The host galaxy and persistent radio counterpart of FRB 20201124A
Abstract
The physical properties of fast radio burst (FRB) host galaxies provide important clues towards the nature of FRB sources. The 16 FRB hosts identified thus far span three orders of magnitude in mass and specific star formation rate, implicating a ubiquitously occurring progenitor object. FRBs localized with ∼arcsecond accuracy also enable effective searches for associated multiwavelength and multi-time-scale counterparts, such as the persistent radio source associated with FRB 20121102A. Here we present a localization of the repeating source FRB 20201124A, and its association with a host galaxy (SDSS J050803.48+260338.0, z = 0.098) and persistent radio source. The galaxy is massive (∼3×10¹⁰M⊙), star-forming (few solar masses per year), and dusty. Very Large Array and Very Long Baseline Array observations of the persistent radio source measure a luminosity of 1.2 × 10²⁹ erg s⁻¹ Hz⁻¹, and show that is extended on scales ≳50 mas. We associate this radio emission with the ongoing star formation activity in SDSS J050803.48+260338.0. Deeper, high-resolution optical observations are required to better utilize the milliarcsecond-scale localization of FRB 20201124A and determine the origin of the large dispersion measure (150–220 pc cm⁻³) contributed by the host. SDSS J050803.48+260338.0 is an order of magnitude more massive than any galaxy or stellar system previously associated with a repeating FRB source, but is comparable to the hosts of so far non-repeating FRBs, further building the link between the two apparent populations.
Additional Information
© 2022 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2022 February 1. Received 2022 January 31; in original form 2021 June 17. Published: 25 April 2022. We thank the staff of the VLBA for rapidly scheduling and executing the observations presented here. This research was supported by the National Science Foundation under grants AST-1836018 and AST-2022546. KA and SBS acknowledge support from NSF grant AAG-1714897. SBS is a CIFAR Azrieli Global Scholar in the Gravity and the Extreme Universe program. The NANOGrav project receives support from National Science Foundation (NSF) Physics Frontier Center award number 1430284. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Data Availability: Original data presented herein include VLA, VLBA, and P200/DBSP observations. The VLA and VLBA primary data products are archived at the NRAO Data Archive (https://archive.nrao.edu/archive/advquery.jsp). The VLA secondary (realfast) data products are will soon be available through the NRAO archive, but are currently available on request. The raw data obtained during the P200/DBSP observations are available upon request. All data that shown in figures are available upon request.Attached Files
Published - stac465.pdf
Submitted - 2106.09710.pdf
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Additional details
- Eprint ID
- 112540
- Resolver ID
- CaltechAUTHORS:20211217-233220950
- AST-1836018
- NSF
- AST-2022546
- NSF
- AAG-1714897
- NSF
- Canadian Institute for Advanced Research (CIFAR)
- PHY-1430284
- NSF
- NASA/JPL/Caltech
- Created
-
2021-12-20Created from EPrint's datestamp field
- Updated
-
2022-05-17Created from EPrint's last_modified field
- Caltech groups
- Astronomy Department