AbstractWe investigate the dark matter distributions in the central region of two clusters of galaxies (A1835 and MKW3S) using Chandra data. N-body simulations in the standard cold dark matter (CDM) model predict the dark matter distribution shows a cuspy dark matter profile: ρ(r)∝rα, with α in the range 1–2, while observations of dwarf and low surface brightness galaxies seem to favor the presence of a relatively flat core: 0<α<1. To investigate the dark matter distributions in the central region of clusters of galaxies, we analyze the Chandra data of A1835 and MKW3S with a deprojection method. We derive the mass profiles without the assumption of analytical models. We examine the inner slope of derived mass profiles assuming the dark matter profile is described with a power-law expression. The values of the slope α are 0.95±0.10 for A1835 and 1.33±0.12 for MKW3S within the radius of 200 kpc. These are consistent with the result of the CDM simulations. However, within the radius of 100 kpc, the value of α is less than unity for A1835 (0.47±0.31). Our result implies that the central dark matter profile of some clusters cannot be described by CDM halos.
X-ray measurements of the dark matter distribution in clusters of galaxies with Chandra
Advances in Space Research ; 34 , 12 ; 2519-2524
2003-06-13
6 pages
Article (Journal)
Electronic Resource
English
X-Ray Measurements of the Dark Matter Distribution in Clusters of Galaxies With Chandra
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