Constraining Galaxy Halos from the Dispersion and Scattering of Fast Radio Bursts and Pulsars
Stella Koch Ocker, J. M. Cordes, Shami Chatterjee
Abstract
Abstract 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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>τ</mml:mi> <mml:mo>∝</mml:mo> <mml:mo stretchy="false">(</mml:mo> <mml:mover accent="true"> <mml:mrow> <mml:mi>F</mml:mi> </mml:mrow> <mml:mrow> <mml:mo stretchy="true">˜</mml:mo> </mml:mrow> </mml:mover> <mml:mo>×</mml:mo> <mml:msup> <mml:mrow> <mml:mi>DM</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> </mml:msup> <mml:mo stretchy="false">)</mml:mo> <mml:msub> <mml:mrow> <mml:mi>A</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>τ</mml:mi> </mml:mrow> </mml:msub> </mml:math> , where DM is the dispersion measure, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover accent="true"> <mml:mrow> <mml:mi>F</mml:mi> </mml:mrow> <mml:mrow> <mml:mo stretchy="true">˜</mml:mo> </mml:mrow> </mml:mover> </mml:math> quantifies electron density variations with <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover accent="true"> <mml:mrow> <mml:mi>F</mml:mi> </mml:mrow> <mml:mrow> <mml:mo stretchy="true">˜</mml:mo> </mml:mrow> </mml:mover> <mml:mo>=</mml:mo> <mml:mn>0</mml:mn> </mml:math> for a smooth medium, and the dimensionless constant A τ 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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover accent="true"> <mml:mrow> <mml:mi>F</mml:mi> </mml:mrow> <mml:mrow> <mml:mo stretchy="true">˜</mml:mo> </mml:mrow> </mml:mover> </mml:math> is at least an order of magnitude smaller in the halo than in the Galactic disk. The maximum pulse broadening from the halo is τ ≲ 12 μ 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.