J/ApJ/850/161 Konus-Wind cat. of GRBs with redshifts. I. (Tsvetkova+, 2017)
The Konus-Wind catalog of gamma-ray bursts with known redshifts.
I. Bursts detected in the triggered mode.
Tsvetkova A., Frederiks D., Golenetskii S., Lysenko A., Oleynik P.,
Pal'shin V., Svinkin D., Ulanov M., Cline T., Hurley K., Aptekar R.
<Astrophys. J., 850, 161 (2017)>
=2017ApJ...850..161T 2017ApJ...850..161T
ADC_Keywords: GRB; Redshifts
Keywords: catalogs ; gamma-ray burst: general ; methods: data analysis
Abstract:
In this catalog, we present the results of a systematic study of
gamma-ray bursts (GRBs) with reliable redshift estimates detected in
the triggered mode of the Konus-Wind (KW) experiment during the period
from 1997 February to 2016 June. The sample consists of 150 GRBs
(including 12 short/hard bursts) and represents the largest set of
cosmological GRBs studied to date over a broad energy band. From the
temporal and spectral analyses of the sample, we provide the burst
durations, the spectral lags, the results of spectral fits with two
model functions, the total energy fluences, and the peak energy
fluxes. Based on the GRB redshifts, which span the range 0.1≤z≤5, we
estimate the rest-frame, isotropic-equivalent energy, and peak
luminosity. For 32 GRBs with reasonably constrained jet breaks, we
provide the collimation- corrected values of the energetics. We
consider the behavior of the rest-frame GRB parameters in the
hardness-duration and hardness-intensity planes, and confirm the
"Amati" and "Yonetoku" relations for Type II GRBs. The correction for
the jet collimation does not improve these correlations for the KW
sample. We discuss the influence of instrumental selection effects on
the GRB parameter distributions and estimate the KW GRB detection
horizon, which extends to z∼16.6, stressing the importance of GRBs as
probes of the early universe. Accounting for the instrumental bias, we
estimate the KW GRB luminosity evolution, luminosity and
isotropic-energy functions, and the evolution of the GRB formation
rate, which are in general agreement with those obtained in previous
studies.
Description:
Here, we present a complete sample of 150 gamma-ray bursts (GRBs) with
reliably measured redshifts that triggered the Konus-Wind (KW; 13keV
to 10MeV range) from 1997 February to 2016 June.
The KW bursts observed in the waiting mode will be presented in a
forthcoming catalog (A. Tsvetkova et al. 2017, in preparation).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 92 150 General information
table2.dat 145 150 Durations and spectral lags
table3.dat 127 513 Spectral parameters
table4.dat 178 150 Burst energetics
table5.dat 92 41 Collimation-corrected parameters
refs.dat 152 182 References
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See also:
J/A+A/427/87 : List of GRBs (Gorosabel+, 2004)
J/ApJ/609/935 : Gamma-ray burst formation rate (Yonetoku+, 2004)
J/ApJS/175/179 : The BAT1 gamma-ray burst catalog (Sakamoto+, 2008)
