Evaporation and Excess X-Ray Emission from the Central Giant Galaxy in a Cluster of Galaxies

Abstract

Evaporation of gas from the central giant galaxy in a cluster of galaxies is investigated in connection with the point source in its extended X-ray source. We calculate the stationary outflow of the gas supplied by the stellar mass loss and heated by the conduction from the hot intracluster gas. The central point source identified with M87 in the Virgo cluster of galaxies can be well explained by the X-ray emission from the outflowing gas in the central massive galaxy. However, the point source identified with NGC 1275 in the Perseus cluster of galaxies can be explained only if the central galaxy is as massive as 10"M<;:> and its three-dimensional velocity dispersion exceeds 10 3 km/sec. of the extended source, while in the cooling model the softening of the energy spectrum is expected. These observations suggest that the heat conduction works very effectively.Secondly, according to the large accretion rate they have suggested, 30"'-'100 M 0 /y, the cool gas should accumulate in the central galaxy as much as 3 X 10 11 at East Tennessee State University on May 30, 2015

Uniformity in the Temperature and Metallicity of the X-Ray Emitting Gas in the Abell 1060 Cluster of Galaxies

“…Thus, the ram-pressure stripping will not work, and much of their ISM will remain trapped in the local galaxy potential, which has a virial temperature of ~ 1 keV. To insulate the ISM against heat conduction from ICM (Takahara, Takahara 1979), and to suppress the radiative cooling instability, magnetic fileds may be needed (Rosner, Tucker 1989;Makishima 1994Makishima , 1995aMakishima , 1995b. Since the ISM must be metal enriched by the type-la SNe in the cD galaxy over the Hubble time, we thus expect a metal concentration and cool emission to occur within the cD potential.…”

Stable Heating of Cluster Cooling Flows by Cosmic-Ray Streaming

“…Many mechanisms for heat sources of the ICM have been proposed. Thermal conduction from the hot outer layers of clusters is one popular idea (Takahara & Takahara 1979, 1981Tucker & Rosner 1983). This model may work for clusters with a middle or high temperature if the conductivity is ∼ 30% of the Spitzer one (Zakamska & Narayan 2003).…”

Tsunamis in Galaxy Clusters: Heating of Cool Cores by Acoustic Waves

“…Numerical simulations suggest that buoyant bubbles created by the AGNs mix and heat the ambient ICM to some extent (Churazov et al 2001;Quilis, Bower, & Balogh 2001;Saxton, Sutherland, & Bicknell 2001;Brüggen & Kaiser 2002;Basson & Alexander 2003). The other possible heat source is thermal conduction from the hot outer layers of clusters (Takahara & Takahara 1979, 1981Tucker & Rosner 1983;Friaca 1986;Gaetz 1989;Böhringer & Fabian 1989;Sparks 1992;Saito & Shigeyama 1999;Narayan & Medvedev 2001).…”