Collision-induced Galaxy Formation

We present a semianalytical model in which galaxy collisions and strong tidal interactions, both in the field and during the collapse phase of groups and clusters, help determine galaxy morphology. From a semianalytical analysis based on simulation results of tidal collisions (Aguilar & White), we propose simple rules for energy exchanges during collisions that allow one to discriminate between different Hubble types: efficient collisions result in the disruption of disks and substantial star formation, leading to the formation of elliptical galaxies; inefficient collisions allow a large gas reservoir to survive and form disks. Assuming that galaxy formation proceeds in an Ω₀ = 1 cold dark matter universe, the model both reproduces a number of observations and makes predictions, among which are the redshifts of formation of the different Hubble types in the field. When the model is normalized to the present-day abundance of X-ray clusters, the amount of energy exchange needed to produce elliptical galaxies in the field implies that they formed at z ≳ 2.5 while spiral galaxies formed at z ≲ 1.5. The model also offers a natural explanation for biasing between the various morphological types. We find that the present-day morphology-density relation in the field is well reproduced under the collision hypothesis. Finally, predictions of the evolution of the various galaxy populations with redshift are made, in the field as well as in clusters.