  We consider a simulated population of isolated Galactic neutron stars. The
rotational frequency of each neutron star evolves through a combination of
electromagnetic and gravitational wave emission. The magnetic field strength
dictates the dipolar emission, and the ellipticity (a measure of a neutron
star's deformation) dictates the gravitational wave emission. Through both
analytic and numerical means, we assess the detectability of the Galactic
neutron star population and bound the magnetic field strength and ellipticity
parameter space of Galactic neutron stars with or without a direct
gravitational wave detection. While our simulated population is primitive, this
work establishes a framework by which future efforts can be conducted.
