  In order to understand the formation process of elliptical galaxies which are
not rotationally supported, we have carried out numerical simulations of the
galaxy formation from the density perturbation with a rotation corresponding to
a small spin parameter. The three-dimensional TREE N-Body/SPH simulation code
used in this paper includes the dark matter and gas dynamics, radiative
cooling, star formation, supernova feedback, and metal enrichment. The initial
condition is a slowly rotating, top-hat over-dense sphere on which the
perturbations expected in a cold dark matter (CDM) universe are superposed. By
means of the stellar population synthesis, we calculated the surface brightness
profile, the metallicity distribution, and the photometric properties of the
end-product, and found that these properties quantitatively agree with the
observed properties of bright elliptical galaxies. Thus, we conclude that, in a
CDM universe, the proto-galaxy which has a spin-parameter as small as 0.02
evolves into an elliptical galaxy.
