these groups are hard to model because they are within the local supercluster.

Table \[tab:env\] lists $\frac{N_{n}}{N_{\rm int,env}}$ for RSCG’s with average redshifts greater than 2300 km s$^{-1}$. $N_{\rm int,env}$ is the expected number of interlopers within 1.5 $h^{-1}$ Mpc of the group center in the velocity interval $[v_{\rm med}-1500,v_{\rm med}+1500]$; $$N_{\rm int,env} \approx \int_{V_{\rm env}} \overline{\rho} dV,$$ where $\overline{\rho}$ is the average density of the relevant portion of the survey and $V_{\rm env}$ is the volume of the environment of the group. Similarly, $$N_{n} \approx \int_{V_{\rm env}} \rho_{\rm env} dV,$$ where $\rho_{\rm env}$ is the density of the environment of the group. Therefore, $$\frac{N_{n}}{N_{\rm int,env}} \approx \frac{ \langle\rho_{\rm env}\rangle}
{\langle \overline{\rho} \rangle},$$ where the brackets denote averaging over the volume of the environment of the RSCG. To calculate this expected number of interlopers we integrate over the [*true*]{} luminosity function (Table \[tab:lumrd\]). We use the true luminosity function instead of the observed one for ease of calculation; the error introduced is small. Therefore, $$N_{\rm int,env}=\int_{v_{\rm med}-1500}^{v_{\rm med}+1500}  
\int_{-\infty}^{M_{\rm lim}(v)} \pi \left( \frac{1.5\  {\rm Mpc} \times v}{v_{\rm med}}\right)^{2}
\Phi_{\rm true}(M) dM \frac{dv}{H_{0}}, \label{eqn:nint}$$ where $M_{\rm lim}(v)$ is the limiting absolute magnitude at redshift $v$, $\Phi_{\rm true}$ is the true luminosity 