Detection of two bright radio bursts from magnetar SGR 1935 + 2154

Kirsten, F.; Snelders, M. P.; Jenkins, M.; Nimmo, K.; Eijnden, J. van den; Hessels, J. W. T.; Gawroński, M.; Yang, Jun

doi:10.1038/s41550-020-01246-3

Cited by 114 publications

(92 citation statements)

References 52 publications

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“…We find that the two fainter radio bursts detected by Kirsten et al (2020), which were separated by 1.4 s, are offset from the X-ray pulse peaks. As pointed out by those authors, it is not yet clear what the origin of such radio bursts is, whether they are driven by similar physical and emission mechanisms that resulted in the FRB or different ones.…”

Section: The Frb Connectionmentioning

confidence: 68%

“…In all panels, green dashed lines show the average of the values inferred from historical NICERobservations obtained in 2017-2019, before the source burst active period. The blue vertical dashed, dotted, and dashed-dotted lines, respectively, mark the times of the FRB-like event, two additional weak radio bursts (Kirsten et al 2020), and another weak radio burst reported by FAST (Zhang et al 2020) from the source. The red solid curves in the top two panels constitute the best-fit double exponential decay models to the flux and BB temperature, displaying an initial very rapid rise and then a much slower decline.…”

Section: Sgr1935+2154 Burst Storm Comparison To Other Magnetarsmentioning

confidence: 97%

“…Bottom panel: pulse profile of the persistent emission as observed during days 21-39 postoutburst (ObsIDs 3020560105-3020560119). The dotted lines are the phases of the two radio bursts observed by Kirsten et al (2020). The rms pulsed fraction is 6.7%±0.8%.…”

Section: Properties Of Bursts Beyond the Burst Stormmentioning

confidence: 99%

“…We measure an rms pulsed fraction of 6.7%±0.8%. The dotted lines are the corresponding phases of the two radio bursts detected on 2020 May 24 (Kirsten et al 2020).…”

Section: Timingmentioning

confidence: 99%

“…This exceptional FRB−X-ray burst association placed magnetars at center stage as the potential origin of at least some extragalactic FRBs. Interestingly, SGR1935+2154 has since shown several millisecond radio bursts with fluences between 3 and 7 orders of magnitude smaller than the FRB-like burst (Good & Chime/ Frb Collaboration 2020;Kirsten et al 2020;Pleunis & CHIME/FRB Collaboration 2020;Zhang et al 2020;Zhu et al 2020).…”

Section: Introductionmentioning

confidence: 99%

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NICER View of the 2020 Burst Storm and Persistent Emission of SGR 1935+2154

Younes

Güver

Kouveliotou

et al. 2020

ApJL

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We report on NICER observations of the magnetar SGR1935+2154, covering its 2020 burst storm and long-term persistent emission evolution up to ∼90 days postoutburst. During the first 1120s taken on April 28 00:40:58 UTC, we detect over 217 bursts, corresponding to a burst rate of >0.2 burstss −1. Three hours later, the rate was 0.008burstss −1 , remaining at a comparatively low level thereafter. The T 90 burst duration distribution peaks at 840 ms; the distribution of waiting times to the next burst is fit with a lognormal with an average of 2.1 s. The 1-10 keV burst spectra are well fit by a blackbody, with an average temperature and area of kT=1.7 keV and R 2 =53 km 2. The differential burst fluence distribution over ∼3 orders of magnitude is well modeled with a power-law form dN/dF∝F −1.5±0.1. The source persistent emission pulse profile is double-peaked hours after the burst storm. We find that the burst peak arrival times follow a uniform distribution in pulse phase, though the fast radio burst associated with the source aligns in phase with the brighter peak. We measure the source spin-down from heavy-cadence observations covering days 21-39 postoutburst, n =-´-3.72 3 10 12 ()  Hzs −1 , a factor of 2.7 larger than the value measured after the 2014 outburst. Finally, the persistent emission flux and blackbody temperature decrease rapidly in the early stages of the outburst, reaching quiescence 40 days later, while the size of the emitting area remains unchanged.

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Section: The Frb Connectionmentioning

confidence: 68%

Section: Sgr1935+2154 Burst Storm Comparison To Other Magnetarsmentioning

confidence: 97%

Section: Properties Of Bursts Beyond the Burst Stormmentioning

confidence: 99%

“…We measure an rms pulsed fraction of 6.7%±0.8%. The dotted lines are the corresponding phases of the two radio bursts detected on 2020 May 24 (Kirsten et al 2020).…”

Section: Timingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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NICER View of the 2020 Burst Storm and Persistent Emission of SGR 1935+2154

Younes

Güver

Kouveliotou

et al. 2020

ApJL

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Fast radio bursts at the dawn of the 2020s

Petroff

Hessels

Lorimer

2022

Astron Astrophys Rev

Self Cite

130

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Since the discovery of the first fast radio burst (FRB) in 2007, and their confirmation as an abundant extragalactic population in 2013, the study of these sources has expanded at an incredible rate. In our 2019 review on the subject, we presented a growing, but still mysterious, population of FRBs—60 unique sources, 2 repeating FRBs, and only 1 identified host galaxy. However, in only a few short years, new observations and discoveries have given us a wealth of information about these sources. The total FRB population now stands at over 600 published sources, 24 repeaters, and 19 host galaxies. Higher time resolution data, sustained monitoring, and precision localisations have given us insight into repeaters, host galaxies, burst morphology, source activity, progenitor models, and the use of FRBs as cosmological probes. The recent detection of a bright FRB-like burst from the Galactic magnetar SGR 1935 + 2154 provides an important link between FRBs and magnetars. There also continue to be surprising discoveries, like periodic modulation of activity from repeaters and the localisation of one FRB source to a relatively nearby globular cluster associated with the M81 galaxy. In this review, we summarise the exciting observational results from the past few years. We also highlight their impact on our understanding of the FRB population and proposed progenitor models. We build on the introduction to FRBs in our earlier review, update our readers on recent results, and discuss interesting avenues for exploration as the field enters a new regime where hundreds to thousands of new FRBs will be discovered and reported each year.

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The physics of fast radio bursts

Xiao

Wang

Dai

2021

Sci. China Phys. Mech. Astron.

127

103

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In 2007, a very bright radio pulse was identified in the archival data of the Parkes Telescope in Australia, marking the beginning of a new research branch in astrophysics. In 2013, this kind of millisecond bursts with extremely high brightness temperature takes a unified name, fast radio burst (FRB). Over the first few years, FRBs seemed very mysterious because the sample of known events was limited. With the improvement of instruments over the last five years, hundreds of new FRBs have been discovered. The field is now undergoing a revolution and understanding of FRB has rapidly increased as new observational data increasingly accumulate. In this review, we will summarize the basic physics of FRBs and discuss the current research progress in this area. We have tried to cover a wide range of FRB topics, including the observational property, propagation effect, population study, radiation mechanism, source model, and application in cosmology. A framework based on the latest observational facts is now under construction. In the near future, this exciting field is expected to make significant breakthroughs. fast radio burst, neutron star, cosmology

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Detection of two bright radio bursts from magnetar SGR 1935 + 2154

Cited by 114 publications

References 52 publications

NICER View of the 2020 Burst Storm and Persistent Emission of SGR 1935+2154

NICER View of the 2020 Burst Storm and Persistent Emission of SGR 1935+2154

Fast radio bursts at the dawn of the 2020s

The physics of fast radio bursts

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