this is for holding javascript data
Andrew Wetzel edited abstract.tex
about 9 years ago
Commit id: 0309fac2bf5d6db359e8da196a45b26625e50807
deletions | additions
diff --git a/abstract.tex b/abstract.tex
index 9e532e2..db06399 100644
--- a/abstract.tex
+++ b/abstract.tex
...
In the Local Group, nearly all of the
dwarf galaxies
with $\mstar\lesssim10^9\msun$ ($\mstar\lesssim10^9\msun$) that are satellites within $300\kpc$ (the virial radius) of the Milky Way (MW) and Andromeda (M31) have quiescent star formation and little-to-no cold gas.
This contrasts strongly with comparatively isolated dwarf galaxies, which are almost all actively star-forming and gas-rich.
This near dichotomy implies a \emph{rapid} transformation after falling into the halos of the MW or M31.
We combine the observed quiescent fractions for satellites of the MW and M31 with the infall times of satellites from the ELVIS suite of cosmological simulations to determine the typical timescales over which environmental processes within the MW/M31 halos remove gas and quench star formation in
low-mass satellite galaxies.
The quenching timescales
at for satellites with $\mstar<10^8\msun$ are short, $\lesssim2\gyr$, and decrease
with decreasing satellite mass. at lower $\mstar$.
%and are comparable to a virial-radius crossing time.
These quenching timescales can be $1-2\gyr$ longer if environmental preprocessing in lower-mass groups prior to MW/M31 infall is important.
We compare with timescales for more massive satellites from previous works, which indicates that the environmental quenching timescale increases rapidly with satellite
mass, $\mstar$, peaking at $\approx9.5\gyr$ for
$\mstar\approx10^9\msun$, $\mstar\sim10^9\msun$, and rapidly decreases at higher
satellite mass $\mstar$ to less than $5\gyr$ at $\mstar>5\times10^9\msun$.
Thus, satellites with
masses $\mstar\sim10^9\msun$, similar to
the Magellanic Clouds Magellanic-Cloud masses, exhibit the longest environmental quenching timescales.