Evidence for a deficit of pulsars in the inner Galaxy

I investigate the Galactic radial distribution of pulsars in the light of recently completed high-frequency surveys and demonstrate that, however sensitive, low-frequency surveys are incapable of discriminating between different distributions of pulsars within 3 kpc of the Galactic Centre due to the severe interstellar scattering. In contrast, the high-frequency surveys can penetrate the inner regions of the Galaxy. I show that a simple Gaussian radial distribution would result in the detection of many more pulsars in the inner few kpc than are actually observed. An improved model for the radial distribution is derived, with a peak in the pulsar distribution at 4 kpc from the Galactic Centre. This model is discussed in the context of distributions of related objects.