J/A+A/656/A144 Superclusters in local Universe at z≤0.03 (Bohringer+, 2021)
The Cosmic Large-Scale Structure in X-rays (CLASSIX) Cluster Survey.
IV. Superclusters in the local Universe at z ≤ 0.03.
Bohringer H., Chon G.
<Astron. Astrophys., 656, A144 (2021)>
=2021A&A...656A.144B 2021A&A...656A.144B (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; X-ray sources
Keywords: galaxies: clusters: general - cosmology: observations -
large-scale structure of Universe - X-rays: galaxies: clusters
Abstract:
It is important to map the large-scale matter distribution in the
local Universe for cosmological studies, such as the tracing of the
large-scale peculiar velocity flow, the characterisation of the
environment for different astronomical objects, and for precision
measurements of cosmological parameters. We used X-ray luminous
clusters to map this matter distribution and find that about 51% of
the groups and clusters are members of superclusters which occupy only
a few percent of the volume. In this paper we provide a detailed
description of these large-scale structures. With a friends-to-friends
algorithm, we find eight superclusters with a cluster overdensity
ratio of at least two with five or more galaxy group and cluster
members in the cosmic volume out to z=0.03. The four most prominent
ones are the Perseus-Pisces, the Centaurus, the Coma, and the Hercules
supercluster, with lengths from about 40 to over 100Mpc and estimated
masses of 0.6-2.2x1016M☉. The largest of these structures
is the Perseus-Pisces supercluster. The four smaller superclusters
include the Local and the Abell 400 supercluster and two superclusters
in the constellations Sagittarius and Lacerta. We provide detailed
maps, member catalogues, and physical descriptions of the eight
superclusters. By constructing superclusters with a range of cluster
sub-samples with different lower X-ray luminosity limits, we show that
the main structures are always reliably recovered.
Description:
Groups and clusters for six superclusters.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tables.dat 106 58 Groups and clusters (tables 3-8, A1)
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Byte-by-byte Description of file: tables.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- Tab Table number (1)
4- 18 A15 --- Name Name
20- 27 F8.4 deg RAdeg Right ascension (J2000)
29- 36 F8.4 deg DEdeg Declination (J2000)
38- 43 F6.4 --- z Redshift
44 A1 --- n_z [a] Note on redshift (2)
46- 53 F8.4 10-15W/m2 FX Flux in the 0.1-2.4keV band
(in 10-12erg/s/cm2)
55- 59 F5.2 % e_FX Error in FX in per cent unit
61- 66 F6.4 10+37W LX X-ray luminosity (in 10+44erg/s)
68- 72 F5.3 10+14Msun M200 Cluster mass estimated from the LX-mass
relation within r200
74- 77 F4.1 arcmin rout ?=- Radius out to which the X-ray
luminosity is detected in the RASS
79- 82 F4.1 10+20cm-2 nH Interstellar column density in the
line-of-sight
84- 85 A2 --- Memb Name of the SC of which the cluster is a
member (3)
87-104 A18 --- AName Name of the central dominant galaxy of
the group
106 A1 --- Notes Notes (2)
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Note (1): Tables the data are coming from as follows:
3 = Groups and clusters which are members of the Local SC
4 = Groups and clusters which are members of the Centaurus SC
5 = Groups and clusters which are members of the Coma SC
6 = Groups and clusters which are members of the Hercules SC at z≤0.03
7 = Groups and clusters which are members of the Sagittarius SC
8 = Groups and clusters which are members of the Lacerta SC
A1 = Groups and clusters which were found with the alternative linking
schemes to be SC members
Note (2): Notes as follows:
a = M86 has a blueshift in a heliocentric reference system of about 223km/s.
Here we give as a distance measure the redshift of the Virgo cluster,
to which M86 belongs.
b = These two clusters were previously identified in the RASS North Ecliptic
Pole survey by Henry et al. (1995ApJ...449..422H 1995ApJ...449..422H) and are listed there
by their RASS source names: RX J1736.4+6804 and RX J1755.8+6236.
c = The central galaxy of the group is WISEA J00035.61-383736.4 with z=0.01946
and a brightness of around 15th magnitude. Another member of this group
somewhat offset from the centre is IC4931 at z=0.02004.
d = This group was also identified in the search for galaxy groups in the
2MASS redshift survey as object no. 12252 by Crook et al.
(2007ApJ...655..790C 2007ApJ...655..790C, Cat. J/ApJ/655/790).
e = Also identified as WBL group 679 (White et al., 1999AJ....118.2014W 1999AJ....118.2014W,
Cat. J/AJ/118/2014).
f = Also identified as WBL group 681, the redshift above is that of the group.
g = The group features two bright elliptical galaxies, UC 12064 with a
distance of about 3.4 arcmin to the reference coordinate and
MCG+06-49-027 with a distance of about 5.2 arcmin, both at the
redshift of the group.
h = Central dominant galaxy is UGC 12491.
Note (3): supercluster of which the cluster is a member as follows:
C = Centaurus
G = Coma Supercluster
L = Local
H = Hercules at z≤0.03
S = Sagittarius
La = Lacerta
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History:
From electronic version of the journal
References:
Bohringer et al., Paper I 2016A&A...596A..22B 2016A&A...596A..22B
Bohringer et al., Paper II 2021A&A...651A..15B 2021A&A...651A..15B
Bohringer et al., Paper III 2021A&A...651A..16B 2021A&A...651A..16B
(End) Patricia Vannier [CDS] 21-Feb-2022