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


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.20CEST19:54:55

2015A&A...575A..38P - Astronomy and Astrophysics, volume 575A, 38-38 (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

goto Full paper

goto View the reference in ADS

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 - 2019
#notes
1 ACO 85 ClG 00 41 37.8 -09 20 33           ~ 766 0
2 ACO 133 ClG 01 02 39.0 -21 57 15           ~ 325 1
3 NGC 507 BiC 01 23 39.950 +33 15 22.22   13.0       ~ 385 3
4 ACO 189 ClG 01 23 40.4 +01 38 38           ~ 98 1
5 NAME NGC 507 Group GrG 01 23.7 +33 15           ~ 72 0
6 ACO 262 ClG 01 52 50.4 +36 08 46           ~ 645 1
7 2MAXI J0254+416 ClG 02 54 32.2 +41 35 10           ~ 295 1
8 ACO 3112 ClG 03 17 52.4 -44 14 35           ~ 283 1
9 ACO 426 ClG 03 19 47.2 +41 30 47           ~ 1882 1
10 NGC 1316 GiP 03 22 41.789 -37 12 29.52 9.81 9.15 8.53 7.66   ~ 1161 1
11 NGC 1399 BiC 03 38 29.083 -35 27 02.67 11.05 9.74 9.59 8.12   ~ 1416 1
12 ACO S 373 ClG 03 38 30 -35 27.3           ~ 1490 0
13 ZwCl 0335+0956 ClG 03 38 35.3 +09 57 54           ~ 338 1
14 NGC 1404 GiP 03 38 51.917 -35 35 39.81 11.53 10.69 10.00 9.03   ~ 647 1
15 NGC 1550 BiC 04 19 37.921 +02 24 35.58   14.0       ~ 141 1
16 ClG 0422-09 ClG 04 25 51.02 -08 33 38.5           ~ 82 0
17 ACO 496 ClG 04 33 30.3838 -13 14 21.584           ~ 653 2
18 NAME Hya A LIN 09 18 05.651 -12 05 43.99   14.38 14.8     ~ 878 1
19 NGC 3411 BiC 10 50 26.104 -12 50 42.26   9.0   11.60   ~ 60 1
20 NAME NGC 4073 Group GrG 12 04 21.7 +01 50 19     13.53     ~ 241 0
21 NGC 4261 LIN 12 19 23.21607184 +05 49 29.7000920   13.92 12.87     ~ 1089 0
22 NGC 4325 BiC 12 23 06.662 +10 37 16.45   15.0       ~ 111 1
23 M 84 Sy2 12 25 03.74333 +12 53 13.1393 12.67 12.09 10.49     ~ 1609 2
24 M 86 GiG 12 26 11.814 +12 56 45.49 10.32 9.83 8.90   7.50 ~ 994 1
25 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5645 0
26 M 49 Sy2 12 29 46.798 +08 00 01.48   13.21 12.17     ~ 1924 2
27 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6026 3
28 M 89 LIN 12 35 39.8 +12 33 23 11.29 10.73 9.75     ~ 906 2
29 NGC 4636 LIN 12 42 49.867 +02 41 16.01   12.62 11.84     ~ 1025 1
30 M 60 GiP 12 43 40.008 +11 33 09.40   10.3       ~ 1223 0
31 ACO 3526 ClG 12 48 51.8 -41 18 21           ~ 957 2
32 HCG 62 CGG 12 53 05.6 -09 12 21           ~ 290 0
33 NGC 5044 BiC 13 15 23.969 -16 23 08.00   11.9   10.74   ~ 438 0
34 ACO 1795 ClG 13 49 00.5 +26 35 07           ~ 1134 0
35 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 611 1
36 ACO 3581 ClG 14 07 29.8 -27 01 04           ~ 159 3
37 ACO 1991 ClG 14 54 30.2 +18 37 51           ~ 300 1
38 NGC 5813 LIN 15 01 11.265 +01 42 07.09 12.00 11.45 10.46 10.06   ~ 564 1
39 NGC 5846 BiC 15 06 29.253 +01 36 20.29   11.9   9.74   ~ 755 1
40 ACO 2029 ClG 15 10 58.7 +05 45 42           ~ 835 0
41 ACO 2052 ClG 15 16 45.5 +07 00 01           ~ 664 1
42 NAME NGC 5920 Group ClG 15 21 50.7 +07 42 18     15.13     ~ 281 0
43 ACO 2199 ClG 16 28 37.0 +39 31 28           ~ 1084 1
44 ACO S 1101 ClG 23 13 58.5 -42 43 39           ~ 228 1
45 ACO 2597 ClG 23 25 19.70 -12 07 27.7           ~ 483 0
46 ACO 2626 ClG 23 36 31.0 +21 09 36           ~ 204 0
47 ACO 4038 ClG 23 47 31.1 -28 12 10           ~ 309 3
48 ACO 4059 ClG 23 56 40.7 -34 40 18           ~ 345 1

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2015A&A...575A..38P and select 'bookmark this link' or equivalent in the popup menu


2019.10.20-19:54:55

© Université de Strasbourg/CNRS

    • Contact