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Chandra X-ray galaxy clusters at z < 1.4: Constraints on the inner slope of the density profiles

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Abstract

A reconstruction of the total mass (the fraction of dark matter, intercluster gas, and the brightest galaxy of the cluster) of 128 X-ray galaxy clusters at redshifts 0.01–1.4 based on Chandra observations is presented. The total mass M 200 and the baryonic mass M b have been measured for all the sample objects, as well as the concentration parameter c 200, which characterizes the size of the dark matter halo. The existence of a tight correlation between c 200 and M 200 is confirmed, c ∝ M avir /(1 + z)b with a = −0.56 ± 0.15 and b = 0.80 ± 0.25 (95% confidence level), in good agreement with the predictions of numerical simulations and previous observations. Fitting the inner dark-matter density slope α with a generalized NFW model yields α = 1.10 ± 0.48 at the 2σ confidence level, combining the results for the entire sample, for which the model gives a good description of the data. There is also a tight correlation between the inner slope of the dark-matter density profile α and the baryonic mass contentM b for massive galaxy clusters, namely, α decreases with increasing baryonic mass content. A simple power-law model is used to fit the α − M b distributions, yielding the break point for the inner slope of the dark-matter density profile b = 1.72 ± 0.37 (68% confidence level).

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Authors and Affiliations

  1. Main Astronomical Observatory, National Academy of Sciences of Ukraine, Kyiv, Ukraine

    Yu. V. Babyk & I. B. Vavilova

  2. Università di Catania, Catania, Italy

    A. Del Popolo

  3. Universidade de São Paulo, São Paulo, Brazil

    A. Del Popolo

Authors
  1. Yu. V. Babyk
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  2. A. Del Popolo
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  3. I. B. Vavilova
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Correspondence to Yu. V. Babyk.

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Original Russian Text © Yu.V. Babyk, A. Del Popolo, I.B. Vavilova, 2014, published in Astronomicheskii Zhurnal, 2014, Vol. 91, No. 9, pp. 679–704.

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Babyk, Y.V., Del Popolo, A. & Vavilova, I.B. Chandra X-ray galaxy clusters at z < 1.4: Constraints on the inner slope of the density profiles. Astron. Rep. 58, 587–610 (2014). https://doi.org/10.1134/S1063772914090017

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  • DOI: https://doi.org/10.1134/S1063772914090017

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