J/other/PASA/33.45 FRBCAT: The Fast Radio Burst (FRB) Catalog (Petroff+, 2016)
FRBCAT: The Fast Radio Burst Catalogue
Petroff E., Barr E.D., Jameson A., Keane E.F., Bailes M., Kramer M.,
Morello V., Tabbara D., van Straten W.
<Publ. Astron. Soc. Australia, 33, 45 (2016)>
=2016PASA...33...45P 2016PASA...33...45P (SIMBAD/NED BibCode)
ADC_Keywords: Radio sources; Fundamental catalog
Keywords: catalogs; methods: data analysis; telescopes;
Astrophysics - High Energy Astrophysical Phenomena
Abstract:
Here, we present a catalogue of known Fast Radio Burst sources in the
form of an online catalogue, FRBCAT. The catalogue includes
information about the instrumentation used for the observations for
each detected burst, the measured quantities from each observation,
and model-dependent quantities derived from observed quantities. To
aid in consistent comparisons of burst properties such as width and
signal-to-noise ratios, we have re-processed all the bursts for which
we have access to the raw data, with software which we make available.
The originally derived properties are also listed for comparison.
Description:
This catalogue contains the population of fast radio bursts (FRBs)
published up to July 2020.
Default values for cosmological parameters are:
ΩM=0.286, Ωvac=0.714, and H0=69.6
Acknowledging FRBCAT in publications:
You may use the data presented in this catalogue for publications;
however, we ask that you cite this paper (Petroff et al., 2016) and
provide the url (http://www.frbcat.org/).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
frbcat.dat 438 118 FRB Catalogue (FRBCAT) - up to July 2020
(not maintained anymore)
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See also:
J/ApJ/846/44 : Luminous persistent sources in nearby galaxies (Ofek, 2017)
J/ApJ/888/40 : Fast radio bursts with AstroSat/CZTI (Anumarlapudi+, 2020)
http://www.frbcat.org/ : Online FRB Catalogue (no longer updated)
http://www.wis-tns.org/ : Transient Name Server (contains up to date FRBs)
Byte-by-byte Description of file: frbcat.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Name FRB name
20- 29 A10 "Y/M/D" Obs.date Date of observation (UTC)
31- 32 I2 h Obs.h Hour of observation (UTC)
33 A1 --- --- [:]
34- 35 I2 min Obs.m Minute of observation (UTC)
36 A1 --- --- [:]
37- 42 F6.3 s Obs.s Second of observation (UTC)
44- 52 A9 --- Tel Telescope used to take the observation (1)
54- 62 A9 --- Receiver Receiver system on the telescope (2)
64- 81 A18 --- Backend Data recording system used for
the observation (3)
83- 85 I3 --- Beam [1/212]? Telescope beam number in which
the FRB was detected (4)
87- 93 F7.3 arcmin amaj [0.002/270]? Beam semi-major axis
95- 101 F7.4 arcmin bmin [0.0006/40]? Beam semi-minor axis
103- 105 I3 deg Rangle [0/120]? Beam rotation angle
107- 108 I2 h RAh Hour of right ascension (J2000)
110- 111 I2 min RAm Minute of right ascension (J2000)
113- 118 F6.3 s RAs ? Second of right ascension (J2000)
120 A1 --- DE- Sign of declination (J2000)
121- 122 I2 deg DEd Degree of declination (J2000)
124- 125 I2 arcmin DEm Arcminute of declination (J2000)
127- 132 F6.3 arcsec DEs ? Arcsecond of declination (J2000)
134- 143 F10.6 deg GLON Galactic longitude of the best estimate
of the FRB position
145- 154 F10.6 deg GLAT [-66.6/89.5] Galactic latitude of the
best estimate of the FRB position
156- 165 F10.6 ms Stime [0.06/100]? Sampling time
167- 174 F8.3 MHz Band [2.5/1024] Observing bandwidth
176- 181 F6.1 MHz Freq0 [111/1411] The centre frequency of
the observation
183 I1 --- Npol [1/2]? Number of polarisations used
to record the total signal
185 I1 --- Bits [1/8]? Bits per sample
187- 192 F6.3 K/Jy Gain [0.029/10]? The telescope gain
194- 199 F6.2 K Tsys [1/400]? The receiver system temperature
201- 206 F6.2 --- DMgal [13/523] DMgalaxy (5)
208- 242 A35 --- Model Galactic electron model
244- 251 F8.3 cm-3.pc DM [103.5/2596.1] Measured dispersion measure
of the FRB (6)
253- 258 F6.3 cm-3.pc e_DM [0.002/14]? DM uncertainty
260- 267 F8.3 ms Width [0.08/5000] Measured width of the FRB
269- 274 F6.2 --- S/N [0/411] Signal-to-noise ratio of the burst
276- 282 F7.3 Jy Speak [0.039/161]? The observed peak flux
density of the burst (7)
284- 288 F5.3 --- DMInd [1.99/2.02]? DM index of the burst,
α (8)
290- 294 F5.3 --- e_DMInd [0.001/0.03]? DMInd uncertainty
296- 300 F5.2 --- ScInd [-5.86/-3.5]? Scattering index (9)
302- 305 F4.2 --- e_ScInd [0.4/1.98]? ScInd uncertainty
