$D$ discussed in Section \[ss:dist\] using $$\label{MLtrans}
   M/L_B = (M/L_F) \> (D_{\rm orig}/D) \> 10^{0.4 [(B-F) - (B-F)_{\rm
           \odot}]} .$$ Here $M/L_F$ is the mass-to-light ratio in some other band $F$ for the distance $D_{\rm orig}$, as given in the original literature source; $B-F$ is the relevant broad-band color of the galaxy, and $(B-F)_{\rm
\odot}$ is the color of the sun.

For the transformation in equation (\[MLtrans\]) we needed colors of the sample galaxies in various bands. For $B-V$ we used the data of Faber [[et al. ]{}]{}(1989, hereafter F89), who presented data for almost 600 nearby early-type galaxies. Their colors refer to apertures $\leq
30''$ in diameter around the galaxy center. The average color for the galaxies in our sample is $\langle B-V \rangle = 0.95$. We used this average color for the 8 galaxies in our final sample for which a $B-V$ was needed but for which none was available from F89. For those galaxies for which we needed the color $B-R_{\rm J}$ we used the transformation $B-R_{\rm J} = 1.839(B-V) + 0.064$. This was obtained from the equations $B-R_{\rm J} = 1.14 (B-R_{\rm C}) + 0.04$ and $V-R_{\rm C} = 0.613(B-V) + 0.021$ derived for early-type galaxies 