J/A+A/676/A17 Fast radio burst FRB20180916B (Trudu+, 2023)
Simultaneous and panchromatic observations of the
fast radio burst FRB 20180916B.
Trudu M., Pilia M., Nicastro L., Guidorzi C., Orlandini M., Zampieri L.,
Marthi V.R., Ambrosino F., Possenti A., Burgay M., Casentini C.,
Mereminskiy I., Savchenko V., Palazzi E., Panessa F., Ridolfi A.,
Verrecchia F., Anedda M., Bernardi G., Bachetti M., Burenin R.,
Burtovoi A., Casella P., Fiori M., Frontera F., Gajjar V., Gardini A.,
Ge M., Guijarro-Roman A., Ghedina A., Hermelo I., Jia S., Li C., Liao J.,
Li X., Lu F., Lutovinov A., Naletto G., Ochner P., Papitto A., Perri M.,
Pittori C., Safonov B., Semena A., Strakhov I., Tavani M., Ursi A.,
Xiong S.L., Zhang S.N., Zheltoukhov S.
<Astron. Astrophys. 676, A17 (2023)>
=2023A&A...676A..17T 2023A&A...676A..17T (SIMBAD/NED BibCode)
ADC_Keywords: X-ray sources ; Radio sources
Keywords: methods: observational - instrumentation: photometers -
X-ray: bursts - stars: magnetars - stars: neutron - stars: flare
Abstract:
Fast radio bursts are bright radio transients whose origins are not
yet understood. The search for a multi-wavelength counterpart of those
events can set a tight constraint on the emission mechanism and the
progenitor source.
We conducted a multi-wavelength observational campaign on
FRB 20180916B between October 2020 and August 2021 over eight activity
cycles of the source. Observations were carried out in the radio band
by the SRT both at 336 and 1547MHz and the uGMRT at 400MHz.
Simultaneous observations were conducted by the optical telescopes
Asiago (Galileo and Copernico), CMO SAI MSU, CAHA 2.2m, RTT-150 and
TNG, and X/gamma-ray detectors on board the AGILE, Insight-HXMT,
INTEGRAL, and Swift satellites.
We present the detection of 14 new radio bursts detected with the SRT
at 336MHz and seven new bursts with the uGMRT from this source. We
provide the deepest prompt upper limits in the optical band for FRB
20180916B to date. In fact, the TNG/SiFAP2 observation simultaneous to
a burst detection by uGMRT gives an upper limit
Eoptical-Eradio<1.3x102. Another burst detected by the SRT at
336MHz was also co-observed by Insight-HXMT. The non-detection in
the X-rays yields an upper limit (1-30keV band) of EX-ray=Eradio
in the range of (0.9-1.3)107, depending on the model that is
considered for the X-ray emission.
Description:
We performed a MWL observing campaign on R3, focusing on
different activity cycles, from 2020/10/23 to 2021/08/30.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 53 3 Details of the radio instruments involved in
the R3 MWL campaign
table2.dat 77 22 Properties of the detected bursts
tablea1.dat 74 43 Log of the optical observations of R3 carried
out with Aqueye+ at Copernicus and IFI+Iqueye
at Galileo
tablea2.dat 48 9 Observation log of CMO SAI MSU, RTT-150,
CAHA 2.2m, and TNG
tablea3.dat 41 21 AGILE Coverage and MCAL upper limits (ULs)
during the R3 radio bursts
tablea4.dat 66 7 Insight-HXMT observation log
tablea5.dat 64 28 INTEGRAL observation log
tablea6.dat 41 21 INTEGRAL upper limits (ULs)
tablea7.dat 47 15 Swift coverage and flux upper limits
(ULs, 0.3-10keV band)
tablea8.dat 54 63 Insight-HXMT high-energy upper limits (ULs)
for the 6 observed FRBs
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Tel Telescope
7- 16 A10 --- Rec Receiver
18- 21 I4 MHz nuc Central frequency
23- 25 I3 MHz BW Observational bandwidth
27- 32 F6.2 us dt Sampling time
34- 40 F7.2 kHz dv Spectral resolution
42- 49 A8 Jy SEFD System equivalent flux density (1)
51- 53 F3.1 Jy.ms Fnummm Fluence density threshold (S/N=6) (2)
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Note (1): NA is the number of antennas deployed with the uGMRT array.
