2011ApJ...734...95M


Query : 2011ApJ...734...95M

2011ApJ...734...95M - Astrophys. J., 734, 95 (2011/June-3)

Star formation efficiency in the cool cores of galaxy clusters.

McDONALD M., VEILLEUX S., RUPKE D.S.N., MUSHOTZKY R. and REYNOLDS C.

Abstract (from CDS):

We have assembled a sample of high spatial resolution far-UV (Hubble Space Telescope Advanced Camera for Surveys/Solar Blind Channel) and Hα (Maryland-Magellan Tunable Filter) imaging for 15 cool core galaxy clusters. These data provide a detailed view of the thin, extended filaments in the cores of these clusters. Based on the ratio of the far-UV to Hα luminosity, the UV spectral energy distribution, and the far-UV and Hα morphology, we conclude that the warm, ionized gas in the cluster cores is photoionized by massive, young stars in all but a few (A1991, A2052, A2580) systems. We show that the extended filaments, when considered separately, appear to be star forming in the majority of cases, while the nuclei tend to have slightly lower far-UV luminosity for a given Hα luminosity, suggesting a harder ionization source or higher extinction. We observe a slight offset in the UV/Hα ratio from the expected value for continuous star formation which can be modeled by assuming intrinsic extinction by modest amounts of dust (E(B - V) ∼ 0.2) or a top-heavy initial mass function in the extended filaments. The measured star formation rates vary from ∼0.05 M/yr in the nuclei of non-cooling systems, consistent with passive, red ellipticals, to ∼5 M/yr in systems with complex, extended, optical filaments. Comparing the estimates of the star formation rate based on UV, Hα, and infrared luminosities to the spectroscopically determined X-ray cooling rate suggests a star formation efficiency of 14+18_- 8_%. This value represents the time-averaged fraction, by mass, of gas cooling out of the intracluster medium, which turns into stars and agrees well with the global fraction of baryons in stars required by simulations to reproduce the stellar mass function for galaxies. This result provides a new constraint on the efficiency of star formation in accreting systems.

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: 19

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Number of rows : 19
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 426 ClG 03 19 47.2 +41 30 47           ~ 2116 1
2 3C 84 Sy2 03 19 48.1599902040 +41 30 42.108850836   13.10 12.48 11.09   ~ 3805 3
3 ACO 970 ClG 10 17 34.3 -10 42 01           ~ 81 0
4 MKW 3 ClG 11 48 29 -03 10.7     14.88     ~ 51 1
5 ACO 1644 ClG 12 57 11.6 -17 24 34           ~ 346 1
6 ACO 1650 ClG 12 58 36.76 -01 43 34.2           ~ 280 0
7 ACO 1795 ClG 13 49 00.5 +26 35 07           ~ 1205 0
8 ACO 1837 ClG 14 01 36.2 -11 07 48           ~ 101 0
9 ACO 1991 ClG 14 54 30.2 +18 37 51           ~ 315 1
10 ACO 2029 ClG 15 10 58.7 +05 45 42           ~ 896 0
11 ACO 2052 ClG 15 16 45.5 +07 00 01           ~ 703 1
12 ACO 2142 ClG 15 58 20.00 +27 14 00.3           ~ 718 0
13 ACO 2151 ClG 16 05 15.0 +17 44 55           ~ 570 3
14 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3396 1
15 NAME Oph Cluster ClG 17 12 24.7 -23 21 01           ~ 259 0
16 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 13179 0
17 ACO 2580 ClG 23 21 23.3 -23 11 16           ~ 48 0
18 ACO 2597 ClG 23 25 19.70 -12 07 27.7           ~ 519 0
19 ACO 4059 ClG 23 56 40.7 -34 40 18           ~ 368 1

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2022.09.26-09:29:05

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