  Ejection velocity fields of asteroid families are largely unconstrained due
to the fact that members disperse relatively quickly on Myr time-scales by
secular resonances and the Yarkovsky effect. The spreading of fragments in $a$
by the Yarkovsky effect is indistinguishable from the spreading caused by the
initial ejection of fragments. By examining families $<$20 Myrs-old, we can use
the V-shape identification technique to separate family shapes that are due to
the initial ejection velocity field and those that are due to the Yarkovsky
effect. $<$20 Myr-old asteroid families provide an opportunity to study the
velocity field of family fragments before they become too dispersed. Only the
Karin family's initial velocity field has been determined and scales inversely
with diameter, $D^{-1}$. We have applied the V-shape identification technique
to constrain young families' initial ejection velocity fields by measuring the
curvature of their fragments' V-shape correlation in semi-major axis, $a$, vs.
$D^{-1}$ space. Curvature from a straight line implies a deviation from a
scaling of $D^{-1}$. We measure the V-shape curvature of 11 young asteroid
families including the \FYnospace, Aeolia, Brangane, Brasilia, Clarissa,
Iannini, Karin, Konig, Koronis(2), Theobalda and Veritas asteroid families. We
find that the majority of asteroid families have initial ejection velocity
fields consistent with $\sim D^{-1}$ supporting laboratory impact experiments
and computer simulations of disrupting asteroid parent bodies.
