  The first two LIGO and Virgo observation runs have been important milestones
in the gravitational wave (GW) field, thanks to the detection of GW signals
from ten binary black hole systems and a binary neutron star system. In order
to fully characterize the emitting source, the remnant object and its
environment, electromagnetic follow-up observations at different wavelengths
are essential, as learned from the GW170817/GRB170817A case. Given the quite
large localization uncertainties provided by interferometers, the main
challenge faced by facilities with a narrow field of view (e.g. Imaging
Atmospheric Cherenkov Telescopes, IACTs) is to setup a suitable follow-up
strategy in order to observe sky regions with the highest probability to host
the electromagnetic (EM) counterpart of the GW signal. As member of the EM
follow-up community, the MAGIC collaboration joined this effort in 2014. As the
third observation run (O3) is currently ongoing, where both LIGO and Virgo are
expected to have much better sensitivities, MAGIC is refining its follow-up
strategy to maximize the chances of observing the EM counterparts as soon as
possible. In this contribution we will describe this strategy, focusing on the
different observation cases, which mainly depends on the information available
from both GW and EM partner facilities.
