2009A&A...497..713B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.06CEST21:53:17

2009A&A...497..713B - Astronomy and Astrophysics, volume 497, 713-728 (2009/4-3)

Frequency and properties of bars in cluster and field galaxies at intermediate redshifts.

BARAZZA F.D., JABLONKA P., DESAI V., JOGEE S., ARAGON-SALAMANCA A., DE LUCIA G., SAGLIA R.P., HALLIDAY C., POGGIANTI B.M., DALCANTON J.J., RUDNICK G., MILVANG-JENSEN B., NOLL S., SIMARD L., CLOWE D.I., PELLO R., WHITE S.D.M. and ZARITSKY D.

Abstract (from CDS):

We present a study of large-scale bars in field and cluster environments out to redshifts of ∼0.8 using a final sample of 945 moderately inclined disk galaxies drawn from the EDisCS project. We characterize bars and their host galaxies and look for relations between the presence of a bar and the properties of the underlying disk. We investigate whether the fraction and properties of bars in clusters are different from their counterparts in the field. The properties of bars and disks are determined by ellipse fits to the surface brightness distribution of the galaxies using HST/ACS images in the F814W filter. The bar identification is based on quantitative criteria after highly inclined (>60°) systems have been excluded. The total optical bar fraction in the redshift range z=0.4-0.8 (median z=0.60), averaged over the entire sample, is 25% (20% for strong bars). For the cluster and field subsamples, we measure bar fractions of 24% and 29%, respectively. We find that bars in clusters are on average longer than in the field and preferentially found close to the cluster center, where the bar fraction is somewhat higher (∼31%) than at larger distances (∼18%). These findings however rely on a relatively small subsample and might be affected by small number statistics. In agreement with local studies, we find that disk-dominated galaxies have a higher optical bar fraction (∼45%) than bulge-dominated galaxies (∼15%). This result is based on Hubble types and effective radii and does not change with redshift. The latter finding implies that bar formation or dissolution is strongly connected to the emergence of the morphological structure of a disk and is typically accompanied by a transition in the Hubble type. The question whether internal or external factors are more important for bar formation and evolution cannot be answered definitely. On the one hand, the bar fraction and properties of cluster and field samples of disk galaxies are quite similar, indicating that internal processes are crucial for bar formation. On the other hand, we find evidence that cluster centers are favorable locations for bars, which suggests that the internal processes responsible for bar growth are supported by the typical interactions taking place in such environments.

Abstract Copyright:

Journal keyword(s): galaxies: spiral - galaxies: structure - galaxies: clusters: general - galaxies: evolution - galaxies: formation

Simbad objects: 20

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Number of rows : 20

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 ACO 901 ClG 09 55 56.9256 -10 01 46.519           ~ 100 1
2 ACO 902 ClG 09 56 33.600 -10 09 13.10           ~ 57 1
3 ClG J1037-1243 ClG 10 37 52.6 -12 43 44           ~ 39 0
4 [MNH2008] cl J1037.9-1243a ClG 10 37.9 -12 43           ~ 10 0
5 ClG J1040-1155 ClG 10 40 41.6 -11 55 51           ~ 55 0
6 ClG J1054-1146 ClG 10 54 24.2 -11 46 18           ~ 50 0
7 ClG J1054-1245 ClG 10 54 43.5 -12 45 50           ~ 54 0
8 ClG J1103-1246 ClG 11 03 34.9 -12 46 46           ~ 20 0
9 ClG J1103-1244 ClG 11 03 36.5 -12 44 22           ~ 18 0
10 ClG J1103-1245 ClG 11 03 42.9 -12 45 18           ~ 16 1
11 ClG J1138-1133 ClG 11 38 10.3 -11 33 59           ~ 44 0
12 [MNH2008] cl J1138.2-1133a ClG 11 38.2 -11 33           ~ 13 0
13 ClG J1216-1201 ClG 12 16 45.10 -12 01 17.3           ~ 66 0
14 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5824 0
15 ClG J1227-1138 ClG 12 27 53.9 -11 38 20           ~ 45 0
16 [MNH2008] cl J1227.9-1138a ClG 12 27.9 -11 38           ~ 10 0
17 ClG J1232-1250 ClG 12 32 30.5 -12 50 33           ~ 48 0
18 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4208 2
19 ClG J1354-1230 ClG 13 54 09.5 -12 30 59           ~ 45 0
20 [MNH2008] cl J1354.2-1230a ClG 13 54.2 -12 30           ~ 9 0

    Equat.    Gal    SGal    Ecl

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2020.07.06-21:53:17

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