J/ApJ/950/30 Rest-frame parameters of short and long GRBs (Zhu+, 2023)
The intrinsic statistical properties and correlations of short gamma-ray bursts.
Zhu S.-Y., Liu Z.-Y., Shi Y.-R., Ding X.-K., Sun W.-P., Zhang F.-W.
<Astrophys. J., 950, 30 (2023)>
=2023ApJ...950...30Z 2023ApJ...950...30Z
ADC_Keywords: GRB; Redshifts; Gamma rays; Galaxies
Keywords: Gamma-ray bursts
Abstract:
The intrinsic statistical properties and correlations of short
gamma-ray bursts (SGRBs) have not been fully determined, due to the
limitations of observations. In this paper, we compile a more
extensive sample of 82 SGRBs with measured redshifts and present a
comprehensive study of their intrinsic characteristics. We obtain the
median values of the intrinsic duration (T90,z), peak energy (Ep,z),
isotropic energy (Eiso), and peak luminosity (Liso) as 0.47s, 466keV,
8.21x1050erg, and 3.22x1051erg/s, respectively. We update the
spectrum-energy correlations, and report
Ep,z∝Eiso0.36±0.05 and
Ep,z∝Liso0.33±0.04, which further confirm the previous
results that the Ep,z-Eiso correlations of SGRBs and long
gamma-ray bursts (LGRBs) are different and that this correlation can
be used to distinguish GRB types. We report for the first time that
there is a tighter correlation between the isotropic energy of the
prompt emission of SGRBs and the star formation rate of their host
galaxies, which reads sSFR∝Eiso0.38±0.11. Using the
measured jet break time (tjet) of 11 SGRBs, we tentatively
investigate the Eiso-Ep,z-tjet,z and Liso-Ep,z-tjet,z
correlations of SGRBs and find that three-parameter correlations of
SGRBs also exist and are different from those of LGRBs. Based on the
Eiso-Ep,z-tjet,z correlation, we estimate the tjet,z values of
other SGRBs and calculate the opening angles of SGRBs. We find that
the median value of the SGRB opening angle is 7.5°, which is
larger than that of LGRBs.
Description:
The spectral data are mainly taken from the catalog of Fermi/GBM and
Konus-Wind.
We only select the gamma-ray bursts (GRBs) that were only detected by
Swift/BAT with spectra that could be fitted by the cutoff power-law
(CPL) model. We collect all the SGRBs with known redshifts and
well-measured spectra that can be well fitted by the CPL model or Band
model from 2005 May to 2022 January as our sample.
In addition, for comparison, 178 LGRBs taken from
Xue+ (2019ApJ...876...77X 2019ApJ...876...77X) are used for the analysis.
The cosmological constants in this paper are H0=71km/s/Mpc,
ΩM=0.27, and ΩΛ=0.73.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 137 87 The properties of short gamma-ray bursts (SGRBs)
in the observed frame
table2.dat 234 87 The properties of SGRBs in the rest frame
table3.dat 116 178 The properties of long gamma-ray bursts (LGRBs)
in the rest frame
refs.dat 94 49 References
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See also:
J/ApJ/607/665 : Type Ia supernovae at z>1 discovered by HST (Riess+, 2004)
J/ApJ/609/935 : Gamma-ray burst formation rate (Yonetoku+, 2004)
J/MNRAS/418/2202 : Analysis of γ-ray bursts (Dainotti+, 2011)
J/ApJ/774/157 : Swift GRBs with X-ray afterglows & z<9.5 (Dainotti+, 2013)
