J/ApJS/224/10 The second Konus-Wind short GRB catalog (Svinkin+, 2016)
The second Konus-Wind catalog of short gamma-ray bursts.
Svinkin D.S., Frederiks D.D., Aptekar R.L., Golenetskii S.V.,
Pal'shin V.D., Oleynik P.P., Tsvetkova A.E., Ulanov M.V., Cline T.L.,
Hurley K.
<Astrophys. J. Suppl. Ser., 224, 10 (2016)>
=2016ApJS..224...10S 2016ApJS..224...10S (SIMBAD/NED BibCode)
ADC_Keywords: Gamma rays
Keywords: catalogs; gamma-ray burst: general
Abstract:
In this catalog, we present the results of a systematic study of 295
short gamma-ray bursts (GRBs) detected by Konus-Wind (KW) from 1994 to
2010. From the temporal and spectral analyses of the sample, we
provide the burst durations, the spectral lags, the results of
spectral fits with three model functions, the total energy fluences,
and the peak energy fluxes of the bursts. We discuss evidence found
for an additional power-law spectral component and the presence of
extended emission in a fraction of the KW short GRBs. Finally, we
consider the results obtained in the context of the Type I
(merger-origin)/Type II (collapsar-origin) classifications.
Description:
Between 1994 November and 2010 December, the Konus-Wind spectrometer
(KW; see section 2 for details) detected 1939 GRBs in the triggered
mode, 295 of which were classified as short-duration GRBs or short
bursts with extended emission (EE).
The count rates are recorded in three energy windows G1 (13-50keV), G2
(50-200keV), and G3 (200-760keV) with 2.944s time resolution.
The catalog includes about twice the number of bursts as the first
Konus catalog of short GRBs (Mazets et al. arXiv:astro-ph/0209219).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 55 295 Konus-WIND short GRB observation details
table2.dat 84 295 Durations and classification
table3.dat 128 947 Spectral parameters (multichannel spectra)
table4.dat 83 79 Spectral parameters (three-channel spectra)
table6.dat 63 293 Fluences and Peak Fluxes
table7.dat 132 30 Short GRBs with extended emission (EE)
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See also:
J/ApJS/208/21 : The BATSE 5B GRB spectral catalog (Goldstein+, 2013)
J/ApJS/207/38 : IPN localizations of Konus short GRBs (Pal'shin+, 2013)
J/ApJS/195/2 : The second Swift BAT GRB catalog (BAT2) (Sakamoto+, 2011)
J/PAZh/36/744 : SPI-ACS/INTEGRAL short gamma-ray bursts (Minaev+, 2010)
J/ApJ/609/935 : Gamma-ray burst formation rate (Yonetoku+, 2004)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [GRB]
4- 18 A15 --- ID GRB designation (G1)
20- 31 A12 "h:m:s" Time UT time of the observation
33- 39 A7 --- GRB GRB name (YYMMDDA) (1)
41- 42 A2 --- Det Triggered detector (S1 or S2) (2)
44- 46 I3 deg Ang [0/104] Incident angle (angle between the GRB
direction and the detector axis)
48- 50 I3 deg e_Ang [-92/0]? Lower uncertainty in Ang (3)
52- 53 I2 deg E_Ang [0/83]? Upper uncertainty in Ang
55 I1 --- Loc Location type (4)
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Note (1): The GRB name as provided in the Gamma-ray Coordinates Network
circulars, if available.
Note (2): Konus-Wind (KW) consists of two identical NaI(Tl) detectors S1 and S2,
each with a 2π field of view. The detectors are mounted on
opposite faces of the rotationally stabilized Wind spacecraft, such
that one detector (S1) points toward the south ecliptic pole, thereby
observing the south ecliptic hemisphere, while the other (S2)
observes the north ecliptic hemisphere. Each detector has an effective
area of ∼80-160cm2 depending on the photon energy and incident
angle. The nominal energy range of gamma-ray measurements covers the
incident photon energy interval from 13keV up to 10MeV.
Note (3): The Ang uncertainties correspond to the difference of the
ecliptic latitudes of the box corners or
ecliptic latidude 2σ uncertainties.
Note (4): Location type as follows:
1 = detected by imaging instruments (incident angle error is not given);
2 = localized to a box or segment, localization center is used;
3 = localized to a box or segment, ecliptic latitude estimate is used;
4 = burst localized to a single annulus, point on the annulus center line
which is better consistent with ecliptic latitude estimate is used;
5 = observed by Konus-WIND only, ecliptic latitude estimate is used.
