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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: dbdcd6ce1b3eb6c24f5d572a70df83cfa47f77bb
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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
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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 all
such 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 of
the 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.