### A study of stellar orbit fractions: simulated IllustrisTNG galaxies compared to CALIFA observations

by
Xu, Dandan; Zhu, Ling; Grand, Robert; Springel, Volker; Mao, Shude; van de Ven, Glenn; Lu, Shengdong; Wang, Yougang; Pillepich, Annalisa; Genel, Shy; Nelson, Dylan; Rodriguez-Gomez, Vicente; Pakmor, Rüdiger; Weinberger, Rainer; Marinacci, Federico; Vogelsberger, Mark; Torrey, Paul; Naiman, Jill; Hernquist, Lars

abstract
Motivated by the recently discovered kinematic `Hubble sequence’ shown by the stellar orbit-circularity distribution of 260 CALIFA galaxies, we make use of a comparable galaxy sample at z = 0 with a stellar mass range of M_{*}/M_{\odot }\in [10^{9.7}, 10^{11.4}] selected from the IllustrisTNG simulation and study their stellar orbit compositions in relation to a number of other fundamental galaxy properties. We find that the TNG100 simulation broadly reproduces the observed fractions of different orbital components and their stellar mass dependences. In particular, the mean mass dependences of the luminosity fractions for the kinematically warm and hot orbits are well reproduced within model uncertainties of the observed galaxies. The simulation also largely reproduces the observed peak and trough features at M_{*}≈ 1{-}2× 10^{10} M_{\odot } in the mean distributions of the cold- and hot-orbit fractions, respectively, indicating fewer cooler orbits and more hotter orbits in both more- and less-massive galaxies beyond such a mass range. Several marginal disagreements are seen between the simulation and observations: the average cold-orbit (counter-rotating) fractions of the simulated galaxies below (above) M_{*}≈ 6× 10^{10} M_{\odot } are systematically higher than the observational data by ≲ 10{{ per cent}} (absolute orbital fraction); the simulation also seems to produce more scatter for the cold-orbit fraction and less so for the non-cold orbits at any given galaxy mass. Possible causes that stem from the adopted heating mechanisms are discussed.

published in
Monthly Notices of the Royal Astronomical Society, Volume 489, Issue 1, p.842-854, October 2019