2013ApJ...767..157G

Query : 2013ApJ...767..157G

2013ApJ...767..157G - Astrophys. J., 767, 157 (2013/April-3)

Probing of the interactions between the hot plasmas and galaxies in clusters from z = 0.1 to 0.9.

GU L., GANDHI P., INADA N., KAWAHARADA M., KODAMA T., KONAMI S., NAKAZAWA K., SHIMASAKU K., XU H. and MAKISHIMA K.

Abstract (from CDS):

Based on optical and X-ray data for a sample of 34 relaxed rich clusters of galaxies with redshifts of 0.1-0.9, we studied relative spatial distributions of the two major baryon contents, the cluster galaxies and the hot plasmas. Using multi-band photometric data taken with the UH88 telescope, we determined the integrated (two-dimensional) radial light profiles of member galaxies in each cluster using two independent approaches, i.e., the background subtraction and the color-magnitude filtering. The intracluster medium (ICM) mass profile of each cluster in our sample, also integrated in two dimensions, was derived from a spatially resolved spectral analysis using XMM-Newton and Chandra data. Then, the radially integrated light profile of each cluster was divided by its ICM mass profile, to obtain a profile of "galaxy light versus ICM mass ratio." When the sample is divided into three subsamples with redshift intervals of z = 0.11-0.22, 0.22-0.45, and 0.45-0.89, the ratio profiles over the central 0.65 R500 regions were found to steepen from the higher- to lower-redshift subsamples, meaning that the galaxies become more concentrated in the ICM sphere toward lower redshifts. A Kolmogorov-Smirnov test indicates that this evolution in the cluster structure is significant on ≥ 94% confidence level. A range of systematic uncertainties in the galaxy light measurements, as well as many radius-/redshift-dependent biases to the galaxy versus ICM profiles, have been assessed, but none of them are significant against the observed evolution. Besides, the galaxy light versus total mass ratio profiles also exhibit gradual concentration toward lower redshift. We interpret that the galaxies, the ICM, and the dark matter components followed a similar spatial distribution in the early phase (z > 0.5), while the galaxies have fallen toward the center relative to the others. Such galaxy infall is likely to be caused by the drag exerted from the ICM to the galaxies as they move through the ICM and interact with it, while gravitational drag can enhance the infall of the most massive galaxies.

Abstract Copyright: ∼

Journal keyword(s): galaxies: clusters: general - galaxies: evolution - intergalactic medium - X-rays: galaxies: clusters

