2005/10/19 by F. Gastaldello, Gastaldello, F., David A. Buote +15
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0510592
2 pages, to appear in the proceedings for the conference "The X-ray Universe 2005", San Lorenzo del Escorial, Madrid; typo in one reference corrected
openalex publication_date 2005/10/19 · arxiv created 2005/10/28 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The Chandra and XMM data for a sample of 19 relaxed groups/poor clusters, covering the temperature range 1-3 keV and selected to have the best available data, reveal a remarkable similarity in their temperature profile: cool cores outside of which the temperatures reach a peak for radii less than 0.1 of the virial radius and then decline. We fitted the derived mass profiles using an NFW model, which provides a good fit to the data when accounting for the central galaxy in the inner region. The concentration parameters and virial masses are in the range c = 5-22 and M = 2 x 1013 - 4 x 1014 solar masses, in general agreement with the concentrations found in numerical simulations.