  The age of a young asteroid family can be determined by tracking the orbits
of family members backward in time and showing that they converge at some time
in the past. Here we consider the Veritas family. We find that the membership
of the Veritas family increased enormously since the last detailed analysis of
the family. Using backward integration, we confirm the convergence of nodal
longitudes $\Omega$, and, for the first time, also obtain a simultaneous
convergence of pericenter longitudes $\varpi$. The Veritas family is found to
be $8.23^{+0.37}_{-0.31}$~Myr old. To obtain a tight convergence of $\Omega$
and $\varpi$, as expected from low ejection speeds of fragments, the Yarkovsky
effect needs to be included in the modeling of the past orbital histories of
Veritas family members. Using this method, we compute the Yarkovsky semi-major
axis drift rates, ${\rm d}a/{\rm d}t$, for 274 member asteroids. The
distribution of ${\rm d}a/{\rm d}t$ values is consistent with a population of
C-type objects with low densities and low thermal conductivities. The accuracy
of individual ${\rm d}a/{\rm d}t$ measurements is limited by the effect of
close encounters of member asteroids to (1) Ceres and other massive asteroids,
which cannot be evaluated with confidence.
