Predicting the Properties of the Remnants of Dissipative Galaxy Mergers

Details Predicting the Properties of the Remnants of Dissipative Galaxy Mergers Predicting the Properties of the Remnants of Dissipative Galaxy Mergers

2007-10-24

arxiv.org/abs/0710.4584v1

Astronomy and Astrophysics

Astrophysics

14 pages, 9 figures. MNRAS accepted

Scientific paper

10.1111/j.1365-2966.2007.12601.x

We construct a physically motivated model for predicting the properties of the remnants of gaseous galaxy mergers, given the properties of the progenitors and the orbit. The model is calibrated using a large suite of SPH merger simulations. It implements generalized energy conservation while accounting for dissipative energy losses and star formation. The dissipative effects are evaluated from the initial gas fractions and from the orbital parameters via an "impulse" parameter, which characterizes the strength of the encounter. Given the progenitor properties, the model predicts the remnant stellar mass, half-mass radius, and velocity dispersion to an accuracy of 25%. The model is valid for both major and minor mergers. We provide an explicit recipe for semi-analytic models of galaxy formation.

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