Note (2): Throughout this work, we refer to the source irradiated energy per
surface unit as the 'fluence', and to the fluence per frequency unit as
the 'fluence density'.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Burst Burst ID (SRT-P-NN or uGMRT-NN)
10- 20 F11.5 d TOA Barycentric time of arrival at infinite
frequency (MJD)
22- 27 F6.4 --- rho Bursts phase
29- 32 F4.1 ms Dt FWHM width {DELTA}t of the burst
34- 36 F3.1 ms e_Dt FWHM width {DELTA}t of the burst error
38- 41 F4.1 Jy S Peak flux density of the burst
43- 45 F3.1 Jy e_S Peak flux density of the burst error
47- 51 F5.1 Jy.ms Fnu Fluence density of the burst
53- 56 F4.1 Jy.ms e_Fnu Fluence density of the burst error
58- 62 F5.2 10+20J E Isotropic energy of the burst (1027erg)
64- 67 F4.2 10+20J e_E Isotropic energy of the burst error (1027erg)
69- 73 F5.1 MHz/ms nu ?=- Linear drift rate of the burst
75- 77 F3.1 MHz/ms e_nu ? Linear drift rate of the burst error
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 20 A20 --- Cam Camera (telescope)
22- 41 A20 --- ObsId Observation ID
45- 67 A23 --- StTime Start Time (topocentric) (UTC)
69- 73 I5 s Exp Exposure time
74 A1 --- New [*] I for radio burst detected
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 22 A22 --- Cam Camera telescope)
24- 42 A19 "datime" StTime Start time (topocentric)
44- 48 F5.2 s Exp Exposure time
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Burst Burst ID
10- 12 A3 --- MCALFoV [YES NO] presence or absence of the source in
the FoV of the onboard detector MCAL
14- 16 A3 --- MCALDA [YES NO] presence or absence of MCAL data
acquisition
18- 20 A3 --- GRIDFoV [YES NO] presence or absence of the source in
the FoV of the onboard detector GRID
22- 28 E7.3 10-7J/cm2 Ul3s ?=- Upper limit fluence at 3σ evaluated
on existing MCAL data acquisitions at the
burst times and correspond to a fluence of
3σ above the background (erg/cm2)
30- 36 E7.3 10-7J/cm2 Uksubms ?=- Upper limit fluence at sub-ms evaluated
on the basis of the data acquisition (if
present); otherwise, they refer to the UL
fluences which would be required to issue a
trigger with the onboard sub-ms MCAL trigger
logic timescale (erg/cm2)
38- 41 A4 --- Note [E.O. I.M.] E.O. for earth occultation,
I.M. idle mode
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Byte-by-byte Description of file: tablea4.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- ObsID Observation ID
13- 31 A19 "datime" StTime Star time (topocentric)
33- 51 A19 "datime" ETime Strop time (topocentric)
53- 56 F4.1 ks LeExp LE exposure time
58- 61 F4.1 ks MeExp ME exposure time
63- 66 F4.1 ks HeExp HE exposure time
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Byte-by-byte Description of file: tablea5.dat
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Bytes Format Units Label Explanations
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1- 16 A16 "datime" StTime Start time (topocentric)
18- 33 A16 "datime" ETime Stop time (topocentric)
35- 59 A25 --- PointID Pointing ID
61- 64 F4.1 ks Exp Exposure time
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Byte-by-byte Description of file: tablea6.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Burst Burst ID
10- 21 I12 --- ScW ID of the Science Window Data catalogue
23- 27 F5.1 deg theta off-axis angle theta
29- 34 F6.1 deg phi off-axis angle rho
36- 41 E6.3 mW/m2 UL INTEGRAL upper limit fluence of the burst
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Byte-by-byte Description of file: tablea7.dat
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Bytes Format Units Label Explanations
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1- 19 A19 "datime" StTime Start time (topocentric)
21- 39 A19 "datime" ETime Stop time (topocentric)
41- 47 E7.3 mW/m2 UL Swift (0.3-10keV band) upper limit fluence
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Byte-by-byte Description of file: tablea8.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Burst Burst ID
10- 23 A14 --- Mod Spectral model (1)
25- 28 I4 s TIl Lower value of time interval
30- 35 F6.1 s TIu Upper value of time interval
38- 40 I3 ms BinTime Bin time
42- 45 F4.1 10-17J/cm2 FluenceUL Upper limit fluence (in 10-10erg/cm2)
47- 50 F4.1 10-17J/cm2 Fluence1-100 ? Upper limit 1-100keV passband fluence
52- 54 F3.1 --- Conf Confidence level (Gaussian 2σ)
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Note (1): Spectral model are:
PL = power-law with photon index Gamma=2
OTTB = optically thin thermal bremsstrahlung
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Acknowledgements:
Matteo Trudu, matteo.trudu(at)inaf.it
(End) Patricia Vannier [CDS] 02-Jul-2023