  Studying the trajectories of objects like stars, globular clusters or
satellite galaxies in the Milky Way allows to trace the dark matter halo but
requires reliable models of its gravitational potential. Realistic, yet simple
and fully analytical models have already been presented in the past. However,
improved as well as new observational constraints have become available in the
meantime calling for a recalibration of the respective model parameters. Three
widely used model potentials are revisited. By a simultaneous least-squared fit
to the observed rotation curve, in-plane proper motion of Sgr A*, local
mass/surface density and the velocity dispersion in Baade's window, parameters
of the potentials are brought up-to-date. The mass at large radii - and thus in
particular that of the dark matter halo - is hereby constrained by imposing
that the most extreme halo blue horizontal-branch star known has to be bound to
the Milky Way. The Galactic mass models are tuned to yield a very good match to
recent observations. The mass of the dark matter halo is - within the
limitations of the applied models - estimated in a fully consistent way. As a
first application, the trajectory of the hypervelocity star HE 0437-5439 is
re-investigated to check its suggested origin in the Large Magellanic Cloud
(LMC). Despite their simplicity, the presented Milky Way mass models are well
able to reproduce all observational constraints. Their analytical and simple
form makes them ideally suited for fast and accurate orbit calculations. The
LMC cannot be ruled out as HE 0437-5439's birthplace.
