  Microlensing is able to reveal multiple body systems located several
kilo-parsec away from the Earth. Since it does not require the measurement of
light from the lens, microlensing is sensitive to a range of objects from
free-floating planets to stellar black holes. But if the lens emits enough
light, the microlensing model predictions can be tested with high-resolution
imaging and/or radial velocity methods. Such follow-up was done for the
microlensing event OGLE-2011-BLG-0417, which was expected to be a close by
($\le$ 1 kpc), low-mass ($\sim 0.8 M_\odot$) binary star with a period $P\sim
1.4$ yr. The spectroscopic follow-up observations conducted with the VLT did
not measure any variation in the radial velocity, in strong contradiction with
the published microlensing model. In the present work, we remodel this event
and find a simpler model in agreement with all the available measurements,
including the recent GAIA DR2 parallax constraints. We also present a new way
to distinguish degenerate models by using the GAIA DR2 proper motions. This
work stresses the importance of thorough microlensing modeling, especially with
the horizon of the {\it WFIRST} and the {\it Euclid} microlensing space
missions.
