The radial structure of galaxy groups and clusters

Y. Ascasibar; G. Yepes; V. Mueller; S. Gottloeber

doi:10.1111/j.1365-2966.2003.07116.x

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arXiv · astro-ph/0306264

The radial structure of galaxy groups and clusters

Y. Ascasibar·G. Yepes·V. Mueller·S. Gottloeber

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Abstract

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.

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Y. Ascasibar, G. Yepes, V. Mueller, S. Gottloeber. 2003-12-09. The radial structure of galaxy groups and clusters. https://doi.org/10.1111/j.1365-2966.2003.07116.x

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