J/ApJS/180/192 : BeppoSAX/GRBM γ-ray Burst Catalog (Frontera+, 2009)
J/ApJ/701/824 : Afterglows of short and long-duration GRBs (Nysewander+, 2009)
J/ApJ/704/1405 : Testing the Epeak-Eiso relation for GRBs (Krimm+, 2009)
J/A+A/535/A57 : g'r'i'z'JH light curves of GRB 091127 (Filgas+, 2011)
J/ApJ/731/103 : Redshift catalog for Swift long GRBs (Xiao+, 2011)
J/ApJS/195/2 : The second Swift BAT GRB catalog (BAT2) (Sakamoto+, 2011)
J/ApJ/746/170 : Follow-up resources for high-redshift GRBs (Morgan+, 2012)
J/ApJS/208/21 : The BATSE 5B GRB spectral catalog (Goldstein+, 2013)
J/A+A/557/A100 : Fermi and Swift GRBs Epeak-Eiso relation (Heussaff+, 2013)
J/ApJS/207/38 : IPN localizations of Konus short GRBs (Pal'shin+, 2013)
J/ApJS/207/39 : IPN supplement to the Fermi GBM (Hurley+, 2013)
J/ApJS/209/20 : Swift GRB catalog with X-ray data (Grupe+, 2013)
J/ApJ/778/128 : GRB-host galaxies photometry (Perley+, 2013)
J/ApJS/211/13 : The second Fermi/GBM GRB catalog (4yr) (von Kienlin+, 2014)
J/A+A/581/A125 : UV/Optical/NIR spectroscopy GRB hosts (Kruehler+, 2015)
J/A+A/582/A111 : List of 389 GRBs (Li+, 2015)
J/A+A/584/A48 : New redshifts of 357 GBBs (Horvath+, 2015)
J/ApJ/806/52 : 8 Fermi GRB afterglows follow-up (Singer+, 2015)
J/ApJ/807/76 : 373 GRBs between 0.008<z<6.7 (Li+, 2015)
J/ApJ/811/93 : Fermi/GBM GRB minimum timescales (Golkhou+, 2015)
J/ApJS/224/10 : The second Konus-Wind short GRB catalog (Svinkin+, 2016)
J/ApJS/224/20 : 10yr of Swift/XRT obs. of GRBs (Yi+, 2016)
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- 10 A7 --- GRB Gamma-ray burst identifier (YYMMDDA)
12- 13 I2 h Trig.h Hour of KW trigger time
15- 16 I2 min Trig.m Minute of KW trigger time
18- 23 F6.3 s Trig.s Second of KW trigger time
25- 26 I2 h Geo.h Hour of the geocenter time (1)
28- 29 I2 min Geo.m Minute of the geocenter time (1)
31- 36 F6.3 s Geo.s Second of the geocenter time (1)
38- 39 A2 --- Type Burst classification (2)
41- 54 A14 --- Inst Mission/instrument (3)
56- 58 I3 --- r_Inst [1/158] Reference for Inst (see refs.dat file)
60- 64 A5 --- OObs Other observations (4)
66- 67 A2 --- Det KW triggered detector
69- 73 F5.1 deg Angle [4.8/102.4] Incident angle between the GRB
direction and the detector axis
75- 81 F7.5 --- z [0.09/5] Redshift
83 A1 --- n_z [sp] Redshift type (s: spectroscopic or
p: photometric)
85- 87 I3 --- r_z [2/159] Reference for z (see refs.dat file)
89- 92 A4 --- f_z Flag(s) on z (5)
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Note (1): Corrected for the burst front propagation from Wind to the
Earth center.
Note (2): Burst classification as follows:
I = GRBs are the merger-origin, typically short/hard bursts;
II = GRBs are the collapsar-origin, typically long/soft GRBs.
Note (3): That provided the most accurate GRB localization from
prompt emission observations.
Note (4): Other instrument as follows:
1 = CGRO-BATSE;
2 = HETE-2;
3 = BeppoSAX-GRBM;
4 = Swift-BAT;
5 = Fermi-GBM;
6 = Fermi-LAT.
