A $\tau-$DM relation for FRB hosts?

TL;DR

This study evaluates the potential of using scattering time ($ au$) and dispersion measure (DM) correlations in FRB hosts to estimate redshifts, concluding that observational limitations hinder this approach despite theoretical expectations.

Contribution

The paper demonstrates through simulations that the $ au - $DM relation cannot be reliably inferred from FRB observations due to large variances and biases, challenging previous assumptions.

Findings

The $ au - $DM relation is not observable in current FRB data.

Large variances and observational biases obscure the correlation.

The lack of observed correlation aligns with the study's predictions.

Abstract

It has been proposed that measurements of scattering times ($\tau$) from fast radio bursts (FRB) may be used to infer the FRB host dispersion measure (DM) and its redshift. This approach relies on the existence of a correlation between $\tau$ and DM within FRB hosts such as that observed for Galactic pulsars. We assess the measurability of a $\tau - $DM$_{\rm host}$ relation through simulated observations of FRBs within the ASKAP/CRAFT survey, taking into account instrumental effects. We show that even when the FRB hosts intrinsically follow the $\tau - $DM relation measured for pulsars, this correlation cannot be inferred from FRB observations; this limitation arises mostly from the large variance around the average cosmic DM value given by the Macquart relation, the variance within the $\tau - $DM relation itself, and observational biases against large $\tau$ values. We argue that theoretical relations have little utility as priors on redshift, e.g., for purposes of galaxy identification, and that the recent lack of an observed correlation between scattering and DM in the ASKAP/CRAFT survey is not unexpected, even if our understanding of a $\tau - $DM$_{\rm host}$ relation is correct.