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Dynamical models are crucial for uncovering the internal dynamics ofgalaxies, however, most of the results to date assume axisymmetry, which is notrepresentative for a significant fraction of massive galaxies. Here, we buildtriaxial Schwarschild orbit-superposition models of galaxies taken from theSAMI Galaxy Survey, in order to reconstruct their inner orbital structure andmass distribution. The sample consists of 161 passive galaxies with totalstellar masses in the range $10^{9.5}$ to $10^{12} M_{\odot}$. We find that thechanges in internal structures within 1$R_{\rm e}$ are correlated with thetotal stellar mass of the individual galaxies. The majority of the galaxies inthe sample ($73\% \pm 3\%$) are oblate, while $19\% \pm 3\%$ are mildlytriaxial and $8\% \pm 2\%$ have triaxial/prolate shape. Galaxies with $\logM_{\star}/M_{\odot} > 10.50$ are more likely to be non-oblate. We find a meandark matter fraction of $f_{\rm{DM}} = 0.28 \pm 0.20$, within 1$R_{\rm e}$.Galaxies with higher intrinsic ellipticity (flatter) are found to have morenegative velocity anisotropy $\beta_r$ (tangential anisotropy). $\beta_r$ alsoshows an anti-correlation with the edge-on spin parameter \lam, so that$\beta_r$ decreases with increasing \lam. We see evidence of an increasingfraction of hot orbits with increasing stellar mass, while warm and cold orbitsshow a decreasing trend. We also find that galaxies with different ($V/\sigma$- $h_3$) kinematic signatures have distinct combinations of orbits. Theseresults are in agreement with a formation scenario in which slow- andfast-rotating galaxies form through two main channels.

astrophysical journal/the astrophysical journal

The SAMI Galaxy Survey: The internal orbital structure and mass  distribution of passive galaxies from triaxial orbit-superposition  Schwarzschild models