  Integral field spectroscopy has been obtained for the nuclear regions of 3
large, well-studied, early-type galaxies. From these spectra we have obtained
line strength maps for about 20 absorption lines, mostly belonging to the Lick
system. An extensive comparison with multi-lenslet spectroscopy shows that
accurate kinematic maps can be obtained, and also reproducible line strength
maps. Comparison with long-slit spectroscopy also produces good agreement. We
show that Mg is enhanced with respect to Fe in the inner disk of one of the
three galaxies studied, the Sombrero. [Mg/Fe] there is larger than in the rest
of the bulge. The large values of Mg/Fe in the central disk are consistent with
the centres of other early-type galaxies, and not with large disks, like the
disk of our Galaxy, where [Mg/Fe] is approximately 0. We confirm with this
observation a recent result of Worthey (1998) that Mg/Fe is determined by the
central kinetic energy, or escape velocity, of the stars, only, and not by the
formation time scale of the stars. A stellar population analysis using the
models of Vazdekis et al. (1996) shows that our observed H gamma agrees well
with what is predicted based on the other lines. Using the line strength of the
Ca II IR triplet as an indicator of the abundance of Ca, we find that Ca
follows Fe, and not Mg, in these galaxies. This is peculiar, given the fact
that Ca is an alpha-element. Finally, by combining the results of this paper
with those of Vazdekis et al. (1997) we find that the line strength gradients
in the three galaxies are primarily caused by variations in metallicity.
