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Andrew Wetzel edited figures/qu.time_v_m.star_sat.first.t/caption.tex
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\label{fig:quench_times}
Environmental quenching timescales
of for satellite galaxies across the observable range of stellar mass, $\mstar$ (top axis shows subhalo $\mpeak$ from abundance matching).
Blue circles show satellites of the MW and M31, obtained by matching the observed quiescent fractions in Figure~\ref{fig:quiescent_fraction} to
rank-ordered virial-infall times of satellites from the ELVIS simulations \citep{Wetzel2015} in 1-dex bins of $\mstar$.
At $\mstar=10^{4-5}\msun$ (light blue), some satellite may have been quenched prior to infall via reionization, so interpret with care.
Error bars
are derived come from the 68\% uncertainty in
the observed quiescent fractions in Figure~\ref{fig:quiescent_fraction}.
Left panel uses time since first infall into the current
MW/M31 MW/M31-like halo, while right panel uses time since first infall into \emph{any} host halo, including possible effects of group preprocessing.
Gray triangle shows lower limit for the LMC/SMC system using its infall time from its measured
proper motion orbital velocity \citep{Kallivayalil2013}.
Red squares show
times inferred for satellites with $\mstar=10^{8.5}$, $10^{9.5}\msun$ in SDSS \citep{Wheeler2014}, and green curve shows
the same for more massive satellites in groups of $\mvir=10^{12-13}$ in SDSS \citep{Wetzel2013}.
The satellite
dwarfs of dwarf galaxies in the MW/M31 halos
were quenched much more rapidly after infall than more massive satellites
in (in other
hosts, hosts), with the timescale being longest near
Magellanic-Cloud-masses. Magellanic-Cloud masses.