Note (5): Flag as follows:
1 = "Dark" burst according to the classification presented in the
redshift reference paper;
2 = "Dark" burst according to Fynbo et al. (2009ApJS..185..526F 2009ApJS..185..526F);
3 = Although this burst is referred to as GRB 020819 in all related GCN
circulars and in some other publications, this is the second GRB
observed by KW on 2002 August 19;
4 = This burst was initially referred to as GRB 050820, but, after the
detection of GRB 050820B on the same day, it was renamed to GRB 050820A;
5 = The redshift at 95% confidence level is z=2.77+0.15-0.20;
6 = Although GRB 060121 is a short-duration burst, it was classified as
Type II (see e.g. Zhang+ (2009ApJ...703.1696Z 2009ApJ...703.1696Z) or
Svinkin (2016, J/ApJS/224/10) for details);
7 = The redshift study of GRB 060121 (de Ugarte Postigo+ 2006ApJ...648L..83D 2006ApJ...648L..83D)
revealed two probability peaks. The main one (with a 63% likelihood)
places the burst at z=4.6±0.5. A secondary peak (with a 35%
likelihood) would imply that the afterglow lies at z=1.7±0.4;
8 = The type of GRB 060614 is uncertain: a SN-less, long-duration burst
(Gehrels+ 2006Natur.444.1044G 2006Natur.444.1044G ; Gal-Yam+ 2006Natur.444.1053G 2006Natur.444.1053G ;
Fynbo+ 2006Natur.444.1047F 2006Natur.444.1047F ; Della Valle+ 2006Natur.444.1050D 2006Natur.444.1050D) is
suggested to be a Type I burst based on its host galaxy low specific
star-forming rate (Zhang+ 2009ApJ...703.1696Z 2009ApJ...703.1696Z), while in the KW data this
GRB was classified as a Type II burst based on duration and hardness only
(see Svinkin+ 2016, J/ApJS/224/10 for details);
9 = This burst is a short burst with extended emission (EE) according to
Sakamoto+ (2011, J/ApJS/195/2) and Svinkin+ (2016, J/ApJS/224/10);
10 = The 95% confidence redshift range is 1.37<z<2.20;
11 = The redshift at the 2σ confidence level is z=4.35±0.15;
12 = A rather wide 95% confidence range 1.14<z<2.34 is reported
for this estimate;
13 = Since there is an ambiguity with the host galaxy identification, this
redshift may not correspond to the burst. See text (Section 3)
for details;
14 = Although this GRB cannot be unambiguously assigned to the Type I
population, we classify it as Type I. See text (Section 3) for details.
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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- 10 A7 --- GRB Gamma-ray burst identifier (YYMMDDA)
12- 19 F8.3 s t0 [-265.3/260.7] Start time of T100
21- 27 F7.3 s T100 [0.1/485] Total burst duration
29- 36 F8.3 s t5 [-241.7/188]? Start time of T90
38- 43 F6.3 s e_t5 [0/73]? The 1σ uncertainty in t5
45- 51 F7.3 s T90 [0/441]? Time interval containing 5% - 95% of
total burst fluence
53- 58 F6.3 s e_T90 [0/76.6]? The 1σ uncertainty in T90
60- 66 F7.3 s t25 [-56/190.3]? Start time of T50
68- 73 F6.3 s e_t25 [0/39.2]? The 1σ uncertainty in t25
75- 81 F7.3 s T50 [0/167.3]? Time interval containing 25%-75% of
total burst fluence
83- 88 F6.3 s e_T50 [0/39.3]? The 1σ uncertainty in T50
90- 97 F8.5 s tlagG2G1 [-0.2/2.5]? Spectral lag between G2 and G1 KW
energy channels (6)
99-106 F8.5 s e_tlagG2G1 [0/1.2]? The 1σ uncertainty in tlagG2G1
108-115 F8.5 s tlagG3G1 [0/5.2]? Spectral lag between G3 and G1 KW
energy channels (6)
117-124 F8.5 s e_tlagG3G1 [0/1.1]? The 1σ uncertainty in tlagG3G1
126-133 F8.5 s tlagG3G2 [-0.3/0.8]? Spectral lag between G3 and G2 KW
energy channels (6)
135-142 F8.5 s e_tlagG3G2 [0/0.4]? The 1σ uncertainty in tlagG3G2
144-145 A2 --- Comm Additional comments (7)
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Note (6): A positive spectral lag corresponds to the delay of the
softer emission.
