Published December 1, 2024 | Version Published
Journal Article Open

A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB

  • 1. ROR icon University of Toronto
  • 2. ROR icon University of California, Santa Cruz
  • 3. ROR icon York University
  • 4. ROR icon Columbia University
  • 5. ROR icon California Institute of Technology
  • 6. ROR icon University of Minnesota
  • 7. ROR icon United States Naval Research Laboratory
  • 8. ROR icon Tata Institute of Fundamental Research
  • 9. ROR icon National Centre for Radio Astrophysics
  • 10. ROR icon Canadian Institute for Advanced Research
  • 11. ROR icon Massachusetts Institute of Technology
  • 12. ROR icon Northwestern University
  • 13. ROR icon Carnegie Mellon University
  • 14. ROR icon West Virginia University
  • 15. ROR icon Cornell University
  • 16. ROR icon McGill University
  • 17. ROR icon University of Amsterdam
  • 18. ROR icon Netherlands Institute for Radio Astronomy
  • 19. ROR icon Chalmers University of Technology
  • 20. ROR icon Perimeter Institute

Abstract

The identification of persistent radio sources (PRSs) coincident with two repeating fast radio bursts (FRBs) supports FRB theories requiring a compact central engine. However, deep nondetections in other cases highlight the diversity of repeating FRBs and their local environments. Here, we perform a systematic search for radio sources towards 37 CHIME/FRB repeaters using their arcminute localizations and a combination of archival surveys and targeted observations. Through multiwavelength analysis of individual radio sources, we identify two (20181030A-S1 and 20190417A-S1) for which we disfavor an origin of either star formation or an active galactic nucleus in their host galaxies and thus consider them candidate PRSs. We do not find any associated PRSs for the majority of the repeating FRBs in our sample. For eight FRB fields with Very Large Array imaging, we provide deep limits on the presence of PRSs that are 2–4 orders of magnitude fainter than the PRS associated with FRB 20121102A. Using Very Large Array Sky Survey imaging of all 37 fields, we constrain the rate of luminous (≳1040 erg s−1) PRSs associated with repeating FRBs to be low. Within the context of FRB-PRS models, we find that 20181030A-S1 and 20190417A-S1 can be reasonably explained within the context of magnetar, hypernebulae, gamma-ray burst afterglow, or supernova ejecta models—although we note that both sources follow the radio luminosity versus rotation measure relationship predicted in the nebula model framework. Future observations will be required to both further characterize and confirm the association of these PRS candidates with the FRBs.

Copyright and License

© 2024. The Author(s). Published by the American Astronomical Society.

Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.

Acknowledgement

We acknowledge Gabriele Bruni and Yuan-Pei Yang for their useful conversations.

We acknowledge that CHIME is located in the traditional, ancestral, and unceded territory of the Syilx/Okanagan people. We are grateful to the staff of the Dominion Radio Astrophysical Observatory, which is operated by the National Research Council of Canada. CHIME is funded by a grant from the Canada Foundation for Innovation (CFI) 2012 Leading Edge Fund (project 31170) and by contributions from the provinces of British Columbia, Quebec, and Ontario. The CHIME/FRB Project is funded by a grant from the CFI 2015 Innovation Fund (project 33213) and by contributions from the provinces of British Columbia and Quebec, and by the Dunlap Institute for Astronomy and Astrophysics at the University of Toronto. Additional support was provided by the Canadian Institute for Advanced Research (CIFAR), McGill University, and the McGill Space Institute thanks to the Trottier Family Foundation and the University of British Columbia. The CHIME/FRB baseband system is funded in part by a Canada Foundation for Innovation John R. Evans Leaders Fund award to IHS.

The National Radio Astronomy Observatory (NRAO) is a facility of the National Science Foundation operated under a cooperative agreement by Associated Universities, Inc. We would like to acknowledge NRAO for telescope time awarded through the Karl G. Jansky Very Large Array (VLA) interferometer for program Nos. 20B-280, 20A-469, 21B-176, and 21A-387. We also thank the NRAO staff for their help in the preparation of observations.

The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto.

Some of this work is based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciência e Tecnologia (Brazil), and SECYT (Argentina). We appreciate the Gemini team for granting us observing time for the program IDs: GN-2022A-Q-212, GN-2022B-Q-308, and GN-2022B-Q-116.

Basic research in radio astronomy at the U.S. Naval Research Laboratory is supported by 6.1 Base funding. The construction and installation of VLITE were supported by the NRL Sustainment Restoration and Maintenance fund.

