Abstract
The dominant X-ray emission from galaxy clusters is very likely to be thermal Bremsstrahlung from a diffuse, hot intracluster medium (ICM) with maximum density n ≃ 10−3 cm−3, temperature T ≃ 108 °K and near-solar composition. The main evidence is based on integrated spectra: shape and intensity of the continuum, and strength of very high excitation lines up to Fe XXV and XXVI in several clusters (Mushotzky et al. 1978 and references therein).In dependent evidence of a dense hot ICM extending out to several core radii rc has been provided by the discovery and the interpretation of “head-tail” radio galaxies (TRG, reviewed by Harris 1977). Direct evidence of extended X-ray emission had been obtained from coarse scannings by the UHURU satellite (cf. Gursky and Schwartz 1977) and from imaging observations of Perseus and Coma Clusters (Gorenstein et al. 1978, 1979).
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
