2013A&A...558A.146V


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST03:54:51

2013A&A...558A.146V - Astronomy and Astrophysics, volume 558A, 146-146 (2013/10-1)

Radio emission at the centre of the galaxy cluster Abell 3560: evidence for core sloshing?

VENTURI T., ROSSETTI M., BARDELLI S., GIACINTUCCI S., DALLACASA D., CORNACCHIA M. and KANTHARIA N.G.

Abstract (from CDS):

We study the interplay between the radio emission associated with the dominant galaxy in clusters and the properties of the surrounding intracluster medium on the basis of its X-ray emission. Previous radio observations of the galaxy cluster A3560, located in the Shapley Concentration core, revealed complex radio emission associated with the brightest cluster member. To understand the origin of this radio emission we performed a detailed multiwavelength study with high-quality proprietary data in the radio and X-ray bands and by means of optical data available in the literature. We observed the cluster with the Giant Metrewave Radio Telescope, the Very Large Array, and the Australia Telescope Compact array at 240 and 610MHz, 1.28, 1.4, 2.3, 4.8, and 8.4GHz, and performed a detailed morphological and spectral study of the radio emission associated with the brightest cluster galaxy (BCG). Furthermore, we observed the cluster with the XMM-Newton and Chandra observatories to derive the properties of the intracluster gas. Finally, we made use of literature data to obtain the bidimensional distribution of the galaxies in the cluster. The radio emission, associated with the north-eastern nucleus of the dumb-bell BCG, is the result of two components: an active radio galaxy, with jets and lobes, plus aged diffuse emission, which is not refurbished with new electrons at present. Our Chandra data show that the radio active nucleus of the BCG has extended X-ray emission, which we classify as a low-luminosity corona. A residual image of the XMM-Newton brightness distribution shows a spiral-like feature, which we interpret as the signature of gas sloshing. A sub-group is clearly visible in the surface brightness residual map, and this is also supported by the XMM-Newton temperature analysis. The optical bidimensional analysis shows substructure in A3560. A galaxy clump was detected at the location of the X-ray sub-group, and another group is present south of the cluster core, in the region where the spiral-like feature was detected. The aged part of the radio emission closely follows the spiral pattern of the X-ray residual brightness distribution, while the two active radio lobes are bent in a completely different direction. We conclude that the complex radio emission associated with the cluster BCG is the result of a minor merger event in A3560. The aged diffuse emission is strongly affected by the sloshing motion in the intracluster gas and most likely bears information on the trajectory of the cluster BCG during the dynamical evolution of the cluster. On the other hand, the bent jets and lobes of the current radio AGN activity may reflect a complex gas velocity field in the innermost cluster regions and/or sloshing-induced oscillations in the motion of the cD galaxy.

Abstract Copyright:

Journal keyword(s): galaxies: clusters: general - galaxies: clusters: individual: A3560 - radio continuum: galaxies

Simbad objects: 17

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Number of rows : 17

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 ACO 262 ClG 01 52 50.4 +36 08 46           ~ 652 1
2 NGC 1407 GiG 03 40 11.904 -18 34 49.36   10.64 9.67 9.13   ~ 526 1
3 ZwCl 0735+7421 ClG 07 41 40.3 +74 14 58     17.70     ~ 217 0
4 NAME Hya A LIN 09 18 05.651 -12 05 43.99   14.38 14.8     ~ 907 1
5 HCG 62 CGG 12 53 05.6 -09 12 21           ~ 293 0
6 NGC 4874 LIN 12 59 35.709 +27 57 33.80 13.01 13.7 11.40 12.122 11.386 ~ 713 3
7 NAME SHAPLEY-CENTAURUS CL SCG 13 06.0 -33 04           ~ 500 0
8 NGC 5044 BiC 13 15 23.969 -16 23 08.00   11.9   10.74   ~ 451 0
9 ACO 3558 ClG 13 27 54.8 -31 29 32           ~ 406 2
10 LEDA 47626 PaG 13 32 23.60 -33 08 21.4           ~ 21 1
11 ACO 3560 ClG 13 32 23.7 -33 08 21           ~ 120 1
12 ACO 3562 ClG 13 33 31.8 -31 40 23           ~ 283 1
13 PKS 1330-328 BLL 13 33 35.79 -33 05 13.5           ~ 9 1
14 IC 4296 AGN 13 36 39.03275288 -33 57 57.0783023   11.52 12.99 10.00   ~ 441 2
15 NGC 5813 LIN 15 01 11.265 +01 42 07.09 12.00 11.45 10.46 10.06   ~ 578 1
16 ACO 2142 ClG 15 58 20.00 +27 14 00.3           ~ 672 0
17 ACO 3653 ClG 19 53 14.4041 -52 03 59.306           ~ 21 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-03:54:51

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