The fast radio burst FRB 20201124A in a star-forming region: Constraints to the progenitor and multiwavelength counterparts

Piro, L.; Bruni, G.; Troja, E.; O’Connor, B.; Panessa, F.; Ricci, R.; Zhang, B.; Burgay, M.; Dichiara, S.; Lee, K. J.; Lotti, Simone; Niu, Jiarui; Pilia, M.; Possenti, A.; Trudu, M.; Xu, Heng; Zhu, Weiwei; Kutyrev, A.; Veilleux, Sylvain

doi:10.1051/0004-6361/202141903

Cited by 41 publications

(43 citation statements)

References 64 publications

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“…A fluence of few × 10 −19 erg cm −2 yields a characteristic isotropic-equivalent radio energy of 10 37 -10 38 erg, an energy scale that is typical for FRBs (repeaters and apparent nonrepeaters) with accurate localizations such as FRB 121102, FRB 180924, FRB 181112, and FRB 20201124A (Tendulkar et al 2017;Bannister et al 2019;Prochaska et al 2019;Kilpatrick et al 2021;Lanman et al 2022;Piro et al 2021). This is consistent with models that predict a narrow universal luminosity function (e.g., Beniamini et al 2020) for FRBs.…”

Section: Summary and Discussionmentioning

confidence: 99%

Simultaneous View of FRB 180301 with FAST and NICER during a Bursting Phase

Laha

Younes

Wadiasingh

et al. 2022

ApJ

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FRB 180301 is one of the most actively repeating fast radio bursts (FRBs) that has shown polarization angle changes in its radio burst emission, an indication for their likely origin in the magnetosphere of a highly magnetized neutron star. We carried out a multiwavelength campaign with the FAST radio telescope and NICER X-ray observatory to investigate any possible X-ray emission temporally coincident with the bright radio bursts. The observations took place on 2021 March 4, 9 and 19. We detected five bright radio bursts with FAST, four of which were strictly simultaneous with the NICER observations. The peak flux density of the radio bursts ranged between 28 and 105 mJy, the burst fluence between 27 and 170 mJy ms, and the burst durations between 1.7 and 12.3 ms. The radio bursts from FRB 180301 exhibited a complex time domain structure, and subpulses were detected in individual bursts, with no significant circular polarization. The linear degree of polarization in the L band reduced significantly compared to the 2019 observations. We do not detect any X-ray emission in excess of the background during the 5, 10, 100 ms, 1 and 100 s time intervals at/around the radio-burst barycenter-corrected arrival times, at a > 5σ confidence level. The 5σ upper limits on the X-ray (a) persistent flux is <7.64 × 10−12 erg cm−2 s−1, equivalent to L X < 2.50 × 1045 erg s−1 and (b) 5 ms fluence is <2 × 10−11 erg cm−2, at the radio burst regions. Using the 5 ms X-ray fluence upper limit, we can estimate the radio efficiency η R/X ≡ L radio/L X−ray ≳ 10−8. The derived lower limit on η R/X is consistent with both magnetospheric models and synchrotron maser models involving relativistic shocks.

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Section: Summary and Discussionmentioning

confidence: 99%

Simultaneous View of FRB 180301 with FAST and NICER during a Bursting Phase

Laha

Younes

Wadiasingh

et al. 2022

ApJ

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“…Recently, three repeating FRB sources were localized in nearby star-forming regions of galaxies (Bassa et al 2017;Marcote et al 2020;Piro et al 2021). This may indicate young stellar populations as a possible origin of repeating FRBs.…”

Section: Immediate Localization By Bursttmentioning

confidence: 93%

BURSTT: Bustling Universe Radio Survey Telescope for Taiwan

Lin¹,

Lin²,

Li³

et al. 2022

Preprint

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Fast Radio Bursts (FRBs), bright millisecond-duration radio transients are happening thousands of times per day. FRBs' astrophysical mechanisms are still puzzling. Bustling Universe Radio Survey Telescope for Taiwan (BURSTT) is optimized to discover and localize a large sample of bright and nearby FRBs. BURSTT will have a large field-of-view (FoV) of ∼10 4 deg 2 for monitoring the whole visible sky all the time, a 400 MHz effective bandwidth between 300-800 MHz, and the sub-arcsecond localization capability with several outrigger stations hundreds to thousands of km away. Initially, BURSTT will equip with 256 antennas, which we will test different designs and improve the system performance. Through the scalable features, BURSTT could equip with more antennas and eventually optimized designs. We expect that BURSTT initially would detect and localize ∼100 bright (≥100 Jy ms) and nearby FRBs per year to sub-arcsecond precision. Besides, the large FoV yields monitoring FRBs with high cadence, which is crucial to understanding the repetition of FRBs. Multi-

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“…Another active repeater FRB 20201124A (Lanman et al 2021;Kumar et al 2021;Nimmo et al 2021;Hilmarsson et al 2021) is found in a Milky-Way-sized, metal-rich, barred-spiral host galaxy at z = 0.098 (Xu et al 2021;Fong et al 2021;Ravi et al 2021;Piro et al 2021). This repeater indicates a significant, irregular, variation of the Faraday rotation over 36 days.…”

Section: Introductionmentioning

confidence: 92%

Temporal Scattering, Depolarization, and Persistent Radio Emission from Magnetized Inhomogeneous Environments Near Repeating Fast Radio Burst Sources

Yang,

Lu,

Feng

et al. 2022

Preprint

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Some repeating fast radio burst (FRB) sources exhibit complex polarization behaviors, including frequency-dependent depolarization, variation of rotation measure (RM), and oscillating spectral structures of polarized components. Very recently, Feng et al. (2022) reported that active repeaters exhibit conspicuous frequency-dependent depolarization and a strong correlation between RM scatter (σ RM ) and the temporal scattering time (τ s ), σ RM ∝ τ 1.0±0.2 s , both of which can be well described by multipath propagation through a magnetized inhomogeneous plasma screen. This observation strongly suggests that the temporal scattering and RM scatter originate from the same region. Besides, a particular finding of note in Feng et al. ( 2022) is that the FRBs with compact persistent radio sources (PRS) tend to have extreme σ RM . In this work, we analyze the temporal scattering, RM scatter and the PRS emission contributed by the magnetized inhomogeneous plasma screen near an FRB source. The behaviors of the RM scatter imply that the magnetized plasma environment is consistent with a supernova remnant or a pulsar wind nebula, and the predicted σ RM -τ s relation is σ RM ∝ τ (0.54−0.83) s for different astrophysical scenarios. We also show that the specific luminosity of a PRS should have a positive correlation with the RM contributed by the plasma screen. This is consistent with the observations of FRB 121102 and FRB 190520B.

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The fast radio burst FRB 20201124A in a star-forming region: Constraints to the progenitor and multiwavelength counterparts

Cited by 41 publications

References 64 publications

Simultaneous View of FRB 180301 with FAST and NICER during a Bursting Phase

Simultaneous View of FRB 180301 with FAST and NICER during a Bursting Phase

BURSTT: Bustling Universe Radio Survey Telescope for Taiwan

Temporal Scattering, Depolarization, and Persistent Radio Emission from Magnetized Inhomogeneous Environments Near Repeating Fast Radio Burst Sources

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