B.M.G. acknowledges the support of the Natural Sciences and Engineering Research Council of Canada (NSERC) through grant RGPIN-2022-03163 and of the Canada Research Chairs program. M.R.D. acknowledges support from the NSERC through grant RGPIN-2019-06186, and of the Canada Research Chairs Program, and the Dunlap Institute at the University of Toronto. V.M.K. holds the Lorne Trottier Chair in Astrophysics & Cosmology, a Distinguished James McGill Professorship, and receives support from an NSERC Discovery grant (RGPIN-228738-13) and from the FRQNT CRAQ. J.W.T.H. is a Canada Excellence Research Chair in Transient Astrophysics.

N.S. acknowledges the support from NASA (grant No. 80NSSC22K0332), NASA FINESST (grant No. 80NSSC22K1597), Columbia University Dean's fellowship, and a grant from the Simons Foundation. T. E. is supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51504.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. A.M.C. is funded by an NSERC Doctoral Postgraduate Scholarship. A.B.P. is a Banting Fellow, a McGill Space Institute (MSI) Fellow, and a Fonds de Recherche du Quebec—Nature et Technologies (FRQNT) postdoctoral fellow. K.W.M. holds the Adam J. Burgasser Chair in Astrophysics and is supported by NSF grants (2008031, 2018490). S.P.T. is a CIFAR Azrieli Global Scholar in the Gravity and Extreme Universe Program. Z.P. was a Dunlap Fellow and is supported by an NWO Veni fellowship (VI.Veni.222.295). A.P. is funded by the NSERC Canada Graduate Scholarships—Doctoral program. K.N. is an MIT Kavli Fellow. F.K. acknowledges support from Onsala Space Observatory for the provisioning of its facilities/observational support. The Onsala Space Observatory national research infrastructure is funded through Swedish Research Council grant No. 2017-00648. M.B. is a McWilliams fellow and an International Astronomical Union Gruber fellow. M.B. also receives support from the McWilliams seed grant.

Facilities

CHIME - , VLA - Very Large Array, Gemini:Gillett - Gillett Gemini North Telescope.

Software References

FRUITBAT (A. Batten 2019), PHOTUTILS (L. Bradley et al. 2023), SExtractor (E. Bertin & S. Arnouts 1996), IRAF (S. Blondin et al. 2012), PYRAF (Science Software Branch at STScI 2012), PypeIt (J. Prochaska et al. 2020), CASA (J. P. McMullin et al. 2007), pwkit (P. K. G. Williams et al. 2017), AEGEAN (P. J. Hancock et al. 2018), Astropy (Astropy Collaboration et al. 201320182022), Matplotlib (J. D. Hunter 2007), NumPy (C. R. Harris et al. 2020), SAOImage DS9 (W. A. Joye & E. Mandel 2003).

Files

Ibik_2024_ApJ_976_199.pdf

Files (3.5 MB)

Name Size Download all
md5:1f0268cad22192af6c76dd7188fa88a6
3.5 MB Preview Download

Additional details

Related works

Is new version of
Discussion Paper: arXiv:2409.11533 (arXiv)

Funding

Canada Foundation for Innovation
31170
Canada Foundation for Innovation
33213
University of Toronto
Dunlap Institute for Astronomy and Astrophysics
Canadian Institute for Advanced Research
McGill University
Trottier Family Foundation
University of British Columbia
United States Naval Research Laboratory
6.1 Base funding
Natural Sciences and Engineering Research Council
RGPIN-2022-03163
Canada Research Chairs
Natural Sciences and Engineering Research Council
RGPIN-2019-06186
Natural Sciences and Engineering Research Council
RGPIN-228738-13
Fonds de Recherche du Québec – Nature et Technologies
National Aeronautics and Space Administration
80NSSC22K0332
National Aeronautics and Space Administration
80NSSC22K1597
Columbia University
Dean's Fellowship
Simons Foundation
National Aeronautics and Space Administration
HST-HF2-51504.001-A
National Aeronautics and Space Administration
NAS5-26555
Government of Canada
Banting Fellowship
National Science Foundation
2008031
National Science Foundation
AST-2018490
Dutch Research Council
VI.Veni.222.295
Massachusetts Institute of Technology
Kavli Fellowship
Swedish Research Council
2017-00648
Carnegie Mellon University
McWilliams Fellowship
Union astronomique internationale

Dates

Accepted
2024-09-24
Accepted
Available
2024-11-22
Published

Caltech Custom Metadata

Publication Status
Published