J/A+A/557/A12 : Opt. light curves of γ-ray bursts (Zaninoni+, 2013)
J/ApJ/818/18 : Jet angles & gamma-ray energetics (Goldstein+, 2016)
J/ApJS/227/7 : Long & short GRBs with host galaxies data (Li+, 2016)
J/ApJ/829/7 : The third Swift/BAT GRB catalog (∼11yrs) (Lien+, 2016)
J/ApJ/850/161 : Konus-Wind cat. of GRBs with z. I. (Tsvetkova+, 2017)
J/MNRAS/486/L46 : Gamma-ray burst redshifts (Amati+, 2019)
J/MNRAS/492/1919 : Type I GRBs & a new classification method (Minaev+, 2020)
J/ApJ/893/46 : The fourth Fermi-GBM GRB cat.: 10yrs (von Kienlin+, 2020)
J/other/RAA/21.254 : GRB isotropic energy function (Liu+, 2021)
J/ApJS/261/25 : Optical LC fit parameters for 179 GRBs (Dainotti+, 2022)
J/ApJ/940/56 : Short GRB host galaxies. I. opt-NIR imaging (Fong+, 2022)
J/ApJ/925/15 : Radio afterglow emission of GRBs (Levine+, 2022)
J/ApJ/932/1 : LBT/MODS sp. of the host gal. of GRB200826A (Rossi+, 2022)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- GRB GRB name (YYMMDDA)
9 A1 --- f_GRB [ab] Flag on GRB (G1)
11- 16 F6.4 --- z [0.0093/4.6] Redshift
18- 24 F7.3 s T90 [0.04/123.65] Duration, T90
26- 30 F5.2 s e_T90 [0.01/30] T90 uncertainty
32- 37 F6.3 --- alpha [-2.08/1.42] Low-energy spectral index
39- 43 F5.2 --- beta [-2.46/-2.05]? High-energy spectral index
45- 50 F6.1 keV Ep [8/4727] Peak energy, Ep
52- 54 I3 keV e_Ep [1/918] Lower uncertainty on Ep
56- 59 I4 keV E_Ep [1/2009] Upper uncertainty on Ep
61- 67 F7.2 10-3J/m2 Sgam-7 [0.12/5420] Fluence, Sγ,-7,
in erg/cm2
69- 73 F5.2 10-3J/m2 e_Sgam-7 [0.03/80] Lower uncertainty on Sgam-7
75- 79 F5.2 10-3J/m2 E_Sgam-7 [0.03/80] Upper uncertainty on Sgam-7
81- 86 F6.2 mW/m2 Fp-6 [0.02/138] Peak flux, Fp,-6, in erg/cm2s
88- 92 F5.2 mW/m2 e_Fp-6 [0.01/15.2] Lower uncertainty on Fp-6
94- 98 F5.2 mW/m2 E_Fp-6 [0.01/23] Upper uncertainty on Fp-6
100 A1 --- f_Fp-6 [c] Flag on Fp-6 (G1)
102- 106 F5.2 d Tjet [0.03/29]? Jet break time, tjet
108- 111 F4.2 d e_Tjet [0.01/2.9]? Lower uncertainty on Tjet
113- 116 F4.2 d E_Tjet [0.01/2.9]? Upper uncertainty on Tjet
118- 125 A8 keV Range Energy range
127 A1 --- Group [A-D] Group (A=gold sample) (1)
129- 137 A9 --- Ref Reference(s) (see refs.dat file)
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Note (1): According to the different characteristics of each short GRB (SGRB),
the SGRB sample was divided into four groups. See Section 2.
Code as follows:
D = 22 SGRBs with photometric redshifts
C = 23 SGRBs observed only by Swift/BAT without accurate Ep
B = six special GRBs (GRB 211227A, GRB 211211A, GRB 200826A, GRB 170817A,
GRB 100816A, and GRB 060614)
A = the remaining 31 SGRBs with well-measured redshifts and spectral
parameter (gold sample)
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- GRB GRB name (YYMMDDA)
9 A1 --- f_GRB [ab] Flag on GRB (G1)
11- 16 F6.2 s T90z [0.03/110] Intrinsic duration, T90,z
(T90/(1+z))
18- 22 F5.2 s e_T90z [0.01/20.1] T90z uncertainty
24- 27 I4 keV Epz [12/8996] Rest-frame peak energy, Ep,z
(Ep(1+z))
29- 32 I4 keV e_Epz [1/2347] Lower uncertainty on Epz
34- 37 I4 keV E_Epz [1/4952] Upper uncertainty on Epz
39- 47 F9.3 10+42J Eiso [0.003/65258] Isotropic energy, in 1049erg
(G2)