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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- 3 A3 --- --- [GRB]
4- 18 A15 --- ID GRB designation (G1)
20- 25 F6.3 s Ti GRB start time relative to the trigger time
27- 32 F6.3 s T100 [0.01/13.5] GRB duration in the G2+G3 band (5)
34- 38 F5.3 s T50 [0.006/0.6] T50 duration, 25% to 75% total burst
count fluence
40- 44 F5.3 s e_T50 1σ uncertainty in T50
46- 50 F5.3 s T90 [0.01/3.9] T90 duration, 5% to 95% total burst
count fluence
52- 56 F5.3 s e_T90 1σ uncertainty in T90
58- 63 A6 --- Type Burst type (6)
65- 67 I3 10-3s Tlag32 [-49/123]? Spectral lag between G3 (200-760keV)
and G2 (50-200keV) (ms)
69- 70 I2 10-3s e_Tlag32 ? 1σ uncertainty in Tlag32
72- 74 I3 10-3s Tlag31 [-36/277]? Spectral lag between G3 (200-760keV)
and G1 (13-50keV) (ms)
76- 77 I2 10-3s e_Tlag31 ? 1σ uncertainty in Tlag31
79- 81 I3 10-3s Tlag21 [-59/168]? Spectral lag between G2 (50-200keV)
and G1 (13-50keV) (ms)
83- 84 I2 10-3s e_Tlag21 ? 1σ uncertainty in Tlag21
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Note (5): GRB19960325_T69892 and GRB19980614_T31854 have data gaps in
G3 (200-760keV); duration was calculated using the G2 (50-200keV)
light curve only.
Note (6): Burst type, as given in Svinkin et al. (in prep.).
Burst type as follows:
I = merger-origin;
II = collapsar-origin;
I/II = uncertain type;
Iee = type I with extended emission;
Iee/II = type is uncertain, either Iee or II
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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- 3 A3 --- --- [GRB]
4- 18 A15 --- ID GRB designation (G1)
20 A1 --- SpT [ip] Spectrum type (1)
22 I1 --- Best [0/1] Best-fit spectral model flag?
(0=model is not the best-fit spectral model)
24- 28 F5.3 s SpTi Start of the spectrum accumulation interval
30- 34 F5.3 s SpDT [0.06/9.5] Spectrum accumulation time
36- 39 A4 --- Model Spectral model (BAND, CPL or PL)
41- 45 F5.2 --- Alpha [-2.4/3] Low-energy spectral index (2)
47- 51 F5.2 --- e_Alpha [-3.6/-0.03] Lower 90% uncertainty in Alpha
53- 57 F5.2 --- E_Alpha [0.03/11] Upper 90% uncertainty in Alpha
59- 63 F5.2 --- Beta [-4/-1.2]? High-energy spectral index (2)
65- 69 F5.2 --- e_Beta [-9/-0.1]? Lower 90% uncertainty in Beta
71- 74 F4.2 --- E_Beta [0.08/5.6]? Upper 90% uncertainty in Beta
76- 79 I4 keV Ep [40/3550]? EFE spectrum peak energy
81- 85 I5 keV e_Ep [-2754/-7]? Lower 90% uncertainty in Ep
87- 90 I4 keV E_Ep [8/5036]? Upper 90% uncertainty in Ep
92- 97 F6.2 10-9W/m2 Flux [0.1/445] Energy flux in the 10keV-10MeV band
(normalization); 10-6erg/cm2/s
99-104 F6.2 10-9W/m2 e_Flux [-48/-0.03] Lower 90% uncertainty in Flux
106-110 F5.2 10-9W/m2 E_Flux [0.04/47] Upper 90% uncertainty in Flux
112-116 F5.1 --- Chi2 [2/168] Chi-square statistic of the fit
118-119 I2 --- dof [3/99] Number of degrees of freedom
121-128 E8.2 --- Prob [0/1] Null hypothesis probability
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Note (1): Spectrum type as follows:
i = the spectrum is time-integrated and is used to calculate the burst
total energy fluence;
p = the spectrum is measured near the maximum count rate and is used to
calculate the burst energy peak flux.
Note (2): Spectral Index - Alpha was allowed to vary in the (-1.99--+10)
interval in the fits. Beta was allowed to vary in the (-10--+2)
interval in the fits.
