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We investigate how the stellar rotational support changes as a function of spatially resolved stellar population age (Dₙ4000) and relative central stellar surface density (₁) for MaNGA isolated/central disk galaxies. We find that the galaxy rotational support ₑ䂰 varies smoothly as a function of ₁ and Dₙ4000. Dₙ4000 vs. ₁ follows a "J-shape", with ₑ䂰 contributing to the scatters. In this "J-shaped" pattern rotational support increases with central Dₙ4000 when ₁ is low but decreases with ₁ when ₁ is high. Restricting attention to low- ₁ (i. e, large-radius) galaxies, we suggest that the trend of increasing rotational support with Dₙ4000 for these objects is produced by a mix of two different processes, a primary trend characterized by growth in ₑ䂰 along with mass through gas accretion, on top of which disturbance episodes are overlaid, which reduce rotational support and trigger increased star formation. An additional finding is that star forming galaxies with low ₁ have relatively larger radii than galaxies with higher ₁ at fixed stellar mass. Assuming that these relative radii rankings are preserved while galaxies are star forming then implies clear evolutionary paths in central Dₙ4000 vs. ₁. The paper closes with comments on the implications that these paths have for the evolution of pseudo-bulges vs. classical-bulges. The utility of using Dₙ4000- ₁ to study ₑ䂰 reinforces the notion that galaxy kinematics correlate both with structure and with stellar-population state, and indicates the importance of a multi-dimensional description for understanding bulge and galaxy evolution.
Wang et al. (Mon,) studied this question.