Chandra Mass Profiles Of High Redshift Clusters Of Galaxies: Halo Concentration As A Function Of Redshift And Mass

Details Chandra Mass Profiles Of High Redshift Clusters Of Galaxies: Halo Concentration As A Function Of Redshift And Mass Chandra Mass Profiles Of High Redshift Clusters Of Galaxies: Halo Concentration As A Function Of Redshift And Mass

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.1504z&link_type=abstract

American Astronomical Society, HEAD meeting #9, #15.04; Bulletin of the American Astronomical Society, Vol. 38, p.378

Astronomy and Astrophysics

Astronomy

Scientific paper

The mass profiles of dark matter halos produced in ΛCDM N-body simulations show concentration parameters (c) that are decreasing functions of redshift (z) and virial mass (Mvir). To test these relations we have analyzed Chandra archival data for a sample of 15 high-z clusters of galaxies (z 0.3-1.0). The clusters have been selected to have relaxed morphologies and best available data. For all the objects we have measured density and temperature profiles and, through the assumption of hydrostatic equilibrium, obtained radial mass profiles with relative c and Mvir values (assuming an NFW model). We find that high-z halos are less massive than the low-z ones, in qualitative agreement with the hierarchical formation scenario. However in contrast with the predictions our c values increase with z. This has an impact also on the z-corrected c values that show a dependence in Mvir stronger than expected. Implications of this result and possible explanations will be discussed.

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