The Light Side of Dark Matter:Luminous Convolution Model

We present a new, heuristic, two-parameter model for predicting the rotation curves of disc galaxies, the Luminous Convolution Model. The model is tested on (22) randomly chosen galaxies, represented in (33) data sets, and compared  to both the NFW Model and MOND fits when available.  The  Luminous Convolution  model[LCM] is derived from an exact solution to the covariant exterior Kerr wave equation; where small changes in the photon's frequencies result from the curved space time.  These frequencies  are used in the same sense as those in the gravitational redshift, as the fundamental observable.  These frequency shifts are convolved into a functional model to predict galaxy rotation curves, which do differ from the linearized Kerr theory's expectations.  The LCM function is parametrized with only the diffuse, luminous stellar and gaseous masses reported in each galactic data set.   Our first parameter (Β) scales the luminous mass to light ratios  by a constant. Our second parameter relates the LCM function to the Dark Matter component. We find that this parameter  (Ã) demonstrates interesting structure.  The LCM is very successful across a wide range of spiral galaxies for predicting observed rotation curves. We do not propose that the LCM is fundamental, but a working heuristic model.