Dynamical analysis of compact groups provides important tests of models of compact group formation and evolution. By compiling 2066 redshifts from FLWO/FAST, from the literature, and from SDSS DR12 in the fields of compact groups in McConnachie et al. (2009), we construct the largest sample of compact groups with complete spectroscopic redshifts in the redshift range 0.01 < z < 0.22. This large redshift sample shows that the interloper fraction in the McConnachie et al. (2009) compact group candidates is  42%. A secure sample of 332 compact groups includes 192 groups with four or more member galaxies and 140 groups with three members. The fraction of early-type galaxies in these compact groups is 62%, higher than for the original Hickson compact groups. The velocity dispersions of early- and late-type galaxies in compact groups change little with groupcentric radius; the radii sampled are less than 100 h−1 kpc, smaller than the radii typically sampled by members of massive clusters of galaxies. The physical properties of our sample compact groups include size, number density, velocity dispersion, and local environment; these properties slightly differ from those derived for the original Hickson compact groups and for the DPOSS II compact groups. Differences result from subtle differences in the way the group candidates were originally selected. The abundance of the compact groups changes little with redshift over the range covered by this sample. The approximate constancy of the abundance for this sample is a potential constraint on the evolution of compact groups on a few Gigayear timescale.

Abstract
1. INTRODUCTION
2. DATA
    2.1. Parent Sample
    2.2. Redshift Data
3. A SAMPLE OF COMPACT GROUPS WITHREDSHIFTS
4. COMPACT GROUP PROPERTIES
    4.1. The Compact Groups
    4.2. Comparison with Other Compact Group Samples
5. SUMMARY
REFERENCES

• Jubee Sohn(Department of Physics and Astronomy, Seoul National University/Smithsonian Astrophysical Observatory) Corresponding author
• Ho Seong Hwang(School of Physics, Korea Institute for Advanced Study)
• Margaret J. Geller(Smithsonian Astrophysical Observatory)
• Antonaldo Diaferio(Dipartimento di Fisica, Universit`a degli Studi di Torino, V. Pietro Giuria/Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Torino)
• Kenneth J. Rines(Department of Physics and Astronomy, Western Washington University)
• Myung Gyoon Lee(Department of Physics and Astronomy, Seoul National University)
• Gwang-Ho Lee(Department of Physics and Astronomy, Seoul National University)