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Published December 10, 2014 | Published + Submitted
Journal Article Open

The MUSIC of CLASH: Predictions on the Concentration-Mass Relation


We present an analysis of the MUSIC-2 N-body/hydrodynamical simulations aimed at estimating the expected concentration-mass relation for the CLASH (Cluster Lensing and Supernova Survey with Hubble) cluster sample. We study nearly 1,400 halos simulated at high spatial and mass resolution. We study the shape of both their density and surface-density profiles and fit them with a variety of radial functions, including the Navarro-Frenk-White (NFW), the generalized NFW, and the Einasto density profiles. We derive concentrations and masses from these fits. We produce simulated Chandra observations of the halos, and we use them to identify objects resembling the X-ray morphologies and masses of the clusters in the CLASH X-ray-selected sample. We also derive a concentration-mass relation for strong-lensing clusters. We find that the sample of simulated halos that resembles the X-ray morphology of the CLASH clusters is composed mainly of relaxed halos, but it also contains a significant fraction of unrelaxed systems. For such a heterogeneous sample we measure an average two-dimensional concentration that is ~11% higher than is found for the full sample of simulated halos. After accounting for projection and selection effects, the average NFW concentrations of CLASH clusters are expected to be intermediate between those predicted in three dimensions for relaxed and super-relaxed halos. Matching the simulations to the individual CLASH clusters on the basis of the X-ray morphology, we expect that the NFW concentrations recovered from the lensing analysis of the CLASH clusters are in the range [3-6], with an average value of 3.87 and a standard deviation of 0.61.

Additional Information

© 2014 American Astronomical Society. Received 2014 April 10; accepted 2014 September 25; published 2014 November 21. The research was in part carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. M.M. thanks ORAU and NASA for supporting his research at JPL. M.M., C.G., and L.M. acknowledge support from the contracts ASI/INAF I/023/12/0, INFN/PD51, and the PRIN MIUR 2010–2011 "The dark universe and the cosmic evolution of baryons: From current surveys to Euclid." E.R. acknowledges support from the National Science Foundation AST-1210973, SAO TM3-14008X (issued under NASA Contract No. NAS8-03060). C.G.'s research is part of the project GLENCO, funded under the European Seventh Framework Programme, Ideas, grant agreement No. 259349. K.U. acknowledges support from the National Science Council of Taiwan (grant NSC100-2112-M-001-008-MY3) and from the Academia Sinica Career Development Award. Support for A.Z. is provided by NASA through Hubble Fellowship grant #HST-HF-51334.01-A awarded by STScI. D.G., S.S., and P.R. were supported by SFB Transregio 33 The Dark Universe by the Deutsche Forschungsgemeinschaft (DFG) and the DFG cluster of excellence Origin and Structure of the Universe. This work was supported in part by contract research "Internationale Spitzenforschung II/2-6" of the Baden Württemberg Stiftung. The Dark Cosmology Centre is funded by the DNRF. J.S. was supported by NSF/AST1313447, NASA/NNX11AB07G, and the Norris Foundation CCAT Postdoctoral Fellowship. The MUSIC simulations were performed at the Barcelona Supercomputing Center (BSC), and the initial conditions were done at the Leibniz Rechenzentrum Munich (LRZ). G.Y. and F.S. acknowledge support from MINECO under research grants AYA2012-31101, FPA2012-34694, and MultiDark CSD2009-00064. We thank Stefano Borgani and the whole computational astrophysics group at the University of Trieste and at INAF-OATS for giving us access to their set of hydrodynamical simulations.

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Published - 0004-637X_797_1_34.pdf

Submitted - 1404.1384v2.pdf


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