  Ultracompact binaries with orbital periods less than a few hours will
dominate the gravitational wave signal in the mHz regime. Until recently, 10
systems were expected have a predicted gravitational wave signal strong enough
to be detectable by the Laser Interferometer Space Antenna (LISA), the
so-called `verification binaries'. System parameters, including distances, are
needed to provide an accurate prediction of the expected gravitational wave
strength to be measured by LISA. Using parallaxes from {\sl Gaia} Data Release
2 we calculate signal-to-noise ratios (SNR) for $\approx$50 verification binary
candidates. We find that 11 binaries reach a SNR$\geq$20, two further binaries
reaching a SNR$\geq$5 and three more systems are expected to have a
SNR$\approx$5 after four years integration with LISA. For these 16 systems we
present predictions of the gravitational wave amplitude ($\mathcal{A}$) and
parameter uncertainties from Fisher information matrix on the amplitude
($\mathcal{A}$) and inclination ($\iota$).
