of inclination angles is estimated to be 142 pc cm$^{-3}$. However the host contribution to the DM from high redshift galaxies can be small due to cosmological time dilation and the corresponding redshifting of frequency [@Zhou]. It also does not account for any bias in FRB locations within galaxies.

The S/Ns, DMs and widths of all three FRBs have been computed using the <span style="font-variant:small-caps;">destroy</span> single pulse search software, <span style="font-variant:small-caps;">psrchive</span> with scripts made publicly available through the FRBCAT repository. The observed widths of all three FRBs are dominated by dispersion smearing as shown in Table \[tab:specs\]. This is due to our small bandwidth and limited number of channels (40 channels). We have now implemented a fine channel mode (320 channels) which will potentially increase our sensitivity and the FRB detection rate by a factor of $\sqrt{8}$. Our total bandwidth of only 31.25 MHz is too narrow to permit a measurement of dispersion index. Single pulses from the Vela pulsar were used to test our sensitivity to the DM index. The DM and the DM index $\delta$ where the dispersive delay is given by, $$\Delta t \propto \Delta\nu^{-\delta}$$ are found to be highly correlated, so that we can place no 