–¼ŒÃ‰®‘åŠwUŒ¤XüƒOƒ‹[ƒv
–¼ŒÃ‰®‘åŠw‘åŠw‰@—ŠwŒ¤‹†‰È@‘f—±Žq‰F’ˆ•¨—ŠwêU@‰F’ˆ•¨—ŠwŒ¤‹†Žº
§464-8602 @–¼ŒÃ‰®ŽsçŽí‹æ•s˜V’¬@Tel:052-789-2921@Fax:052-789-2919
 
Home Uir Site map English
ƒwƒbƒ_[
Œ¤‹†ŽºÐ‰î Œ¤‹†ƒvƒƒWƒFƒNƒg Œ¤‹†ŠT—v Œ¤‹†¬‰Ê ƒAƒNƒZƒXƒ}ƒbƒv ‚¨–â‚¢‡‚킹 ŠÖ˜AƒŠƒ“ƒN
Œ¤‹†¬‰Ê
˜_•¶
˜_•¶ƒŠƒXƒgEnglish
1990~1999
˜_•¶ƒŠƒXƒgEnglish
2000~
˜_•¶ƒŠƒXƒg
”ŽŽm˜_•¶ƒŠƒXƒg
CŽm˜_•¶ƒŠƒXƒg
V•·‹LŽ–
 
publication
Statistical Approach to X-ray Properties of Hot Gas in Cluster of Galaxies

Fumie Akimoto, M. Watanabe, A. Furuzawa, Y. Tawara, H. Kumai, S, Satoh and K. Yamashita

Abstract

X-ray properties of 35 clusters of galaxies(z=0.004-0.37) observed with ASCA are presented. These are classified from group of galaxies to rich cluster of galaxies. We analysed their X-ray spectra and X-ray images using common manner to minimize systematic deviation due to instrumental characteristics, and obtained following physical parameters and their ranges; X-ray luminosity Lx(1040-46 erg s-1), flux-weighted temperature kT(0.7-12keV), iron abundance (0.07-0.6 solar), parameters for surface brightness distribution(core radius Rc(<300 kpc), beta(0.3-0.9)), and the gas mass and gravitational mass, etc. Based on this analysis the results were compared with the each other and also with optical properties taken from the literature, such as velocity dispersion, galaxy number density, and cluster morphological type. From their correlations, we investigate structure and evolution of hot gas from the galaxy to group or cluster of galaxies.

 
Copyright (c) 2008 Nagoya University . All Rights Reserved.  
 
ƒgƒbƒvƒy[ƒW‚É–ß‚é