deletions | additions       diff --git a/quiescent_fraction.tex b/quiescent_fraction.tex  index a94da44..5eeca56 100644  --- a/quiescent_fraction.tex  +++ b/quiescent_fraction.tex 
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\subsection{Observed Satellite  Quiescent Fractions} Based on our above definitions of ``satellite'' and ''quiescent'' dwarf galaxies, we group all satellites in the LG into 1-dex bins of $\mstar$ and compute the fraction of which that  are quiescent in each bin. We do not attempt any correction for observational completeness as a function of $\mstar$, because we measure the \emph{relative fraction} that are quiescent in each bin, which bin.  This  is likely an unbiased metric, absent significant differential completeness as a function of recent star formation.  We consider the latter formation, which is  unlikely because star-forming galaxies are generally brighter, but the quiescent fraction is near unity across our range in almost all  $\mstar$.(We do take into account the maximum observed distance of dwarfs at each $\mstar$ bin when we compute the virial-infall times using the simulations, see below.)  Figure~\ref{fig:quiescent_fraction} shows the quiescent fraction for all satellite dwarf galaxies of the MW or M31 versus $\mstar$ \citep[see also][]{Phillips2014, SlaterBell2014}).  We show fractions for all such satellites (blue circles) as well as separately for those in the MW (violet squares) and M31 (green triangles). triangles) halos.  The error bars show 68\% uncertainty for a beta distribution \citep{Cameron2011} based on the observed counts. counts in each bin.  Of the NNN satellites, 56 satellites in Figure~\ref{fig:quiescent_fraction},  only 4 (7\%)  are star-forming/gas-rich: the LMC and SMC around the MW, LGS 3 and IC 10 around M31. Moreover, at $\mstar<8\times10^7\msun$, 50 only 1 (LGS 3)  of the  51 satellites are quiescent, star-forming,  and at $\mstar<9 \times10^5\msun$ $\mstar<9\times10^5\msun$  \emph{all} NNN 40  satellites are quiescent.The error bars show 68\% uncertainty for a beta distribution \citep{Cameron2011} based on the observed counts.  These high near-unity  quiescent fractions contrast strongly with the fact that essentially all isolated effectively \emph{zero} quiescent fraction \citep{Geha2012, Phillips2014} for dwarf  galaxies (that are not environmentally affected) at $\mstar<10^9\msun$ that  are star-forming. isolated ($>1500\kpc$ from a more massive host).  The only known exception is KKR 25, a dwarf spheroidal with $\mstar=1.4\times10^6\msun$ that is $1853\kpc$ from M31.