Volume 604, August 2017
|Number of page(s)||14|
|Section||Cosmology (including clusters of galaxies)|
|Published online||14 August 2017|
Calibrating the Planck cluster mass scale with CLASH
1 APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
2 Centro Brasileiro de Pesquisas Físicas, rua Dr. Xavier Sigaud 150, 22290-180 Rio de Janeiro, RJ, Brazil
3 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, CA91109, USA
4 Department of Physics, University of Arizona, Tucson, AZ 85721, USA
5 DRF/Irfu/SPP, CEA-Saclay, 91191 Gif-sur-Yvette Cedex, France
6 Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
7 Deparment of Physics and Michigan Center for Theoretical Physics, University of Michigan, Ann Arbor, MI 48109, USA
8 Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA
9 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21208, USA
10 Kavli Institute for Particle Astrophysics & Cosmology, PO Box 2450, Stanford University, Stanford, CA 94305, USA
11 SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA
Received: 28 October 2016
Accepted: 12 June 2017
We determine the mass scale of Planck galaxy clusters using gravitational lensing mass measurements from the Cluster Lensing And Supernova survey with Hubble (CLASH). We have compared the lensing masses to the Planck Sunyaev-Zeldovich (SZ) mass proxy for 21 clusters in common, employing a Bayesian analysis to simultaneously fit an idealized CLASH selection function and the distribution between the measured observables and true cluster mass. We used a tiered analysis strategy to explicitly demonstrate the importance of priors on weak lensing mass accuracy. In the case of an assumed constant bias, bSZ, between true cluster mass, M500, and the Planck mass proxy, MPL, our analysis constrains 1−bSZ = 0.73 ± 0.10 when moderate priors on weak lensing accuracy are used, including a zero-mean Gaussian with standard deviation of 8% to account for possible bias in lensing mass estimations. Our analysis explicitly accounts for possible selection bias effects in this calibration sourced by the CLASH selection function. Our constraint on the cluster mass scale is consistent with recent results from the Weighing the Giants program and the Canadian Cluster Comparison Project. It is also consistent, at 1.34σ, with the value needed to reconcile the Planck SZ cluster counts with Planck’s base ΛCDM model fit to the primary cosmic microwave background anisotropies.
Key words: galaxies: clusters: general / cosmology: observations / cosmological parameters / dark matter
© ESO, 2017
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