Improving pulsar distances by modelling interstellar scattering

We present here a method to study the distribution of electron density fluctuations in pulsar directions as well as to estimate pulsar distances. The method, based on a simple two-component model of the scattering medium discussed by Gwinn, Bartel & Cordes, uses scintillation and proper motion data in addition to the measurements of angular broadening and temporal broadening to solve for the model parameters, namely, the fractional distance to a discrete scatterer and the associated relative scattering strength. We show how this method can be used to estimate pulsar distances reliably, when the location of a discrete scatterer (e.g. an H II region), if any, is known. Considering the specific example of PSR B0736-40, we illustrate how a simple characterization of the Gum nebula region (using the data on the Vela pulsar) is possible and can be used along with the temporal broadening measurements to estimate pulsar distances.