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The (supermassive black hole mass, $M_\text{BH}$)-(bulge stellar mass,$M_{\rm*,sph}$) relation is, obviously, derived using two quantities. Weendeavor to provide accurate values for the latter via detailed multicomponentgalaxy decompositions for the current full sample of 43 spiral galaxies havingdirectly measured $M_\text{BH}$ values; 35 of these galaxies have been allegedto contain pseudobulges, 21 have water maser measurements, and three appearbulgeless. This more than doubles the previous sample size of spiral galaxieswith a finessed image analysis. We have analyzed near-infrared images,accounting for not only the bulge, disk (exponential, truncated, or inclined),and bar but also for spiral arms and rings and additional central components(active galactic nuclei (AGNs), etc.). A symmetric Bayesian analysis finds$\log\left(M_\text{BH}/M_{\odot}\right)=\left(2.44_{-0.31}^{+0.35}\right)\log\left\{M_{\rm*,sph}/[\upsilon(1.15\times10^{10}\,M_{\odot})]\right\}+(7.24\pm0.12)$,with $\upsilon$ a stellar mass-to-light ratio term. The level of scatter equalsthat about the $M_{\rm BH}$-$\sigma_*$ relation. The nonlinear slope rules outthe idea that many mergers, coupled with the central limit theorem, producedthis scaling relation, and it corroborates previous observational studies andsimulations, which have reported a near-quadratic slope at the low-mass end ofthe $M_\text{BH}$-$M_{\rm*,sph}$ diagram. Furthermore, bulges with AGNs followthis relation; they are not offset by an order of magnitude, and models thathave invoked AGN feedback to establish a linear $M_{\rm BH}$-$M_{\rm*,sph}$relation need revisiting. We additionally present an updated$M_\text{BH}$-(S\'ersic index, $n_\text{sph}$) relation for spiral galaxybulges with a comparable level of scatter and a new $M_{\rm*,sph}$-(spiral-armpitch angle, $\phi$) relation.

Black Hole Mass Scaling Relations for Spiral Galaxies. I. $M_{\rm BH}$-$M_{\rm *,sph}$