J/other/Nat/598.267 List of radio bursts (Li+, 2021)
A bimodal burst energy distribution of a repeating fast radio burst source.
Li D., Wang P., Zhu W.W., Zhang ? B., Zhang X.X., Duan R., Zhang Y.K.,
Feng Y., Tang N.Y., Chatterjee S., Cordes J.M., Cruces M., Dai S.,
Gajjar V., Hobbs G., Jin C., Kramer M., Lorimer D.R., Miao C.C., Niu C.H.,
Niu J.R., Pan Z.C., Qian L., Spitler L., Werthimer D., Zhang G.Q.,
Wang F.Y., Xie X.Y., Yue Y.L., Zhang L., Zhi Q.J., Zhu Y.
<Nature, 598, 267-271 (2021)>
=2021Natur.598..267L 2021Natur.598..267L (SIMBAD/NED BibCode)
ADC_Keywords: Radio sources
Abstract:
The event rate, energy distribution and time-domain behaviour of
repeating fast radio bursts (FRBs) contain essential information
regarding their physical nature and central engine, which are as yet
unknown. As the first precisely localized source, FRB 121102 has been
extensively observed and shows non-Poisson clustering of bursts over
time and a power-law energy distribution. However, the extent of
the energy distribution towards the fainter end was not known. Here we
report the detection of 1,652 independent bursts with a peak burst
rate of 122h-1, in 59.5 hours spanning 47 days. A peak in the
isotropic equivalent energy distribution is found to be approximately
4.8x1037erg at 1.25GHz, below which the detection of bursts is
suppressed. The burst energy distribution is bimodal, and well
characterized by a combination of a log-normal function and a
generalized Cauchy function. The large number of bursts in hour-long
spans allows sensitive periodicity searches between 1ms and 1000s.
The non-detection of any periodicity or quasi-periodicity poses
challenges for models involving a single rotating compact object. The
high burst rate also implies that FRBs must be generated with a high
radiative efficiency, disfavouring emission mechanisms with large
energy requirements or contrived triggering conditions.
Description:
A continuous monitoring campaign of FRB 121102 with the
Five-hundredmeter Aperture Spherical radio Telescope (FAST) has been
carried out since August 2019. Between 29 August and 29 October 2019,
we detected 1,652 independent burst events (Table S1) in a total of
59.5h, covering 1.05GHz to 1.45GHz with 98.304-us sampling and
0.122-MHz frequency resolution.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tables1.dat 98 1652 All relevant data for the 1652 detected burst events
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Byte-by-byte Description of file: tables1.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- Burst Burst ID
6- 20 F15.9 d MJD Burst time (MJD) (1)
22- 26 F5.1 pc/cm3 DM Dispersion measure
28- 30 F3.1 pc/cm3 e_DM Dispersion measure error
33- 37 F5.2 ms Width Pulse width error
39- 42 F4.2 ms e_Width Pulse width
44- 48 F5.3 GHz Bandwidth Bandwidth (2)
52- 59 F8.3 mJy Fp Peak flux
61- 64 F4.1 mJy e_Fp Peak flux error
66- 71 F6.4 Jy.ms Fluence Fluence
73- 78 F6.4 Jy.ms e_Fluence Fluence error
80- 88 E9.4 10-7W E Energy
90- 98 E9.4 10-7W e_E Energy error
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Note (1): Arrival time of burst peak at the solar system barycenter, after
correcting to the frequency of 1.5GHz.
Note (2): A conservative 30% fractional error is assumed.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 18-Feb-2022