2005A&A...431..433C


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.08CET02:40:19

2005A&A...431..433C - Astronomy and Astrophysics, volume 431, 433-449 (2005/2-4)

An ISOCAM survey through gravitationally lensing galaxy clusters. IV. Luminous infrared galaxies in Cl 0024+1654 and the dynamical status of clusters.

COIA D., McBREEN B., METCALFE L., BIVIANO A., ALTIERI B., OTT S., FORT B., KNEIB J.-P., MELLIER Y., MIVILLE-DESCHENES M.-A., O'HALLORAN B. and SANCHEZ-FERNANDEZ C.

Abstract (from CDS):

Observations of the core of the massive cluster Cl 0024+1654, at a redshift z∼0.39, were obtained with the Infrared Space Observatory using ISOCAM at 6.7µm (hereafter 7µm) and 14.3µm (hereafter 15µm). Thirty five sources were detected at 15µm and thirteen of them are spectroscopically identified with cluster galaxies. The remaining sources consist of four stars, one quasar, one foreground galaxy, three background galaxies and thirteen sources with unknown redshift. The sources with unknown redshift are all likely to be background sources that are gravitationally lensed by the cluster. The spectral energy distributions (SEDs) of twelve cluster galaxies were fit from a selection of 20 models using the program GRASIL. The ISOCAM sources have best-fit SEDs typical of spiral or starburst models observed 1 Gyr after the main starburst event. The star formation rates were obtained for cluster members. The median infrared luminosity of the twelve cluster galaxies is ∼1.0x1011L, with 10 having infrared luminosity above 9x1010L, and so lying near or above the 1x1011 L threshold for identification as a luminous infrared galaxy (LIRG). The [OII] star formation rates obtained for 3 cluster galaxies are one to two orders of magnitude lower than the infrared values, implying that most of the star formation is missed in the optical because it is enshrouded by dust in the starburst galaxy. The cluster galaxies in general are spatially more concentrated than those detected at 15µm. However the velocity distributions of the two categories are comparable. The colour-magnitude diagramme is given for the galaxies within the ISOCAM map. Only 20% of the galaxies that are significantly bluer than the cluster main sequence were detected at 15µm, to the limiting sensitivity recorded. The counterparts of about half of the 15µm cluster sources are blue, luminous, star-forming systems and the type of galaxy that is usually associated with the Butcher-Oemler effect. HST images of these galaxies reveal a disturbed morphology with a tendency for an absence of nearby companions. Surprisingly the counterparts of the remaining 15µm cluster galaxies lie on the main sequence of the colour-magnitude diagramme. However in HST images they all have nearby companions and appear to be involved in interactions and mergers. Dust obscuration may be a major cause of the 15µm sources appearing on the cluster main sequence. The majority of the ISOCAM sources in the Butcher-Oemler region of the colour-magnitude diagram are best fit by spiral-type SEDs whereas post-starburst models are preferred on the main sequence, with the starburst event probably triggered by interaction with one or more galaxies. Finally, the mid-infrared results on Cl 0024+1654 are compared with four other clusters observed with ISOCAM. Scaling the LIRG count in Cl 0024+1654 to the clusters Abell 370, Abell 1689, Abell 2218 and Abell 2390 with reference to their virial radii, masses, distances, and the sky area scanned in each case, we compared the number of LIRGs observed in each cluster. The number in Abell 370 is smaller than expected by about an order of magnitude, even though the two clusters are very similar in mass, redshift and optical richness. The number of LIRGs detected in each of Abell 1689, Abell 2218 and Abell 2390 is 0, whereas 3 were expected from the comparison with Cl 0024+1654. A comparison of the mid-infrared sources in Abell 1689 and Abell 2218 shows that the sources in Abell 1689 are more luminous and follow the same trend identified in the comparison between Cl 0024+1654 and Abell 370. These trends seem to be related to the dynamical status and history of the clusters.

Abstract Copyright:

Journal keyword(s): galaxies: clusters: general - galaxies: clusters: individual: Cl 0024+1654 - infrared: galaxies

Nomenclature: Table 2: ISO-Cl0024 NN (Nos 1-30). Table 3: ISO-Cl0024 Ns (Nos 1s-5s).

