  We test the hypothesis that the apparent axis ratio of an elliptical galaxy
is correlated with the age of its stellar population. We find that old
ellipticals (with estimated stellar ages t > 7.5 Gyr) are rounder on average
than younger ellipticals. The statistical significance of this shape difference
is greatest at small radii; a Kolmogorov-Smirnov test comparing the axis ratios
of the two populations at R = Re/16 yields a statistical significance greater
than 99.96 percent. The relation between age and apparent axis ratio is linked
to the core/powerlaw surface brightness profile dichotomy. Core ellipticals
have older stellar populations, on average, than powerlaw ellipticals and are
rounder in their inner regions. Our results are consistent with a scenario in
which powerlaw ellipticals are formed in gas-rich mergers while core
ellipticals form in dissipationless mergers, with cores formed and maintained
by the influence of a binary black hole.
