J/ApJS/175/179 The BAT1 gamma-ray burst catalog (Sakamoto+, 2008)
The first Swift BAT gamma-ray burst catalog.
Sakamoto T., Barthelmy S.D., Barbier L., Cummings J.R., Fenimore E.E.,
Gehrels N., Hullinger D., Krimm H.A., Markwardt C.B., Palmer D.M.,
Parsons A.M., Sato G., Stamatikos M., Tueller J., Ukwatta T.N., Zhang B.
<Astrophys. J. Suppl. Ser., 175, 179-190 (2008)>
=2008ApJS..175..179S 2008ApJS..175..179S
ADC_Keywords: Gamma rays
Mission_Name: Swift
Keywords: gamma rays: bursts
Abstract:
We present the first Swift Burst Alert Telescope (BAT) catalog of
gamma-ray bursts (GRBs), which contains bursts detected by the BAT
between 2004 December 19 and 2007 June 16. This catalog (hereafter the
BAT1 catalog) contains burst trigger time, location, 90% error radius,
duration, fluence, peak flux, and time-averaged spectral parameters
for each of 237 GRBs, as measured by the BAT. The BAT-determined
position reported here is within 1.75' of the Swift X-Ray Telescope
(XRT)-determined position for 90% of these GRBs. The BAT T90 and T50
durations peak at 80 and 20s, respectively. From the fluence-fluence
correlation, we conclude that about 60% of the observed peak energies,
Eobspeak, of BAT GRBs could be less than 100keV. We confirm that
GRB fluence to hardness and GRB peak flux to hardness are correlated
for BAT bursts in analogous ways to previous missions' results. The
correlation between the photon index in a simple power-law model and
Eobspeak is also confirmed. We also report the current status for
the on-orbit BAT calibrations based on observations of the Crab
Nebula.
Description:
The BAT is a highly sensitive, large field of view (FOV) (1.4sr for
>50% coded FOV and 2.2sr for >10% coded FOV), coded-aperture telescope
that detects and localizes GRBs in real time. The fast and accurate
BAT GRB positions with 1'-3' error radii are the key to autonomously
slewing the spacecraft to point the XRT and the the Swift UV/Optical
Telescope (UVOT).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 131 237 BAT GRB summary
table2.dat 95 237 BAT GRB energy fluence
table3.dat 84 237 BAT GRB 1-s peak photon flux
table4.dat 80 237 BAT GRB 1-s peak energy flux
table5.dat 84 237 BAT time-averaged spectral parameters
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See also:
IX/36 : GRANAT/PHEBUS catalog of cosmic gamma-ray bursts (Terekhov+, 1994-2003)
IX/20 : The Fourth BATSE Burst Revised Catalog (Paciesas+ 1999)
J/A+A/438/1175 : First INTEGRAL SPI-ACS Gamma-Ray Burst Catalogue (Rau+, 2005)
J/ApJ/616/1072 : The GUSBAD catalog of gamma-ray bursts (Schmidt+, 2004)
J/A+AS/129/1 : GRANAT/WATCH catalogue of gamma-ray bursts (Sazonov+ 1998)
J/ApJ/446/115 : Gamma ray burst localizations (Vrba+ 1995)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- GRB GRB name (YYMMDDA)
9- 14 I6 --- Trigger Trigger number
16- 38 A23 --- TriggerTime Trigger time in the UTC time (1)
40- 46 F7.3 deg RAdeg Right Ascension in decimal degrees (J2000)
48- 54 F7.3 deg DEdeg Declination in decimal degrees (J2000)
56- 60 F5.1 --- SNR ? Signal-to-noise ratio
62- 64 F3.1 arcmin ePos 90% error radius
66- 72 F7.3 s T90 ? Burst duration with 5-95% of fluence
74- 80 F7.3 s T50 ? Burst duration with 25-75% of fluence
82- 87 F6.1 s Start ? Burst start time from BAT trigger
89- 93 F5.1 s Stop ? Burst stop time from BAT trigger
95-131 A37 --- Com Comment (2)
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Note (1): In YYYY-MM-DD hh:mm:ss.fff format (millisecond accuracy).
Note (2): The comment includes number with the meaning:
1 = The event data are not available during this very early phase of
operations.
2 = battblocks failed because of the weak short nature of the burst.
3 = The event data of the last part of the burst emission are not available
due to the downlink problem.
4 = The event data of the brightest part of the burst emission are not
available due to the entering to the SAA.
5 = The burst duration was longer than the period of the event data.
6 = Markwardt et al. (2005, GCN Circ. 4037)
7 = The time interval calculated by the BAT flight software was used to
create the image.
