2011ApJ...731...33M


Query : 2011ApJ...731...33M

2011ApJ...731...33M - Astrophys. J., 731, 33 (2011/April-2)

The effect of environment on the formation of hα filaments and cool cores in galaxy groups and clusters.

McDONALD M., VEILLEUX S. and MUSHOTZKY R.

Abstract (from CDS):

We present the results of a combined X-ray and Hα study of 10 galaxy groups and 17 galaxy clusters using the Chandra X-ray Observatory and the Maryland Magellan Tunable Filter. We find no difference in the morphology or detection frequency of Hα filaments in groups versus clusters over the mass range 1013 < M500< 1015 M. The detection frequency of Hα emission is shown to be only weakly dependent on the total mass of the system at the 52% confidence level. In contrast, we find that the presence of Hα filaments is strongly correlated with both the global (89% confidence level) and core (84%) intracluster medium (ICM) entropy, as well as the X-ray cooling rate (72%). The Hα filaments are therefore an excellent proxy for the cooling ICM. The Hα filaments are more strongly correlated with the cooling properties of the ICM than with the radio properties of the brightest cluster galaxy; this further supports the scenario where these filaments are directly associated with a thermally unstable, rapidly cooling ICM, rather than radio bubbles. The ICM cooling efficiency, defined as the X-ray cooling rate per unit gas mass, is shown to correlate with the total system mass, indicating that groups are more efficient at cooling than clusters. This result implies that, in systems with cool cores, active galactic nucleus feedback scales with the total mass of the system, in agreement with earlier suggestions.

Abstract Copyright:

Journal keyword(s): galaxies: active - galaxies: clusters: general - galaxies: clusters: intracluster medium - galaxies: elliptical and lenticular, cD - galaxies: star formation - ISM: jets and outflows

Simbad objects: 32

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Number of rows : 32
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 ACO 85 ClG 00 41 37.8 -09 20 33           ~ 844 0
2 ACO 133 ClG 01 02 39.0 -21 57 15           ~ 351 1
3 UGC 842 BLL 01 18 53.6237165304 -01 00 07.248153600   15.0       ~ 64 1
4 RXC J0252.8-0116 ClG 02 52 49.4 -01 16 27           ~ 101 0
5 NGC 1132 GiG 02 52 51.82 -01 16 29.0   13.9   12.16   ~ 157 0
6 ACO 426 ClG 03 19 47.2 +41 30 47           ~ 2118 1
7 3C 84 Sy2 03 19 48.1599902040 +41 30 42.108850836   13.10 12.48 11.09   ~ 3808 3
8 NAME III ZW 54 Group ClG 03 41 16.9 +15 24 27           ~ 39 0
9 ACO 3158 ClG 03 42 39.6 -53 37 50           ~ 284 0
10 ACO 478 ClG 04 13 20.7 +10 28 35           ~ 482 0
11 ACO 496 ClG 04 33 30.3838 -13 14 21.584           ~ 671 2
12 ACO 3376 ClG 06 01 25.000 -39 59 51.00           ~ 286 0
13 ACO 644 ClG 08 17 24.5 -07 30 46           ~ 210 0
14 ACO 744 ClG 09 07 20.0 +16 39 25           ~ 76 0
15 NAME Hya A LIN 09 18 05.6783347248 -12 05 43.634531472   14.38 14.8     ~ 964 1
16 ACO 780 ClG 09 18 30 -12 15.7           ~ 445 0
17 NGC 3411 BiC 10 50 26.0811795768 -12 50 42.313849764   9.0   11.60   ~ 69 1
18 ACO 1139 ClG 10 58 10.98 +01 36 16.4           ~ 153 3
19 NAME NGC 4073 Group GrG 12 04 21.7 +01 50 19     13.53     ~ 255 0
20 1RXS J122306.6+103722 ClG 12 23 06.5 +10 37 26           ~ 45 0
21 NGC 4325 BiC 12 23 06.662 +10 37 16.45   15.0       ~ 123 1
22 ACO 1644 ClG 12 57 11.6 -17 24 34           ~ 346 1
23 ACO 1650 ClG 12 58 36.76 -01 43 34.2           ~ 280 0
24 ACO 1795 ClG 13 49 00.5 +26 35 07           ~ 1205 0
25 ACO 1991 ClG 14 54 30.2 +18 37 51           ~ 315 1
26 ACO 2029 ClG 15 10 58.7 +05 45 42           ~ 896 0
27 ACO 2052 ClG 15 16 45.5 +07 00 01           ~ 703 1
28 ACO 2142 ClG 15 58 20.00 +27 14 00.3           ~ 718 0
29 ACO 2151 ClG 16 05 15.0 +17 44 55           ~ 570 3
30 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3396 1
31 ACO S 1101 ClG 23 13 58.5 -42 43 39           ~ 243 1
32 ACO 4059 ClG 23 56 40.7 -34 40 18           ~ 369 1

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2022.09.28-03:13:02

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