Coma Cluster: Hot and Cool Mixture

Details Coma Cluster: Hot and Cool Mixture Coma Cluster: Hot and Cool Mixture

Jun 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996pasj...48l..37i&link_type=abstract

Publications of the Astronomical Society of Japan, v.48, p.L37-L39.

Astronomy and Astrophysics

Astronomy

18

Clusters Of Galaxies: Individual (Coma Cluster), Galaxies: Intergalac Tic Medium, Hydrodynamics

Scientific paper

ASCA has revealed a rather complex temperature structure in the intraclus ter medium (ICM) around the Coma cluster. Significantly, hot parts (with kT g eq 10 keV) are located far ( ~ 1 Mpc) distant from both the center of the Coma cluster and the galaxy group NGC 4839. There also exist relatively cool re gions (with kT <~ 5 keV). Using N-body + Hydrodynamic simulations, w e have demonstrated that such an observed temperature distribution is naturally accounted for if the subgroup NGC 4839 passed through the center of the Coma c luster about 1 Gyr ago, which was first proposed by Burns et al. When the subc luster passed through the Coma cluster, the ICM in the subcluster was compresse d due to the ram pressure by the ICM in the Coma, and there formed a bow shock with an arc shape just between the two centers. The ICM has thus been heated th ere, emitting hard radiation. A part of the ICM is reflected by the shock front , and flows backward (with respect to the! direction of the subcluster motio n) around the Coma cluster center, being cooled due to an adiabatic expansion. After detouring the center, cooled gas collides with each other at the opposit e side of the Coma cluster (to the place of the subcluster), producing another hot region. These simulate d features are in good agreement with what ASCA found. Further, we present rath er unique features in the temperature profiles that can be caused by a merger ( or an encounter) with a subgroup of galaxies.

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