Galaxy morphology in the ΛCDM cosmology

Abstract

We investigate the origins of galaxy morphology (defined by bulge-to-total K-band luminosity) in the LambdaCDM cosmology using two galaxy formation models ,based on the Millennium simulation, by Bower et al. (the Durham model) and De Lucia & Blaizot (the MPA model). There are many similarities, but also fundamental disagreements in the predictions of the two models for galaxy morphology. For example, taking into account uncertainties in the available observational data, both produce a realistic morphological mix today, but its evolution is very different. A main cause of this and other differences is the treatment of disk instabilities which play a more prominent role in the Durham model. Our analysis confirms previous theoretical predictions that elliptical galaxies form most of their stars before the bulk of the galaxy is assembled. Spirals tend to have later `assembly' times as a consequence of in-situ star formation. With the exception of the brightest ellipticals (stellar mass > 2.5e11 M_sun/h), we find that major mergers are not the primary mechanism by which most spheroids (ellipticals and spiral bulges) assemble their mass. In fact, the majority of ellipticals (and the overwhelming majority of spirals) never experience a major merger (above the resolution limit of our simulation.) Most ellipticals and spiral bulges acquire their stellar mass through minor mergers or disk instabilities. These conclusions are common to both models. The rotation properties of spheroids may help to constrain the importance of disk instabilities in these models.