J/ApJ/908/83 Konus-Wind catalog of GRBs with redshifts. II. (Tsvetkova+, 2021)
The Konus-Wind Catalog of Gamma-Ray Bursts with Known Redshifts.
II. Waiting-Mode Bursts Simultaneously Detected by Swift/BAT.
Tsvetkova A., Frederiks D., Svinkin D., Aptekar R., Cline T.L.,
Golenetskii S., Hurley K., Lysenko A., Ridnaia A., Ulanov M.
<Astrophys. J., 908, 83 (2021)>
=2021ApJ...908...83T 2021ApJ...908...83T
ADC_Keywords: Gamma-ray burst; Redshifts
Keywords: Catalogs ; Gamma-ray bursts ; Astronomy data analysis
Abstract:
In the second part of The Konus-Wind Catalog of Gamma-Ray Bursts with
Known Redshifts (the first part: Tsvetkova+, 2017, J/ApJ/850/161;
T17), we present the results of a systematic study of gamma-ray bursts
(GRBs) with reliable redshift estimates detected simultaneously by the
Konus-Wind (KW) experiment (in the waiting mode) and by the Swift/BAT
(BAT) telescope during the period from 2005 January to the end of
2018. By taking advantage of the high sensitivity of BAT and the wide
spectral band of KW, we were able to constrain the peak spectral
energies, the broadband energy fluences, and the peak fluxes for the
joint KW- BAT sample of 167 weak, relatively soft GRBs (including four
short bursts). Based on the GRB redshifts, which span the range
0.04≲z≲9.4, we estimate the rest frame, isotropic-equivalent energy,
and peak luminosity. For 14 GRBs with reasonably constrained jet
breaks, we provide the collimation-corrected values of the energetics.
This work extends the sample of KW GRBs with known redshifts to 338
GRBs, the largest set of cosmological GRBs studied to date over a
broad energy band. With the full KW sample, accounting for the
instrumental bias, we explore GRB rest-frame properties, including
hardness-intensity correlations, GRB luminosity evolution, luminosity
and isotropic-energy functions, and the evolution of the GRB formation
rate, which we find to be in general agreement with those reported in
T17 and other previous studies.
Description:
Konus-Wind (KW) is a gamma-ray spectrometer designed to study temporal
and spectral characteristics of Gamma-Ray Bursts (GRBs), solar flares
(SFs), soft gamma repeaters, and other transient phenomena over a wide
energy range from 13keV to 10MeV.
The Burst Alert Telescope (Swift/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 BAT is composed of a detector plane that has 32768 CdZnTe
(CZT) detectors, and a coded-aperture mask that has ∼52000 lead tiles.
The BAT energy range is 14-150keV for imaging.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 65 167 Joint KW/Swift-BAT sample
table2.dat 111 365 Spectral parameters
table4.dat 158 167 Burst energetics
table5.dat 88 22 Collimation-corrected parameters
refs.dat 68 131 References used for table1
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See also:
J/ApJ/609/935 : Gamma-ray burst formation rate (Yonetoku+, 2004)
J/ApJS/175/179 : The BAT1 gamma-ray burst catalog (Sakamoto+, 2008)
J/ApJ/720/1513 : The afterglows of Swift-era GRBs. I. (Kann+, 2010)
J/ApJS/195/2 : The second Swift BAT GRB catalog (BAT2) (Sakamoto+, 2011)
J/ApJ/778/128 : GRB-host galaxies photometry (Perley+, 2013)
J/A+A/581/A125 : UV/Optical/NIR spectroscopy GRB hosts (Kruehler+, 2015)
J/ApJ/829/7 : The 3rd Swift/BAT GRB catalog (past ∼11yrs) (Lien+, 2016)
J/ApJS/224/10 : The second Konus-Wind short GRB catalog (Svinkin+, 2016)
J/ApJ/850/161 : Konus-Wind cat. of GRBs with redshifts. I. (Tsvetkova+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- ID Burst identifier
12- 17 I6 --- NumID [103780/871316] Swift/BAT GRB Trigger number
19- 30 A12 --- Time Swift/BAT trigger time, UT hh:mm:ss
32- 38 F7.5 --- z [0.03/9.38] Redshift
40- 42 A3 --- f_z Type for z (1)
44- 46 A3 --- r_z Reference code for z
48 A1 --- Com Comment on the burst (2)
50- 57 F8.3 s t0 [-230/60] Start time of T100 relative to Trig
59- 65 F7.3 s T100 [0.83/445] Total burst duration
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Note (1): Types as follows:
s = spectroscopic (153 occurrences)
p = photometric (13 occurrences)
s+p = both (1 occurrence)
Note (2): Comment as follows:
1 = There are two sources located within the revised XRT error circle.
