2010A&A...517A..94D


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST04:19:48

2010A&A...517A..94D - Astronomy and Astrophysics, volume 517, A94-94 (2010/7-1)

The clusters Abell 222 and Abell 223: a multi-wavelength view.

DURRET F., LAGANA T.F., ADAMI C. and BERTIN E.

Abstract (from CDS):

The Abell 222 and 223 clusters are located at an average redshift z∼0.21 and are separated by 0.26deg. Signatures of mergers have been previously found in these clusters, both in X-rays and at optical wavelengths, thus motivating our study. In X-rays, they are relatively bright, and Abell 223 shows a double structure. A filament has also been detected between the clusters both at optical and X-ray wavelengths. We analyse the optical properties of these two clusters based on deep imaging in two bands, derive their galaxy luminosity functions (GLFs) and correlate these properties with X-ray characteristics derived from XMM-Newton data. The optical part of our study is based on archive images obtained with the CFHT Megaprime/Megacam camera, covering a total region of about 1deg2, or 12.3x12.3Mpc2 at a redshift of 0.21. The X-ray analysis is based on archive XMM-Newton images. The GLFs of Abell 222 in the g' and r' bands are well fit by a Schechter function; the GLF is steeper in r' than in g'. For Abell 223, the GLFs in both bands require a second component at bright magnitudes, added to a Schechter function; they are similar in both bands. The Serna & Gerbal (1996A&A...309...65S) method allows to separate well the two clusters. No obvious filamentary structures are detected at very large scales around the clusters, but a third cluster at the same redshift, Abell 209, is located at a projected distance of 19.2Mpc. X-ray temperature and metallicity maps reveal that the temperature and metallicity of the X-ray gas are quite homogeneous in Abell 222, while they are very perturbed in Abell 223. The Abell 222/Abell 223 system is complex. The two clusters that form this structure present very different dynamical states. Abell 222 is a smaller, less massive and almost isothermal cluster. On the other hand, Abell 223 is more massive and has most probably been crossed by a subcluster on its way to the northeast. As a consequence, the temperature distribution is very inhomogeneous. Signs of recent interactions are also detected in the optical data where this cluster shows a ``perturbed'' GLF. In summary, the multiwavelength analyses of Abell 222 and Abell 223 are used to investigate the connection between the ICM and the cluster galaxy properties in an interacting system.

Abstract Copyright:

Journal keyword(s): galaxies: clusters: individual: Abell 222 - X-rays: galaxies: clusters - galaxies: clusters: individual: Abell 223 - galaxies: clusters: intracluster medium

Simbad objects: 9

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Number of rows : 9

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 209 ClG 01 31 57.5 -13 34 35           ~ 250 0
2 ACO 222 ClG 01 37 27.4 -12 58 45           ~ 122 1
3 ACO 223 ClG 01 37 55.9 -12 49 11           ~ 108 1
4 NAME Sgr Stream St* 02 22 +00.0           ~ 644 0
5 NGC 4874 LIN 12 59 35.709 +27 57 33.80 13.01 13.7 11.40 12.122 11.386 ~ 713 3
6 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4208 2
7 NGC 4889 BiC 13 00 08.097 +27 58 37.29 12.93 13.0 11.30 11.652 10.906 ~ 642 1
8 ACO 1763 ClG 13 35 20.1 +41 00 04           ~ 261 0
9 ACO 1770 ClG 13 40 03 +41 16.8           ~ 18 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-04:19:48

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