function of the relevant survey and $v_{\rm med}$ is the median RSCG velocity. When calculating $N_{\rm int, env}$ we integrate over 1.5 $h^{-1}$ projected Mpc, although some groups are centered on the edge of the survey where we do not observe all galaxies in the neighborhood. We indicate these groups in the table.

We also list $N_{\rm int,cg}$ in Table \[tab:env\]. We calculate this number by replacing 1.5 Mpc with $R_{\rm cg}$, the group radius in Mpc, in Equation \[eqn:nint\]. We then compute the overdensity of the RSCG, $\frac{N_{\rm cg}}{N_{\rm int,cg}} \approx \frac{\langle \rho_{\rm cg} \rangle}
{\langle \overline{\rho} \rangle }$. $N_{\rm cg}$ is the number of galaxies in the RSCG and $\rho_{\rm cg}$ is the density of the compact group. The RSCG’s have $460 < \frac{\langle \rho_{\rm cg} \rangle}
{\overline{\langle \rho}\rangle } < 150,000$.

For $cz \geq 2300$ km s$^{-1}$, 43 RSCG’s (74%) have $\langle \rho_{\rm env}  \rangle \ \gg \ \langle \overline{\rho} \rangle$. This result gives the same impression as the conclusion of Ramella et al. that most but not all HCG’s are embedded in looser systems.

All 10 RSCG’s with $cz \geq 2300\ {\rm km\ s}^{-1}$ which fail the “isolation” criterion (§6) satisfy $N_{n} > N_{\rm int} + 