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Andrew Wetzel edited figures/qu.frac_v_m.star_lg_mw_m31_gas.ratio.0.1/caption.tex
about 9 years ago
Commit id: 5a05494689a1adbf4a5fcc2f77422e6c9d4bf65b
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\label{fig:quiescent_fraction}
Observed fraction of For all observed satellite dwarf galaxies that are
quiescent (gas-poor) versus stellar mass, $\mstar$, for all satellites within $300
\kpc \approx \rvir$ \kpc$ ($\approx \rvir$) of the MW or M31
that also and have
a measurement/upper-limit of cold atomic gas
measurements or upper-limits. 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.
At $\mstar < 8 \times 10 ^ 7 \msun$, 50 of 51 satellites are quiescent, and at $\mstar < 9 \times 10 ^ 5 \msun$, \emph{all} are quiescent.
The error bars show 68\% uncertainty in this fraction using a beta distribution \citep{Cameron2011}.