  We have exploited the very precise parallaxes, proper motions and photometry
of \textit{Gaia}\, Data Release~2 to study white dwarf members of the Hyades
star cluster.
  Gaia photometry and parallaxes for the eight DA white dwarfs confirmed
members have been then used to compute absolute magnitudes and colours. These
were compared to three independent sets of white dwarf evolutionary tracks, to
derive cooling times and white dwarf (final) masses. All sets of models provide
the same mass values, with only small differences in the cooling ages. The
precision in the derived masses and cooling ages is typically 1-3%. Our derived
masses are generally consistent with spectroscopic estimates from the
literature, whilst cooling ages are generally larger.
  The recent estimate of the cluster age from the Gaia Data Release~2 main
sequence turn off colour-magnitude-diagram (790Myr) has been employed to derive
progenitor (initial) masses. We find a slope of the initial-final mass relation
for the Hyades white dwarfs (masses between ~0.67 and ~0.84 Mo) steeper than
that derived for the same mass range from global estimates --averaged over the
whole spectrum of white dwarf masses-- irrespectively of the cooling models
adopted. However, when considering the error in this age estimate (+160 -100
Myr), a definitive conclusion on this issue cannot be reached yet. The lower
limit of 690Myr (closer to the classical Hyades age of 600-650Myr) would
provide a slope of the initial-final mass relation closer to the global
determinations.
  We also find hints of an intrinsic spread of the cluster initial-final mass
relation for the cluster.
