  We use numerical models which include star formation to analyze the mass
profiles of remnants formed by mergers of disk galaxies. During a merger,
dissipation in gas and ensuing star formation leave behind a dense stellar core
in the remnant. Rather than joining smoothly onto a de Vaucouleurs profile, the
starburst population leads to a sharp break in the surface density profile at a
few percent the effective radius. While our results are preliminary, the lack
of such signatures in most elliptical galaxies suggests that mergers of
gas-rich disk galaxies may not have contributed greatly to the population of
present-day ellipticals.
