# 2011A&A...535A.105E

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 Query : 2011A&A...535A.105E

2011A&A...535A.105E - Astronomy and Astrophysics, volume 535A, 105-105 (2011/11-1)

Testing the low-mass end of X-ray scaling relations with a sample of Chandra galaxy groups.

ECKMILLER H.J., HUDSON D.S. and REIPRICH T.H.

Abstract (from CDS):

Well-determined scaling relations between X-ray observables and cluster mass are essential for using large cluster samples to constrain fundamental cosmological parameters. Scaling relations between cluster masses and observables, such as the luminosity-temperature, mass-temperature, luminosity-mass relations, have been investigated extensively, however the question of whether these relations hold true also for poor clusters and groups remains unsettled. Some evidence supports a break'' at the low end of the group/cluster mass range, possibly caused by the stronger influence of non-gravitational physics on low-mass systems. The main goal of this work is to test local scaling relations for the low-mass range in order to check whether or not there is a systematic difference between clusters and groups, and to thereby extend this method of reliable and convenient cluster mass determination for future large samples down to the group regime. We compiled a statistically complete sample of 112 X-ray galaxy groups, 26 of which have usable Chandra data. Temperature, metallicity, and surface brightness profiles were created for these 26 groups, and used to determine the main physical quantities and scaling relations. We then compared the group properties to those of the HIFLUGCS clusters, as well as several other group and cluster samples. We present radial profiles for the individual objects and scaling relations of the whole sample (Lx-T, M-T, Lx-M, Mg-M, M-Yx, Lx-Yx, fg-T). Temperature and metallicity profiles behave universally, except for the core regions. The Lx-T, M-T, Lx-M, Mg-M, M-Yx, and Lx-Yx relations of the group sample are generally in good agreement with clusters. The Lx-T relation steepens for T<3keV, which could point to a larger impact of heating mechanisms on cooler systems. We found a significant drop in the gas mass fraction below ≲1keV, as well as a correlation with radius, which indicates the ICM is less dominant in groups compared to clusters and the galaxies have a stronger influence on the global properties of the system. In all relations the intrinsic scatter for groups is larger than for clusters, which appears not to be correlated with merger activity but could be due to scatter caused by baryonic physics in the group cores. We also demonstrate the importance of selection effects. We have found some evidence for a similarity break between groups and clusters. However this does not have a strong effect on the scaling relations.

Journal keyword(s): X-rays: galaxies: clusters - cosmology: observations - galaxies: clusters: general - galaxies: groups: general

Full paper

 Number of rows : 44
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NGC 326 rG 00 58 22.6298561088 +26 51 58.701156300   14.9 13     ~ 172 2
2 IC 1633 BiC 01 09 55.5490585560 -45 55 52.102562844   12.23       ~ 84 3
3 ACO 160 ClG 01 12 59.572 +15 29 28.65           ~ 167 0
4 NGC 499 LIN 01 23 11.4954761664 +33 27 36.656232300   13.0 12.3     ~ 161 0
5 2E 0120.4+3312 ClG 01 23 12.2 +33 27 40           ~ 30 0
6 NGC 507 BiC 01 23 39.950 +33 15 22.22   13.0       ~ 413 3
7 NGC 508 GiG 01 23 40.5740498304 +33 16 50.482644528   14.5       ~ 63 0
8 ZwCl 0120+3300 ClG 01 23 41.0 +33 15 40           ~ 74 0
9 NGC 533 GiG 01 25 31.4074984248 +01 45 33.236656812   13.1 14.11     ~ 217 0
10 NGC 777 Sy2 02 00 14.9065707744 +31 25 45.850721628 13.09 12.49 11.45     ~ 168 2
11 RXC J0252.8-0116 ClG 02 52 49.4 -01 16 27           ~ 101 0
12 NGC 1132 GiG 02 52 51.82 -01 16 29.0   13.9   12.16   ~ 156 0
13 NGC 1550 BiC 04 19 37.9450450152 +02 24 35.918168940   14.0       ~ 163 1
14 ACO S 463 ClG 04 29 13.4 -53 44 02           ~ 47 0
15 ESO 552-20 BiC 04 54 52.262 -18 06 56.12   13.34   11.64   ~ 61 1
16 NGC 2736 HII 09 00.2 -45 57           ~ 18 0
17 NGC 2737 GiG 09 03 59.7215040432 +21 54 23.627982096   14.8       ~ 26 0
18 MCXC J1022.0+3830 ClG 10 22 04.7 +38 30 43           ~ 47 0
19 NGC 3411 BiC 10 50 26.0811795768 -12 50 42.313849764   9.0   11.60   ~ 68 1
20 NAME NGC 3411 Group GrG 10 50 26.9 -12 50 26           ~ 46 0
21 ACO 1177 ClG 11 09 27 +21 41.7           ~ 97 1
22 NAME NGC 4073 Group GrG 12 04 21.7 +01 50 19     13.53     ~ 255 0
23 NGC 4073 BiC 12 04 27.0598775760 +01 53 45.611893752   13.8 13.21 14.249   ~ 190 1
24 1RXS J122306.6+103722 ClG 12 23 06.5 +10 37 26           ~ 45 0
25 NGC 4325 BiC 12 23 06.662 +10 37 16.45   15.0       ~ 122 1
26 HCG 62 CGG 12 53 05.6 -09 12 21           ~ 299 0
27 NGC 4761 BiC 12 53 05.6960048016 -09 12 14.579980632   13.79   11.25   ~ 81 1
28 NGC 4936 LIN 13 04 17.091 -30 31 34.71   11.76 12.23 10.13 10.9 ~ 101 0
29 NGC 5129 LIN 13 24 10.0256041224 +13 58 35.575742748   13.3       ~ 120 1
30 BAX 201.0418+13.9765 ClG 13 24 11.9 +13 58 45           ~ 85 0
31 IC 4296 AGN 13 36 39.03275288 -33 57 57.0783023   11.52 12.99 10.00   ~ 463 2
32 ACO S 753 ClG 14 03 35.9 -33 59 16           ~ 83 1
33 NGC 5419 BiC 14 03 38.7225244848 -33 58 41.881842120   11.77 11.33 10.21   ~ 180 2
34 NAME NGC 5718 Group ClG 14 40 38.5 +03 28 20     14.31     ~ 109 0
35 NGC 6265 GiG 16 57 29.1136022304 +27 50 39.454733904   15.4       ~ 31 0
36 NGC 6269 GiG 16 57 58.1011343880 +27 51 15.883449192   14.4 13.73     ~ 100 0
37 NAME NGC 6269 Group ClG 16 58 00.8 +27 51 16     14.00     ~ 58 0
38 NGC 6338 Bla 17 15 22.9842192336 +57 24 40.346559936   14.2   8   ~ 165 2
39 IC 1262 BiC 17 33 02.0176600056 +43 45 34.803150516   14.9       ~ 70 0
40 NGC 6482 GiG 17 51 48.8339247888 +23 04 18.889271112 12.71 12.35 11.45     ~ 198 1
41 NGC 7236 LIN 22 14 44.9886363216 +13 50 47.450963760   14.3 14.3     ~ 263 2
42 SDSS-C4-DR3 2030 GrG 22 14 48.0 +13 50 17           ~ 31 0
43 [VV2010c] J221452.9+135118 SyG 22 14 53.7 +13 51 19           ~ 10 1
44 HCG 97 CGG 23 47 24.0 -02 19 08           ~ 94 0

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2022.05.28-22:22:16

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