2010A&A...522A..92E


C.D.S. - SIMBAD4 rel 1.7 - 2019.09.21CEST12:00:42

2010A&A...522A..92E - Astronomy and Astrophysics, volume 522, A92-92 (2010/11-1)

The Sloan Great Wall. Rich clusters.

EINASTO M., TAGO E., SAAR E., NURMI P., ENKVIST I., EINASTO P., HEINAEMAEKI P., LIIVAMAEGI L.J., TEMPEL E., EINASTO J., MARTINEZ V.J., VENNIK J. and PIHAJOKI P.

Abstract (from CDS):

We present the results of the study of the substructure and galaxy content of ten rich clusters of galaxies in three different superclusters of the Sloan great wall, the richest nearby system of galaxies (hereafter SGW). We determine the substructure in clusters using the ``Mclust'' package from the ``R'' statistical environment and analyse their galaxy content with information about colours and morphological types of galaxies. We analyse the distribution of the peculiar velocities of galaxies in clusters and calculate the peculiar velocity of the first ranked galaxy. We show that five clusters in our sample have more than one component; in some clusters the different components also have different galaxy content. In other clusters there are distinct components in the distribution of the peculiar velocities of galaxies. We find that in some clusters with substructure the peculiar velocities of the first ranked galaxies are high. All clusters in our sample host luminous red galaxies; in eight clusters their number exceeds ten. Luminous red galaxies can be found both in the central areas of clusters and in the outskirts, some of them have high peculiar velocities. About 1/3 of the red galaxies in clusters are spirals. The scatter of colours of red ellipticals is in most clusters larger than that of red spirals. The fraction of red galaxies in rich clusters in the cores of the richest superclusters is larger than the fraction of red galaxies in other very rich clusters in the SGW. The presence of substructure in rich clusters, signs of possible mergers and infall, and the high peculiar velocities of the first ranked galaxies suggest that the clusters in our sample are not yet virialized. We present merger trees of dark matter haloes in an N-body simulation to demonstrate the formation of present-day dark matter haloes via multiple mergers during their evolution. In simulated dark matter haloes we find a substructure similar to that in observed clusters.

Abstract Copyright:

Journal keyword(s): large-scale structure of the Universe - galaxies: clusters: general

CDS comments: Fig.2 SDSS galaxy J10351.33+051130.8 not identified, incomplete format.

Simbad objects: 21

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Number of rows : 21

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 1066 ClG 10 39 06.62 +05 12 35.2           ~ 80 1
2 NAME VELA SUPERCL SCG 10 53.0 +02 44           ~ 24 0
3 ACO 1205 ClG 11 13 21.37 +02 32 39.4           ~ 57 0
4 ACO 1367 ClG 11 44 44.6 +19 41 59           ~ 974 1
5 ACO 1424 ClG 11 57 30.50 +05 05 24.5           ~ 55 0
6 NAME VIRGO-COMA SUPERCL SCG 12 04 +09.0           ~ 16 0
7 ACO 1516 ClG 12 18 50.20 +05 13 56.6           ~ 45 1
8 ACO 1650 ClG 12 58 36.76 -01 43 34.2           ~ 261 0
9 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4073 2
10 2MASX J13011606-0328288 Sy2 13 01 16.1001452955 -03 28 29.122567613   18.15 17.71     ~ 9 0
11 6dFGS gJ130116.7-032825 G 13 01 16.685 -03 28 23.65   17.64   16.25   ~ 5 0
12 ACO 1658 ClG 13 01 21.05 -03 34 00.1           ~ 15 0
13 SDSS J130152.60-024012.3 G 13 01 52.605 -02 40 12.39           ~ 1 0
14 ACO 1663 ClG 13 02 52.55 -02 31 04.0           ~ 90 0
15 ACO 1750 ClG 13 30 49.94 -01 52 22.1           ~ 142 1
16 ACO 1773 ClG 13 42 11.73 +02 13 28.2           ~ 103 0
17 BSCG 11 SCG 13 47 +03.4           ~ 12 0
18 ACO 1809 ClG 13 53 03.72 +05 08 17.7           ~ 151 0
19 ACO 2151 ClG 16 05 15.0 +17 44 55           ~ 546 3
20 ACO 2197 ClG 16 28 10.4 +40 54 26           ~ 269 0
21 NAME Sloan Great Wall ? ~ ~           ~ 150 0

    Equat.    Gal    SGal    Ecl

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2019.09.21-12:00:42

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