  We have performed N-body simulations of the formation of hyper-velocity stars
(HVS) in the centre of the Milky Way due to inspiralling intermediate-mass
black holes (IMBHs). We considered IMBHs of different masses, all starting from
circular orbits at an initial distance of 0.1 pc.
  We find that the IMBHs sink to the centre of the Galaxy due to dynamical
friction, where they deplete the central cusp of stars. Some of these stars
become HVS and are ejected with velocities sufficiently high to escape the
Galaxy. Since the HVS carry with them information about their origin, in
particular in the moment of ejection, the velocity distribution and the
direction in which they escape the Galaxy, detecting a population of HVS will
provide insight in the ejection processes and could therefore provide indirect
evidence for the existence of IMBHs.
  Our simulations show that HVS are generated in short bursts which last only a
few Myrs until the IMBH is swallowed by the supermassive black hole (SMBH). HVS
are ejected almost isotropically, which makes IMBH induced ejections hard to
distinguish from ejections due to encounters of stellar binaries with a SMBH.
After the HVS have reached the galactic halo, their escape velocities correlate
with the distance from the Galactic centre in the sense that the fastest HVS
can be found furthest away from the centre. The velocity distribution of HVS
generated by inspiralling IMBHs is also nearly independent of the mass of the
IMBH and can be quite distinct from one generated by binary encounters.
  Finally, our simulations show that the presence of an IMBH in the Galactic
centre changes the stellar density distribution inside r<0.02 pc into a core
profile, which takes at least 100 Myrs to replenish.
