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We present N-body and hydrodynamical simulations of the response of the MilkyWay's baryonic disc to the presence of the Large Magellanic Cloud during afirst infall scenario. For a fiducial galactic model reproducing the grossproperties of the Galaxy, we explore a set of six initial conditions for theLMC of varying mass which all evolve to fit the measured constraints on itscurrent position and velocity with respect to the Galactic Center. We find thatthe LMC can produce strong disturbances - warping of the stellar and gaseousdiscs - in the Galaxy, without violating constraints from the phase-spacedistribution of stars in the Solar Neighbourhood. All models correctlyreproduce the phases of the warp and its anti-symmetrical shape about thedisc's mid-plane. If the warp is due to the LMC alone, then the largest massmodel is favoured ($2.5\times10^{11}\,\rm{M_{\odot}}$). Still, somequantitative discrepancies remain, including deficits in height of $\DeltaZ=0.7 \, \rm{kpc}$ at $R=22 \,\rm{kpc}$ and $\Delta Z=0.7\, \rm{kpc}$ at $R=16\,\rm{kpc}$. This suggests that even higher infall masses for the LMC's haloare allowed by the data. A comparison with the vertical perturbations inducedby a heavy Sagittarius dSph model ($10^{11}\,\rm{M_{\odot}}$) suggest thatpositive interference with the LMC warp is expected at $R=16 \, \rm{kpc}$. Weconclude that the vertical structure of the Galactic disc beyond the SolarNeighbourhood may jointly be shaped by its most massive satellites. As such,the current structure of the MW suggests we are seeing the process of discheating by satellite interactions in action.

Response of the Milky Way's disc to the Large Magellanic Cloud in a first infall scenario