Radial Distribution of the Mass-to-Luminosity Ratio in Spiral Galaxies and Massive Dark Cores

We derive radial profiles of the surface-mass-density for 19 spiral galaxies directly from their high-resolution rotation curves. Using the corresponding luminosity profiles, we obtain the radial distribution of the mass-to-luminosity ratios ($M/L$) from the inner bulge ($\sim$ a few 100 pc) to the outer disk ($\geq$ 2-10 kpc) for 11 galaxies (with inclination < $70^{\circ}$ in order to reduce the influence of the interstellar extinction. The $M/L$s in the bulges of two galaxies with sufficient resolution, NGC 4527 and NGC 6946, are found to increase steeply toward the center at radii $\sim$ 100-500 pc at rates of 15$\pm$3 and 7$\pm$2 times per kpc, respectively. Some other galaxies with fairly high resolution also show signs of an increase toward the center. Such an increase may indicate the existence of a new component, a ``massive dark core'', which may be an object linking the bulge and a central black hole. Based on radial variations of the $M/L$, we further discuss the variation of the dark-mass fraction in spiral galaxies.