  We address the problem of deriving, from the observed projected metallicity
gradients, the intrinsic metallicity distribution of elliptical galaxies as a
function of their integrals of motion. The method is illustrated by an
application to anisotropic spherical Hernquist models. We also compare the
derived metallicity distribution with those expected from two very simple
models of galaxy formation and find that the more dissipative scheme agrees
better with the typical metallicity distribution of ellipticals.
