The connection between galaxy structure and quenching efficiency
  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 $9 < \log(M_*/M_\odot) < 11.5$, 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 $9 < \log(M_*/M_\odot) < 9.5$ 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. 
Conor Omand, Michael Balogh, Bianca Poggianti
astro-ph.GA astro-ph.CO