Detection of the Mass-Dependent Dual-Type Transition of Galaxy Spins in
  IllustrisTNG Simulations
  A numerical detection of the mass-dependent spin transition of the galaxies
is presented. Analyzing a sample of the galaxies with stellar masses in the
range of $10^{9}< (M_{\star}/M_{\odot})\le 10^{11}$ from the IllustrisTNG300-1
simulations, we explore the alignment tendency between the galaxy baryon spins
and the three eigenvectors of the linearly reconstructed tidal field as a
function of $M_{\star}$ and its evolution in the redshift range of $0\le z \le
1.5$. Detecting a significant signal of the occurrence of the mass-dependent
transition of the galaxy spins, we show that the centrals differ from the
satellites in their spin transition type. As $M_{\star}$ increases beyond a
certain threshold mass, the preferred directions of the central galaxy spins
transit from the minor to the intermediate tidal eigenvectors (type two) at
$z=0.5$ and $1$, while those of the satellites transit from the minor to the
major tidal eigenvectors (type one) at $z=1$ and $1.5$. It is also shown that
the mass range and type of the spin transition depend on the galaxy morphology,
degree of the alignments between the baryon and total spin vectors as well as
on the environmental density. Meanwhile, the stellar spins of the galaxies are
found to yield a weak signal of the T1 transitions at $z=0$, whose strength and
trend depend on the degree of the alignments between the stellar and baryon
spins. The possible mechanisms responsible for the T1 and T2 spin transitions
are discussed.
