SIMBAD references

We derive circular velocity curves (CVCs) from stellar dynamical models for ∼6000 nearby galaxies in the final data release of the Sloan Digital Sky Survey-IV MaNGA survey with integral-field spectroscopy, exploring connections between the inner gravitational potential (traced by CVC amplitude/shape) and galaxy properties. The maximum circular velocity (${V}_{{\rm{circ}}}^{{\rm{\max }}}$) and circular velocity at the half-light radius (${V}_{{\rm{circ}}}({R}_{{\rm{e}}}^{{\rm{maj}}})$) both scale linearly with the stellar second velocity moment ${\sigma }_{{\rm{e}}}^{2}\equiv \langle {V}^{2}+{\sigma }^{2}\rangle $ within the half-light isophote, following ${V}_{{\rm{circ}}}^{{\rm{\max }}}\approx 1.72{\sigma }_{{\rm{e}}}$ (7% error) and ${V}_{{\rm{circ}}}({R}_{{\rm{e}}}^{{\rm{maj}}})\approx 1.62{\sigma }_{{\rm{e}}}$ (7% error). CVC shapes (rising, flat, declining) correlate strongly with structural and stellar population properties: declining curves dominate in massive, early-type, bulge-dominated galaxies with old, metal-rich stars and early quenching, while rising CVCs prevail in disk-dominated systems with younger stellar populations and ongoing star formation. Using a unified bulge-disk-halo model, we predict CVC shapes with minimal bias, identifying three governing parameters: bulge-to-total mass ratio (B/T), dark matter fraction within R_e, and bulge Sérsic index. The distribution of CVC shapes across the mass-size plane reflects evolutionary pathways driven by (i) in situ star formation (spurring bulge growth) and (ii) dry mergers. This establishes CVC morphology as a diagnostic for galaxy evolution, linking dynamical signatures to structural and stellar population histories.