Other
Scientific paper
Jan 2012
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21932904c&link_type=abstract
American Astronomical Society, AAS Meeting #219, #329.04
Other
Scientific paper
The majority of galaxies in the Universe lie in galaxy groups which range from 'poor' systems containing few galaxies (commonly identified via optical selection methods) to massive groups (often identified via X-ray emission from the Intra-Group Medium, IGM). In order to study groups spanning a significant mass and evolutionary range, we have defined two samples at a mean redshift of 0.4, one via optical spectroscopy and the other via X-ray emission. By comparing both the global properties and those of the galaxy populations of these two samples, we aim to illuminate the roles of galaxy interactions and mergers (prevalent in the 'poor', dynamically active systems) and the IGM (dominant in the more massive, evolved groups) in shaping the local galaxy population. I focus first on the global properties and scaling relations of our systems, presenting our findings regarding group definition, masses and mass fractions, dynamical complexity, and evidence for a population of X-ray underluminous systems. I then combine knowledge of these global group properties with galaxy composition in order to explore galaxy evolution, differentiating between the effects of age, mass, and the IGM on observed galaxy properties.
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