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 b3917b6..777b904 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 observedsatellite  dwarf galaxies that are within satellites (within  $300 \kpc$ ($\approx \rvir$) \kpc \approx \rvir$  of the MW or M31 M31)  and have a measurement/upper-limit of 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 all such satellites, violet squares show satellites of the MW, green triangles show satellites 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.