A measurement of Hubble's Constant using Fast Radio Bursts

Abstract

We constrain the Hubble constant H${}_0$ using Fast Radio Burst (FRB) observations from the Australian Square Kilometre Array Pathfinder (ASKAP) and Murriyang (Parkes) radio telescopes. We use the redshift-dispersion measure (`Macquart') relationship, accounting for the intrinsic luminosity function, cosmological gas distribution, population evolution, host galaxy contributions to the dispersion measure (DM${}_{\mathrm{host}}$), and observational biases due to burst duration and telescope beamshape. Using an updated sample of 16 ASKAP FRBs detected by the Commensal Real-time ASKAP Fast Transients (CRAFT) Survey and localised to their host galaxies, and 60 unlocalised FRBs from Parkes and ASKAP, our best-fitting value of H${}_0$ is calculated to be $73_{-8}^{+12}$ km s${}^{-1}$ Mpc${}^{-1}$. Uncertainties in FRB energetics and DM${}_{\mathrm{host}}$ produce larger uncertainties in the inferred value of H${}_0$ compared to previous FRB-based estimates. Using a prior on H${}_0$ covering the 67--74 km s${}^{-1}$ Mpc${}^{-1}$ range, we estimate a median DM${}_{\mathrm{host}}=186_{-48}^{+59}$ km s${}^{-1}$ Mpc${}^{-1}$, exceeding previous estimates. We confirm that the FRB population evolves with redshift similarly to the star-formation rate. We use a Schechter luminosity function to constrain the maximum FRB energy to be ${\log }_{10}{E}_{\max }=41.26_{-0.22}^{+0.27}$ erg assuming a characteristic FRB emission bandwidth of 1 GHz at 1.3 GHz, and the cumulative luminosity index to be $\gamma =-0.95_{-0.15}^{+0.18}$. We demonstrate with a sample of 100 mock FRBs that H${}_0$ can be measured with an uncertainty of $\pm 2.5$ km s${}^{-1}$ Mpc${}^{-1}$, demonstrating the potential for clarifying the Hubble tension with an upgraded ASKAP FRB search system. Last, we explore a range of sample and selection biases that affect FRB analyses.

arXiv comment21 pages, 19 figures, 6 tables, accepted by MNRAS, updated Table 5 and Figure 5

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