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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- 3 A3 --- --- [GRB]
4- 18 A15 --- ID GRB designation (G1)
20- 25 F6.3 s SpTi Start of the spectrum accumulation interval
27- 31 F5.3 s SpDT [0.01/2] Spectrum accumulation time
33- 35 A3 --- Model Spectral model (CPL or PL)
37- 41 F5.2 --- Alpha [-1.4/10] Low-energy spectral index (1)
43- 47 F5.2 --- e_Alpha [-9/0] Lower 90% uncertainty in Alpha
49- 52 F4.2 --- E_Alpha [0.06/10] Upper 90% uncertainty in Alpha
54- 57 I4 keV Ep [138/1910]? EFE spectrum peak energy (2)
59- 63 I5 keV e_Ep [-1540/-16]? Lower 90% uncertainty in Ep
65- 68 I4 keV E_Ep [45/9480]? Upper 90% uncertainty in Ep
70- 73 F4.1 10-9W/m2 Flux [0.3/32.5] Energy flux in the 10keV-10MeV band
(normalization); 10-6erg/cm2/s
75- 78 F4.1 10-9W/m2 e_Flux [-8/-0.1] Lower 90% uncertainty in Flux
80- 83 F4.1 10-9W/m2 E_Flux [0.2/32] Upper 90% uncertainty in Flux
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Note (1): Alpha was allowed to vary in the (-1.99--+10) interval in the fits.
Note (2): Ep was allowed to vary in the (10keV--10MeV) interval in the fits.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [GRB]
4- 18 A15 --- ID GRB designation (G1)
20- 25 F6.2 10-9J/m2 S [0.2/144] Energy fluence (10keV-10MeV);
10-6erg/cm2
27- 31 F5.2 10-9J/m2 e_S [-6/-0.05] Lower 90% uncertainty in S
33- 37 F5.2 10-9J/m2 E_S [0.06/14] Upper 90% uncertainty in S
39- 44 F6.3 s Tpk [-0.5/1] Start time of the 16-ms peak count rate
interval relative to the trigger time
46- 50 F5.2 10-8W/m2 PF [0.2/85.4] Peak energy flux on the 16ms timescale
(10keV-10MeV); 10-5erg/cm2/s
52- 57 F6.2 10-8W/m2 e_PF [-11/-0.1] Lower 90% uncertainty in PF
59- 63 F5.2 10-8W/m2 E_PF [0.1/18] Upper 90% uncertainty in PF
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [GRB]
4- 18 A15 --- ID GRB designation (G1)
20- 25 F6.3 s EETi EE start time relative to the trigger time
27- 33 F7.3 s EEdT [3.7/161] EE duration
35- 39 A5 --- Ch The KW band where EE was detected (1)
41- 47 A7 --- Inst Other instruments which also detected EE
(BAT, BATSE, GBM or SPI-ACS)
49- 54 F6.3 s SpTi ? Start time of the EE spectrum
56- 61 F6.3 s SpDT [8/79]? EE spectrum accumulation time
63- 65 A3 --- Model Best-fit spectral model (CPL or PL)
67- 71 F5.2 --- Alpha [-2.6/-0.2]? Low-energy spectral index
73- 77 F5.2 --- e_Alpha [-1/-0.08]? Lower 90% uncertainty in Alpha
79- 82 F4.2 --- E_Alpha [0.08/2]? Upper 90% uncertainty in Alpha
84- 87 I4 keV Ep [157/2250]? EFE spectrum peak energy
89- 93 I5 keV e_Ep [-1076/-24]? Lower 90% uncertainty in Ep
95- 98 I4 keV E_Ep [39/2418]? Upper 90% uncertainty in Ep
100-104 F5.2 10-9J/m2 S [2.4/80.1]? Energy fluence (10 keV - 10 MeV)
106-111 F6.2 10-9J/m2 e_S [-13/-0.6]? Lower 90% uncertainty in S
113-117 F5.2 10-9J/m2 E_S [0.8/24]? Upper 90% uncertainty in S
119-122 F4.1 --- Chi2 [41/100]? Chi-square statistic of the fit
124-125 I2 --- dof [52/97]? Number of degrees of freedom
127-132 F6.4 --- Prob [0/1]? Null hypothesis probability
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Note (1): The KW energy bands are: G1 (13-50keV), G2 (50-200keV), and
G3 (200-760keV).
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Global notes:
Note (G1): The burst designation in the form "GRBYYYYMMDD_Tsssss," where
YYYYMMDD is the burst date, and sssss is the KW trigger time T0 (UT)
truncated to integer seconds (note that due to Wind's large distance
from Earth, this trigger time can differ by up to ∼7s from the
Earth-crossing time; see Pal'shin et al. 2013, J/ApJS/207/38).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 01-Jul-2016