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CHANDRA observations of the NGC 1550 galaxy group -- implication for the temperature and entropy profiles of 1 keV galaxy groups | M. Sun
; W. Forman
; A. Vikhlinin
; A. Hornstrup
; C. Jones
; S. S. Murray
; | Date: |
3 Aug 2003 | Journal: | Astrophys.J. 598 (2003) 250-259 | Subject: | astro-ph | Abstract: | We present a detailed chandra study of the galaxy group NGC 1550. For its temperature (1.37$pm$0.01 keV) and velocity dispersion ($sim$ 300 km s$^{-1}$), the NGC 1550 group is one of the most luminous known galaxy groups (L$_{
m bol}$ = 1.65$ imes10^{43}$ erg s$^{-1}$ within 200 kpc, or 0.2
v). We find that within $sim 60$ kpc, where the gas cooling time is less than a Hubble time, the gas temperature decreases continuously toward the center, implying the existence of a cooling core. The temperature also declines beyond $sim$ 100 kpc (or 0.1
v). There is a remarkable similarity of the temperature profile of NGC 1550 with those of two other 1 keV groups with accurate temperature determination. The temperature begins to decline at 0.07 - 0.1
v, while in hot clusters the decline begins at or beyond 0.2
v. Thus, there are at least some 1 keV groups that have significantly different temperature profiles from those of hot clusters, which may reflect the role of non-gravitational processes in ICM/IGM evolution. NGC 1550 has no isentropic core in its entropy profile, in contrast to the predictions of `entropy-floor’ simulations. We compare the scaled entropy profiles of three 1 keV groups (including NGC 1550) and three 2 - 3 keV groups. The scaled entropy profiles of 1 keV groups show much larger scatter than those of hotter systems, which implies varied pre-heating levels. We also discuss the mass content of the NGC 1550 group and the abundance profile of heavy elements. | Source: | arXiv, astro-ph/0308037 | Services: | Forum | Review | PDF | Favorites |
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