declines in the central cooling region as given by [@Allen:2001]. The JACO software pipeline developed by [@Mahdavi:2007] uses separate parametrization of the gas, dark matter and stellar components, assuming hydrostatic equilibrium, to jointly fit to high significance X-ray spectra from *Chandra* and *XMM-Newton*, weak lensing shear from Canada-France-Hawaii telescope, optical data on the brightest cluster galaxy from the Hubble space telescope and the SZ effect from the Cosmic Background Imager. For sufficiently resolved SZ maps, the temperature and mass profiles can be reconstructed by de-projection techniques, for example see [@Ameglio:2007; @Ameglio:2009] for a comparison of the method to simulations and [@Nord:2009] for direct application to SZ and X-ray data. However with many SZ experiments the data are generally not very well resolved, and so combined analysis with X-ray surface brightness data requires the application of a parameterized model that reproduces the observed temperatures and masses from X-ray observations and simulations. [@Mroczkowski:2009] successfully use an NFW parameterized pressure profile developed by [@Nagai:2007] to fit to data from the Sunyaev-Zel’dovich Array (SZA), and then combine with X-ray surface brightness to reproduce temperature profiles out to large radii. This model has also been adopted by [@Arnaud:2010] in order derive a universal pressure profile 