J/MNRAS/274/1071 Edinburgh-Milano cluster redshift survey (Collins+ 1995)
The Edinburgh-Durham Southern Galaxy Catalogue -
VII. The Edinburgh-Milano cluster redshift survey
Collins C.A., Guzzo L., Nichol R.C., Lumsden S.L.
<Mon. Not. R. Astron. Soc. 274, 1071 (1995)>
=1995MNRAS.274.1071C 1995MNRAS.274.1071C (SIMBAD/NED BibCode)
ADC_Keywords: Redshifts ; Clusters, galaxy
Keywords: catalogues - surveys - galaxies: clusters: general -
galaxies: distances and redshifts - cosmology: observations -
large-scale structure of Universe
Abstract:
In this paper, we present the redshifts of the galaxies and galaxy
clusters which form the Edinburgh-Milano (EM) cluster redshift survey.
A total of 777 galaxy redshifts have been measured in 94 clusters
extracted from the digitized Edinburgh-Durham Cluster Catalogue. We
also present the radial velocity dispersions for 37 clusters.
Observational and data reduction techniques are discussed in detail,
together with the strategy adopted to determine the mean redshift of a
cluster and to identify and discard plausible phantom clusters. Some
10 per cent of our clusters show heavy contamination, indicating that
projection is a serious problem for optically selected, rich clusters.
The median velocity dispersion estimated for a subsample of richness
R≥1 clusters is 742±63km/s. From a simple comparison with
{OMEGA}=1 cold dark matter models of structure formation, these
results favour a biasing parameter b=1.6-2.0 and are inconsistent with
a bias outside of the range b=1.3-2.5.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2 65 31 Results for galaxies in the survey with two
independent observations either at the
ESO 3.6-m and 2.2-m telescopes or at the AAT.
table3 45 776 The galaxies observed in the EM cluster
redshift survey ESO and AAT
table4 59 94 The clusters observed in the EM redshift survey
table5 88 97 *List of selected clusters
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Note to table5: Clusters selected from the EDSGC using a reduced
Abell radius of 1.0h-1Mpc and subject to the selection criteria
given in Sect. 7, used as the basis for the clustering analysis
of Nichol et al. (1992MNRAS.255p..21N 1992MNRAS.255p..21N)
and Martin et al. (1995MNRAS.274..623M 1995MNRAS.274..623M).
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See also:
VII/175 : Edingburgh-Durham Cluster Catalogue (Lumdsen+ 1992)
Byte-by-byte Description of file: table2
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Bytes Format Units Label Explanations
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1- 3 I3 --- EDCC Edingburgh-Durham Cluster Catalogue (EDCC,
Cat VII/175) cluster identification name
5- 6 I2 h RAh Right ascension (B1950)
8- 9 I2 min RAm Right ascension (B1950)
11- 14 F4.1 s RAs Right ascension (B1950)
16 A1 --- DE- Declination sign
17- 18 I2 deg DEd Declination (B1950)
20- 21 I2 arcmin DEm Declination (B1950)
23- 24 I2 arcsec DEs Declination (B1950)
26- 30 F5.2 mag bj Approximate (±0.25mag) apparent magnitude
of the galaxy in the photographic b, band
from the EDSGC
32- 36 I5 km/s cz1 Radial velocity determined form Tel1 observations
38- 45 A8 --- Tel1 Telescope (ESO 3.6m, ESO 2.2m or ATT)
47- 51 I5 km/s cz2 Radial velocity determined form Tel2 observations
53- 60 A8 --- Tel2 Telescope (ESO 3.6m, ESO 2.2m or ATT)
62- 65 I4 km/s HV Heliocentric velocity
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Byte-by-byte Description of file: table3
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Bytes Format Units Label Explanations
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1- 3 I3 --- EDDC EDCC cluster identification name
5- 6 I2 h RAh ? Right ascension (B1950) (see note 1)
8- 9 I2 min RAm ? Right ascension (B1950) (see note 1)
11- 14 F4.1 s RAs ? Right ascension (B1950) (see note 1)
16 A1 --- DE- Declination sign
17- 18 I2 deg DEd ? Declination (B1950) (see note 1)
20- 21 I2 arcmin DEm ? Declination (B1950) (see note 1)
23- 24 I2 arcsec DEs ? Declination (B1950) (see note 1)
26- 30 F5.2 mag bj ? Approximate (±0.25mag) apparent magnitude
of the galaxy in the photographic b, band
from the EDSGC.
32- 36 I5 km/s cz Heliocentric velocity of each galaxy
38- 40 I3 km/s e_cz Internal redshift error from the
cross-correlation routine, described in
Section 4.2.
42- 45 A4 --- Note Note on observations (1)
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Note (1): E: ESO observation
A: AAT observation
AC: A larger than normal error in the coordinates and magnitude.
This is the case for galaxies which are not detected in the
EDSGC, e.g. objects merged with other object images in the
digitization process.
