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Structure, Formation and Ages of Elliptical Galaxies

The structural properties of elliptical galaxies are consistent with their formation in a merging hierarchy. In this picture, the role of gaseous processes and dissipation decreased with increasing mass creating preferentially rotationally flattend disky ellipticals (and S0s) at lower luminosities and boxy, anisotropic ellipticals (often with peculiar kinematics) at higher luminosities. However, gas and dissipation processes must have been important even in the formation of the most luminous ellipticals. They played key roles in determining the phase space structure of Es and possibly ensured a tight fundamental plane. The bulk of the stars in the majority of luminous cluster ellipticals formed at redshifts above two, likely above three. This follows from their homogenous colors and line strengths and their essentially passive evolution with redshift. Low luminosity ellipticals (and probably field ellipticals) may have had extended star formation histories, possibly associated with the presence of disks. The star-formation time-scales can presumably be constrained on the basis of abundance ratios and seem to be inversely related to galaxy mass. Massive ellipticals are likely to have formed the bulk of their stars within one Gigayear.