The Structure of Simulated Galaxy Remnants Compared to Observations

Gregory Novak, University of California, Santa Cruz

We report on the 3D and projected spatial and kinematic structure of the remnants resulting from a comprehensive suite of more than 100 spiral galaxy hydrodynamic merger simulations (Cox 2004, Cox et al. 2005). For each remnant, we compute the shape and 3D orientation as a function of radius and time, velocity anisotropy as a function of radius, and map the projected kinematics including mean velocity, velocity dispersion, and Gauss-Hermite moments H3 and H4 for many different viewing angles. We consider both the statistical properties of the set of merger remnants and the properties of individual remnants. Most of the remnants are close to isothermal, oblate, show little figure rotation, and show little misalignment between the shapes at different radii. Qualitatively, they compare favorably with Integral Field Unit data from the SAURON survey (Emsellem et al. 2004). However, some of the remnants are triaxial or prolate, show figure rotation, and have shape orientations which are a function of radius.

Abstract Author(s): G. S. Novak, T. J. Cox, J. R. Primack, S. M. Faber