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

¹ INAF–Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, 35122 Padova, Italy
e-mail: mario.radovich@oapd.inaf.it
² INAF–Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
³ Dipartimento di Fisica, Università Tor Vergata, via della Ricerca Scientifica 1, 00133 Roma, Italy
⁴ Institute of Theoretical Astrophysics, University of Oslo, Blindern, Oslo, Norway
⁵ Institut d’Astrophysique Spatiale, CNRS (UMR 8617) Université Paris-Sud 11, Bât. 121, 91405 Orsay, France
⁶ CNRS, IRAP, 9 avenue du colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France
⁷ Laboratoire AIM, IRFU/Service d’Astrophysique, CEA/DSM, CNRS, Université Paris Diderot, Bât. 709, CEA-Saclay, 91191 Gif-sur-Yvette Cedex, France
⁸ INAF–Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy
⁹ Dipartimento di Fisica e Astronomia Alma Mater Studiorum – Universitá di Bologna, viale Berti Pichat 6/2, 40127 Bologna, Italy
¹⁰ INFN–Sezione di Bologna, viale Berti-Pichat 6/2, 40127 Bologna, Italy
¹¹ Université de Toulouse, UPS-OMP, IRAP, 31028 Toulouse Cedex 4, France

Received: 30 December 2014
Accepted: 5 May 2015

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.