deletions | additions       diff --git a/summary_discussion.tex b/summary_discussion.tex  index 2b517b2..02e60e3 100644  --- a/summary_discussion.tex  +++ b/summary_discussion.tex 
...
Furthermore, the same internal stellar feedback that regulates the low star-formation efficiency in such dwarf galaxies and likely drives significant gas flows to large radii \citep[e.g.,][]{Muratov2015} would strongly assist such environmental stripping to make even more efficient in dwarf galaxies.  In this sense, the rapid environmental quenching timescales for dwarf galaxies likely arise not just from the role of the external environment, but from the non-linear interplay of internal feedback and external stripping \citep[e.g.,][]{NicholsBlandHawthorn2011,BaheMcCarthy2015}.  The above scenario may also help to explain the curious similarity of Figure~\ref{fig:quench_times} with the mass dependence of the underlying galaxy-halo $\mstar/\mvir$ relation \citep[e.g.,][]{Behroozi2013}, \citep[e.g.,][]{Behroozi2013c},  which peaks at $\mstar\sim10^{10}\msun$ (higher but similar mass). In particular, at high $\mstar$, the same process that lowers $\mstar/\mvir$ with increases mass also lowers the underlying gas fraction, which in turn causes more massive satellites to quench more rapidly after infall.  At low $\mstar$, the same shallower potential wells that allow internal feedback to lower $\mstar/\mvir$ also allows external stripping to occur more easily.