A timing constraint on the (total) mass of the Large Magellanic Cloud
  This paper explores the effect of the LMC on the mass estimates obtained from
the timing argument. We show that accounting for the presence of the LMC
systematically lowers the Local Group mass ($M_{\rm LG}$) derived from the
relative motion of the Milky Way--Andromeda pair. Motivated by this result we
apply a Bayesian technique devised by Pe\~narrubia et al. (2014) to
simultaneously fit (i) distances and velocities of galaxies within 3~Mpc and
(ii) the relative motion between the Milky Way and Andromeda derived from HST
observations, with the LMC mass ($M_{\rm LMC}$) as a free parameter. Our
analysis returns a Local Group mass $M_{\rm LG}=2.64^{+0.42}_{-0.38}\times
10^{12}M_\odot$ at a 68\% confidence level. The masses of the Milky Way,
$M_{\rm MW}=1.04_{-0.23}^{+0.26}\times 10^{12}M_\odot$, and Andromeda, $M_{\rm
M31}=1.33_{-0.33}^{+0.39}\times 10^{12}M_\odot$, are consistent with previous
estimates that neglect the impact of the LMC on the observed Hubble flow. We
find a (total) LMC mass $M_{\rm LMC}=0.25_{-0.08}^{+0.09}\times
10^{12}M_\odot$, which is indicative of an extended dark matter halo and
supports the scenario where this galaxy is just past its first pericentric
approach. Consequently, these results suggest that the LMC may induce
significant perturbations on the Galactic potential.
