deletions | additions       diff --git a/introduction.tex b/introduction.tex  index 835a3f0..c84b286 100644  --- a/introduction.tex  +++ b/introduction.tex 
...
Galaxies in denser environments are more likely to have suppressed (quiescent) star formation and little-to-no cold gas than galaxies of similar stellar mass, $\mstar$, in less dense environments.  The observed environmental effects within the Local Group (LG) on the satellite galaxies within the halos of the Milky Way (MW) and Andromeda (M31) are particularly strong \citep[e.g.,][]{Einasto1974, Mateo1998, McConnachie2012, Phillips2014, SlaterBell2014, Spekkens2014}, even compared to the already strong effects on (more massive) satellites within massive groups/clusters.  Specifically, the dwarf galaxies around the MW/M31 show a strikingly sharp and nearly complete transition in their properties within $\approx 300 \kpc$ (approximately the virial radius, $\rvir$, of the MW or M31), from irregular to spheroidal morphologies, from having most of their baryonic mass in cold atomic gas to having little-to-no measured cold gas, and from actively star-forming to quiescent.  This trend has just a few exceptions: 4 gas-rich, star-forming galaxies persist within the halos of the MW (the LMC and SMC) and M31 (LGS 3 and IC 10), and3 -  4 - 5  quiescent, gas-poor galaxies reside well  beyond $\rvir$ of either  the MW (Cetus and Tucana) and or  M31 (KKR \[Cetus \citep{Lewis2007}, Tucana \citep{Fraternali2009}, KKR  25 \citep{Makarov2012}, KKs 3 \citep{Karachentsev2015},  and possibly Andromeda XVIII), XVIII\],  though Cetus and Tucana likely may have  orbited within the MW halo \citep{Lewis2007, Fraternali2009, Teyssier2012}. \citep{Teyssier2012}.  This efficient satellite quenching is particularly striking because, other than KKR 25, 25 and KKs 3,  at $\mstar<10^9\msun$ \emph{all} all  known galaxies that are sufficiently isolated ($>1500\kpc$ from a more massive galaxy) are star-forming \citep{Geha2012, Phillips2014}. Thus, the MW and M31 halos exert the strongest environmental influence on their satellites of any known systems, so the LG is a compelling laboratory for studying environmental processes on galaxies.  Several such processes within a host halo can regulate the gas content, star formation, morphology, and eventual disruption of satellite galaxies, including gravitational tidal forces \citep[e.g.,][]{Dekel2003}, galaxy-galaxy interactions \citep[e.g.,][]{FaroukiShapiro1981} and mergers \citep[e.g.,][]{Deason2014a}, ram-pressure stripping of extended gas \citep[e.g.,][]{Larson1980, McCarthy2008} or of cold inter-stellar medium \citep[e.g.,][]{GunnGott1972, Tonnesen2009}, some of which may be assisted by stellar feedback within the satellite \citep[e.g.,][]{BaheMcCarthy2015}.