We compute M _ { 260 } ^ { dyn } , the dynamical mass interior to a radius of 260 h ^ { -1 } kpc , for a set of 809 isolated host galaxies in the 100k data release of the 2dF Galaxy Redshift Survey .
The hosts are surrounded by 1556 satellite galaxies , as defined by a set of specific selection criteria .
Our mass estimator and host/satellite selection criteria are taken from those used by the Sloan Digital Sky Survey ( SDSS ) collaboration for an analysis of M _ { 260 } ^ { dyn } for SDSS galaxies and , overall , our results compare well with theirs .
In particular , for L \mathrel { \raise 1.505 pt \hbox { $ \scriptstyle > $ } \kern - 6.0 pt \lower 1.72 pt \hbox { { $% \scriptstyle \sim$ } } } 2 L ^ { \ast } we find ( M _ { 260 } ^ { dyn } / L ) _ { b _ { J } } = ( 193 \pm 14 ) h~ { } M _ { \odot } / L _ { \odot } , with a weak tendency for hosts with L < 2 L ^ { \ast } to have a somewhat higher M / L .
Additionally , we investigate M / L for bright ( b _ { J } \mathrel { \raise 1.505 pt \hbox { $ \scriptstyle < $ } \kern - 6.0 pt \lower 1.72 pt% \hbox { { $ \scriptstyle \sim$ } } } 18 ) galaxies with elliptical , S0 , and spiral morphologies .
There are 159 hosts in the elliptical/S0 sample and , similar to the full sample , we find ( M _ { 260 } ^ { dyn } / L ) _ { b _ { J } } = ( 271 \pm 26 ) h~ { } M _ { \odot } / L _ { \odot } 
for galaxies with L \mathrel { \raise 1.505 pt \hbox { $ \scriptstyle > $ } \kern - 6.0 pt \lower 1.72 pt \hbox { { $% \scriptstyle \sim$ } } } 2 L ^ { \ast } , and a weak tendency for intrinsically fainter galaxies to have a somewhat higher M / L .
In stark contrast to this , we find the line of sight velocity dispersion for the 243 spiral hosts to be independent of the host luminosity , with a value of \sigma _ { v } = 189 \pm 19 km s ^ { -1 } .
Thus , for spiral hosts we find that ( M _ { 260 } ^ { dyn } / L ) _ { b _ { J } } \propto L ^ { -1.0 \pm 0.2 } , where ( M _ { 260 } ^ { dyn } / L ) _ { b _ { J } } for a 2 L ^ { \ast } spiral is of order 200 h~ { } M _ { \odot } / L _ { \odot } .