A simple parametric model for spherical galaxy clusters
  We present an analytic parametric model to describe the baryonic and dark
matter distributions in clusters of galaxies with spherical symmetry. It is
assumed that the dark matter density follows a Navarro, Frenk and White (NFW)
profile and that the gas pressure is described by a generalised NFW (GNFW)
profile. By further demanding hydrostatic equilibrium and that the gas fraction
is small throughout the cluster, one obtains unique functional forms, dependent
on basic cluster parameters, for the radial profiles of all the properties of
interest in the cluster. We show these profiles are consistent both with
numerical simulations and multi-wavelength observations of clusters. We also
use our model to analyse six simulated SZ clusters as well as A611 SZ data from
the Arcminute Microkelvin Imager (AMI). In each case, we derive the radial
profile of the enclosed total mass and the gas pressure and show that the
results are in good agreement with our model prediction.
