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J/ApJS/115/1 MX northern Abell cluster redshift survey (Slinglend+ 1998)
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The MX northern Abell cluster redshift survey.
Slinglend K., Batuski D., Miller C., Haase S., Michaud K., Hill J.M.
<Astrophys. J. Suppl. Ser. 115, 1 (1998)>
=1998ApJS..115....1S (SIMBAD/NED BibCode)
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ADC_Keywords: Clusters, galaxy ; Redshifts
Keywords: galaxies: clusters: general - galaxies: distances and redshifts -
large-scale structure of universe
Abstract:
The results from the COBE satellite show the existence of structure on
scales ~ 10% or more of the horizon scale of the universe. Rich
clusters of galaxies from the Abell/Abell, Corwin, & Olowin catalogs
(Cat. <VII/110>) show evidence of structure on scales of 100h^-1^Mpc
and hold the promise of confirming structure on the scale of the COBE
results. An impediment to that promise has been that redshift
information has been unavailable for a large percentage of these
clusters, so knowledge of their three-dimensional distribution has had
large uncertainties. We have been working to greatly expand the sample
of Abell clusters with reliable redshifts. Our approach in this
effort, through the MX Northern Abell Cluster Redshift Survey, has
been to measure redshifts of at least 25 galaxies in each of 95 R>=1
Abell cluster fields with m_10_<=16.8 and zero or one previously
measured redshift. Of these 95 observed Abell clusters, 88 new cluster
redshifts were obtained with an average of nine cluster member galaxy
redshifts per field. Two clusters were found to be chance projections
of galaxies along the line of sight, while five cluster observations
did not provide enough galaxy redshifts to make a positive
identification. This work has resulted in a deeper, 98% complete, and
more reliable sample of three-dimensional positions of rich Abell
clusters in the northern hemisphere. The primary intent of this survey
has been to produce a larger and more complete sample of rich Abell
clusters that can be used as tracers for large-scale structure.
Through analyses with tools such as the two-point correlation
function, power spectrum, and velocity dispersions, this sample can be
used to constrain theoretical models better for the formation of
structure we see in the universe today.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 47 105 MX survey cluster velocities
table2.dat 43 1162 Individual galaxy velocities
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See also:
VII/110 : Rich Clusters of Galaxies (Abell+ 1989)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Cluster Abell cluster name
6 A1 --- m_Cluster [ab] Multiplicity index on Cluster
7 A1 --- n_Cluster [*] Note on Cluster (1)
8- 11 F4.1 mag m10 ? Magnitude of the tenth brightest galaxy
in the cluster
13- 18 A6 --- Class Bautz-Morgan (1970ApJ...162L.149B) class
20- 24 I5 km/s mu ? Mean velocity
25 A1 --- n_mu [AC] Note on {mu} velocity (2)
27- 31 I5 km/s CBI ? Biweight estimate of the data's
central location
33- 36 I4 km/s sigma ? Standard deviation velocity
38- 41 I4 km/s SBI ? Biweight estimate of the data's scale
43- 44 I2 --- Ncluster ? Number of galaxy velocities (within each
group) that went into each calculation
46 A1 --- Note [*bf] Notes (3)
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Note (1): * : Includes five galaxies from CfA survey.
Note (2): A: Clusters that not have enough measured galaxies for a clear
determination
C: Clusters that are not clusters at all but rather are simply many
galaxies (i.e. 15 or so observed) along the line of sight.
Note (3): *: Mean velocity is the accepted velocity
b: Clearly identified background group
f: Clearly identified foreground group
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Cluster Abell cluster name (1)
8- 9 I2 h RAh Right ascension (2000.0) (1)
11- 12 I2 min RAm Right ascension (2000.0) (1)
14- 18 F5.2 s RAs Right ascension (2000.0) (1)
21 A1 --- DE- Declination sign (1)
22- 23 I2 deg DEd Declination (2000.0) (1)
25- 26 I2 arcmin DEm Declination (2000.0) (1)
28- 31 F4.1 arcsec DEs Declination (2000.0) (1)
34- 38 I5 km/s Vel ? Velocity
39 A1 --- n_Vel [a] Note on Vel (2)
41- 42 I2 km/s e_Vel rms uncertainty on Vel
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Note (1): Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD
Note (2): a : cD galaxy or brightest central galaxy in the cluster.
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History: From WWW site http://kramer.ume.maine.edu/~panda/phyast/mxdata
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(End) James Marcout, Patricia Bauer [CDS] 16-Oct-1998