2009A&A...508..191L


C.D.S. - SIMBAD4 rel 1.7 - 2021.02.26CET17:59:25

2009A&A...508..191L - Astronomy and Astrophysics, volume 508, 191-200 (2009/12-2)

Metallicity map of the galaxy cluster A3667.

LOVISARI L., KAPFERER W., SCHINDLER S. and FERRARI C.

Abstract (from CDS):

We use XMM-Newtondata of the merging cluster Abell 3667 to analyze its metallicity distribution. A detailed abundance map of the central 1.1x1.1 Mpc region indicates that metals are inhomogeneously distributed in the cluster showing a non-uniform and very complex metal pattern. The highest peak in the map corresponds to a cold region, slightly offset South of the X-ray center. This could be interpreted as stripped gas due to a merger between a group moving from NW towards the SE and the main cluster. We note several clumps of high metallicity also in the opposite direction with respect to the X-ray peak. Furthermore we determined abundances for 5 elements (O, Si, S, Ar, Fe) in four different regions of the cluster. Comparisons between these observed abundances and theoretical supernovae yields allow to get constraints on the relative number of SN Ia and II contributing to the enrichment of the intra-cluster medium. To reproduce the observed abundances of the best determined elements (Fe, O and Si) in a region of 7' around the X-ray center, 65-80% of SN II are needed. The comparison between the metal map, a galaxy density map obtained using 550 spectroscopically confirmed cluster members and, our simulations suggest a recent merger between the main cluster and the group in the SE.

Abstract Copyright:

Journal keyword(s): galaxies: cluster: general - galaxies: abundances - X-rays: galaxies: clusters - galaxies: clusters: individual: Abell 3667

Simbad objects: 2

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Number of rows : 2

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 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5856 1
2 ACO 3667 ClG 20 12 33.68 -56 50 26.3           ~ 572 1

    Equat.    Gal    SGal    Ecl

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