Measurement of the Temperature Distributions of Galaxy Clusters

Details Measurement of the Temperature Distributions of Galaxy Clusters Measurement of the Temperature Distributions of Galaxy Clusters

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21714915f&link_type=abstract

American Astronomical Society, AAS Meeting #217, #149.15; Bulletin of the American Astronomical Society, Vol. 43, 2011

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Scientific paper

We utilize a Markov Chain Monte Carlo analysis to measure a new galaxy cluster parameter, the width of the ICM temperature distribution (σ_logkT), as well median temperature, emission measure, cluster size, and abundance. Critical to measuring σ_logkT, the MCMC avoids typical assumptions such as spherical symmetry and isothermality by modeling the ICM as a collection of X-ray emitting, smoothed particles of plasma, each with its own set of parameters including temperature, emission measure, position, and abundance. The resulting distribution of particle temperatures is then representative of the ICM temperature distribution, and similarly for the other parameters. The cluster temperature and σ_logkT are defined as the median and standard deviation of the temperature distribution, respectively. The cluster emission measure is simply the sum of the particle emission measures, and the characteristic cluster size is determined from the particle spatial positions. We have so far performed this analysis on XMM-Newton observations of 20 clusters with temperatures of 1keV-13keV in order to search for correlations between the temperature width and other cluster parameters.

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