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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- 7 A7 --- GRB GRB name (YYMMDDA)
9 A1 --- f_GRB [1] if S100-150 is an upper limit
11- 13 A3 --- Mod ? Best fit model name (G1)
15- 20 F6.2 fJ/cm2 S15-25 ? Energy fluence in 15-25keV (1)
22- 26 F5.2 fJ/cm2 e_S15-25 ? 90% error in S15-25 (1)
28- 32 F5.1 fJ/cm2 S25-50 ? Energy fluence in 25-50keV (1)
34- 37 F4.1 fJ/cm2 e_S25-50 ? 90% error in S25-50 (1)
39- 45 F7.2 fJ/cm2 S50-100 ? Energy fluence in 50-100keV (1)
47- 51 F5.2 fJ/cm2 e_S50-100 ? 90% error in S50-100 (1)
53- 59 F7.2 fJ/cm2 S100-150 ? Energy fluence in 100-150keV (1)
61- 65 F5.2 fJ/cm2 e_S100-150 ? 90% error in S100-150 (1)
67- 72 F6.1 fJ/cm2 S15-150 ? Energy fluence in 15-150keV (1)
74- 77 F4.1 fJ/cm2 e_S15-150 ? 90% error in S15-150 (1)
79- 86 F8.3 s S.start ? Start time used to calculate the fluence
88- 95 F8.3 s S.stop ? Stop time used to calculate the fluence
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Note (1): In units of 10-8erg/cm2 (10-11J/m2)
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- GRB GRB name (YYMMDDA)
9 A1 --- f.p [12] Flag on GRB 1-s peak photon fluxes (1)
12- 14 A3 --- Mod.p ? Best fit model name (G1)
16- 20 F5.2 ph/cm2/s p15-25 ? 1-s peak photon flux in 15-25keV
22- 25 F4.2 ph/cm2/s e_p15-25 ? 90% error in Pph15-25
27- 31 F5.2 ph/cm2/s p25-50 ? 1-s peak photon flux in 25-50keV
33- 36 F4.2 ph/cm2/s e_p25-50 ? 90% error in Pph25-50
38- 42 F5.2 ph/cm2/s p50-100 ? 1-s peak photon flux in 50-100keV
44- 47 F4.2 ph/cm2/s e_p50-100 ? 90% error in Pph50-100
49- 53 F5.3 ph/cm2/s p100-150 ? 1-s peak photon flux in 100-150keV
55- 59 F5.3 ph/cm2/s e_p100-150 ? 90% error in Pph100-150
61- 65 F5.2 ph/cm2/s p15-150 ? 1-s peak photon flux in 15-150keV
67- 70 F4.2 ph/cm2/s e_p15-150 ? 90% error in Pph15-150
72- 77 F6.1 s p.start ? Start time used for peak photon flux
79- 84 F6.1 s p.stop ? Stop time used for peak photon flux
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Note (1): Flag as follows:
1 = The signal-to-noise ratio of the peak spectrum is too low to perform
a spectral fit.
2 = Upper limit for Pph15-25.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- GRB GRB name (YYMMDDA)
9 A1 --- f.E [1234] Flag on 1-s peak energy flux (1)
12- 14 A3 --- Mod.E ? Best fit model for 1-s peak energy (G1)
16- 20 F5.2 fW/cm2 E15-25 ? 1-s peak energy flux in 15-25keV (2)
22- 25 F4.2 fW/cm2 e_E15-25 ? 90% error in P15-25
27- 30 F4.1 fW/cm2 E25-50 ? 1-s peak energy flux in 25-50keV (2)
32- 34 F3.1 fW/cm2 e_E25-50 ? 90% error in P25-50
36- 40 F5.1 fW/cm2 E50-100 ? 1-s peak energy flux in 50-100keV (2)
42- 44 F3.1 fW/cm2 e_E50-100 ? 90% error in P50-100
46- 50 F5.2 fW/cm2 E100-150 ? 1-s peak energy flux in 100-150keV (2)
52- 55 F4.2 fW/cm2 e_E100-150 ? 90% error in P100-150
57- 61 F5.1 fW/cm2 E15-150 ? 1-s peak energy flux in 15-150keV (2)
63- 66 F4.1 fW/cm2 e_E15-150 ? 90% error in P15-150
68- 73 F6.1 s E.start ? Start time used for peak energy flux
75- 80 F6.1 s E.stop ? Stop time used for peak energy flux
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Note (1): Flag as follows:
1 = The signal-to-noise ratio of the peak spectrum is too low to perform
a spectral fit.
2 = Upper limit for P15-25
3 = Upper limit for P100-150
4 = Upper limit for P50-100 and P100-150.
Note (2): unit is 10-8erg/cm2/s (10-11W/m2)
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- GRB GRB name (YYMMDDA)
9- 13 F5.2 --- alpha ? Power-law photon index for the
simple power-law model (PL) (G1)
15- 18 F4.2 --- e_alpha ? 90% error in AlphaPL
20- 25 F6.1 ph/cm2/s/keV K(50) ? PL Normalization at 50 keV
27- 30 F4.1 ph/cm2/s/keV e_K(50) ? 90% error in K50PL
32- 36 F5.1 --- chi2 ? PL χ2 (57 dof)
38- 41 F4.1 --- alpha1 ? Power-law photon index for the
cutoff power-law model (CPL) (G1)
43- 45 F3.1 --- e_alpha1 ? 90% lower level in alpha1
47- 50 F4.1 --- E_alpha1 ? 90% upper level in alpha1
52- 54 I3 keV Ep ? Ep parameter in model (G1)
56- 57 I2 keV e_Ep ? 90% lower level in Ep
59- 62 I4 keV E_Ep ? 90% upper level in Ep
64- 67 I4 ph/cm2/s/keV K1(50) ? CPL Normalization at 50keV
69- 72 I4 ph/cm2/s/keV e_K1(50) ? 90% lower level in K50CPL
74- 79 I6 ph/cm2/s/keV E_K1(50) ? 90% upper level in K50CPL
81- 84 F4.1 --- chi.1 ? CPL χ2 (56 dof)
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Global Notes:
Note (G1): The models are:
PL = simple power-law: f(E){prot.to}Eα
CPL = cuf-off power-law: f(E){prot.to}Eα.exp(-(2+α)E/Ep)
History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 12-Jun-2009