Weighing galaxy clusters on Stripe 82 through weak gravitational lensing

Galaxy clusters are powerful tools to study the content and evolution of the Universe. Determining their abundances as a function of mass and redshift is one of the main observables for current and forthcoming surveys such as the Dark Energy Survey (DES) and the Large Synoptic Survey Telescope (LSST). Galaxy clusters act as gravitational lenses producing efects on the background sources such as shear (weak lensing), magni_cation and multiple images (strong lensing). The study of these efects enables us to obtain the mass distribution of the clusters without relying on assumptions about their physical and dynamical states. A widely used method to obtain average mass estimates of clusters is based on the measurements of the tangential shear pro_les of the background sources, which can be converted to a projected mass density contrast and _tted by theoretical models, such as the Navarro-Frenk-White (NFW) pro_le. In this work we focus on the weak lensing mass measurements for galaxy clusters in the CFTH Stripe 82 survey (CS82) footprint and identi_ed in the Sloan Digital Sky Survey (SDSS) by the redMaPPer and the Voronoi Tessellation (VT) algorithms. We present the first weak lensing calibration of µ*, a new galaxy cluster mass proxy corresponding to the total stellar mass of red and blue members, in these two cluster samples: 230 redMaPPer clusters at redshift 0.1 ≤ z < 0.33 and 136 VT clusters at 0.1 ≤ z < 0.6. We use the CS82 shear catalog and stack the clusters in µ* bins to measure a mass-observable power law relation. We show that our results are consistent, internally and with the literature, indicating that our method can be Applied to any cluster _nding algorithm. In particular, we have seen that µ* is the suitable mass proxy for VT clusters. Catalogs including µ* measurements will enable its use in studies of galaxy Evolution in clusters and cluster cosmology. In the strong lensing regime we describe how to obtain a mass estimate for the galaxy clusters through the measurements of the curvature radius of gravitational arcs. This technique will be applied to systems with arcs in the SOAR Gravitational Arc Survey (SOGRAS). We also present the preliminary results for stacked weak lensing mass measurements of a sample of SOGRAS clusters in the CS82 footprint.