The effects of LMC-mass environments on their dwarf satellite galaxies
  in the FIRE simulations
  Characterizing the predicted environments of dwarf galaxies like the Large
Magellanic Cloud (LMC) is becoming increasingly important as next generation
surveys push sensitivity limits into this low-mass regime at cosmological
distances. We study the environmental effects of LMC-mass halos ($M_{200m} \sim
10^{11}$ M$_\odot$) on their populations of satellites ($M_\star \geq 10^4$
M$_\odot$) using a suite of zoom-in simulations from the Feedback In Realistic
Environments (FIRE) project. Our simulations predict significant hot coronas
with $T\sim10^5$ K and $M_\text{gas}\sim10^{9.5}$ M$_\odot$. We identify
signatures of environmental quenching in dwarf satellite galaxies, particularly
for satellites with intermediate mass ($M_\star = 10^{6-7}$ M$_\odot$). The gas
content of such objects indicates ram-pressure as the likely quenching
mechanism, sometimes aided by star formation feedback. Satellites of LMC-mass
hosts replicate the stellar mass dependence of the quiescent fraction found in
satellites of MW mass hosts (i.e. that the quiescent fraction increases as
stellar mass decreases). Satellites of LMC-mass hosts have a wider variety of
quenching times when compared to the strongly bi-modal distribution of
quenching times of nearby centrals. Finally, we identify significant tidal
stellar structures around four of our six LMC-analogs, suggesting that stellar
streams may be common. These tidal features originated from satellites on close
orbits, extend to $\sim$80 kpc from the central galaxy, and contain
$\sim10^{6-7}$ M$_\odot$~of stars.
