Estimating the Contribution of Foreground Halos to the FRB 180924 Dispersion Measure

Fast radio burst (FRB) dispersion measures (DMs) record the presence of ionized baryons that are otherwise invisible to other techniques enabling resolution of the matter distribution in the cosmic web. In this work, we aim to estimate the contribution to FRB 180924 DM from foreground galactic halos. Localized by ASKAP to a massive galaxy, this sightline is notable for an estimated cosmic web contribution to the DM (DMcosmic =220 pc cm(-3)), which is less than the average value at the host redshift (z = 0.3216) estimated from the Macquart relation (280 pc cm(-3)). In the favored models of the cosmic web, this suggests few intersections with foreground halos at small impact parameters (less than or similar to 100 kpc). To test this hypothesis, we carried out spectroscopic observations of the field galaxies within similar to 1 ' of the sightline with VLT/MUSE and Keck/LRIS. Furthermore, we developed a probabilistic methodology that leverages photometric redshifts derived from wide-field DES and WISE imaging. We conclude that there is no galactic halo that closely intersects the sightline and also that the net DM contribution from halos DMhalos < 45 pc cm(-3) (95% c.l.). This value is lower than the DMhalos estimated from an average sightline (121 pc cm(-3)) using the Planck ?CDM model and the Aemulus halo mass function and reasonably explains its low DMcosmic value. We conclude that FRB 180924 represents the predicted majority of sightlines in the universe with no proximate foreground galactic halos. Our framework lays the foundation for a comprehensive analysis of FRB fields in the near future.

Automated summary

The study used spectroscopic observations and probabilistic methods to determine that there were no galactic halos closely intersecting the sightline, representing the majority of sightlines in the universe for FRB 180924. The results showed that the net DM contribution from foreground halos was lower, in line with its low DMcosmic value.