Comparison of physical and observational galaxy cluster modelling
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Abstract
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