Comparison of physical and observational galaxy cluster modelling

Understand

We present a comparison between three cluster models applied to data obtained by the Arcminute Microkelvin Imager radio interferometer system.

• The physical model (PM) parameterises a cluster in terms of its physical quantities to model the dark matter and baryonic components of the cluster using NFW and GNFW profiles respectively.
• The observational models (OM I and OM II) model only the gas content of the cluster.
• The two OMs vary only in the priors they use in Bayesian inference: OM I has a joint prior on angular radius $\theta$ and integrated Comptonisation $Y$, derived from simulations, while OM II uses separable priors on $\theta$ and $Y$ which are based on calculations of the physical model.