J/A+A/675/A99 FRBs search with Fermi-LAT (Principe+, 2023)
Hunting for gamma-ray emission from fast radio bursts.
Principe G., Di Venere L., Negro M., Di Lalla N., Omodei N., Di Tria R.,
Mazziotta M.N., Longo F.
<Astron. Astrophys. 675, A99 (2023)>
=2023A&A...675A..99P 2023A&A...675A..99P (SIMBAD/NED BibCode)
ADC_Keywords: Gamma rays ; Radio sources
Keywords: gamma-rays: general
Abstract:
Fast radio bursts (FRBs) are a recently discovered class of GHz-band,
ms-duration, Jy-level-flux astrophysical transients, which origin is
still a mystery. Exploring their gamma-ray counterpart is crucial for
constraining their origin and emission mechanism. Thanks to more than
13 years of gamma-ray data collected by the Fermi-Large Area
Telescope, and to more than 1000 FRB events, one of the largest sample
created as of today, we perform the largest and deepest search for
gamma-ray emission from FRB sources to date. In addition to the study
of individual FRB events on different time-scales (from few seconds up
to several years), we performed, for the first time, a stacking
analysis on the full sample of FRB events as well as a search for
triplet photons in coincidence with the radio event. We do not detect
significant emission, reporting the most stringent constraints, on
short time scales, for the FRB-like emission from SGR 1935+2154 with
E<1041erg, corresponding to a factor <107 with respect to the
emitted radio energy. For the stacked signal of steady emission from
all repeaters, the obtained upper limit (UL) on the FRBs luminosity
(L<1.6x1043erg/s) is more than two orders of magnitudes lower than
those derived from the individual sources. Finally, no individual or
triplet photons have been significantly associated with FRB events. We
derived the LAT ms energy sensitivity to be
E<1047(DL/150Mpc)2erg, ruling out a gamma-ray-to-radio energy
ratio greater than 109 on ms timescales. The results reported here
represent the most stringent UL reported so far on the high-energy
emission from FRBs on short and long time scales, as well as on
cumulative emission and individual photon searches. While the origin
of FRBs is still unclear, our work provides important constraints for
FRB modeling, which might shed light on their emission mechanism.
Description:
We present the results of the FRBs' search with Fermi-LAT on
different time-scales (from few seconds up to several years) as well
as the results of a stacking analysis on the full sample of FRB events
as well as a search for triplet photons in coincidence with the radio
event.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablec1.dat 780 1020 FRB-event sample results
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Note ion tablea1.dat: The values of the parameters of the analysis on events
outside the LAT field of view or with low exposure are set to " ".
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See also:
J/other/PASA/33.45 : FRBCAT: The Fast Radio Burst Catalog (Petroff+, 2016)
J/ApJ/888/40 : Fast radio bursts with AstroSat/CZTI
(Anumarlapudi+, 2020)
J/ApJS/257/59 : First CHIME/FRB FRB Catalog (CHIME/FRB Col.+, 2021)
J/other/Nat/598.267 : List of radio bursts (Li+, 2021)
Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Name FRB name (FRBYYYYMMDD) (Name)
15- 34 F20.16 deg RAdeg Right ascension (J2000) (RA)
36- 56 F21.17 deg DEdeg Declination (J2000) (dec)
58- 76 F19.14 pc/cm3 DM Dispersion measure (DM)
78- 96 F19.17 --- z Redshift (z)
98-117 F20.14 Mpc Dist Luminosity distance (Dist)
119-142 F24.17 Jy Fradio ? Radio flux density at peak time
(Flux_radio)
144-166 F23.16 Jy.ms Flradio ? Radio fluence (Fluence_radio)
168-193 A26 "datime" Time Time in UTC (YYYY-MM-DDThh:mm:ss.ss) (Time)
195-205 F11.6 s Width ? FRB width (Width)
207-228 E22.17 10-7W Lradio ? Radio luminosity (Lum_radio)
230-251 E22.17 10-7J Enradio ? Radio energy (En_radio)
253-275 E23.17 --- TS10s ? Test Statistic (T=10s) (TS_10s) (1)
