Internal mass distributions and orbital structures of SAMI passive galaxies

Galaxy mergers play an important role in how galaxies evolve over time, however extragalactic astronomers do not yet completely understand the process by which those mergers happen. The merger history of a galaxy is thought to be one of the major factors that determines the internal kinematic structures of galaxies, with galaxies having undergone more mergers predicted to show different properties. Therefore, we expect that the internal kinematic structures of passive galaxies could show different characteristics depending on their merging history. We apply orbitsuperposition Schwarzschild models to passive galaxies in the SAMI Galaxy Survey, in order to reconstruct their internal kinematic structure and mass distribution. We find intriguing signs of different orbital structures in galaxies with different kinematic signatures. The future larger surveys that will be enabled by new MOS and IFU facilities will be needed to further explore these intriguing signs in a statistical sample.