J/ApJS/115/1 J/ApJS/115/1 MX northern Abell cluster redshift survey K Slinglend D Batuski C Miller S Haase K Michaud J M Hill Astrophys. J. Suppl. Ser. 115 1 1998 1998ApJS..115....1S VII/110 : Rich Clusters of Galaxies (Abell+ 1989) Clusters, galaxy Redshifts galaxies: clusters: general galaxies: distances and redshifts large-scale structure of universe 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 m10 less than or equal to 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.

Cluster Abell cluster name --- m_Cluster Multiplicity index on Cluster --- n_Cluster Note on Cluster number=1 * : Includes five galaxies from CfA survey. --- m10 Magnitude of the tenth brightest galaxy in the cluster mag Class Bautz-Morgan (1970ApJ...162L.149B) class --- mu Mean velocity km/s n_mu Note on {mu} velocity number=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. --- CBI Biweight estimate of the data's central location km/s sigma Standard deviation velocity km/s SBI Biweight estimate of the data's scale km/s Ncluster Number of galaxy velocities (within each group) that went into each calculation --- Note Notes number=3 *: Mean velocity is the accepted velocity b: Clearly identified background group f: Clearly identified foreground group --- Cluster Abell cluster name number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD --- RAh Right ascension (2000.0) number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD h RAm Right ascension (2000.0) number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD min RAs Right ascension (2000.0) number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD s DE- Declination sign number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD --- DEd Declination (2000.0) number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD deg DEm Declination (2000.0) number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD arcmin DEs Declination (2000.0) number=1 Name "[SBM98] ACO NNNN JHHMMSS.ss+DDMMSS.s" in SIMBAD arcsec Vel Velocity km/s n_Vel Note on Vel number=2 a : cD galaxy or brightest central galaxy in the cluster. --- e_Vel rms uncertainty on Vel km/s James Marcout, Patricia Bauer CDS 1998Oct16 UNKNOWN UNKNOWN //kramer.ume.maine.edu/~panda/phyast/mxdata J_ApJS_115_1.xml