Dynamical History of the Local Group in $\Lambda$CDM
  The positions and velocities of galaxies in the Local Group (LG) measure the
gravitational field within it. This is mostly due to the Milky Way (MW) and
Andromeda (M31). We constrain their masses using distance and radial velocity
(RV) measurements of 32 LG galaxies. To do this, we follow the trajectories of
many simulated particles starting on a pure Hubble flow at redshift 9. For each
observed galaxy, we obtain a trajectory which today is at the same position.
Its final velocity is the model prediction for the velocity of that galaxy.
  Unlike previous simulations based on spherical symmetry, ours are
axisymmetric and include gravity from Centaurus A. We find the total LG mass is
${4.33^{+0.37}_{-0.32}\times{10}^{12}M_\odot}$, with $0.14 \pm 0.07$ of this
being in the MW. We approximately account for IC 342, M81, the Great Attractor
and the Large Magellanic Cloud.
  No plausible set of initial conditions yields a good match to the RVs of our
sample of LG galaxies. Observed RVs systematically exceed those predicted by
the best-fitting $\Lambda$CDM model, with a typical disagreement of
${45.1^{+7.0}_{-5.7}}$ km/s and a maximum of ${110 \pm 13}$ km/s for DDO 99.
Interactions between LG dwarf galaxies can't easily explain this.
  One possibility is a past close flyby of the MW and M31. This arises in some
modified gravity theories but not in $\Lambda$CDM. Gravitational slingshot
encounters of material in the LG with either of these massive fast-moving
galaxies could plausibly explain why some non-satellite LG galaxies are moving
away from us even faster than a pure Hubble flow.
