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For refcode 1996AJ....112..378P:
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1996AJ....112..378P PROPERTIES OF SIMULATED COMPACT GROUPS OF GALAXIES RACHEL A. PILDIS Department of Astronomy, University of Michigan, Ann Arbor, Michigan 48109-1090 Electronic mail: rpildis@cfa.harvard.edu AUGUST E. EVRARD Department of Physics, University of Michigan, Ann Arbor, Michigan 48109-1120 Electronic mail: evrard@umich.edu JOEL N. BREGMAN Department of Astronomy, University of Michigan, Ann Arbor, Michigan 48109-1090 Electronic mail: jbregman@astro.lsa.umich.edu Received 1995 December 13; revised 1996 April 17 ABSTRACT We analyze compact groups of galaxies appearing in a galaxy formation simulation dominated by cold dark matter ({OMEGA}_0_ = 1, {OMEGA}_baryon_ = 0 1). The simulation uses an N-body code to model the behavior of the non-baryonic matter and smoothed particle hydrodynamics to model the baryons. One run includes gas dynamics alone, and the other incorporates star formation as well. Groups identified as physically compact at z = 0 form originally along filaments and become compact in the final ~20% of the simulation; they contain x-ray-luminous diffuse gas well before becoming compact. The component masses, baryon fractions, and gas-to- galaxy mass fractions of the simulated groups are roughly similar to those of Hickson compact groups (HCGs), although they tend to be somewhat more gas rich and have x-ray temperatures a factor of 3 lower than those seen in HCGs. These discrepancies may be alleviated by adding the effects of energy input into the diffuse group gas by star formation and supernovae.
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