Chandra Observations of low velocity dispersion groups

Details Chandra Observations of low velocity dispersion groups Chandra Observations of low velocity dispersion groups

2004-09-29

arxiv.org/abs/astro-ph/0409713v1

Astrophys.J. 618 (2005) 679-691

Astronomy and Astrophysics

Astrophysics

Accepted for publication in ApJ

Scientific paper

10.1086/426009

Deviations of galaxy groups from cluster scaling relations can be understood in terms of an excess of entropy in groups. The main effect of this excess is to reduce the density and thus luminosity of the intragroup gas. Given this, groups should also should show a steep relationship between X-ray luminosity and velocity dispersion. However, previous work suggests that this is not the case with many measuring slopes flatter than the cluster relation. Examining the group L_X:\sigma relation shows that much of the flattening is caused by a small subset of groups which show very high X-ray luminosities for their velocity dispersions (or vice versa). Detailed Chandra study of two such groups shows that earlier ROSAT results were subject to significant (~30-40%) point source contamination, but confirm that a significant hot IGM is present in these groups, although these are two of the coolest systems in which intergalactic X-ray emission has been detected. Their X-ray properties are shown to be broadly consistent with those of other galaxy groups, although the gas entropy in NGC 1587 is unusually low, and its X-ray luminosity correspondingly high for its temperature, compared to most groups. This leads us to suggest that the velocity dispersion in these systems has been reduced in some way, and we consider how this might have come about.

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