  $v_W$ leptokurtic asteroid families are families for which the distribution
of the normal component of the terminal ejection velocity field $v_W$ is
characterized by a positive value of the ${\gamma}_2$ Pearson kurtosis, i.e.,
they have a distribution with a more concentrated peak and larger tails than
the Gaussian one. Currently, eight families are known to have ${\gamma}_2(v_W)
> 0.25$. Among these, three are highly inclined asteroid families, the Hansa,
Barcelona, and Gallia families. As observed for the case of the Astrid family,
the leptokurtic inclination distribution seems to be caused by the interaction
of these families with node secular resonances. In particular, the Hansa and
Gallia family are crossed by the $s-s_V$ resonance with Vesta, that
significantly alters the inclination of some of their members.
  In this work we use the time evolution of ${\gamma}_2(v_W)$ for simulated
families under the gravitational influence of all planets and the three most
massive bodies in the main belt to assess the dynamical importance (or lack of)
node secular resonances with Ceres, Vesta, and Pallas for the considered
families, and to obtain independent constraints on the family ages. While
secular resonances with massive bodies in the main belt do not significantly
affect the dynamical evolution of the Barcelona family, they significantly
increase the ${\gamma}_2(v_W)$ values of the simulated Hansa and Gallia
families. Current values of the ${\gamma}_2(v_W)$ for the Gallia family are
reached over the estimated family age only if secular resonances with Vesta are
accounted for.
