  We report the first characterisation of the individual discs in the
intermediate separation binary systems KK Oph and HD 144668 at millimetre
wavelengths. In both systems the circum-primary and the circum-secondary discs
are detected in the millimetre continuum emission, but not in $^{13}$CO nor
C$^{18}$O lines. Even though the disc structure is only marginally resolved, we
find indications of large-scale asymmetries in the outer regions of the primary
discs, most likely due to perturbation by the companion. The derived dust
masses are firmly above debris disc level for all stars. The primaries have
about three times more dust in their discs than the secondaries. In the case of
HD 144668 the opacity spectral index of the primary and secondary differ by the
large margin of 0.69 which may be a consequence of the secondary disc being
more compact. Upper limits on the gas masses imply less than 0.1
M$_{\textrm{jup}}$ in any of these discs, meaning that giant planets can no
longer form in them. Considering that there have been no massive gas discs
identified to date in intermediate separation binaries (i.e., binaries at a few
hundred au separation), this opens space for speculation whether their binarity
causes the removal of gas, with tidal interaction truncating the discs and
hence shortening the accretion timescale. More systematic studies in this
respect are sorely needed.
