CDROM/AJ/V110/P0463
The Shapley Supercluster (Quintana+ 1995)
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The Shapley Supercluster. I. Spectroscopic Observations in the Central
Region
H. Quintana, A. Ramirez, Jorge Melnick, Somak Raychaudhury, &
Eric Slezak
<1995, AJ, 110, 463>
=1995AJ....110..463Q
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Abstract:
We present a new analysis of the kinematics of the Shapley supercluster
based on radial velocities for 1087 galaxies in the clusters A3558
(Shapley 8), A3528 (Klemola 21), A3532 (Klemola 22), A3530, A3556 (SC
1321-314), A3559 (CE 1327-292), A3560, A3562, SC 1329-314 and in the
intercluster region of the core of the supercluster, of which 367 are
new measurements. We also present accurate positions from APM and MAMA
scans of the ESO/SERC Southern Sky Survey photographic plates. We
obtain new velocity dispersions and estimate the masses of the member
clusters, evaluating dynamical models of the supercluster. The
supercluster is found to be significantly flattened. We find that for
Omega_0=0.3, H_0=75 km/s/Mpc, the gravitational pull of the
supercluster may account for up to 25% of the peculiar velocity of the
Local Group required to explain the dipole anisotropy of the Cosmic
Microwave Background radiation, in which case the mass of the
supercluster would be dominated by intercluster dark matter. This
fractional contribution would be considerably higher for combinations
of significantly lower values of Omega_0 and higher values of H_0.
File Summary:
------------------------------------------------------------------------------File Name
Lrecl
Records
Explanations
------------------------------------------------------------------------------table2.dat
80
497
Galaxy velocities
------------------------------------------------------------------------------Byte-by-byte Description of file: table2.dat
------------------------------------------------------------------------------Bytes Format Units
Label
Explanations
------------------------------------------------------------------------------1- 7
A7
--Region
*ACO cluster name or cluster area
code
8- 9
2X
----Blank
10-13
A4
--ID
Observing identifications
14-15
2X
----Blank
16-18
I3
--ESO
ESO field
19-20
2X
----Blank
21-26
A6
--Coord
*APM, MAMA cat. numbers or other
codes
27
1X
----Blank
28-30
I3
h
RAh
[]? Right ascension, epoch 1950
31-33
I3
min
RAm
[]? R.A.
34-38
F5.1
s
RAs
[]? R.A.
39
1X
----Blank
40
A1
--DEDeclination sign
41-42
I2
deg
DEd
[]? Declination, epoch 1950
43-45
I3
arcmin
DEm
[]? Dec.
46-48
I3
arcsec
DEs
[]? Dec.
49
A1
--u_RADE
Equatorial coordinate uncertainty
flag
50
1X
----Blank
51
A1
--Code
*[R:<( ] Codes for following fields
52-56
F5.1
mag
m_J
[]? Ptg. J mag, measured from APM
survey
57-63
I7
km/s
RadVel
Heliocentric velocities
64-67
I4
km/s
e_RadVel
Heliocentric velocities error
68
1X
----Blank
69-73
A5
--R_nl
*R value or number of lines
74-75
2X
----Blank
76-80
A5
--Ref
*Code for observer or velocity
reference
------------------------------------------------------------------------------Notes for file: table2.dat
------------------------------------------------------------------------------Region:
Gives either the ACO cluster name, ordered by ascending number, or a
code for the area where the cluster is located. These areas denote
(1 degree x 5 min) regions (approx 1 square degree) in which we
divided the field to program the observations, and are named by the
coordinates of the NW corner. If this field is blank, the data in
the Code, RadVel, R_nl, and Ref fields are continuations for the
previous object.
Coord:
The APM, MAMA catalogue numbers or other codes used as source for
coordinates. Most coordinates are either from digital scans of the
SERC IIIa-J atlas, using the APM facility in Cambridge, England or
from scans of ESO/SRC R fields done with the MAMA machine at
Paris. For galaxies not found in the APM and MAMA scans, positions
are quoted from the ESO/Uppsala catalog (Lauberts 1982). Coordinates
for galaxies in A3558 were measured with the Optronics machine at
ESO, Garching.
Code:
R = m_J is R magnitude from the MAMA survey.
:
<
(
= m_J is uncertain (saturated image on plate or estimated by eye)
= m_J is an upper limit (the magnitude quoted being the total
magnitude of a merged image of which the galaxy is a part)
= velocities are not used in the mean values of redshifts.
R_nl:
The R value of the cross-correlation, or the number of lines
measured in each spectra, if the line position method was used.
The R value is a real value and the number of lines is an integer
value.
Ref:
The code of observer/telescope/date or a reference code if the
galaxy also has a velocity reported in the literature.
Q1-Q7,M1-M3: observing sessions as in Table 1
of the printed paper.
MGS87
Metcalfe et al. 1987, MNRAS, 225, 581
TCG90
Teague et al. 1990, ApJS, 72, 715
Da86
da Costa et al. 1986, AJ, 91, 6
Da87
da Costa et al. 1987, AJ, 93, 1338
DS88
Dressler and Shectman 1998, AJ, 95, 284
D091
Dressler 1991, ApJS, 75, 241
Cr87
Cristiani et al. 1987, A&A, 179, 108
R087
Richter, O.-G. 1987, A&A, 67, 261
Ve90
Vettolani et al. 1990, AJ, 99, 1709
Mo88
Monk et al. 1988, MNRAS, 234, 193
Mo89
Mould et al. 1989, ApJ, 338, 654
PGC
Paturel et al. Catalogue of Principal
Galaxies, Monographies de la Base de Donnees
Extragalactiques, No 1, Lyon: Obs. de Lyon;
1737
ZCAT Catalog, Huchra et al. 1993
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(End)
Lee Brotzman [ADS] 06Oct-1995