deletions | additions       diff --git a/figures/qu.frac_v_m.star_lg_mw_m31_gas.ratio.0.1/caption.tex b/figures/qu.frac_v_m.star_lg_mw_m31_gas.ratio.0.1/caption.tex  index ffa64af..a4f6d6c 100644  --- a/figures/qu.frac_v_m.star_lg_mw_m31_gas.ratio.0.1/caption.tex  +++ b/figures/qu.frac_v_m.star_lg_mw_m31_gas.ratio.0.1/caption.tex 
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\label{fig:quiescent_fraction}  For all observed dwarf galaxies that are satellites (within within  $300 \kpc \approx \rvir$) \rvir$  of the Milky Way (MW) or M31 Andromeda (M31)  and have a measurement/upper-limit of measured/constrained  cold atomic gas mass, the fraction that are quiescent (gas-poor) versus stellar mass, $\mstar$. We define quiescence as $\mgas / \mstar < 0.1$.  Blue circles show allsuch  satellites, while  violet squares show satellites those  of the MW, MW and  green triangles show satellites those  of M31. The only star-forming/gas-rich satellites are: LGS 3 ($\mstar = 9.6 \times 10 ^ 5 \msun$) and IC 10 ($\mstar = 9 \times 10 ^ 7$) around M31; LMC ($\mstar = 1.5 \times 10 ^ 9 \msun$) and SMC ($\mstar = 4.6 \times 10 ^ 8 \msun$) around the MW.  At $\mstar < 8 \times 10 ^ 7 \msun$, \msun$  50 ofthe  51 observed satellites are quiescent, quiescent  and at $\mstar < 9 \times 10 ^ 5 \msun$, \msun$  \emph{all} are quiescent. The error bars show 68\% uncertainty for a beta distribution \citep{Cameron2011}  based on the observed counts via a beta distribution \citep{Cameron2011}. counts.