: Flaugher, B.
name: Fosalba, P.
name: Frieman, J.
name: García-Bellido, J.
name: Gaztanaga, E.
name: Gerdes, D. W.
name: Gruendl, R. A.
name: Gschwend, J.
name: Gutierrez, G.
name: Hinton, S. R.
name: Hollowood, D. L.
name: Honscheid, K.
name: James, D. J.
name: Kuehn, K.
name: Kuropatkin, N.
name: Lahav, O.
name: Lima, M.
name: Maia, M. A. G.
name: March, M.
name: Marshall, J. L.
name: Melchior, P.
name: Menanteau, F.
name: Miquel, R.
name: Ogando, R. L. C.
name: Paz-Chinchón, F.
name: Plazas, A. A.
name: Romer, A. K.
name: Sanchez, E.
name: Scarpine, V.
name: Schubnell, M.
name: Serrano, S.
name: Sevilla-Noarbe, I.
name: Smith, M.
name: Suchyta, E.
name: Swanson, M. E. C.
name: Tarle, G.
name: Wechsler, R. H.
name: Weller, J.
name: Zhang, Y.
Publisher: name: arXiv
Year: 2020
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We present the weak lensing mass calibration of the stellar mass based $μ_{\star}$ mass proxy for redMaPPer galaxy clusters in the Dark Energy Survey Year 1. For the first time we are able to perform a calibration of $μ_{\star}$ at high redshifts, $z&gt;0.33$. In a blinded analysis, we use $\sim 6,000$ clusters split into 12 subsets spanning the ranges $0.1 \leqslant z&lt;0.65$ and $μ_{\star}$ up to $\sim 5.5 \times 10^{13} M_{\odot}$, and infer the average masses of these subsets through modelling of their stacked weak lensing signal. In our model we account for the following sources of systematic uncertainty: shear measurement and photometric redshift errors, miscentring, cluster-member contamination of the source sample, deviations from the NFW halo profile, halo triaxiality and projection effects. We use the inferred masses to estimate the joint mass--$μ_{\star}$--$z$ scaling relation given by $\langle M_{200c} | μ_{\star},z \rangle = M_0 (μ_{\star}/5.16\times 10^{12} \mathrm{M_{\odot}})^{F_{μ_{\star}}} ((1+z)/1.35)^{G_z}$. We find $M_0= (1.14 \pm 0.07) \times 10^{14} \mathrm{M_{\odot}}$ with $F_{μ_{\star}}= 0.76 \pm 0.06$ and $G_z= -1.14 \pm 0.37$. We discuss the use of $μ_{\star}$ as a complementary mass proxy to the well-studied richness $λ$ for: $i)$ exploring the regimes of low $z$, $λ&lt;20$ and high $λ$, $z \sim 1$; $ii)$ testing systematics such as projection effects for applications in cluster cosmology.
description: 20 pages, 10 figures, submitted to MNRAS