Using the latest sample of 48 spiral galaxies having a directly measured supermassive black hole mass, , we determine how the maximum disk rotational velocity, (and the implied dark matter halo mass, ), correlates with the (i) , (ii) central velocity dispersion, , and (iii) spiral-arm pitch angle, . We find that , significantly steeper than previously reported, and with a root mean square scatter ( dex) similar to that about the - relation for spiral galaxies - in stark disagreement with claims that does not correlate with disks. Moreover, this - relation is consistent with the unification of the Tully-Fisher relation (involving the total stellar mass, ) and the steep relation observed in spiral galaxies. We also find that $\sigma_0\propto v_{max}^{1.55\pm0.25}\propto M_{DM}^{0.63\pm0.11}$, consistent with past studies connecting stellar bulges (with $\sigma_0\gtrsim100,{\rm km,s}^{-1}v_{max}/\sigma_0$ ratio. Finally, we report that , providing a novel formulation between the geometry (i.e., the logarithmic spiral-arm pitch angle) and kinematics of spiral galaxy disks. While the - relation may facilitate distance estimations to face-on spiral galaxies through the Tully-Fisher relation and using as a proxy for , the - relation provides a path for determining dark matter halo masses from imaging data alone. Furthermore, based on a spiral galaxy sample size that is double the size used previously, the self-consistent relations presented here provide dramatically revised constraints for theory and simulations.

生成讲解博客的中文版本

生成AI智能校验的中文版本