  We study the tidal problem and the resulting $I$-Love-$Q$ approximate
universal relations for rotating superfluid neutron stars in the Hartle-Thorne
formalism. Superfluid stars are described in this work by means of a two-fluid
model consisting of superfluid neutrons and all other charged constituents. We
employ a stationary and axisymmetric perturbation scheme to second order around
a static and spherically symmetric background. Recently, we used this scheme to
study isolated rotating superfluid stars. In this paper it is applied to
analyze the axially symmetric sector of the tidal problem in a binary system.
We show that a consistent use of perturbative matching theory amends the
original two-fluid formalism for the tidal problem to account for the possible
non-zero value of the energy density at the boundary of the star. This is
exemplified by building numerically different stellar models spanning three
equations of state. Significant departures from universality are found when the
correct matching relations are not taken into account. We also present an
augmented set of universal relations for superfluid neutron stars which
includes the contribution to the total mass of the star at second order,
$\delta M$. Therefore, our results complete the set of universal relations for
rotating superfluid stars, generalizing our previous findings in the perfect
fluid case.
