The formation and assembly history of the Milky Way revealed by its
  globular cluster population
  We use the age-metallicity distribution of 96 Galactic globular clusters
(GCs) to infer the formation and assembly history of the Milky Way (MW),
culminating in the reconstruction of its merger tree. Based on a quantitative
comparison of the Galactic GC population to the 25 cosmological zoom-in
simulations of MW-mass galaxies in the E-MOSAICS project, which
self-consistently model the formation and evolution of GC populations in a
cosmological context, we find that the MW assembled quickly for its mass,
reaching $\{25,50\}\%$ of its present-day halo mass already at $z=\{3,1.5\}$
and half of its present-day stellar mass at $z=1.2$. We reconstruct the MW's
merger tree from its GC age-metallicity distribution, inferring the number of
mergers as a function of mass ratio and redshift. These statistics place the
MW's assembly $\textit{rate}$ among the 72th-94th percentile of the E-MOSAICS
galaxies, whereas its $\textit{integrated}$ properties (e.g. number of mergers,
halo concentration) match the median of the simulations. We conclude that the
MW has experienced no major mergers (mass ratios $>$1:4) since $z\sim4$,
sharpening previous limits of $z\sim2$. We identify three massive satellite
progenitors and constrain their mass growth and enrichment histories. Two are
proposed to correspond to Sagittarius (few $10^8~{\rm M}_\odot$) and the GCs
formerly associated with Canis Major ($\sim10^9~{\rm M}_\odot$). The third
satellite has no known associated relic and was likely accreted between
$z=0.6$-$1.3$. We name this enigmatic galaxy $\textit{Kraken}$ and propose that
it is the most massive satellite ($M_*\sim2\times10^9~{\rm M}_\odot$) ever
accreted by the MW. We predict that $\sim40\%$ of the Galactic GCs formed
ex-situ (in galaxies with masses $M_*=2\times10^7$-$2\times10^9~{\rm
M}_\odot$), with $6\pm1$ being former nuclear clusters.
