Testing the Low-Mass End of X-Ray Scaling Relations with a Sample of Chandra Galaxy Groups

Details Testing the Low-Mass End of X-Ray Scaling Relations with a Sample of Chandra Galaxy Groups Testing the Low-Mass End of X-Ray Scaling Relations with a Sample of Chandra Galaxy Groups

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.3404e&link_type=abstract

American Astronomical Society, HEAD meeting #11, #34.04; Bulletin of the American Astronomical Society, Vol. 41, p.711

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Well-determined scaling relations between X-ray observables and cluster mass are essential for using large cluster samples to constrain fundamental cosmological parameters. Scaling relations between cluster masses and observables, such as the luminosity-temperature, mass-temperature, luminosity-mass relations, have been investigated extensively, however the question of whether these relations hold true also for poor clusters and groups remains unsettled. Some evidence supports a "break" at the low end of the group/cluster mass range, possibly caused by the stronger influence of non-gravitational physics on low-mass systems. Our goal is to test local scaling relations for the low-mass range in order to resolve the issue whether or not there is a systematic difference between clusters and groups, and to thereby provide the basis for a reliable and convenient cluster mass determination for future large samples.
We have performed a detailed analysis of a sample of 26 X-ray galaxy groups observed with Chandra, compiled from statisticaly complete parent samples and selected by luminosity and redshift, determined the main physical quantities like temperature and mass, and present various X-ray scaling relations (L-T, M-T, L-M, Mg-M, M-Yx, L-Yx, fg-T). We compare the group properties to those of the HIFLUGCS clusters, as well as several other group and cluster samples. We have found some evidence for a similarity break between groups and clusters, for example the L-T relation steepens for temperatures below 3 keV, and the M-T relation tends to steepen when fitting groups together with clusters, which could indicate a larger impact of heating mechanisms on cooler systems. We also detect a decrease in the gas mass fraction below 1 keV. Also in general the scatter for groups is larger than for clusters, which appears not to be correlated with merger activity but could be due to complex baryonic physics in the group cores.

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