Note (7):
1 = This GRB overlaps a solar flare at ∼T0 + 130s;
2 = Since GRB 081203A was detected during the GRB 081203B data transmission,
there are no light curve data available for this GRB. The T100
duration was determined based on the spectral data with a coarse time
resolution of ∼8s. Accordingly, for this GRB, only the lower limits
on Fp and Liso can be estimated from the KW data;
3 = Since the T100 duration of GRB 120624B exceeds the trigger time
history length, all temporal parameters of this burst were determined
based on the waiting mode time history, i.e. with a coarse time
resolution of ∼3s.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 A3 --- --- [GRB]
4- 10 A7 --- GRB Gamma-ray burst identifier (YYMMDDA)
12 A1 --- SType Spectrum type (1)
14- 20 F7.3 s tstart [-0.3/326.2] Spectrum start time;
relative to T0
22- 28 F7.3 s DeltaT [0.06/371] Spectrum accumulation time
30- 33 A4 --- SMod Spectral model ("CPL"=cutoff power-law,
"Band"=Band et al. 1993ApJ...413..281B 1993ApJ...413..281B or
"PL")
35- 37 A3 --- f_SMod Flag on SMod (0: non-BEST model
or 1: BEST model)
39- 43 F5.2 --- alpha [-2/0.6] Low-energy photon index
45- 48 F4.2 --- e_alpha [0.01/0.9] Lower 1σ uncertainty in alpha
50- 53 F4.2 --- E_alpha [0.01/2.3] Upper 1σ uncertainty in alpha
55 I1 --- l_beta [0/1]? Limit flag on beta (2)
57- 61 F5.2 --- beta [-5/0]? High-energy photon index
63- 66 F4.2 --- e_beta [0/8.2]? Lower 1σ uncertainty in beta
68- 71 F4.2 --- E_beta [0/1.5]? Upper 1σ uncertainty in beta
73- 76 I4 keV Ep [0/4787]? EFE spectrum peak energy
78- 81 I4 keV e_Ep [0/1197]? Lower 1σ uncertainty in Ep
83- 85 I3 keV E_Ep [0/949]? Upper 1σ uncertainty in Ep
87- 92 F6.2 10-9W/m2 F [0.07/749.8] Spectral model normalization
94- 98 F5.2 10-9W/m2 e_F [0.01/19.7] Lower 1σ uncertainty in F
100-104 F5.2 10-9W/m2 E_F [0.01/19.7] Upper 1σ uncertainty in F
106-110 F5.1 --- chi2 [0/800.3]? Chi-square statistic of the fit
112-114 I3 --- DoF [0/103]? Number of degrees of freedom
116 I1 --- l_P [0/1]? Limit flag on P (2)
118-124 F7.4 --- P [0/1.0]? Null hypothesis probability
(no correlation exists)
127 I1 --- Comm ? Comment on the fits (3)
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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): Limit flag as follows:
0 = the best fit value;
1 = the upper limit;
Blank = inapplicable (there is no high-energy photon index in the model).
Note (3): Comment as follows:
1 = 3-channel fit (see Section 4.2.2);
2 = Modeling the 3-channel spectrum for the interval from T0-33.734 s
to T0+5.296 s yields the CPL model parameters which are in agreement
with the provided multichannel fit ones;
3 = 3-channel fit (see Section 4.2.2);
4 = The energy channels above 2 MeV are strongly affected by the high
and variable solar particle background, the spectral fits were
performed up to 2 MeV.
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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- 10 A7 --- GRB Gamma-ray burst identifier (YYMMDDA)
12- 15 F4.2 --- z [0.1/5] Redshift
17- 24 F8.3 10-9J/m2 S [1.1/2863] Energy fluence; 1e-6 erg/s
26- 31 F6.3 10-9J/m2 e_S [0.05/30] Lower 1σ uncertainty in S
33- 38 F6.3 10-9J/m2 E_S [0.06/30] Upper 1σ uncertainty in S
40- 46 F7.3 s Tp1024 [-0.5/367.2] Start time of interval when PCR
on 1024ms time scale reached
48- 48 I1 --- f_Tp1024 ? Flag on Tp1024 (8)
50- 56 F7.3 10-9W/m2 Fp1024 [0.3/509] Peak energy flux from 1024ms
time scale; 1e-6erg/cm2/s
58- 63 F6.3 10-9W/m2 e_Fp1024 [0.04/11] Lower 1σ uncertainty in Fp1024
65- 70 F6.3 10-9W/m2 E_Fp1024 [0.06/11] Upper 1σ uncertainty in Fp1024