Simbad objects: 43

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Number of rows : 43

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 TYC 1180-82-1 * 00 26 24.3639774830 +17 08 18.087049226   11.89 11.72     ~ 1 0
2 QSO B0023+168 QSO 00 26 26.354 +17 09 38.90     19.83   19.223 ~ 11 0
3 2MASS J00262715+1709107 PM* 00 26 27.1516394489 +17 09 10.753998373   18.2   15.9   ~ 2 0
4 [SPP2015] 293 C AGN 00 26 30.80 +17 09 02.9         21.453 ~ 15 0
5 [SPP2015] 777 C EmG 00 26 30.84 +17 10 29.6         20.251 ~ 4 0
6 [MET2005] 06.628750+17.162361 GiC 00 26 30.900 +17 09 44.50         21.334 ~ 3 0
7 [SPP2015] 748 C EmG 00 26 31.0934836204 +17 10 16.435970446     20.56   18.620 ~ 15 0
8 [TEK2003] 38-3-1 GiC 00 26 31.13 +17 09 35.6         20.438 ~ 2 0
9 [MET2005] 06.632000+17.154499 EmG 00 26 31.64 +17 09 16.0         19.400 ~ 9 0
10 [MET2005] 06.632000+17.172701 GiC 00 26 31.680 +17 10 21.72         17.868 ~ 8 0
11 [MET2005] 06.633410+17.167500 EmG 00 26 32.00 +17 10 02.6           ~ 13 0
12 [TEK2003] 38-3-142 GiC 00 26 32.50 +17 09 05.9         22.166 ~ 2 0
13 ASP03 174 EmG 00 26 32.72 +17 10 24.9           ~ 8 0
14 NAME SPLIT ARC IN CL 0024+1654 LeI 00 26 34.5 +17 09 27           ~ 9 1
15 [TEK2003] 0-3-203 GiC 00 26 35.5929 +17 10 00.206         20.110 ~ 9 0
16 ISO-Cl0024 13 IR 00 26 35.9 +17 11 40           ~ 1 0
17 ZwCl 0024+1652 ClG 00 26 36.0 +17 08 36     18.35     ~ 609 1
18 [MET2005] 06.650160+17.176701 GiC 00 26 36.038 +17 10 36.12           ~ 6 0
19 ISO-Cl0024 15 IR 00 26 36.6 +17 10 25           ~ 1 0
20 [MET2005] 06.652960+17.128599 * 00 26 36.6428473235 +17 07 42.957407764           ~ 4 0
21 [TEK2003] 0-3-51 GiC 00 26 37.5995 +17 09 28.043         18.727 ~ 16 0
22 ISO-Cl0024 16 IR 00 26 37.7 +17 11 33           ~ 1 0
23 [TEK2003] 37-3-65 GiC 00 26 39.09 +17 08 04.2         20.451 ~ 3 0
24 [MET2005] 06.668917+17.157917 GiC 00 26 40.540 +17 09 28.50         17.800 ~ 8 0
25 [TEK2003] 12-2-68 GiC 00 26 40.77 +17 11 44.4         21.024 ~ 2 0
26 [MET2005] 06.670040+17.165100 GiC 00 26 40.810 +17 09 54.36         20.111 ~ 6 0
27 ASP03 2836 AGN 00 26 41.50 +17 11 02.3           ~ 5 0
28 [MET2005] 06.674670+17.164600 EmG 00 26 41.90 +17 09 53.3         18.494 ~ 17 0
29 [MET2005] 06.678667+17.161388 GiC 00 26 42.880 +17 09 41.00         20.294 ~ 6 0
30 [TEK2003] 37-4-47 AGN 00 26 42.90 +17 08 23.8         22.043 ~ 3 0
31 ISO-Cl0024 5s IR 00 26 42.9 +17 10 46           ~ 1 0
32 [TEK2003] 37-4-120 GiC 00 26 43.02 +17 08 31.9         20.863 ~ 2 0
33 [TEK2003] 37-4-158 GiC 00 26 43.1173 +17 08 49.460         18.476 ~ 6 0
34 [TEK2003] 37-4-85 EmG 00 26 43.27 +17 09 12.6         20.770 ~ 7 0
35 ISO-Cl0024 28 IR 00 26 45.5 +17 08 31           ~ 1 0
36 2MASS J00264793+1708114 * 00 26 47.9478829854 +17 08 11.544744417         15.102 ~ 2 0
37 ISO-Cl0024 30 IR 00 26 48.0 +17 09 16           ~ 1 0
38 ClG 0055-2754 ClG 00 56 56.8 -27 40 29   21.9       ~ 83 0
39 ACO 370 ClG 02 39 50.5 -01 35 08           ~ 650 0
40 ACO 1689 ClG 13 11 29.5 -01 20 28           ~ 1037 0
41 ACO 2218 ClG 16 35 54.0 +66 13 00           ~ 782 1
42 ACO 2390 ClG 21 53 34.6 +17 40 11           ~ 633 2
43 ACO 2645 ClG 23 41 17.0 -09 01 11           ~ 77 0

    Equat.    Gal    SGal    Ecl

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2021.03.08-02:40:19

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