2015A&A...575A..38P

Query : 2015A&A...575A..38P

2015A&A...575A..38P - Astronomy and Astrophysics, volume 575A38-38 (2015/3-1)

Chemical Enrichment RGS cluster Sample (CHEERS): Constraints on turbulence.

PINTO C., SANDERS J.S., WERNER N., DE PLAA J., FABIAN A.C., ZHANG Y.-Y., KAASTRA J.S., FINOGUENOV A. and AHORANTA J.

Abstract (from CDS):

Feedback from active galactic nuclei, galactic mergers, and sloshing are thought to give rise to turbulence, which may prevent cooling in clusters. We aim to measure the turbulence in clusters of galaxies and compare the measurements to some of their structural and evolutionary properties. It is possible to measure the turbulence of the hot gas in clusters by estimating the velocity widths of their X-ray emission lines. The Reflection Grating Spectrometers aboard XMM-Newton are currently the only instruments provided with sufficient effective area and spectral resolution in this energy domain. We benefited from excellent 1.6Ms new data provided by the Chemical Enrichment RGS cluster Sample (CHEERS) project. The new observations improve the quality of the archival data and allow us to place constraints for some clusters, which were not accessible in previous work. One-half of the sample shows upper limits on turbulence less than 500km/s. For several sources, our data are consistent with relatively strong turbulence with upper limits on the velocity widths that are larger than 1000km/s. The NGC507 group of galaxies shows transonic velocities, which are most likely associated with the merging phenomena and bulk motions occurring in this object. Where both low- and high-ionization emission lines have good enough statistics, we find larger upper limits for the hot gas, which is partly due to the different spatial extents of the hot and cool gas phases. Our upper limits are larger than the Mach numbers required to balance cooling, suggesting that dissipation of turbulence may prevent cooling, although other heating processes could be dominant. The systematics associated with the spatial profile of the source continuum make this technique very challenging, though still powerful, for current instruments. In a forthcoming paper we will use the resonant-scattering technique to place lower-limits on the velocity broadening and provide further insights on turbulence. The ASTRO-H and Athena missions will revolutionize the velocity estimates and discriminate between different spatial regions and temperature phases.

Abstract Copyright: ∼

Journal keyword(s): X-rays: galaxies: clusters - X-rays: galaxies - galaxies: clusters: intracluster medium - techniques: spectroscopic - turbulence - galaxies: kinematics and dynamics

Simbad objects: 48

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Number of rows : 48
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 ACO 85 ClG 00 41 36.21 -09 19 30.4           ~ 974 0
2 ACO 133 ClG 01 02 41.5 -21 52 53           ~ 391 1
3 NAME NGC 507 Group GrG 01 23 39.91 +33 15 21.8           ~ 82 0
4 NGC 507 rG 01 23 39.950 +33 15 22.22   13.0       ~ 459 1
5 ACO 189 ClG 01 23 40.4 +01 38 38           ~ 103 1
6 ACO 262 ClG 01 52 50.4 +36 08 46           ~ 727 1
7 2A 0251+413 ClG 02 54 26.6 +41 33 25           ~ 328 1
8 ACO 3112 ClG 03 17 52.9 -44 15 06           ~ 329 1
9 ACO 426 ClG 03 19 47.6 +41 30 54           ~ 2508 1
10 NGC 1316 rG 03 22 41.789 -37 12 29.52 9.81 9.15 8.53 7.66   ~ 1491 1
11 NGC 1399 rG 03 38 29.083 -35 27 02.67 11.05 9.74 9.59 8.12   ~ 1636 1
12 ACO S 373 ClG 03 38 29.4 -35 27 08           ~ 2029 0
13 ZwCl 0335+0956 ClG 03 38 35.3 +09 57 54           ~ 402 1
14 NGC 1404 rG 03 38 51.917 -35 35 39.81 11.53 10.69 10.00 9.03   ~ 787 1
15 NGC 1550 BiC 04 19 37.9450450152 +02 24 35.918168940   14.0       ~ 183 1
16 ClG 0422-09 ClG 04 25 51.02 -08 33 38.5           ~ 97 0
17 ACO 496 ClG 04 33 40.8 -13 14 34           ~ 728 2
18 MCG-02-24-007 LIN 09 18 05.66848602 -12 05 43.8060823   14.38 14.8     ~ 1077 1
19 NGC 3411 EmG 10 50 26.0811795768 -12 50 42.313849764   9.0   11.60   ~ 78 2
20 NAME NGC 4073 Group GrG 12 04 44.08 +01 48 40.9     13.53     ~ 292 0
21 NGC 4261 LIN 12 19 23.2160630 +05 49 29.700024   13.92 12.87     ~ 1290 0
22 NGC 4325 BiC 12 23 06.662 +10 37 16.45   15.0       ~ 140 1
23 M 84 Sy2 12 25 03.74333 +12 53 13.1393 12.67 12.09 10.49     ~ 1841 2
24 M 86 GiG 12 26 11.814 +12 56 45.49 10.32 9.83 8.90   7.50 ~ 1126 1
25 M 49 Sy2 12 29 46.8 +08 00 01   13.21 12.17     ~ 2174 2
26 NAME Virgo Cluster ClG 12 30 47.8 +12 23 07           ~ 7107 0
27 M 87 AGN 12 30 49.42338414 +12 23 28.0436859 10.16 9.59 8.63   7.49 ~ 7815 3
28 M 89 Sy2 12 35 39.80733343 +12 33 22.8308657 11.29 10.73 9.75     ~ 1037 2
29 NGC 4636 LIN 12 42 49.8333280080 +02 41 15.951929028   12.62 11.84     ~ 1156 1
30 M 60 GiC 12 43 39.9708251934 +11 33 09.688174067   10.3       ~ 1395 1
31 ACO 3526 ClG 12 48 49.2 -41 18 17           ~ 1154 2
32 HCG 62 CGG 12 53 05.6 -09 12 21           ~ 313 0
33 NGC 5044 BiC 13 15 23.9607836592 -16 23 07.547751744   11.9   10.74   ~ 531 0
34 ACO 1795 ClG 13 48 47.4 +26 34 55           ~ 1330 0
35 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 727 1
36 ACO 3581 ClG 14 07 29.8 -27 01 04           ~ 197 3
37 ACO 1991 ClG 14 54 41.53 +18 38 08.4           ~ 349 1
38 NGC 5813 LIN 15 01 11.2302420864 +01 42 07.141569696 12.00 11.45 10.46 10.06   ~ 673 2
39 NGC 5846 rG 15 06 29.253 +01 36 20.29   11.9   9.74   ~ 891 2
40 ACO 2029 ClG 15 10 54.2 +05 44 23           ~ 1020 0
41 ACO 2052 ClG 15 16 41.64 +07 01 45.5           ~ 756 1
42 ACT-CL J1521.8+0742 ClG 15 21 48.8 +07 43 41     15.13     ~ 326 0
43 ACO 2199 ClG 16 28 34.5 +39 32 26           ~ 1206 1
44 ACO S 1101 ClG 23 13 58.5 -42 43 39           ~ 272 1
45 ACO 2597 ClG 23 25 19.70 -12 07 27.7           ~ 572 0
46 ACO 2626 ClG 23 36 31.0 +21 09 36           ~ 265 0
47 ACO 4038 ClG 23 47 31.1 -28 12 10           ~ 349 3
48 ACO 4059 ClG 23 57 02.2 -34 45 58           ~ 400 1

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