A weak lensing analysis of the PLCK G100.2-30.4 cluster

Journal
Date Issued
2015
Author(s)
•
Formicola, I.
•
•
•
Bourdin, H.
•
Mazzotta, P.
•
Moscardini, L.
•
•
Arnaud, M.
•
Pratt, G. W.
•
Aghanim, N.
•
Dahle, H.
•
Douspis, M.
•
Pointecouteau, E.
•
DOI
Description
We thank the referee for the helpful comments that improved the paper. We acknowledge financial contributions from: contract ASI/INAF I/023/12/0 (L.M., M.R., M.M.); PRIN INAF 2009 “Weighing galaxy clusters with strong and weak lensing” (M.R., M.M.); PRIN MIUR 2010-2011 “The dark Universe and the cosmic evolution of baryons: from current surveys to Euclid” (LM, MR,MM); PRIN INAF 2012 “The Universe in the box: multiscale simulations of cosmic structure” (L.M.); contracts ASI-INAF I/009/10/0 and PRIN-INAF 2012 “A unique dataset to address the most compelling open questions about X-Ray Galaxy Clusters” (S.E.). M.R. also acknowledges Prof. P. Benvenuti (Department of Physics and Astronomy, University of Padova), for having made available his computing facilities.
Abstract
We present a mass estimate of the Planck-discovered cluster PLCK G100.2-30.4, derived from a weak lensing analysis of deep Subaru griz images. We perform a careful selection of the background galaxies using the multi-band imaging data, and undertake the weak lensing analysis on the deep (1 h) r -band image. The shape measurement is based on the Kaiser-Squires-Broadhurst algorithm; we adopt the PSFex software to model the point spread function (PSF) across the field and correct for this in the shape measurement. The weak lensing analysis is validated through extensive image simulations. We compare the resulting weak lensing mass profile and total mass estimate to those obtained from our re-analysis of XMM-Newton observations, derived under the hypothesis of hydrostatic equilibrium. The total integrated mass profiles agree remarkably well, within 1σ across their common radial range. A mass M500 ~ 7 × 1014M☉ is derived for the cluster from our weak lensing analysis. Comparing this value to that obtained from our reanalysis of XMM-Newton data, we obtain a bias factor of (1-b) = 0.8 ± 0.1. This is compatible within 1σ with the value of (1-b) obtained in Planck 2015 from the calibration of the bias factor using newly available weak lensing reconstructed masses.

Based on data collected at Subaru Telescope (University of Tokyo).

Volume
579
Start page
1
Uri
Url
Issn Identifier
0004-6361
Ads BibCode
2015A&A...579A...7R
Rights
open.access
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