Measuring the Milky Way mass distribution in the presence of the LMC
  The ongoing interaction between the Milky Way (MW) and its largest satellite
- the Large Magellanic Cloud (LMC) - creates a significant perturbation in the
distribution and kinematics of distant halo stars, globular clusters and
satellite galaxies, and leads to biases in MW mass estimates from these tracer
populations. We present a method for compensating these perturbations for any
choice of MW potential by computing the past trajectory of LMC and MW and then
integrating the orbits of tracer objects back in time until the influence of
the LMC is negligible, at which point the equilibrium approximation can be used
with any standard dynamical modelling approach. We add this orbit-rewinding
step to the mass estimation approach based on simultaneous fitting of the
potential and the distribution function of tracers, and apply it to two
datasets with the latest Gaia EDR3 measurements of 6d phase-space coordinates:
globular clusters and satellite galaxies. We find that models with LMC mass in
the range (1-2)x10^11 Msun better fit the observed distribution of tracers, and
measure MW mass within 100 kpc to be (0.75+-0.1)x10^12 Msun, while neglecting
the LMC perturbation increases it by ~15%.