277-298 E22.17 1/cm2/s Fg10s ? Upper limit (UL) on the gamma-ray flux
(T=10s) (Fluxgamma10s)
300-319 F20.18 mW/m2 EFg10s ? Upper limit (UL) on the gamma-ray energy
flux (T=10s) (Efluxgamma10s)
321-342 E22.17 10-7W Lg10s ? Upper limit (UL) on the gamma-ray
luminosity (T=10s) (Lumgamma10s)
344-365 E22.17 10-7J Eng10s ? Upper limit (UL) on the gamma-ray energy
(T=10s) (Engamma10s)
367-389 E23.17 --- TS100s ? Test Statistic (T=100s) (TS_100s) (1)
391-412 E22.17 1/cm2/s Fg100s ? Upper limit (UL) on the gamma-ray flux
(T=100s) (Fluxgamma100s)
414-434 F21.19 mW/m2 EFg100s ? Upper limit (UL) on the gamma-ray energy
flux (T=100s) (Efluxgamma100s)
436-457 E22.17 10-7W Lg100s ? Upper limit (UL) on the gamma-ray
luminosity (T=100s) (Lumgamma100s)
459-480 E22.17 10-7J Eng100s ? Upper limit (UL) on the gamma-ray energy
(T=100s) (Engamma100s)
482-504 E23.17 --- TS1000s ? Test Statistic (T=1000s) (TS_1000s) (1)
506-527 E22.17 1/cm2/s Fg1000s ? Upper limit (UL) on the gamma-ray flux
(T=1000s) (Fluxgamma1000s)
529-550 F22.20 mW/m2 EFg1000s ? Upper limit (UL) on the gamma-ray energy
flux (T=1000s) (Efluxgamma1000s)
552-573 E22.17 10-7W Lg1000s ? Upper limit (UL) on the gamma-ray
luminosity (T=1000s) (Lumgamma1000s)
575-596 E22.17 10-7J Eng1000s ? Upper limit (UL) on the gamma-ray energy
(T=1000s) (Engamma1000s)
598-620 E23.17 --- TS10000s ? Test Statistic (T=10000s) (TS_10000s) (1)
622-643 E22.17 1/cm2/s Fg10000s ? Upper limit (UL) on the gamma-ray flux
(T=10000s) (Fluxgamma10000s)
645-666 E22.17 mW/m2 EFg10000s ? Upper limit (UL) on the gamma-ray energy
flux (T=10000s) (Efluxgamma10000s)
668-689 E22.17 10-7W Lg10000s ? Upper limit (UL) on the gamma-ray
luminosity (T=10000s) (Lumgamma10000s)
691-712 E22.17 10-7J Eng10000s ? Upper limit (UL) on the gamma-ray energy
(T=10000s) (Engamma10000s)
714-734 F21.16 s DbestTrip ? Delay (since FRB time) of the shortest
duration triplet (Delaybesttriplet)
736-756 E21.16 --- Tripptpval ? P-value of the first triplet after the
FRB event (Tripletposttrialpvalue)
758-780 F23.15 s TripDur ? Interval of time between the first and
third photon of the triplet
(Triplet_duration)
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Note (1): For a conversion of the Test Statistic: the corresponding
significance in sigma units is ~(TS)^1/2 sigma..
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History:
From Giacomo Principe, giacomo.principe(at)ts.infn.it
Acknowledgements:
The effort of the LAT-team Calibration & Analysis Working
Group to develop Pass 8, and also the LAT MMTransient Working Group
for the support given to this project, are gratefully acknowledged. GP
acknowledges the partial support by ICSC - Centro Nazionale di
Ricerca in High Performance Computing, Big Data and Quantum Computing,
funded by European Union - NextGenerationEU. MN acknowledges the
support by NASA under award number 80GSFC21M0002. The Fermi LAT
Collaboration acknowledges generous ongoing support from a number of
agencies and institutes that have supported both the development and
the operation of the LAT as well as scientific data analysis. These
include the National Aeronautics and Space Administration and the
Department of Energy in the United States, the Commissariat a
l'Energie Atomique and the Centre National de la Recherche
Scientifique / Institut National de Physique Nucleaire et de Physique
des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK) and Japan Aerospace
Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg
Foundation, the Swedish Research Council and the Swedish National
Space Board in Sweden. Additional support for science analysis during
the operations phase is gratefully acknowledged from the Istituto
Nazionale di Astrofisica in Italy and the Centre National d'Etudes
Spatiales in France. This work is performed in part under DOE Contract
DE-AC02-76SF00515.
(End) Patricia Vannier [CDS] 23-May-2023