–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

ASCA observation of three bright early-type galaxies: NGC 4472, NGC 4406, and NGC 4636

H. Awaki, R. Mushotzky, T. Tsuru, A.C. Fabian, Y. Fukazawa, M. Loewenstein, K. Makishima, H. Matsumoto, K. Matsushita, T. Mihara, T. Ohashi, G.R. Ricker, P.J. Serlemitsos, Y. Tsusaka and T. Yamazaki

Abstract

We report Advanced Satellite for Cosmology and Astrophysics (ASCA) 0.3-10 keV and X-ray observations of three early type galaxies, NGC 4472, NGC 4406, and NGC 4636. The extended mission in these galaxies is well described by thin thermal eimssion from hot gas. The gas temperature is 0.92 +/- 0.02 keV for NGC 4472, 0.79 +/- 0.01 keV for NGC 4406, and 0.73 +/- 0.02 keV for NGC 4636. The metal abundance for NGC 4472, NGC 4406, and NGC 4636 are, under the assumption of solar ratios, 0.63 +/- 0.15, 0.45 +/- 0.10, and 0.38 +/- 0.07, respectively. Detailed analysis has allowed determination of the abundances of oxygen, silicon, sulfur, and iron. The observed abundances are consistent with the solar ratios. For NGC 4472 and NGC 4406 we also determined the mean temperature of the gas producing the Si lines from the ratio of the Si H to He-like lines and find it to be consistent with the continuum temperature. The X-ray temperature is in good agreement with the observed optical velocity dispersion, stellar density profile, and gas density profile. Our data indicates that the supernova rate should be less than one fifth of the nominal rate in early type galaxies. We derive the mass of these systems within fixed angular scales and find that M/L greater than 40, confirming that elliptical galaxies are dark matter dominated at large radii.

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