72- 78 F7.3 s Tp64 [-0.5/367.2] Start time of interval when PCR
on 64ms time scale reached
80- 86 F7.3 10-9W/m2 Fp64 [0.3/902] Peak energy flux from 64ms
time scale; 1e-6erg/cm2/s
88- 93 F6.3 10-9W/m2 e_Fp64 [0.04/25] Lower 1σ uncertainty in Fp64
95-100 F6.3 10-9W/m2 E_Fp64 [0.05/25] Upper 1σ uncertainty in Fp64
102-108 F7.3 s Tp64r [-0.5/367.2] Start time of interval when PCR
on 64ms(1+z) time scale reached
110-116 F7.3 10-9W/m2 Fp64r [0.3/871] Peak energy flux from 64ms(1+z)
time scale; 1e-6erg/cm2/s
118-123 F6.3 10-9W/m2 e_Fp64r [0.04/24] Lower 1σ uncertainty in Fp64r
125-130 F6.3 10-9W/m2 E_Fp64r [0.05/24] Upper 1σ uncertainty in Fp64r
132-140 F9.4 10+44J Eiso [0.04/5810] Isotropic energy release; 1e+51erg
142-149 F8.4 10+44J e_Eiso [0.005/440] The 1σ uncertainty in Eiso
151-158 F8.3 10+44W Liso [0.2/4650] Peak isotropic luminosity;
in 1e+51erg/s units
160-166 F7.3 10+44W e_Liso [0.05/190] The 1σ uncertainty in Liso
168-172 F5.2 10-9W/m2 Flim [0/25]? Bolometric energy flux corresponding
to GRB detection threshold; 1e-6erg/cm2/s
174-178 F5.2 --- Zmax [0/16.7]? KW GRB detection horizon
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Note (8):
1 = Since the trigger mode light curve begins at T0-0.512s, the
corresponding peak energy flux may be underestimated due to the
absence of high-res data before T0-0.512s.
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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- 3 A3 --- --- [GRB]
4- 10 A7 --- GRB Gamma-ray burst identifier (YYMMDDA)
12- 17 F6.3 d tjet [0.1/35] Jet break time
19- 23 F5.3 d e_tjet [0/6]? Lower 1σ uncertainty on tjet (1)
25- 30 F6.3 d E_tjet [0/12]? Upper 1σ uncertainty on tjet (1)
32- 33 A2 --- CBM Circumburst medium (2)
35- 41 A7 --- Ref Reference(s) to tjet and CBM;
see refs.dat file (3)
43- 47 F5.2 deg theta [1.8/25.6] Jet opening angle θjet (4)
49- 52 F4.2 deg e_theta [0.05/4.2] The 1σ uncertainty in theta
54- 58 F5.2 10-3 Coll [0.5/97.5] Collimation factor (4)
60- 64 F5.2 10-3 e_Coll [0.03/16] The 1σ uncertainty in Coll
66- 72 F7.2 10+42J Egamma [1.2/1234] Collimation-corrected energy release
in 1e+49erg units
74- 79 F6.2 10+42J e_Egamma [0.1/189] The 1σ uncertainty in Egamma
81- 86 F6.2 10+42W Lgamma [0.4/550] Collimation-corrected peak
luminosity; 1e+49erg/s
88- 92 F5.2 10+42W e_Lgamma [0.02/83] The 1σ uncertainty in Lgamma
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Note (1): When no tjet uncertainty is available from the literature, we take
the sample-mean ∼0.2*tjet as a 1σ tjet error for the
calculations.
Note (2): Circumburst medium (CBM) as follows:
HM = In the case of a CBM with constant number density n
WM = In the case of a stellar-wind-like CBM with n(r)∝r-2
In cases where no preferred CBM density profile is available from
the literature, we provide the estimates for both HM and WM.
See section 4.3.3 for further explanations.
Note (3): In cases where two references are given, the first one corresponds
to the jet break time estimate and the second one corresponds to
the preferred CBM.
Note (4): Knowing tjet, one can estimate the collimation-corrected energy
released in gamma-rays Egamma=Eiso(1-cosθjet) and the
collimation-corrected peak luminosity Lgamma=Liso(1-cosθjet),
where θjet is the jet opening angle and (1-cosθjet)
is the collimation factor. See section 4.3.3.
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Ref Reference code
5- 23 A19 --- BibCode ADS bibcode of the reference
25- 48 A24 --- Auth Author's name
50-152 A103 --- Comm Comment
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 02-Jul-2018