The Astrophysical Journal (Jan 2023)

Limits on Fast Radio Burst–like Counterparts to Gamma-Ray Bursts Using CHIME/FRB

  • Alice P. Curtin,
  • Shriharsh P. Tendulkar,
  • Alexander Josephy,
  • Pragya Chawla,
  • Bridget Andersen,
  • Victoria M. Kaspi,
  • Mohit Bhardwaj,
  • Tomas Cassanelli,
  • Amanda Cook,
  • Fengqiu Adam Dong,
  • Emmanuel Fonseca,
  • B. M. Gaensler,
  • Jane F. Kaczmarek,
  • Adam E. Lanmnan,
  • Calvin Leung,
  • Aaron B. Pearlman,
  • Emily Petroff,
  • Ziggy Pleunis,
  • Masoud Rafiei-Ravandi,
  • Scott M. Ransom,
  • Kaitlyn Shin,
  • Paul Scholz,
  • Kendrick Smith,
  • Ingrid Stairs

DOI
https://doi.org/10.3847/1538-4357/ace52f
Journal volume & issue
Vol. 954, no. 2
p. 154

Abstract

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Fast radio bursts (FRBs) are a class of highly energetic, mostly extragalactic radio transients lasting for ∼milliseconds. While over 600 FRBs have been published so far, their origins are presently unclear, with some theories for extragalactic FRBs predicting accompanying high-energy emission. In this work, we use the Canadian Hydrogen Intensity Mapping Experiment (CHIME) Fast Radio Burst (CHIME/FRB) Project to explore whether any FRB-like radio emission coincides in space and time with 81 gamma-ray bursts (GRBs) detected between 2018 July 17 and 2019 July 8 by Swift/BAT and Fermi/GBM. We do not find any statistically significant coincident pairs within 3 σ of each other’s spatial localization regions and within a time difference of up to one week. In addition to searching for spatial matches between known FRBs and known GRBs, we use CHIME/FRB to constrain FRB-like (∼1–10 ms) radio emission before, at the time of, or after the reported high-energy emission at the position of 39 GRBs. For short gamma-ray bursts (SGRBs), we constrain the radio flux in the 400–800 MHz band to be under a few kJy for ∼5.5–12.5 hr post-high-energy burst. We use these limits to constrain models that predict FRB-like prompt radio emission after SGRBs. For long gamma-ray bursts, we constrain the radio flux to be under a few kJy from ∼6 hr pre-high-energy burst to ∼12 hr post-high-energy burst.

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