307- 313 F7.4 --- Sc [0.004/29.1]? Scattering
315- 320 F6.4 --- e_Sc [0.002/6]? Sc uncertainty
322- 379 A58 --- ScMod Scattering model
381- 386 F6.4 --- Pol [0/1.01]? Linear polarisation fraction (10)
388- 393 F6.4 --- e_Pol [0.0006/0.15]? Pol uncertainty
395- 401 F7.4 --- cPol [0/30]? Circular polarisation fraction (11)
403- 409 F7.4 --- e_cPol [0.0005/30]? cPol uncertainty
411- 414 F4.1 --- SpInd [-7/8.8]? Spectral index
416- 418 F3.1 --- e_SpInd [1.9/2]? SpInd uncertainty
420- 425 F6.1 rad/m2 RM [-499.8/474]? Rotation measure
427- 430 F4.1 rad/m2 e_RM [0.6/52]? RM uncertainty
432- 438 F7.5 --- zHost [0.03/0.7]? Redshift of host galaxy
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Note (1): Telescope as follows:
ASKAP = The Australian Square Kilometre Array Pathfinder (32 occurrences)
CHIME/FRB = The Canadian Hydrogen Intensity Mapping Experiment
(30 occurrences) - see http://chime-experiment.ca/
Parkes = The Parkes radio telescope (28 occurrences)
Pushchino = The Pushchino Radio Astronomy Observatory (11 occurrences) - see
http://www.frb.su/catalogue-prao-frb
UTMOST = The Molonglo Radio Telescope (9 occurrences) - see
http://astronomy.swin.edu.au/research/utmost/
GBT = The Green Bank telescopes (2 occurrences)
arecibo = The Arecibo telescope (2 occurrences)
VLA = The Very Large Array radio telescope (1 occurrence)
FAST = The Five-hundred-meter Aperture Spherical radio Telescope
(1 occurrence)
DSA-10 = The Deep Synoptic Array ten-antenna prototype (1 occurrence)
Apertif = The Apertif Radio Transient System (ARTS) for the Westerbork
Synthesis Radio Telescope (WSRT) (1 occurrence)
Note (2): At Parkes, the primary instrument is the 13-beam multibeam receiver
(MB20), at Arecibo the 7-beam ALFA receiver, and at the GBT the 800MHz
receiver.
Note (3): At Parkes, two primary data recording systems have been used:
the analogue filterbank (AFB) and Berkeley Parkes Swinburne Recorder
(BPSR; Keith+ 2010MNRAS.409..619K 2010MNRAS.409..619K). The Mock spectrometers and
the GUPPI backends have been used at Arecibo and the GBT, respectively.
Note (4): For FRBs detected with single-pixel feeds, this value is set to 1.
For detections with an interferometer, this may be the number
designation of the tied-array beam or fan beam.
Note (5): The modelled contribution to the FRB DM by the electrons in the
Galaxy. The Galactic DM contribution is derived using the NE2001
Galactic electron density model (Cordes & Lazio 2002astro.ph..7156C 2002astro.ph..7156C)
and should be taken as an estimate as the free electron content of the
Galactic halo is not well constrained (Dolag+ 2015MNRAS.451.4277D 2015MNRAS.451.4277D).
Note (6): The integrated electron column density along the line-of-sight to
the burst obtained either with a pulse fitting algorithm or by the
search code. For bursts with a published DM produced with a detailed
fitting code such as the one described in Thornton+ (2013Sci...341...53T 2013Sci...341...53T),
this DM is used throughout the re-analysis.
Note (7): The observed peak flux density of the burst is calculated
via the single pulse radiometre equation
(Cordes & McLaughlin 2003ApJ...596.1142C 2003ApJ...596.1142C). Note that this flux density
is derived from observed values and is not necessarily the true peak
flux density that would be measured if the burst occurred at beam
centre or was perfectly localised; this value should be taken as a
lower limit on the true flux density.
Note (8): The DM index of the burst α such that DM∝ν-α
obtained with a pulse fitting algorithm. The DM index for the
propagation of waves through a cold plasma is α=2.
Note (9): The evolution of pulse width as a function of frequency due to
scattering such that W∝ν-β obtained with a pulse fitting
algorithm. The index for the propagation of radio waves through an
inhomogeneous turbulent medium is β=4.
Note (10): If polarised data were recorded for the FRB, the fractional linear
polarisation is reported with errors. The total linear polarisation is
the quadrature sum of Stokes Q and U such that (Q2+U2)^0.5/I.
Note (11): If polarised data were recorded for the FRB, the fractional circular
polarisation is reported with errors. The total absolute value of
circular polarisation is given by |V|/I.
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History:
Downloaded from http://www.frbcat.org/ on 2021 Dec 01.
(End) Emmanuelle Perret [CDS] 18-Nov-2021