this is for holding javascript data
Andrew Wetzel edited quiescent_fraction.tex
about 9 years ago
Commit id: 4fe5de077389f36a86537c850987863aeae39e7d
deletions | additions
diff --git a/quiescent_fraction.tex b/quiescent_fraction.tex
index 1898a99..01d525a 100644
--- a/quiescent_fraction.tex
+++ b/quiescent_fraction.tex
...
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.
This is likely an unbiased metric, absent significant differential completeness as a function of recent star formation, which is unlikely because star-forming galaxies are generally brighter, but the quiescent fraction is near unity across almost all $\mstar$.
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}). 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) halos.
The error bars show 68\% uncertainty for a beta distribution \citep{Cameron2011} based on the counts in each bin.
Of the 56 known satellites, only 4 (7\%) are star-forming/gas-rich: the LMC and SMC around the MW, LGS 3 and IC 10 around M31.