Scintillated microlensing: measuring cosmic distances with fast radio bursts
Anna Tsai, Dylan L. Jow, Daniel Baker, Ue-Li Pen

TL;DR
This paper introduces a new method to measure cosmic distances using scintillated microlensing of fast radio bursts, which could provide precise estimates of the Hubble constant by overcoming systematic uncertainties in traditional methods.
Contribution
The paper proposes using scintillation in the interstellar medium to resolve microlensed images of FRBs, enabling direct and precise measurement of the Hubble constant with minimal systematic errors.
Findings
Estimated 6% uncertainty on H0 from a single event
Sub-percent uncertainty on H0 possible with 30 events
Method feasible with upcoming FRB telescopes
Abstract
We propose a novel means of directly measuring cosmological distances using scintillated microlensing of fast radio bursts (FRBs). In standard strong lensing measurements of cosmic expansion, the main source of systematic uncertainty lies in modeling the mass profile of galactic halos. Using extra-galactic stellar microlensing to measure the Hubble constant avoids this systematic uncertainty as the lens potential of microlenses depends only on a single parameter: the mass of the lens. FRBs, which may achieve nanosecond precision on lensing time delays, are well-suited to precision measurements of stellar microlensing, for which the time delays are on the order of milliseconds. However, typical angular separations between the microlensed images on the order of microarcseconds make the individual images impossible to spatially resolve with ground-based telescopes. We propose leveraging…
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.
Taxonomy
TopicsRadio Astronomy Observations and Technology · Astronomy and Astrophysical Research · Gamma-ray bursts and supernovae
