Weak Lensing Analysis of SPT selected Galaxy Clusters using Dark Energy Survey Science Verification Data

• Published in: Monthly Notices of the Royal Astronomical Society
• Main Authors: Stern, C., Dietrich, J.P., Bocquet, S., Applegate, D., Mohr, J.J., Bridle, S.L., Carrasco Kind, M., Gruen, D., Jarvis, M., Kacprzak, T., Saro, A., Sheldon, E., Troxel, M.A., Zuntz, J., Benson, B.A., Capasso, R., Chiu, I., Desai, S., Rapetti, D., Reichardt, C.L., Saliwanchik, B., Schrabback, T., Gupta, N., Abbott, T.M.C., Abdalla, F.B., Avila, S., Bertin, E., Brooks, D., Burke, D.L., Carnero Rosell, A., Carretero, J., Castander, F.J., D'Andrea, C.B., Da Costa, L.N., Davis, C., De Vicente, J., Diehl, H.T., Doel, P., Estrada, J., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruendl, R.A., Gschwend, J., Gutierrez, G., Hollowood, D., Jeltema, T.
• Other Authors: Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, SPT
• Format: Article in Journal/Newspaper
• Language: English
• Published: HAL CCSD 2019
• Subjects: cosmology: observations; galaxies: clusters: general; gravitational lensing: weak; [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]; South Pole; South pole
• Online Access: https://hal.archives-ouvertes.fr/hal-01724837; https://doi.org/10.1093/mnras/stz234

International audience We present weak-lensing (WL) mass constraints for a sample of massive galaxy clusters detected by the South Pole Telescope (SPT) via the Sunyaev–Zel’dovich effect (SZE). We use griz imaging data obtained from the Science Verification (SV) phase of the Dark Energy Survey (DES) to fit the WL shear signal of 33 clusters in the redshift range 0.25 ≤ |$z$| ≤ 0.8 with NFW profiles and to constrain a four-parameter SPT mass–observable relation. To account for biases in WL masses, we introduce a WL mass to true mass scaling relation described by a mean bias and an intrinsic, lognormal scatter. We allow for correlated scatter within the WL and SZE mass–observable relations and use simulations to constrain priors on nuisance parameters related to bias and scatter from WL. We constrain the normalization of the ζ−M_500 relation, |$A_\mathrm{SZ}=12.0_{-6.7}^{+2.6}$| when using a prior on the mass slope B_SZ from the latest SPT cluster cosmology analysis. Without this prior, we recover |$A_\mathrm{SZ}=10.8_{-5.2}^{+2.3}$| and |$B_\mathrm{SZ}=1.30_{-0.44}^{+0.22}$|. Results in both cases imply lower cluster masses than measured in previous work with and without WL, although the uncertainties are large. The WL derived value of B_SZ is |${\approx } 20{{\ \rm per\ cent}}$| lower than the value preferred by the most recent SPT cluster cosmology analysis. The method demonstrated in this work is designed to constrain cluster masses and cosmological parameters simultaneously and will form the basis for subsequent studies that employ the full SPT cluster sample together with the DES data.