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The UZC-SSRS2 Group Catalog
We apply a friends-of-friends algorithm to the combined Updated ZwickyCatalog and Southern Sky Redshift Survey to construct a catalog of 1168groups of galaxies; 411 of these groups have five or more members withinthe redshift survey. The group catalog covers 4.69 sr, and all groupsexceed the number density contrast threshold, δρ/ρ=80. Wedemonstrate that the groups catalog is homogeneous across the twounderlying redshift surveys; the catalog of groups and their membersthus provides a basis for other statistical studies of the large-scaledistribution of groups and their physical properties. The medianphysical properties of the groups are similar to those for groupsderived from independent surveys, including the ESO Key Programme andthe Las Campanas Redshift Survey. We include tables of groups and theirmembers.
| The second Kiso Survey for ultraviolet-excess galaxies. II.
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| Gas-rich Dwarfs from the PSS-II. III. H I Profiles and Dynamical Masses
We present Arecibo neutral hydrogen data on a sample of opticallyselected dwarf galaxies. The sample ranges in H I mass from106 to 5×109 Msolar, with a meanof 7.9×108 Msolar. Using estimated H Iradii, the H I surface densities range from 0.6 to 20 Msolarpc-2, all well below the critical threshold for starformation (Kennicutt 1998). MH I/L values of the LSB dwarfsrange from 0.3 to 12 with a mean value of 2.0. Dynamical masses,calculated from the H I profile widths, range from 108 to1011 Msolar. There is a strong correlation betweenoptical luminosity and dynamical mass for LSB dwarfs implying that thedark matter (whether baryonic or nonbaryonic) follows the detectablebaryonic matter.
| Gas-rich Dwarfs from the Second Palomar Sky Survey. I. Catalog and Characteristics
This project is a visual search for field dwarf galaxies using SecondPalomar Sky Survey photographic plates. A morphologically selectedsample of 310 objects yielded 145 detections of true dwarfs within aredshift search window of 0 to 10,000 km s-1. We confirm the low-mass,dwarf nature of the same by comparison of luminosity, isophotal size, HI mass and H I profile width distribution of other dwarf samples. Thegoal of this project is to use these newly discovered dwarf galaxies tomap large-scale structure as a test of biased galaxy formation. Initialindicators are that the large-scale distribution of dwarf galaxies isidentical to that of bright, high-mass galaxies, in contradiction totheory using biasing. The full analysis of the sample will be reportedin the final paper of our series.
| Kinematics and dynamics of the MKW/AWM poor clusters
We report 472 new redshifts for 416 galaxies in the regions of the 23poor clusters of galaxies originally identified by Morgan, Kayser, andWhite (MKW), and Albert, White, and Morgan (AWM). Eighteen of the poorclusters now have 10 or more available redshifts within 1.5/h Mpc of thecentral galaxy; 11 clusters have at least 20 available redshifts. Basedon the 21 clusters for which we have sufficient velocity information,the median velocity scale is 336 km/s, a factor of 2 smaller than foundfor rich clusters. Several of the poor clusters exhibit complex velocitydistributions due to the presence of nearby clumps of galaxies. We checkon the velocity of the dominant galaxy in each poor cluster relative tothe remaining cluster members. Significantly high relative velocities ofthe dominant galaxy are found in only 4 of 21 poor clusters, 3 of whichwe suspect are due to contamination of the parent velocity distribution.Several statistical tests indicate that the D/cD galaxies are at thekinematic centers of the parent poor cluster velocity distributions.Mass-to-light ratios for 13 of the 15 poor clusters for which we havethe required data are in the range 50 less than or = M/LB(0)less than or = 200 solar mass/solar luminosity. The complex nature ofthe regions surrounding many of the poor clusters suggests that thesegroupings may represent an early epoch of cluster formation. Forexample, the poor clusters MKW7 and MKWS are shown to be gravitationallybound and likely to merge to form a richer cluster within the nextseveral Gyrs. Eight of the nine other poor clusters for which simpletwo-body dynamical models can be carried out are consistent with beingbound to other clumps in their vicinity. Additional complex systems withmore than two gravitationally bound clumps are observed among the poorclusters.
| Eighth list of compact galaxies .
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1975AJ.....80..545Z&db_key=AST
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