Physical modelling of galaxy clusters detected by Planck
  We present a comparison of mass estimates for $54$ galaxy cluster candidates
from the second Planck catalogue (PSZ2) of Sunyaev-Zel'dovich sources. We
compare the mass values obtained with data taken from the Arcminute Microkelvin
Imager (AMI) radio interferometer system and from the Planck satellite. The
former of these uses a Bayesian analysis pipeline that parameterises a cluster
in terms of its physical quantities, and models the dark matter & baryonic
components of a cluster using NFW and GNFW profiles respectively. Our mass
estimates derived from Planck data are obtained from the results of the
Bayesian detection algorithm PowellSnakes (PwS), are based on the methodology
detailed in the PSZ2 paper, and produce two sets of mass estimates; one
estimate is calculated directly from the angular radius $\theta$ - integrated
Comptonisation parameter $Y$ posterior distributions, and the other uses a
`slicing function' to provide information on $\theta$ based on X-ray
measurements and previous Planck mission samples. We find that for $37$ of the
clusters, the AMI mass estimates are lower than both values obtained from
Planck data. However the AMI and slicing function estimates are within one
combined standard deviation of each other for $31$ clusters. We also generate
cluster simulations based on the slicing-function mass estimates, and analyse
them in the same way as we did the real AMI data. We find that inclusion in the
simulations of radio-source confusion & CMB noise and measurable radio-sources
causes AMI mass estimates to be systematically low.
