The radial structure of galaxy groups and clusters

Details The radial structure of galaxy groups and clusters The radial structure of galaxy groups and clusters

2003-06-12

arxiv.org/abs/astro-ph/0306264v2

Mon.Not.Roy.Astron.Soc. 346 (2003) 731-745

Astronomy and Astrophysics

Astrophysics

16 pages, 19 figures, minor changes to match published version

Scientific paper

10.1111/j.1365-2966.2003.07116.x

Simple self-consistent models of galaxy groups and clusters are tested against the results of high-resolution adiabatic gasdynamical simulations. We investigate two models based on the existence of a 'universal' dark matter density profile and two versions of the beta-model. The mass distribution of relaxed clusters can be fitted by phenomenological formulae proposed in the literature. Haloes that have experienced a recent merging event are systematically less concentrated and show steeper profiles than relaxed objects near the centre. The hot X-ray emitting gas is found to be in approximate hydrostatic equilibrium with the dark matter potential, and it is well described by a polytropic equation of state. Analytic formulae for the gas density and temperature can be derived from these premises. Though able to reproduce the X-ray surface brightness, the beta-model is shown to provide a poor description of our numerical clusters. We find strong evidence of a 'universal' temperature profile that decreases by a factor of 2-3 from the centre to the virial radius, whereas baryon fraction and entropy are monotonically increasing functions. Numerical resolution and entropy conservation play a key role in the shapes of the profiles at small radii.

Affiliated with

Also associated with

No associations

Rating

The radial structure of galaxy groups and clusters does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with The radial structure of galaxy groups and clusters, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The radial structure of galaxy groups and clusters will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-27019