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Title: 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 threemore » 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.« less
Authors:
 [1] ;  [2] ; ; ;  [3] ; ;  [4] ; ;  [5] ;  [6] ; ;  [7] ;  [8] ;  [9] ;  [10] ;  [11] ;  [12] ;  [13] ;  [14] ;  [15] more »; « less
  1. INAF, Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna (Italy)
  2. Physics Department, University of Michigan, 450 Church Avenue, Ann Arbor, MI 48109 (United States)
  3. Departamento de Fsica Terica, Universidad Autnoma de Madrid, Cantoblanco, E-28049 Madrid (Spain)
  4. Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109 (United States)
  5. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21208 (United States)
  6. Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824 (United States)
  7. Institute of Astronomy and Astrophysics, Academia Sinica, PO Box 23-141, Taipei 10617, Taiwan (China)
  8. INAF-Osservatorio Astronomico di Capodimonte, Via Moiariello 16, I-80131 Napoli (Italy)
  9. Institut fur Theoretische Astrophysik, Universität Heidelberg, Zentrum für Astronomie, Philosophenweg 12, D-69120 Heidelberg (Germany)
  10. Instituto de Astrofísica de Andalucía (CSIC), E-18080 Granada (Spain)
  11. INAF/Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, I-34143 Trieste (Italy)
  12. Leiden Observatory, Leiden University, PO Box 9513, NL-2333 Leiden (Netherlands)
  13. Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218 (United States)
  14. Department of Theoretical Physics and History of Science, University of the Basque Country UPV/EHU, PO Box 644, E-48080 Bilbao (Spain)
  15. Dipartimento di Fisica, Sapienza Universit di Roma, Piazzale Aldo Moro 5, I-00185 Roma (Italy)
Publication Date:
OSTI Identifier:
22370084
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 797; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCOUNTING; CONCENTRATION RATIO; DENSITY; ELEMENT ABUNDANCE; FORECASTING; GALAXY CLUSTERS; GRAVITATION; GRAVITATIONAL LENSES; MASS; MASS RESOLUTION; NONLUMINOUS MATTER; SIMULATION; SURFACES; TWO-DIMENSIONAL CALCULATIONS; X RADIATION