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A numerical detection of the mass-dependent spin transition of the galaxiesis presented. Analyzing a sample of the galaxies with stellar masses in therange of $10^{9}< (M_{\star}/M_{\odot})\le 10^{11}$ from the IllustrisTNG300-1simulations, we explore the alignment tendency between the galaxy baryon spinsand the three eigenvectors of the linearly reconstructed tidal field as afunction of $M_{\star}$ and its evolution in the redshift range of $0\le z \le1.5$. Detecting a significant signal of the occurrence of the mass-dependenttransition of the galaxy spins, we show that the centrals differ from thesatellites in their spin transition type. As $M_{\star}$ increases beyond acertain threshold mass, the preferred directions of the central galaxy spinstransit 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 themajor tidal eigenvectors (type one) at $z=1$ and $1.5$. It is also shown thatthe 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 ason the environmental density. Meanwhile, the stellar spins of the galaxies arefound to yield a weak signal of the T1 transitions at $z=0$, whose strength andtrend depend on the degree of the alignments between the stellar and baryonspins. The possible mechanisms responsible for the T1 and T2 spin transitionsare discussed.

Detection of the Mass-Dependent Dual-Type Transition of Galaxy Spins in IllustrisTNG Simulations