We compare the properties of gas flows on both the near and far side of the Large Magellanic Cloud ( LMC ) disk using Hubble Space Telescope UV absorption-line observations toward an AGN behind ( transverse ) and a star within ( down-the-barrel ) the LMC disk at an impact parameter of 3.2 ~ { } \mathrm { kpc } .
We find that even in this relatively quiescent region gas flows away from the disk at speeds up to \sim 100 ~ { } { km \thinspace s ^ { -1 } } in broad and symmetrical absorption in the low and high ions .
The symmetric absorption profiles combined with previous surveys showing little evidence that the ejected gas returns to the LMC and provide compelling evidence that the LMC drives a global , large-scale outflow across its disk , which is the likely result of a recent burst of star formation in the LMC .
We find that the outflowing gas is multiphase , ionized by both photoionization ( Si ii and Si iii ) and collisional ionization ( Si iv and C iv ) .
We estimate a total mass and outflow rate to be \gtrsim 10 ^ { 7 } ~ { } { M } _ { \sun } and \gtrsim 0.4 ~ { } { M } _ { \sun } ~ { } \mathrm { yr } ^ { -1 } .
Since the velocity of this large-scale outflow does not reach the LMC escape velocity , the gas removal is likely aided by either ram-pressure stripping with the Milky Way halo or tidal interactions with the surrounding galaxies , implying that the environment of LMC-like or dwarf galaxies plays an important role in their ultimate gas starvation .
Finally we reassess the mass and plausible origins of the high-velocity complex toward the LMC given its newly-determined distance that places it in the lower Milky Way halo and sky-coverage that shows it extends well beyond the LMC disk .