This paper presents a detailed analysis of the relationship between black hole (BH) mass, bulge mass, and near-infrared (NIR) luminosity in galaxies. The authors use accurate two-dimensional image analysis to measure NIR bulge structural parameters for galaxies with well-determined BH masses. They find that NIR bulge luminosities and BH masses are tightly correlated, with a scatter similar to that between BH mass and effective stellar velocity dispersion ($\sigma_e$). The intrinsic scatter in $\log M_{\text{BH}}$ is approximately 0.3 dex. By combining bulge effective radii ($R_e$) with $\sigma_e$, they establish a tight linear correlation between $M_{\text{BH}}$ and the virial bulge mass, with a scatter of about 0.25 dex. The analysis also reveals that $M_{\text{BH}}$ depends on both $\sigma_e$ and $R_e$, and that both variables are necessary to drive the correlations between $M_{\text{BH}}$ and other bulge properties. The study suggests that the correlation between BH mass and bulge mass is more robust and less affected by extinction compared to the optical correlations.This paper presents a detailed analysis of the relationship between black hole (BH) mass, bulge mass, and near-infrared (NIR) luminosity in galaxies. The authors use accurate two-dimensional image analysis to measure NIR bulge structural parameters for galaxies with well-determined BH masses. They find that NIR bulge luminosities and BH masses are tightly correlated, with a scatter similar to that between BH mass and effective stellar velocity dispersion ($\sigma_e$). The intrinsic scatter in $\log M_{\text{BH}}$ is approximately 0.3 dex. By combining bulge effective radii ($R_e$) with $\sigma_e$, they establish a tight linear correlation between $M_{\text{BH}}$ and the virial bulge mass, with a scatter of about 0.25 dex. The analysis also reveals that $M_{\text{BH}}$ depends on both $\sigma_e$ and $R_e$, and that both variables are necessary to drive the correlations between $M_{\text{BH}}$ and other bulge properties. The study suggests that the correlation between BH mass and bulge mass is more robust and less affected by extinction compared to the optical correlations.