Using data from the SDSS-DR7 , including structural measurements from 2D surface brightness fits with GIM2D , we show how the fraction of quiescent galaxies depends on galaxy stellar mass M _ { * } , effective radius R _ { e } , fraction of r - band light in the bulge , B / T , and their status as a central or satellite galaxy at 0.01 < z < 0.2 .
For central galaxies we confirm that the quiescent fraction depends not only on stellar mass , but also on R _ { e } .
The dependence is particularly strong as a function of M _ { * } / R _ { e } ^ { \alpha } , with \alpha \sim 1.5 .
This appears to be driven by a simple dependence on B / T over the mass range 9 < \log ( M _ { * } / M _ { \Sun } ) < 11.5 , and is qualitatively similar even if galaxies with B / T > 0.3 are excluded .
For satellite galaxies , the quiescent fraction is always larger than that of central galaxies , for any combination of M _ { * } , R _ { e } and B / T .
The quenching efficiency is not constant , but reaches a maximum of \sim 0.7 for galaxies with 9 < \log ( M _ { * } / M _ { \Sun } ) < 9.5 and R _ { e } < 1 kpc .
This is the same region of parameter space in which the satellite fraction itself reaches its maximum value , suggesting that the transformation from an active central galaxy to a quiescent satellite is associated with a reduction in R _ { e } due to an increase in dominance of a bulge component .