Date:
Tue, 19/05/200912:15-13:15
Location:
Kaplun Bldg, seminar room, 2nd floor
Non-Thermal and Thermal Plasma in Clusters of Galaxies
Clusters of galaxies are the largest relaxed systems in the Universe, and contain hundreds of galaxies a regions which are several Mpc across. The dominant form of baryonic matter is clusters is hot intracluster gas, which has more mass than the stars and galaxies by a factor of about 5. I will describe recent result on two aspects of the nonthermal and thermal content of the intracluster medium. First, the results of recent searches with Suzaku for nonthermal Inverse Compton (IC) emission from clusters will be presented. The X-ray bright, nearby galaxy clusters Coma and Abell 3667 host the brightest radio halo (Coma) and radio relic (A3667) known. These diffuse, Mpc-scale structures are due to synchrotron emission from relativistic electrons, which also produce hard X-ray inverse Compton (IC) emission. The high sensitivity and narrow FOV of the Suzaku PIN Hard X-ray Detector makes it an ideal instrument to search for IC. I will present 180 ks and 95 ks Suzaku observations of the Coma and A3667 clusters, respectively, as well as mosaic XMM-Newton observations of the clusters. The XMM-Newton mosaics allow us to directly determine the thermal emission within the HXD-PIN FOV. Second, I will discuss recent radio and X-ray observations of the central regions of cool core clusters. The nature of the interaction for the central radio sources and X-ray gas will be described.
Clusters of galaxies are the largest relaxed systems in the Universe, and contain hundreds of galaxies a regions which are several Mpc across. The dominant form of baryonic matter is clusters is hot intracluster gas, which has more mass than the stars and galaxies by a factor of about 5. I will describe recent result on two aspects of the nonthermal and thermal content of the intracluster medium. First, the results of recent searches with Suzaku for nonthermal Inverse Compton (IC) emission from clusters will be presented. The X-ray bright, nearby galaxy clusters Coma and Abell 3667 host the brightest radio halo (Coma) and radio relic (A3667) known. These diffuse, Mpc-scale structures are due to synchrotron emission from relativistic electrons, which also produce hard X-ray inverse Compton (IC) emission. The high sensitivity and narrow FOV of the Suzaku PIN Hard X-ray Detector makes it an ideal instrument to search for IC. I will present 180 ks and 95 ks Suzaku observations of the Coma and A3667 clusters, respectively, as well as mosaic XMM-Newton observations of the clusters. The XMM-Newton mosaics allow us to directly determine the thermal emission within the HXD-PIN FOV. Second, I will discuss recent radio and X-ray observations of the central regions of cool core clusters. The nature of the interaction for the central radio sources and X-ray gas will be described.