2008A&A...483...35S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.16CEST17:15:54

2008A&A...483...35S - Astronomy and Astrophysics, volume 483, 35-47 (2008/5-3)

Searching for cool core clusters at high redshift.

SANTOS J.S., ROSATI P., TOZZI P., BOEHRINGER H., ETTORI S. and BIGNAMINI A.

Abstract (from CDS):

We investigate the detection of Cool Cores (CCs) in the distant galaxy cluster population with the purpose of measuring the CC fraction out to redshift 0.7≤z<1.4. Using a sample of nearby clusters spanning a wide range of morphologies, we define criteria to characterize cool cores, which are applicable to the high-redshift sample. We analyzed azimuthally-averaged surface brightness (SB) profiles with the known scaling relations, and we fitted single/double β models to the data. Additionally, we measured a surface brightness concentration, cSB, as the ratio of the peak over the ambient SB. To verify that this is an unbiased parameter as a function of redshift, we developed a model independent ``cloning'' technique to simulate the nearby clusters as they would appear at the same redshifts and luminosities as those in the distant sample. This method is based on the application of the cosmological surface brightness dimming to high-resolution Chandra images, assuming no intrinsic cluster evolution. We obtained a more physical parameterization of the CC presence by computing the cooling time at a radius of 20kpc from the cluster center. The distribution of the SB concentration and the stacked radial profiles of the low-z sample, combined with published information on the CC properties of these clusters, show 3 degrees of SB cuspiness: non-CC, moderate, and strong CC. The same analysis applied to the high-z clusters reveals two regimes: non-CC and moderate CC. The cooling time distribution corroborates this result by showing a strong negative correlation with cSB. Our analysis indicates a significant fraction of distant clusters harboring a moderate CC out to z=1.4, similar to those found in the local sample. The absence of strong cooling is likely linked with a higher merger rate expected at redshift z>0.7, and should also be related to the shorter age of distant clusters, implying less time to develop a cool core.

Abstract Copyright:

Journal keyword(s): X-rays: galaxies: clusters - galaxies: clusters: general - galaxies: cooling flows - galaxies: high-redshift

Simbad objects: 38

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Number of rows : 38

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 ClG J0224-0002 ClG 02 24 34.10 -00 02 30.9           ~ 48 1
2 ClG J0439-2905 ClG 04 39 38.0 -29 04 55           ~ 6 0
3 ClG 0657-56 ClG 06 58 29.6 -55 56 39           ~ 800 1
4 ClG J0848+4453 ClG 08 48 34.800 +44 53 41.90           ~ 122 1
5 ClG J0849+4452 ClG 08 48 56.3 +44 52 16           ~ 104 1
6 ClG J0910+5422 ClG 09 10 44.9 +54 22 09           ~ 86 0
7 ACO 907 ClG 09 58 21.84 -11 03 47.5           ~ 115 0
8 ACO 963 ClG 10 17 09.6 +39 01 00           ~ 350 0
9 ZwCl 1021+0426 ClG 10 23 39.0 +04 11 14   15.6       ~ 250 0
10 ClG 1054-03 ClG 10 57 00.2 -03 37 27     22     ~ 449 0
11 RCS J1107-0523 ClG 11 07 22.8 -05 23 49           ~ 9 0
12 ClG J1113-2615 ClG 11 13 05.7 -26 15 36           ~ 34 0
13 MCS J1137.5+6624 ClG 11 37.5 +66 24           ~ 3 0
14 ACO 1413 ClG 11 55 18.0 +23 24 19           ~ 381 0
15 ClG J1221+4918 ClG 12 21 25.0 +49 18 07           ~ 56 0
16 ClG J1226+3332 ClG 12 26 57.7 +33 32 50           ~ 194 0
17 NAME Hubble Deep Field reg 12 36 49.5 +62 12 58           ~ 1826 1
18 ClG J1252-2927 ClG 12 52 54.4 -29 27 17           ~ 151 0
19 RX J1317.2+2911 X 13 17 13 +29 11.5           ~ 3 0
20 RCS J1325+2858 ClG 13 26 31.040 +29 03 52.02           ~ 3 0
21 ClG J1350+6007 ClG 13 50 48.55 +60 07 06.7           ~ 42 0
22 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 621 1
23 ClG J1415+3611 ClG 14 15 11.1 +36 12 03           ~ 70 1
24 RCS J141658+5305.2 ClG 14 16 58.7 +53 05 15           ~ 4 0
25 ClG J1419+5326 ClG 14 19 10.3 +53 26 08           ~ 20 0
26 ACO 2104 ClG 15 40 06.8 -03 17 39           ~ 97 0
27 ACO 2163 ClG 16 15 34.1 -06 07 26           ~ 519 0
28 ClG J1620+2929 ClG 16 20 09.4 +29 29 26           ~ 17 0
29 ACO 2218 ClG 16 35 54.0 +66 13 00           ~ 780 1
30 ClG J1716+6708 ClG 17 16 49.6 +67 08 30           ~ 130 0
31 ACO 2261 ClG 17 22 28.3 +32 09 13           ~ 283 0
32 RCS J2112.3-6326 ClG 21 12 20.510 -63 26 13.97           ~ 3 0
33 ACO 2390 ClG 21 53 34.6 +17 40 11           ~ 625 2
34 ClG J2156-0448 ClG 21 56 41 -04 48.1           ~ 13 0
35 ClG J2235-2557 ClG 22 35 20.6 -25 57 42           ~ 138 0
36 ClG J2302+0844 ClG 23 02 48.1 +08 43 50           ~ 40 0
37 RCS J2318+0034 ClG 23 18 30.670 +00 34 03.03           ~ 15 0
38 ClG J2319+0038 ClG 23 19 53 +00 38.0           ~ 35 1

    Equat.    Gal    SGal    Ecl

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2020.07.16-17:15:54

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