Measuring the Mass of the Large Magellanic Cloud with Stellar Streams
  Observed by ${S}^5$
  Stellar streams are excellent probes of the underlying gravitational
potential in which they evolve. In this work, we fit dynamical models to five
streams in the Southern Galactic hemisphere, combining observations from the
Southern Stellar Stream Spectroscopic Survey (${S}^5$), Gaia EDR3, and the Dark
Energy Survey (DES), to measure the mass of the Large Magellanic Cloud (LMC).
With an ensemble of streams, we find a mass of the LMC ranging from 14 to $19
\times 10^{10}\ \mathrm{M}_{\odot}$, probed over a range of closest approach
times and distances. With the most constraining stream (Orphan-Chenab), we
measure an LMC mass of $18.8^{+ 3.5}_{- 4.0} \times 10^{10}\
\mathrm{M}_{\odot}$, probed at a closest approach time of 310 Myr and a closest
approach distance of 25.4 kpc. This mass is compatible with previous
measurements, showing that a consistent picture is emerging of the LMC's
influence on structures in the Milky Way. Using this sample of streams, we find
that the LMC's effect depends on the relative orientation of the stream and LMC
at their point of closest approach. To better understand this, we present a
simple model based on the impulse approximation and we show that the LMC's
effect depends both on the magnitude of the velocity kick imparted to the
stream and the direction of this kick.
