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Compact groups (CGs) of galaxies appear to be the densest galaxy systemscontaining a few luminous galaxies in close proximity to each other, which havea typical size of a few tens kilopacsec in observation. On the other hand, inthe modern hierarchical structure formation paradigm, galaxies are assembledand grouped in dark matter haloes, which have a typical size of a few hundredsof kiloparsec. Few studies have explored the physical connection between theobservation based CGs and halo model based galaxy groups to date. In thisstudy, by matching the largest local CG catalog of Zheng & Shen (2020) to thehalo based group catalog of Yang et al. (2007), we find that the CGs arephysically heterogenous systems and can be mainly separated into twocategories, the isolated systems and those embedded in rich groups or clusters.By examining the dynamical features of CGs, we find that the isolated CGs havesystematically lower dynamical masses than that of non-compact ones at the samegroup luminosity, indicating a more evolved stage of isolated CGs. On the otherhand, the embedded CGs are mixtures of chance alignments in poor clusters andrecent infalling groups (sub-structures) of rich clusters.

Compact Groups of Galaxies in Sloan Digital Sky Survey and LAMOST Spectral Survey. II. Dynamical Properties of Isolated and Embedded Groups