2024MNRAS.534.2314H

We study the galactic spiral arm pitch angle dependence with wavelength as predicted by the density wave theory. A sample of 10 barred and unbarred spiral galaxies with two distinct, well-defined arms is used for the measurements. The data sample consists of galaxies with inner arms and galaxies with both inner and outer arms. We use six wavebands, namely 3.6 $\mu$m, 8.0 $\mu$m, B band, H $\alpha$, H I, and CO for the image analysis. The pitch angles are visually measured with the PYTHON-OL SCRIPT and more precise measurements are obtained using SPIRALITY. We find a 1:1 correlation between pitch angle measurements in the 3.6 and 8.0 $\mu$m bands. We predict supermassive black hole (SMBH) masses for 3.6 $\mu$m waveband pitch angles using a standard scaling relation. We find that the black hole mass of a galaxy with both inner and outer arms is determined by the average pitch angle of the inner arms. Using only galaxies with inner arms, we find an SMBH mass-pitch angle relation of $\log (M_{\rm BH}/\mathrm{M}_\odot)=(7.11 \pm 0.33)+(0.003 \pm 0.017){\textit P}$. Using only galaxies with both inner and outer arms, we find an SMBH mass-pitch angle relation of $\log (M_{\rm BH}/\mathrm{M}_\odot)=(7.56 \pm 0.28)-(0.038 \pm 0.013){\textit P}$.