  The Milky Way (MW) is a barred spiral galaxy shaped by tidal interactions
with its satellites. The Large Magellanic Cloud (LMC) and the Sagittarius Dwarf
galaxy (Sgr) are the dominant influences at the present day. This paper
presents a suite of four 10^9 particle N-body simulations, illustrating the
response of the MW's stellar disc to the close approach of the LMC and the
merger of Sgr into the MW. The suite is intended to provide a resource for
others to study the complex interactions between the MW and its satellites
independently and combined, in comparison to an isolated disc control
simulation. Such high resolution simulations are vital to understand the
kinematics and morphology of the MW taking into account the effects of each
satellite. In our preliminary analysis, we find that the influences from the
LMC and Sgr on the MW's disc appear distinct, additive and separable within our
tailored simulations. Notably, the corrugations induced by Sgr reproduce the
large radial velocity wave seen in the data Eilers+20. Overall, our findings
emphasise the need to include both satellites when modelling the present-day
state of the MW structure and kinematics.
