Characterizing the X-ray Properties of Clusters of Galaxies

Details Characterizing the X-ray Properties of Clusters of Galaxies Characterizing the X-ray Properties of Clusters of Galaxies

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008head...10.0901a&link_type=abstract

American Astronomical Society, HEAD meeting #10, #9.01

Mathematics

Logic

Scientific paper

We report on the application of the new Monte Carlo method, Smoothed Particle Inference (SPI), towards analysis and interpretation of X-ray observations of clusters of galaxies with the XMM-Newton satellite.
Our sample includes publicly available well-exposed observations of clusters at redshifts z > 0.069, totaling 101 objects.
We aim to determine the luminosity and temperature structure of the X-ray emitting gas, with the goal to establish the potential robustness of determination of mass from the X-ray data for a given cluster, which in turn is essential towards the use of clusters for measurements of cosmological parameters. We use the luminosity and temperature maps derived via the SPI technique to determine the presence of cooling cores, via measurements of luminosity and temperature contrast. We determine the LX - T relation, where we confirm that LX ∝ T3. Here, we find, at best, a weak redshift dependence (in contrast to some Chandra results).
We establish the level of dynamical activity using the "power ratios'' method, and compare our results to previous application of this method to Chandra data for clusters. We propose a new method, the "temperature two-point correlation function,'' to determine the power spectrum of temperature gradients of the X-ray emitting gas as a function of spatial scale, and show how this method can be fruitfully used to identify cooling core clusters as well as those with disturbed structures, presumably due to on-going or recent merger activity.

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