Here we use the redshift of one of them as a proxy for GRB redshift.
The other source, which is a factor of 2 fainter, is likely to reside
at an even higher redshift.
2 = No emission was detected at the wavelengths shorter than 7500 Angstroms.
This flux 'decrement' may be associated with the IGM at z∼5.2 but
could also be associated with a significant reddening of the afterglow.
3 = A weak absorption system identified at z=0.696 could also be produced
by an intervening system and thus the strict redshift range for this
GRB would be 0.696<z<2.2.
4 = The object is well detected and presents a featureless continuum
except for a weak double line at z=1.036. No other clear features
are detected. Therefore, 1.036<z<2.7 is suggested as redshift
range for this GRB.
5 = Given the low S/N of the spectrum, this redshift measurement should
be considered tentative.
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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- 10 A10 --- ID Burst identifier
12- 12 A1 --- Type Spectral type (1)
14- 21 F8.3 s Tstart [-109/382] Spectrum start time relative to T0
23- 29 F7.3 s dT [2.94/416] Spectrum accumulation time
31- 34 A4 --- Model Spectral model used
36- 40 F5.2 --- Alpha [-1.84/0.71] Low-energy photon index
42- 45 F4.2 --- e_Alpha [0.04/2] Lower 1σ uncertainty in Alpha
47- 50 F4.2 --- E_Alpha [0.05/3] Upper 1σ uncertainty in Alpha
52- 56 F5.2 --- Beta [-3.46/-1.75]? High-energy photon index
58- 61 F4.2 --- e_Beta [0.07/9]? Lower 1σ uncertainty in Beta
63- 66 F4.2 --- E_Beta [0.06/3]? Upper 1σ uncertainty in Beta
68- 70 I3 keV Ep [27/578] EFE spectrum peak energy
72- 74 I3 keV e_Ep [2/293] Lower 1σ uncertainty in Ep
76- 79 I4 keV E_Ep [2/2803] Upper 1σ uncertainty in Ep
81- 84 F4.2 10-10W/m2 F [0.1/8.66] Spectral model normalization flux
(1e-7erg/s/cm2)
86- 89 F4.2 10-10W/m2 e_F [0.01/1.43] Lower 1σ uncertainty in F
91- 94 F4.2 10-10W/m2 E_F [0.02/1.5] Upper 1σ uncertainty in F
96-100 F5.1 --- Chi2 [34.3/103] Chi-square statistic of the fit
102-103 I2 --- DoF [58/59] Number of degrees of freedom
105-111 F7.5 --- Prob [0.0003/1] Null hypothesis probability
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Note (1): Types as follows:
i = the spectrum is time-integrated and is used to calculate
the burst total energy fluence (222 occurrences)
p = the spectrum is measured near the maximum count rate and
is used to calculate the burst energy peak flux (143 occurrences)
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- ID Burst identifier
12- 18 F7.5 --- z [0.03/9.38] Spectroscopic redshift
20- 25 F6.2 10-10J/m2 S [1.36/405] Energy fluence; 1e-7erg/s
27- 32 F6.2 10-10J/m2 e_S [0.2/70] Lower 1σ uncertainty in S
34- 38 F5.2 10-10J/m2 E_S [0.2/89] Upper 1σ uncertainty in S
40- 46 F7.3 s Tp1024 [0/390] Start time of interval when PCR on
1024ms time scale reached (1)
48- 52 F5.2 10-10W/m2 Fp1024 [0.52/10.2] Peak energy flux from 1024ms time
scale (1e-7erg/cm2/s)
54- 58 F5.2 10-10W/m2 e_Fp1024 [0.1/3] Lower 1σ uncertainty in Fp1024
60- 63 F4.2 10-10W/m2 E_Fp1024 [0.1/3] Upper 1σ uncertainty in Fp1024
65- 71 F7.3 s Tp64 [0.008/396] Start time of interval when PCR