Simbad objects: 73

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Number of rows : 73
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 ClG 0016+16 ClG 00 18 33.3 +16 26 36           ~ 517 0
2 CNOC MS 0015 100994 BiC 00 18 33.584 +16 26 15.93           ~ 17 0
3 ZwCl 0024+1652 ClG 00 26 35.6 +17 09 32     18.35     ~ 648 1
4 2MASXI J0026356+170943 BiC 00 26 35.6678 +17 09 43.090         18.115 ~ 23 0
5 ClG J0030+2618 ClG 00 30 33.6 +26 18 16           ~ 65 0
6 [BWE97] J003034.0+261808 BiC 00 30 34.032 +26 18 09.15           ~ 4 0
7 ACO 68 ClG 00 37 06.2 +09 09 33           ~ 195 0
8 2MASX J00370686+0909236 BiC 00 37 06.8375479080 +09 09 24.206067504           ~ 16 1
9 2MASX J01524199+0100257 BiC 01 52 41.963 +01 00 25.53     13.57     ~ 22 1
10 ACO 267 ClG 01 52 43.016 +00 59 58.90           ~ 241 0
11 ACO 383 ClG 02 48 03.3915 -03 31 45.228           ~ 389 0
12 6dFGS gJ024803.4-033145 rG 02 48 03.3956603208 -03 31 45.600488256   17.89   15.76   ~ 26 1
13 ClG 0303+1658 ClG 03 05 31.6 +17 10 02     20.13     ~ 92 0
14 [GMF2004] 46.3821+17.1674 BiC 03 05 31.7 +17 10 03           ~ 1 0
15 ACO 426 ClG 03 19 47.6 +41 30 54           ~ 2508 1
16 2MASX J04370955+0043533 rG 04 37 09.560 +00 43 53.33   18.9       ~ 4 0
17 ACT-CL J0437.1+0043 ClG 04 37 12.0820 +00 43 37.737           ~ 47 0
18 CNOC MS 0451 101234 BiC 04 54 10.84 -03 00 51.6         18.1 ~ 12 1
19 ClG 0451-03 ClG 04 54 10.9 -03 01 07     20.0     ~ 368 0
20 ZwCl 0735+7421 ClG 07 41 40.3 +74 14 58     17.70     ~ 273 0
21 4C 74.13 rG 07 41 44.449 +74 14 39.59   20.15 18.53     ~ 28 2
22 ACO 665 ClG 08 30 45.2 +65 52 55           ~ 457 0
23 2MASX J08305736+6550299 BiC 08 30 57.365 +65 50 29.98   19.3       ~ 14 0
24 ClG J0947+7623 ClG 09 46 59.916 +76 23 43.99           ~ 165 0
25 NVSS J094712+762312 Rad 09 47 12.37 +76 23 09.3           ~ 151 1
26 ACO 907 ClG 09 58 21.84 -11 03 47.5           ~ 137 0
27 NVSS J095821-110347 rG 09 58 22.0045525896 -11 03 50.391575172   17.69   15.98   ~ 10 1
28 ACO 963 ClG 10 17 03.4 +39 02 56           ~ 414 0
29 LEDA 2142331 BiC 10 17 03.6366160416 +39 02 49.485562908           ~ 24 0
30 2MASX J10173435+5933390 BiC 10 17 34.3351194168 +59 33 39.476362212   20.0       ~ 5 1
31 ACO 959 ClG 10 17 35.0 +59 33 28           ~ 76 0
32 ZwCl 1021+0426 ClG 10 23 39.0 +04 11 14   15.6 17.95     ~ 297 0
33 NVSS J102339+041115 rG 10 23 39.634 +04 11 10.66   18.6       ~ 30 0
34 NVSS J104432-070407 rG 10 44 32.8730790384 -07 04 07.424149836   18.10   16.23   ~ 10 0
35 ACO 1084 ClG 10 44 37.1 -07 04 47           ~ 78 0
36 SDSS J112005.61+431809.0 BiC 11 20 05.610 +43 18 09.00           ~ 2 0
37 ClG J1120+4318 ClG 11 20 07.6 +43 18 07           ~ 65 0
38 ClG 1137+66 ClG 11 40 23.0 +66 08 16     21.0     ~ 141 0
39 [DVS99] 9 BiC 11 40 27.4 +66 08 23           ~ 2 0
40 ACO 1348 ClG 11 41 24.0 -12 16 00           ~ 70 0
41 PMN J1141-1216 rG 11 41 24.19701482 -12 16 38.6465880   16.66   14.20   ~ 18 1
42 SDSS J122653.11+333330.8 BiC 12 26 53.12 +33 33 31.1     23.77   21.90 ~ 3 0
43 ClG J1226+3332 ClG 12 26 57.7 +33 32 50           ~ 228 0
44 NAME Virgo Cluster ClG 12 30 47.8 +12 23 07           ~ 7107 0
45 ClG 1231+15 ClG 12 33 55.3 +15 25 58     18.5     ~ 54 0
46 2MASX J12335533+1525593 BiC 12 33 55.3351741920 +15 25 59.046845448           ~ 6 0
47 2MASX J12365866+6311145 BiC 12 36 58.628 +63 11 13.77           ~ 8 0
48 ACO 1576 ClG 12 36 59.5 +63 11 18           ~ 116 0
49 SDSS J124357.98+165354.1 BiC 12 43 57.990 +16 53 54.14           ~ 1 0
50 ClG 1241+17 ClG 12 44 02.6 +16 54 11     19.0     ~ 42 0
51 ACO 1650 ClG 12 58 42.0 -01 45 45           ~ 325 0
52 ZwCl 1332+5043 ClG 13 34 20.0 +50 30 54           ~ 42 0
53 SDSS J133420.56+503103.5 BiC 13 34 20.563 +50 31 03.91           ~ 1 0
54 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 727 1
55 NAME SMM J14010+0252 Sy1 14 01 02.0819944848 +02 52 42.426538140   19.3       ~ 47 2
56 ClG J1504-0248 ClG 15 04 07.4 -02 48 15           ~ 186 0
57 [VV2006] J150407.5-024816 Bla 15 04 07.51896914 -02 48 16.6232484   18.53 18.08     ~ 60 2
58 ACO 2125 ClG 15 41 14.1 +66 15 57           ~ 124 1
59 ACO 3627 ClG 16 14 22.5 -60 52 07           ~ 340 2
60 NVSS J163246+053434 Rad 16 32 46.9 +05 34 33   16.6       ~ 12 1
61 ACO 2204 ClG 16 32 47.7 +05 34 18           ~ 457 0
62 [GHM99] 20 rG 17 16 48.5 +67 08 22           ~ 3 0
63 ClG J1716+6708 ClG 17 16 49.6 +67 08 30           ~ 137 0
64 ACO 2261 ClG 17 22 26.9 +32 07 58           ~ 370 0
65 NVSS J172227+320757 rG 17 22 27.185 +32 07 57.25           ~ 47 1
66 2MASX J19381810+5409402 BiC 19 38 18.105 +54 09 40.28           ~ 1 0
67 CIZA J1938.3+5409 ClG 19 38 18.6 +54 09 33           ~ 42 0
68 CXOU J205621.2-043749 GiC 20 56 21.2 -04 37 49   21.0 21.248   19.20 ~ 6 2
69 ClG 2053-04 ClG 20 56 21.2 -04 37 46   21.0       ~ 168 0
70 NVSS J212940+000522 rG 21 29 39.953 +00 05 21.16           ~ 36 0
71 ClG J2129+0005 ClG 21 29 40.5 +00 05 47           ~ 308 0
72 [OOP2020] Abell 2537 BCG BiC 23 08 22.214 -02 11 31.52           ~ 13 1
73 ACO 2537 ClG 23 08 22.3 -02 11 29           ~ 152 0

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