2010A&A...523A..81D


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.25CET23:23:36

2010A&A...523A..81D - Astronomy and Astrophysics, volume 523, A81-81 (2010/11-2)

Cold fronts and multi-temperature structures in the core of Abell 2052.

DE PLAA J., WERNER N., SIMIONESCU A., KAASTRA J.S., GRANGE Y.G. and VINK J.

Abstract (from CDS):

The physics of the coolest phases in the hot intra-cluster medium (ICM) of clusters of galaxies is yet to be fully unveiled. X-ray cavities blown by the central active galactic nucleus (AGN) contain enough energy to heat the surrounding gas and stop cooling, but locally blobs or filaments of gas appear to be able to cool to low temperatures of 104K. In X-rays, however, gas with temperatures lower than 0.5keV is not observed. We aim to find spatial and multi-temperature structures in the hot gas of the cooling-core cluster Abell 2052 that contain clues on the physics involved in the heating and cooling of the plasma. 2D maps of the temperature, entropy, and iron abundance are derived from XMM-Newton data of Abell 2052. For the spectral fitting, we use differential emission measure (DEM) models to account for the multi-temperature structure. About 130kpc South-West of the central galaxy, we discover a discontinuity in the surface brightness of the hot gas which is consistent with a cold front. Interestingly, the iron abundance jumps from ∼0.75 to ∼0.5 across the front. In a smaller region to the North-West of the central galaxy we find a relatively high contribution of cool 0.5keV gas, but no X-ray emitting gas is detected below that temperature. However, the region appears to be associated with much cooler Hα filaments in the optical waveband. The elliptical shape of the cold front in the SW of the cluster suggests that the front is caused by sloshing of the hot gas in the clusters gravitational potential. This effect is probably an important mechanism to transport metals from the core region to the outer parts of the cluster. The smooth temperature profile across the sharp jump in the metalicity indicates the presence of heat conduction and the lack of mixing across the discontinuity. The cool blob of gas NW of the central galaxy was probably pushed away from the core and squeezed by the adjacent bubble, where it can cool efficiently and relatively undisturbed by the AGN. Shock induced mixing between the two phases may cause the 0.5keV gas to cool non-radiatively and explain our non-detection of gas below 0.5keV.

Abstract Copyright:

Journal keyword(s): galaxies: clusters: general - galaxies: clusters: intracluster medium - galaxies: clusters: individual: Abell 2052 - X-rays: galaxies: clusters

Simbad objects: 11

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Number of rows : 11

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 ACO 426 ClG 03 19 47.2 +41 30 47           ~ 1990 1
2 ZwCl 0335+0956 ClG 03 38 35.3 +09 57 54           ~ 352 1
3 ACO 478 ClG 04 13 20.7 +10 28 35           ~ 474 0
4 ACO 3281 ClG 04 41 08 -38 18.3           ~ 2 0
5 NAME Hya A LIN 09 18 05.651 -12 05 43.99   14.38 14.8     ~ 917 1
6 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6322 3
7 ACO 3526 ClG 12 48 51.8 -41 18 21           ~ 988 2
8 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 630 1
9 UGC 9799 Sy2 15 16 44.4894653562 +07 01 17.830884159   15.19 14.17     ~ 419 3
10 ACO 2052 ClG 15 16 45.5 +07 00 01           ~ 685 1
11 NAME LHB X 16 42.0 +02 19           ~ 271 0

    Equat.    Gal    SGal    Ecl

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2021.01.25-23:23:36

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