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We recently developed an automated method, auto-GMM to decompose simulatedgalaxies. It extracts kinematic structures in an accurate, efficient, andunsupervised way. We use auto-GMM to study the stellar kinematic structures ofdisk galaxies from the TNG100 run of IllustrisTNG. We identify four to fivestructures that are commonly present among the diverse galaxy population.Structures having strong to moderate rotation are defined as cold and warmdisks, respectively. Spheroidal structures dominated by random motions areclassified as bulges or stellar halos, depending on how tightly bound they are.Disky bulges are structures that have moderate rotation but compact morphology.Across all disky galaxies and accounting for the stellar mass within 3half-mass radii, the kinematic spheroidal structures, obtained by summing upstars of bulges and halos, contribute ~45% of the total stellar mass, while thedisky structures constitute 55%. This study also provides important insightsabout the relationship between kinematically and morphologically derivedgalactic structures. Comparing the morphology of kinematic structures with thatof traditional bulge+disk decomposition, we conclude: (1) the morphologicallydecomposed bulges are composite structures comprised of a slowly rotatingbulge, an inner halo, and a disky bulge; (2) kinematically disky bulges, akinto what are commonly called pseudo bulges in observations, are compactdisk-like components that have rotation similar to warm disks; (3) haloscontribute almost 30% of the surface density of the outer part of morphologicaldisks when viewed face-on; and (4) both cold and warm disks are often truncatedin central regions.

Kinematic decomposition of IllustrisTNG disk galaxies: morphology and relation with morphological structures