A Census of Poor Groups: Hot Gas, Cold Gas, and Galaxies

Details A Census of Poor Groups: Hot Gas, Cold Gas, and Galaxies A Census of Poor Groups: Hot Gas, Cold Gas, and Galaxies

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003assl..281..291z&link_type=abstract

The IGM/Galaxy Connection: The Distribution of Baryons at z=0, ASSL Conference Proceedings Vol. 281. Edited by Jessica L. Rosenb

Computer Science

2

Scientific paper

Poor groups are common environments for galaxies, but we know relatively little about what fraction of all baryons lie in groups, how those baryons are distributed spatially, how group baryons are divided among stars and gas, and how the intragroup medium evolves. Our first attempts to answer these questions using groups outside the Local Group yield some surprising results. Groups are important baryon reservoirs in the local Universe, at least as important as rich clusters of galaxies. In groups with luminous X-ray halos, the galaxy and hot gas distributions have multiple components: the dwarf and giant populations occupy different orbits, and the X-ray emission from the central giant elliptical is distinct from that of the diffuse, intragroup medium. Cold, neutral hydrogen gas is detected only in group members --- we find no evidence for high velocity cloud analogs. The similarity of the temperature-luminosity-velocity dispersion relations for X-ray luminous groups and rich clusters suggests that the intergroup and intracluster media evolve in the same manner (whether these relations change for lower mass groups is still controversial). Finally, observations suggest that at least some giant field ellipticals evolve from poor groups, and that different classes of groups give rise to gE's with different X-ray and optical properties.

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