Astronomy Reports

, Volume 60, Issue 6, pp 542–562

Detail studies of the physical properties in the outer regions of galaxy clusters using Suzaku observations

Article

DOI: 10.1134/S1063772916040028

Cite this article as:
Babyk, Y.V. Astron. Rep. (2016) 60: 542. doi:10.1134/S1063772916040028
  • 50 Downloads

Abstract

A detailed physical analysis of five nearby galaxy clusters using Suzaku observationsis presented. The low and stable level of the instrumental background at large radii facilitate the determination of the main physical characteristics in clusters at the virial radius. The temperatures, metal abundances, and entropy profiles have been constructed out to the outskirts of the clusters. The temperature profiles all display the same shape, with a negative gradient towards to the center and a flat outer plateau. The strong temperature gradients in the central parts of the clusters are usually associated with strong peaks of the surface brightness profiles. The temperature systematically decrease outward from the central regions, by a factor of three at and slightly beyond the cluster outskirts. The temperature profiles are compared with profiles predicted by N-body and hydrodynamical simulations obtained using several numerical algorithms. The slopes in the observed and simulated temperature profiles are consistent with each other in the cluster outskirts. The central regions of the clusters are characterized by low entropy and high metallicity. The possible influence of cool cores on the cluster outskirts is also discussed. The total mass profiles were determined using the observed gas-density and temperature profiles, assuming hydrostatic equilibriumand spherical symmetry. The gas-density profiles were fitted using an improved three-dimensional model to fit the inner and outer regions of the cluster independently. The total mass profiles were described using an NFW model out to R200. The measurements show clear evidence for universality of the total mass distribution. The scaled mass profiles in units of R200 and M200 display a dispersion of ~15% at 0.1R200. The fraction of gas out to R200 was also found.

Copyright information

© Pleiades Publishing, Ltd. 2016

Authors and Affiliations

  1. 1.Main Astronomical ObservatoryNational Academy of Sciences of UkraineKyivUkraine
  2. 2.Astrophysics/Astronomy Section, School of Cosmic PhysicsDublin Institute for Advanced StudiesDublin 2Ireland
  3. 3.School of Physical SciencesDublin City UniversityGlasnevin, Dublin 9Ireland

Personalised recommendations