The Luminous Convolution Model for spiral galaxy rotation curves
  The Luminous Convolution Model (LCM) is an empirical formula, based on a
heuristic convolution of Relativistic transformations, which makes it possible
to predict the observed rotation curves of a broad class of spiral galaxies
from luminous matter alone. Since the LCM is independent of distance estimates
or dark matter halo densities, it is the first model of its kind which
constrains luminous matter modeling directly from the observed spectral shifts
of characteristic photon emission/absorption lines. In this paper we present
the LCM solution to a diverse sample of twenty-five (25) galaxies of varying
morphologies and sizes. For the chosen sample, it is shown that the LCM is more
accurate than either Modified Newtonian Dynamics or dark matter models and
returns physically reasonable mass to light ratios and exponential scale
lengths. Unlike either Modified Newtonian Dynamics or dark matter models, the
LCM predicts something which is directly falsifiable through improvements in
our observational capacity, the luminous mass profile. The question, while
interesting, of if the LCM constrains the relation of the baryonic to dark
matter is beyond the scope of the current work.
  The focus of this paper is to show that it is possible to describe a broad
and diverse spectrum of galaxies efficiently with the LCM formula. Moreover,
since the LCM free parameter predicts the ratio of the Milky Way galaxy
baryonic mass density to that of the galaxy emitting the photon, if the Milky
Way mass models can be trusted at face values, we then show that the LCM
becomes a zero parameter model.
  This paper substantially expands the results in arXiv:1309.7370 and
arXiv:1407:7583.
