  Modeling the luminous mass components of spiral galaxies in standard gravity
poses a challenge due to the missing mass problem. However, with the addition
of cold dark matter, the missing mass problem can be circumvented at the cost
of additional free parameters to the theory. The Luminous Convolution Model
(LCM) reconsiders how we interpret rotation curve data, such that
Doppler-shifted spectra measurements can constrain luminous mass discovery. For
a sample of 25 galaxies of varying morphologies and sizes, we demonstrate an
ansatz for relative galaxy curvatures that can explain the missing mass. We
solve for the LCM free parameter, which we report as a ratio of radial
densities of the emitter, to receiver galaxy baryonic mass, to an exponent of
$1.63$. Here, we show that this exponent is sensitive to which Milky Way
luminous mass model one chooses. We then make a first prediction regarding the
Milky Way mass profile in the inner one kpc.
  Thus, with a bound on the LCM free parameter, we pave the way for future
work, where the LCM will tested as a zero-parameter model to predict luminous
mass from rotation curve data.
