Characterizing fast radio bursts through statistical cross-correlations
Name
PhysRevD.102.023528.pdf
Description
Published version
Size
1.25 MB
Format
Unknown
Checksum (MD5)
36d5f8583d6b7d38efa2c40604e8dfae
Author(s)
Rafiei-Ravandi, Masoud
Smith, Kendrick M
Masui, Kiyoshi
Date Issued
2020
Journal
Physical Review D
Publisher
American Physical Society (APS)
Version
Final published version
Abstract
© 2020 American Physical Society. Understanding the origin of fast radio bursts (FRBs) is a central unsolved problem in astrophysics that is severely hampered by their poorly determined distance scale. Determining the redshift distribution of FRBs appears to require arcsecond angular resolution, in order to associate FRBs with host galaxies. In this paper, we forecast prospects for determining the redshift distribution without host galaxy associations, by cross-correlating FRBs with a galaxy catalog such as the SDSS photometric sample. The forecasts are extremely promising: a survey such as CHIME/FRB that measures catalogs of ∼103 FRBs with few-arcminute angular resolution can place strong constraints on the FRB redshift distribution, by measuring the cross-correlation as a function of galaxy redshift z and FRB dispersion measure D. In addition, propagation effects from free electron inhomogeneities modulate the observed FRB number density, either by shifting FRBs between dispersion measure (DM) bins or through DM-dependent selection effects. We show that these propagation effects, coupled with the spatial clustering between galaxies and free electrons, can produce FRB-galaxy correlations that are comparable to the intrinsic clustering signal. Such effects can be disentangled based on their angular and (z,D) dependence, providing an opportunity to study not only FRBs but also the clustering of free electrons.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
Massachusetts Institute of Technology. Department of Physics
Terms of Use
Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.
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DOI of Published Version
https://doi.org/10.1103/PHYSREVD.102.023528
