In this colloquium I will talk about new methods that we are developing to determine the dark matter distributions in disk galaxies. One of these methods focusses on the relationship between spiral arm pitch angle (the measure of how tighly wound spiral structure is) and rotation curve shear (a dynamical measurement reflecting the slope of the rotation curve). I will show some examples as to how this can be used to place constraints upon dark matter density profiles. I will also discuss two major projects, the Arkansas Galaxy Evolution Survey (AGES) and the Carnegie-Irvine Nearby Galaxies Survey (CINGS) and how these projects can be used to determine dark matter distributions, and the possibility that dark matter central densities play a role in supermassive black hole masses.