Constraining Galaxy Halos from the Dispersion and Scattering of Fast Radio Bursts and Pulsars

Fast radio bursts (FRBs) can be scattered by ionized gas in their local environments, host galaxies, intervening galaxies along their lines of sight (LOS), the intergalactic medium, and the Milky Way. The relative contributions of these different media depend on their geometric configuration and the internal properties of the gas. When these relative contributions are well understood, FRB scattering is a powerful probe of density fluctuations along the LOS. The precise scattering measurements for FRB 121102 and FRB 180916 allow us to place an upper limit on the amount of scattering contributed by the Milky Way halo to these FRBs. The scattering time tau proportional to ((F) over tilde x DM2)A tau, where DM is the dispersion measure, (F) over tilde quantifies electron density variations with (F) over tilde = 0 for a smooth medium, and the dimensionless constant A(tau) quantifies the difference between the mean scattering delay and the 1/e scattering time typically measured. A likelihood analysis of the observed scattering and halo DM constraints finds that (F) over tilde is at least an order of magnitude smaller in the halo than in the Galactic disk. The maximum pulse broadening from the halo is t less than or similar to 12 mu s at 1 GHz. We compare our analysis of the Milky Way halo with other galaxy halos by placing limits on the scattering contributions from halos intersecting the LOS to FRB 181112 and FRB 191108. Our results are consistent with halos making negligible or very small contributions to the scattering times of these FRBs.

Automated summary

Fast radio bursts can be scattered by various ionized gas mediums, with different contributions depending on their properties and configurations. Precise measurements of scattering on FRBs can provide insights into density fluctuations. The study suggests that the scattering contribution from the Milky Way halo to FRBs is minimal.