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Burst properties of the highly active FRB20201124A using uGMRT

Marthi, V. R. and Bethapudi, S. and Main, R. A. and Lin, H-H and Spitler, L. G. and Wharton, R. S. and Li, D. Z. and Gautam, T. and Pen, U-L. and Hilmarsson, G. H. (2022) Burst properties of the highly active FRB20201124A using uGMRT. Monthly Notices of the Royal Astronomical Society, 509 (2). pp. 2209-2219. ISSN 0035-8711. doi:10.1093/mnras/stab3067. https://resolver.caltech.edu/CaltechAUTHORS:20220118-661006500

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Abstract

We report the observations of the highly active FRB20201124A with the upgraded Giant Metrewave Radio Telescope (uGMRT) at 550–750 MHz. These observations in the incoherent array mode simultaneously provided an arcsecond localization of bursts from FRB20201124A, the discovery of persistent radio emission associated with the host galaxy, and the detection of 48 bursts. Using the brightest burst in the sample (F = 108 Jy ms), we find a structure-maximizing dispersion measure of 410.8 ± 0.5 pc cm⁻³. We find that our observations are complete down to a fluence level of 10 Jy ms, above which the cumulative burst rate scales as a power law R(>F)=10 h⁻¹(F/10Jyms)^γ, with γ = −1.2 ± 0.2. We find that the bursts are, on average, wider than those reported for other repeating fast radio bursts (FRBs). We find that the waiting time between bursts is well approximated by an exponential distribution with a mean of ∼2.9 min during our observations. We searched for periodicities using both a standard Fourier domain method and the fast folding algorithm, but found no significant candidates. We measure bulk spectro-temporal drift rates between −0.75 and −20 MHz ms⁻¹. Finally, we use the brightest burst to set an upper limit to the scattering time of 11.1 ms at 550 MHz. The localization of FRB20201124A adds strength to the proof-of-concept method described in our earlier work and serves as a potential model for future localizations and follow-up of repeating FRBs with the uGMRT.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stab3067DOIArticle
https://arxiv.org/abs/2108.00697arXivDiscussion Paper
ORCID:
AuthorORCID
Bethapudi, S.0000-0003-1611-0063
Lin, H-H0000-0001-7453-4273
Spitler, L. G.0000-0002-3775-8291
Wharton, R. S.0000-0002-7416-5209
Li, D. Z.0000-0001-7931-0607
Pen, U-L.0000-0003-2155-9578
Hilmarsson, G. H.0000-0002-8965-6203
Additional Information:© 2021 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 2021 October 14. Received 2021 September 29; in original form 2021 August 1. Published: 22 October 2021. We thank the anonymous reviewer for comments, which have helped improve the manuscript. VRM thanks Jayaram Chengalur and Apurba Bera for insightful discussions. We thank the staff of the GMRT who have made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. VRM acknowledges the support of the Department of Atomic Energy, Government of India, under project no. 12-R&D-TFR-5.02-0700. We acknowledge the use of the CHIME/FRB Public Database, provided at https://www.chime-frb.ca/ by the CHIME/FRB Collaboration. We also acknowledge the support of the Natural Sciences and Engineering Research Council of Canada (NSERC) (funding reference number RGPIN-2019-067, CRD 523638-201). We receive support from the Ontario Research Fund – Research Excellence Program (ORF-RE), Canadian Institute for Advanced Research (CIFAR), Canadian Foundation for Innovation (CFI), Simons Foundation, Thoth Technology Inc., and Alexander von Humboldt Foundation. 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. LGS is a Lise Meitner Independent Max Planck Research Group Leader and acknowledges support from the Max Planck Society. Data Availability: The data underlying this paper will be shared on reasonable request to the corresponding authors.
Funders:
Funding AgencyGrant Number
Department of Atomic Energy (India)12-R&D-TFR-5.02-0700
Natural Sciences and Engineering Research Council of Canada (NSERC)RGPIN-2019-067
Natural Sciences and Engineering Research Council of Canada (NSERC)CRD 523638-201
Ontario Research Fund-Research ExcellenceUNSPECIFIED
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Canada Foundation for InnovationUNSPECIFIED
Simons FoundationUNSPECIFIED
Thoth Technology Inc.UNSPECIFIED
Alexander von Humboldt FoundationUNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
Max Planck SocietyUNSPECIFIED
Subject Keywords:scattering – methods: observational – techniques: interferometric
Issue or Number:2
DOI:10.1093/mnras/stab3067
Record Number:CaltechAUTHORS:20220118-661006500
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220118-661006500
Official Citation:V R Marthi, S Bethapudi, R A Main, H-H Lin, L G Spitler, R S Wharton, D Z Li, T Gautam, U-L Pen, G H Hilmarsson, Burst properties of the highly active FRB20201124A using uGMRT, Monthly Notices of the Royal Astronomical Society, Volume 509, Issue 2, January 2022, Pages 2209–2219, https://doi.org/10.1093/mnras/stab3067
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:112946
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:18 Jan 2022 22:44
Last Modified:18 Jan 2022 22:44

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