Milliarcsecond localisation of the repeating FRB 20201124A

Nimmo, K.; Hewitt, D. M.; Hessels, J. W. T.; Kirsten, F.; Marcote, B.; Bach, U.; Blaauw, R.; Burgay, M.; Corongiu, A.; Feiler, R.; Gawroński, M. P.; Giroletti, M.; Karuppusamy, R.; Keimpema, A.; Kharinov, M. A.; Lindqvist, M.; Maccaferri, G.; Melnikov, A.; Mikhailov, A.; Ould-Boukattine, O. S.; Paragi, Z.; Pilia, M.; Possenti, A.; Snelders, M. P.; Surcis, G.; Trudu, M.; Venturi, T.; Vlemmings, W.; Wang, N.; Yang, J.; Yuan, J.

doi:10.48550/arxiv.2111.01600

Cited by 9 publications

(15 citation statements)

References 44 publications

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“…We followed up FRB 20201124A within the PRECISE project during different epochs and, we detected 13 and 5 bursts in two of them [30]. By combining the data from all these bursts, we were able to localize FRB 20201124A with a 1-𝜎 uncertainty of 2.7 milliarcseconds (mas) [31]. This is roughly a factor of 1 000 times better than the previously reported localizations (see Figure 1, left).…”

Section: The Absence Of Compact Persistent Emission Associated With F...mentioning

confidence: 81%

PRECISE localizations of repeating Fast Radio Bursts

Marcote¹,

Kirsten²,

Hessels³

et al. 2022

Preprint

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Fast Radio Bursts (FRBs) are extremely luminous and brief signals (with duration of milliseconds or even shorter) of extragalactic origin. Despite the fact that hundreds of FRBs have been discovered to date, their nature still remains unclear. Precise localizations of FRBs can unveil their host galaxies and local environments -and thus shed light on the physical processes that led to the burst production. However, this has only been achieved for a few FRBs to date. The European VLBI Network (EVN) is currently the only instrument capable of localizing FRBs down to the milliarcsecond level. This level of precision was critical to associate the first localized FRB, 20121102A, to a star-forming region in a low-metallicity dwarf galaxy and physically related it to a compact persistent radio source. Analogously, a second repeating FRB, 20180916B, was found to just outside the edge of a prominent star-forming region of a nearby spiral galaxy. The PRECISE project (Pinpointing REpeating ChIme Sources with EVN dishes), starting from 2019, has observed hundreds of hours per year with a subset of EVN telescopes with the goal of localizing repeating FRBs discovered by the CHIME/FRB Collaboration. The ultimate goal of PRECISE is to disentangling the environments where FRBs can be produced. Here we present the state of the art of the FRB field, the PRECISE project, and the localizations achieved until now, which have unveiled a variety of environments where FRBs can be found that challenges the current models.

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Section: The Absence Of Compact Persistent Emission Associated With F...mentioning

confidence: 81%

PRECISE localizations of repeating Fast Radio Bursts

Marcote¹,

Kirsten²,

Hessels³

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

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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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“…FRB20201124A is a repeater with DM ∼ 410 pc cm (Xu et al 2021), uGMRT (Wharton et al 2021) and VLA (Law et al 2021) and further refined, with a milliarcsecond precision, by the EVN (Nimmo et al 2021b). It was localised in a nearby (𝑧 ∼ 0.098) (Fong et al 2021) galaxy with a high star formation rate which suggests a new-born magnetar as the most likely progenitor (Piro et al 2021).…”

Section: Frb20201124amentioning

confidence: 99%

The Northern Cross Fast Radio Burst project - II. Monitoring of repeating FRB 20180916B, 20181030A, 20200120E and 20201124A

Trudu,

Pilia,

Bernardi

et al. 2022

Preprint

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In this work we report the results of a nineteen-month Fast Radio Burst observational campaign carried out with the North-South arm of the Medicina Northern Cross radio telescope at 408 MHz in which we monitored four repeating sources: FRB20180916B, FRB20181030A, FRB20200120E and FRB20201124A. We present the current state of the instrument and the detection and characterisation of three bursts from FRB20180916B. Given our observing time, our detections are consistent with the event number we expect from the known burst rate (2.7 ± 1.9 above our 10𝜎, 38 Jy ms detection threshold) in the 5.2 day active window of the source, further confirming the source periodicity. We detect no bursts from the other sources. We turn this result into a 95% confidence level lower limit on the slope of the differential fluence distribution 𝛼 to be 𝛼 > 2.1 and 𝛼 > 2.2 for FRB20181030A and FRB20200120E respectively. Given the known rate for FRB20201124A, we expect 1.0 ± 1.1 bursts from our campaign, consistent with our non-detection.

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Milliarcsecond localisation of the repeating FRB 20201124A

Cited by 9 publications

References 44 publications

PRECISE localizations of repeating Fast Radio Bursts

PRECISE localizations of repeating Fast Radio Bursts

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

The Northern Cross Fast Radio Burst project - II. Monitoring of repeating FRB 20180916B, 20181030A, 20200120E and 20201124A

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