Speaker: Paul Giles (Bristol)
One of the most important measurements of galaxy clusters is that of the cluster mass, which can be used to place constraints on various cosmological parameters. However, the cluster mass is not a trivial property to measure, with X-ray methods requiring the assumption of hydrostatic equilibrium of the cluster gas. In this talk I will present work involving a complete sample of 35 galaxy clusters in the redshift range 0.15 – 0.3 observed with Chandra. Using the most dynamically relaxed clusters in the sample, I will present various mass – X-ray observable scaling relations, and show how biases in X-ray selection techniques impact these relations. To eliminate the biases in X-ray selection, I will present the results of a weak lensing selected sample of clusters, and compare the derived scaling relations to those derived via X-ray selection. I also present an in depth look at the cluster A1835, a cluster for which its emission has been detected out to the virial radius.