on 64ms time scale reached (1)
73- 77 F5.2 10-10W/m2 Fp64 [1.36/31.9] Peak energy flux from 64ms time
scale (1e-7erg/cm2/s)
79- 83 F5.2 10-10W/m2 e_Fp64 [0.3/10] Lower 1σ uncertainty in Fp64
85- 88 F4.2 10-10W/m2 E_Fp64 [0.4/9] Upper 1σ uncertainty in Fp64
90- 96 F7.3 s Tp64r [0.01/394] Start time of interval when PCR on
64ms(1+z) time scale reached (1)
98-102 F5.2 10-10W/m2 Fp63r [0.75/28.7] Peak energy flux from 64ms(1+z)
time scale (1e-7erg/cm2/s)
104-108 F5.2 10-10W/m2 e_Fp63r [0.2/9] Lower 1σ uncertainty in Fp64r
110-113 F4.2 10-10W/m2 E_Fp63r [0.3/8] Upper 1σ uncertainty in Fp64r
115-121 F7.2 10+44J Eiso [0.03/1477] Isotropic energy release 1e+51erg
123-129 F7.2 10+44J e_Eiso [0/255] Lower 1σ uncertainty in Eiso
131-136 F6.2 10+44J E_Eiso [0/326] Upper 1σ uncertainty in Eiso
138-143 F6.2 10+44W Liso [0/514] Peak isotropic luminosity; 1e+51erg/s
145-151 F7.2 10+44W e_Liso [0/131] Lower 1σ uncertainty in Liso
153-158 F6.2 10+44W E_Liso [0/104] Upper 1σ uncertainty in Liso
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Note (1): Relative to BAT trigger time.
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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- 10 A10 --- ID Burst identifier
12- 15 F4.2 d tJet [0.03/9.49]? Jet break time
17- 21 F5.2 d e_tJet [0.01/1]? Uncertainty in tJet
23- 25 A3 --- CBM Circumburst medium (1)
27- 29 A3 --- Ref Reference code for tJet and CBM (2)
31- 35 F5.2 deg theta [1.26/10.2] Jet opening angle
37- 40 F4.2 deg e_theta [0.04/0.6] Uncertainty in theta
42- 46 F5.2 10-3 Col [0.24/15.8] Collimation factor
48- 51 F4.2 10-3 e_Col [0.03/0.9] Uncertainty in Col
53- 58 F6.2 10+42J Egamma [0.59/233] Collimation-corrected energy release;
1e+49erg
60- 65 F6.2 10+42J e_Egamma [0.1/56] Lower 1σ uncertainty in Egamma
67- 71 F5.2 10+42J E_Egamma [0.1/57] Upper 1σ uncertainty in Egamma
73- 77 F5.2 10+42W Lgamma [0.43/29.1] Collimation-corrected peak luminosity
1e+49 erg/s
79- 83 F5.2 10+42W e_Lgamma [0.1/8] Lower 1σ uncertainty in Lgamma
85- 88 F4.2 10+42W E_Lgamma [0.1/9] Upper 1σ uncertainty in Lgamma
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Note (1): In cases where the preferred CBM density profile is known, it is
taken from the same paper as tjet. Otherwise, calculations for both
CBMs are provided and the geometric mean of the HM and WM energetics
is used in the calculations.
Note (2): References as follows:
(1) = Ghirlanda+, 2007A&A...466..127G 2007A&A...466..127G
(2) = Afonso+, 2011A&A...526A.154A 2011A&A...526A.154A
(3) = Wang+, 2018ApJ...859..160W 2018ApJ...859..160W
(4) = Kann+, 2010, J/ApJ/720/1513
(5) = Frail+, 2006ApJ...646L..99F 2006ApJ...646L..99F
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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 [1/131] Reference code
5- 33 A29 --- Autor Main autor for the reference
35- 53 A19 --- BIB BIBcode
55- 68 A14 --- Cat. Vizier catalog
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History:
From electronic version of the journal
References:
Tsvetkova et al. Paper I : 2017ApJ...850..161T 2017ApJ...850..161T Cat. J/ApJ/850/161
(End) Prepared by [AAS], Coralie Fix [CDS], 04-Jul-2022