Krajnovic used the SAURON observations of NGC2974 to construct an axisymmetric stellar dynamical model of the galaxy. The best fitting model gave M/L=3.5 and inclination of 60 degrees. The gas is distributed in a disk structure defined by the potential from the best fitting stellar model. The difference between the streaming velocity and circular velocity is due to the asymmetric drift (given by Jeans equations). The gas model was in a good agreement with the observations outside 3.
Cappellari, assisted by McDermid and Krajnovic, worked on the systematic dynamical modeling of SAURON early-type galaxies using the axisymmetric Schwarzschild numerical orbit-superposition technique. A new major counterrotating disk was discovered in NGC 4473. For most of the other modeled galaxies, at least two kinematically-decoupled components, a bulge-like one and a flatter faster-rotating one, were required to explain the integral-field kinematics. Interestingly the more disk-like components also showed up clearly in two-dimensional maps of the metallicity of the stellar population, indicating that gas was involved in the formation of the objects.
Verolme, van de Ven, Cappellari, Emsellem (CRAL, Lyon) and de Zeeuw further developed the Schwarzschild software for triaxial galaxies. It enables the construction of realistic triaxial dynamical models, which fit the observed surface brightness as well as two-dimensional kinematical measurements of elliptical galaxies. Initial application to observations of NGC4365, taken with the integral-field spectrographs SAURON and OASIS, showed that the method was able to reproduce the kinematically decoupled core and other observational features within the errors. Currently the method is being refined, such that besides the best-fitting parameters (the mass-to-light ratio and the black hole mass), it also provides the internal orbital structure of elliptical galaxies. The method is tested against theoretical Abel models, for which the distribution function is known analytically, but allows enough freedom to incorporate many of the observed triaxial features. Once all this is done, this extended Schwarzschild method will allow the detailed study of many of the large elliptical galaxies in the SAURON sample that show significant signatures of non-axisymmetry.