NC: Two galaxies in E178, three in E261, two in E424 and three in
E473 do not have a certain identification in our logfiles
We prefer therefore not to list any coordinate and magnitude
which would be too approximate, although we give the redshift
and the information that the object belongs to that cluster.
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Byte-by-byte Description of file: table4
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Bytes Format Units Label Explanations
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1- 3 I3 --- EDCC EDCC cluster identification name
5- 6 I2 h RAh Right ascension (B1950) (1)
8- 9 I2 min RAm Right ascension (B1950) (1)
11- 14 F4.1 s RAs Right ascension (B1950) (1)
16 A1 --- DE- Declination sign
17- 18 I2 deg DEd Declination (B1950) (1)
20- 21 I2 arcmin DEm Declination (B1950) (1)
23- 24 I2 arcsec DEs Declination (B1950) (1)
26- 27 I2 --- Ntot Total number of redshifts taken for each cluster
(listed in Table 3)
29- 30 I2 --- Nclus ? Number of cluster members determined from the
deprojection algorithm described in Sect. 5.1
32- 36 I5 km/s cz ? Mean heliocentric redshift of the galaxy
members in each cluster
39- 41 I3 km/s e_cz ? 1 sigma errors on the mean redshift of each
cluster
43- 46 I4 km/s sigma ? Radial velocity dispersions for clusters with
N cluster =>6
49- 51 I3 km/s E_sigma ? Error in sigma (upper limit)
54- 56 I3 km/s e_sigma ? Error in sigma (lower limit)
59 A1 --- Note [p] 'p' indicates that the cluster has been
classified as a projection effect (see Sect. 5.1)
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Note (1): Equatorial coordinates of the cluster centroid, taken from
Lumsden et al. (1992MNRAS.258....1L 1992MNRAS.258....1L, Cat. VII/175).
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Byte-by-byte Description of file: table5
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Bytes Format Units Label Explanations
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1- 3 I3 --- EDCC EDCC cluster identification name
6- 7 I2 h RAh Right ascension (B1950) (1)
9- 10 I2 min RAm Right ascension (B1950) (1)
12- 15 F4.1 s RAs Right ascension (B1950) (1)
17 A1 --- DE- Declination sign
18- 19 I2 deg DEd Declination (B1950) (1)
21- 22 I2 arcmin DEm Declination (B1950) (1)
24- 25 I2 arcsec DEs Declination (B1950) (1)
28- 29 I2 --- R1 Number of galaxy members between the magnitudes
m3 and m3+2 calculated using an Abell
radius of 1h-1Mpc
31- 34 F4.1 mag m10 Magnitude of the 10th brightest galaxy, after
background correction, within the 1h-1Mpc
radius
36- 40 F5.3 --- RAbell Angular 'reduced Abell radius' calculated using
the equivalent of Abell's m10 distance
estimate
42- 44 I3 deg PA ? Position angle of the cluster as defined in
Martin et al. (1995MNRAS.274..623M 1995MNRAS.274..623M)
46- 49 F4.2 --- Eps ? [0/1] Eccentricity of the clusters, defined and
used in Martin et al. (1995MNRAS.274..623M 1995MNRAS.274..623M).
51- 55 I5 km/s cz ? Radial velocity of the cluster
57- 58 I2 --- o_cz ? Number of galaxies used to determine cz (2)
60- 88 A29 --- Ref Source of the cluster radial velocity (3)
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Note (1): Equatorial coordinates of the cluster centroid, taken from
Lumsden et al. 1992MNRAS.258....1L 1992MNRAS.258....1L, Cat. VII/175
Note (2): For the EM clusters, this is just N cluster (number of cluster members
determined from the deprojection algorithm)
Note (3): EM : this study
Broadbent 1992 (priv. comm.)
Ciardullo et al. (1985ApJ...293...69C 1985ApJ...293...69C)
Dalton et al. (1994MNRAS.269..151D 1994MNRAS.269..151D, Cat. J/MNRAS/269/151)
Huchra et al. (1992, Cat. VII/193)
Huchra (priv. comm.)
Loveday (1991, PhD thesis, Univ. Cambridge)
Muriel et al. (1990AJ....100..339M 1990AJ....100..339M)
Muriel et al. (1991AJ....101.1997M 1991AJ....101.1997M)
Nicholson (1991, PhD thesis, Univ. Edinburgh)
Olowin et al. (1988A&AS...73..125O 1988A&AS...73..125O)
Peacock (priv. comm.)
Peterson et al. (1986MNRAS.221..233P 1986MNRAS.221..233P)
Postman et al. (1992ApJ...384..404P 1992ApJ...384..404P, Cat. J/ApJ/384/404)
Teague et al. (1990ApJS...72..715T 1990ApJS...72..715T)
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Acknowledgements:
It is a pleasure to thank H. Andernach
and Chris Collins for communicating
questions and solutions about EDCC 80, 258, 285, 348 and 507.
History:
* January 1997: Prepared via OCR at CDS.
* Februray 1997: errors were detected by H. Andernach
and corrected in interaction with
Chris Collins
(End) James Marcout, Patricia Bauer [CDS] 14-Feb-1997