2012A&A...543A..33V

Query : 2012A&A...543A..33V

2012A&A...543A..33V - Astronomy and Astrophysics, volume 543A33-33 (2012/7-1)

The influence of the cluster environment on the star formation efficiency of 12 Virgo spiral galaxies.

VOLLMER B., WONG O.I., BRAINE J., CHUNG A. and KENNEY J.D.P.

Abstract (from CDS):

The influence of the environment on gas surface density and star formation efficiency of cluster spiral galaxies is investigated. We extend previous work on radial profiles by a pixel-to pixel analysis looking for asymmetries due to environmental interactions. The star formation rate is derived from GALEX UV and Spitzer total infrared data based on the 8, 24, 70, and 160µm data. As in field galaxies, the star formation rate for most Virgo galaxies is approximately proportional to the molecular gas mass. Except for NGC 4438, the cluster environment does not affect the star formation efficiency with respect to the molecular gas. Gas truncation is not associated with major changes in the total gas surface density distribution of the inner disk of Virgo spiral galaxies. In three galaxies (NGC 4430, NGC 4501, and NGC 4522), possible increases in the molecular fraction and the star formation efficiency with respect to the total gas, of factors of 1.5 to 2, are observed on the windward side of the galactic disk. A significant increase of the star formation efficiency with respect to the molecular gas content on the windward side of ram pressure-stripped galaxies is not observed. The ram-pressure stripped extraplanar gas of 3 highly inclined spiral galaxies (NGC 4330, NGC 4438, and NGC 4522) shows a depressed star formation efficiency with respect to the total gas, and one of them (NGC 4438) shows a depressed rate even with respect to the molecular gas. The interpretation is that stripped gas loses the gravitational confinement and associated pressure of the galactic disk, and the gas flow is diverging, so the gas density decreases and the star formation rate drops. We found two such regions of low star formation efficiency in the more face-on galaxies NGC 4501 and NGC 4654 which are both undergoing ram pressure stripping. These regions show low radio continuum emission or unusually steep radio spectral index. However, the stripped extraplanar gas in one highly inclined galaxy (NGC 4569) shows a normal star formation efficiency with respect to the total gas. We propose this galaxy is different because it is observed long after peak pressure, and its extraplanar gas is now in a converging flow as it resettles back into the disk.

Abstract Copyright: ∼

Journal keyword(s): galaxies: interactions - galaxies: ISM - galaxies: kinematics and dynamics - galaxies: clusters: individual: Virgo

Simbad objects: 34

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Number of rows : 34
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 Z 477-40 LIN 00 01 38.3220061296 +23 29 01.190922432   13.2       ~ 159 1
2 Z 551-12 GiG 01 16 16.614 +46 44 23.50   14.6       ~ 54 1
3 M 74 G 01 36 41.7451236624 +15 47 01.107512304 10.52 10.00 9.46 9.16   ~ 1934 1
4 NGC 925 H2G 02 27 16.913 +33 34 43.97   10.69 10.12 9.55   ~ 818 1
5 NGC 2403 AGN 07 36 51.3381434280 +65 36 09.650825640 9.31 8.84 8.38 8.19   ~ 1887 1
6 NGC 2841 LIN 09 22 02.6778711696 +50 58 35.737082868 10.43 10.09 9.22     ~ 1113 1
7 NGC 3198 EmG 10 19 54.990 +45 32 58.88 10.83 10.87 10.33     ~ 946 1
8 NGC 3226 rG 10 23 27.0064075320 +19 53 54.674937420   14.32 13.33     ~ 440 1
9 NGC 3227 Sy1 10 23 30.5765149296 +19 51 54.282206700   12.61 11.79     ~ 1807 2
10 M 95 GiP 10 43 57.7313485800 +11 42 13.301191332 10.71 10.51 9.73 9.48   ~ 1238 2
11 NGC 3521 EmG 11 05 48.5680991376 -00 02 09.245076540 10.06 9.83 9.02 10.1 9.6 ~ 879 2
12 M 66 AGN 11 20 15.0 +12 59 29 9.85 9.65 8.92     ~ 1509 4
13 M 99 H2G 12 18 49.625 +14 24 59.36 10.45 10.44 9.87     ~ 1004 2
14 M 100 AGN 12 22 54.9299993592 +15 49 20.296257960 10.04 10.05 9.35     ~ 1963 2
15 NGC 4330 GiG 12 23 17.249 +11 22 04.73   14.0       ~ 246 0
16 NGC 4402 GiC 12 26 07.65312 +13 06 47.9376   12.55       ~ 421 2
17 M 86 GiG 12 26 11.814 +12 56 45.49 10.32 9.83 8.90   7.50 ~ 1126 1
18 NGC 4419 LIN 12 26 56.4505296720 +15 02 50.688833388 12.42 12.08 11.16     ~ 419 2
19 NGC 4430 GiG 12 27 26.4060329472 +06 15 45.972776664   13.4       ~ 168 0
20 NGC 4435 GiG 12 27 40.503 +13 04 44.48 12.23 11.74 10.80     ~ 474 2
21 NGC 4438 LIN 12 27 45.6705493536 +13 00 31.708096380 11.37 11.02 10.17     ~ 668 2
22 NAME Virgo Cluster ClG 12 30 47.8 +12 23 07           ~ 7107 0
23 M 87 AGN 12 30 49.42338414 +12 23 28.0436859 10.16 9.59 8.63   7.49 ~ 7815 3
24 M 88 Sy2 12 31 59.1525062448 +14 25 13.148971824   14.33 13.18     ~ 843 1
25 NGC 4522 GiG 12 33 39.657 +09 10 29.54   13.6       ~ 396 0
26 NGC 4535 H2G 12 34 20.3443516704 +08 11 51.908488116   11.1       ~ 679 0
27 M 91 LIN 12 35 26.4446761320 +14 29 46.760333748   14.63 13.57     ~ 639 0
28 M 90 Sy2 12 36 49.8009839880 +13 09 46.523813040 10.56 10.26 9.54     ~ 953 1
29 M 58 Sy2 12 37 43.59747 +11 49 05.1240 10.80 10.48 9.66     ~ 1140 2
30 NGC 4654 H2G 12 43 56.638 +13 07 34.86   11.8       ~ 600 1
31 M 63 LIN 13 15 49.2741893928 +42 01 45.728076108   9.34 8.59 8.35   ~ 1292 2
32 M 101 GiP 14 03 12.583 +54 20 55.50   8.46 7.86 7.76   ~ 3138 2
33 NAME Stephan's Quintet CGG 22 35 57.5 +33 57 36           ~ 480 1
34 NGC 7331 LIN 22 37 04.0506038088 +34 24 56.800076508 10.65 10.35 9.48     ~ 1284 2

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