49- 57 F9.3 10+42J e_Eiso [0.001/17201] Lower uncertainty on Eiso
59- 66 F8.3 10+42J E_Eiso [0.001/6526] Upper uncertainty on Eiso
68- 76 F9.3 10+42W Liso [0.001/42580] Peak luminosity, in
1049erg/s (G2)
78- 87 F10.4 10+42W e_Liso [0.0005/34271] Lower uncertainty on Liso
89- 97 F9.4 10+42W E_Liso [0.0005/4674] Upper uncertainty on Liso
99- 103 F5.2 d Tjetz [0.03/26.44]? Jet break time, tjet,z
(tjet/(1+z))
105- 108 F4.2 d e_Tjetz [0.01/2.64]? Lower uncertainty on Tjetz
110- 113 F4.2 d E_Tjetz [0.01/2.64]? Upper uncertainty on Tjetz
115- 119 F5.2 kpc Offset [0.49/76.2]? Burst offset from the host
galaxy
121- 125 F5.2 kpc e_Offset [0.03/28]? Offset uncertainty
127- 131 F5.2 Gyr Tm [0.12/10.41]? Mass-weighted age of the host
galaxy, tm
133- 136 F4.2 Gyr e_Tm [0/1.97]? Lower uncertainty on Tm
138- 141 F4.2 Gyr E_Tm [0/2.77]? Upper uncertainty on Tm
143- 147 F5.2 [Msun] logMs [7.92/11.8]? Log of stellar mass of the host
galaxy
149- 152 F4.2 [Msun] e_logMs [0/0.86]? Lower uncertainty on logMs
154- 157 F4.2 [Msun] E_logMs [0/0.89]? Upper uncertainty on logMs
159- 164 F6.2 Msun/yr SFR [0/824.29]? Star formation rate of the host
galaxy
166- 171 F6.2 Msun/yr e_SFR [0/431.56]? Lower uncertainty on SFR
173- 179 F7.2 Msun/yr E_SFR [0/2567.13]? Upper uncertainty on SFR
181- 186 F6.2 [yr-1] logsSFR [-12.34/0]? Specific SFR of the host galaxy
(sSFR=SFR/Ms)
188- 191 F4.2 [yr-1] e_logsSFR [0/3.15]? Lower uncertainty on logsSFR
193- 196 F4.2 [yr-1] E_logsSFR [0/0.8]? Upper uncertainty on logsSFR
198- 202 F5.2 [Sun] logZ [-0.99/0.19]? Log of stellar metallicity of
the host galaxy
204- 207 F4.2 [Sun] e_logZ [0/0.61]? Lower uncertainty on logZ
209- 212 F4.2 [Sun] E_logZ [0/0.49]? Upper uncertainty on logZ
214- 217 F4.2 mag Av [0/2.99]? Total dust attenuation of the host
galaxy
219- 222 F4.2 mag e_Av [0/0.92]? Lower uncertainty on Av
224- 227 F4.2 mag E_Av [0/1.64]? Upper uncertainty on Av
229- 234 A6 --- Ref Reference(s) (see refs.dat file)
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- GRB GRB name (YYMMDDA)
9- 14 F6.2 s T90z [0.77/189] Intrinsic duration, T90,z
(T90/(1+z))
16- 21 F6.2 s e_T90z [0.02/604.4]? Lower uncertainty on T90z
23- 28 F6.2 s E_T90z [0.02/104]? Upper uncertainty on T90z
30- 36 F7.2 keV Epz [11.94/3620] Rest-frame peak energy, Ep,z
(Ep(1+z))
38- 44 F7.2 keV e_Epz [1.29/1887] Lower uncertainty on Epz
46- 52 F7.2 keV E_Epz [1.29/2295] Upper uncertainty on Epz
54- 59 F6.2 10+45J Eiso [0.05/522.34] Isotropic energy, in 1052erg
(G2)
61- 66 F6.3 10+45J e_Eiso [0.001/31.9] Lower uncertainty on Eiso
68- 73 F6.3 10+45J E_Eiso [0.001/27.6] Upper uncertainty on Eiso
75- 80 F6.2 10+45W Liso [0.01/209] Peak luminosity, in 1052erg/s (G2)
82- 88 F7.4 10+45W e_Liso [0.0004/10.2]? Lower uncertainty on Liso
90- 96 F7.4 10+45W E_Liso [0.0004/10.2]? Upper uncertainty on Liso
98- 103 F6.3 d Tjetz [0.001/24.14]? Jet break time, tjet,z
(tjet/(1+z)) (1)
105- 110 F6.3 d e_Tjetz [-0.024/3.5]? Lower uncertainty on Tjetz
112- 116 F5.3 d E_Tjetz [0.001/6.7]? Upper uncertainty on Tjetz
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Note (1): The jet break time sources are Tsvetkova+ (2017, J/ApJ/850/161),
Wang+ (2018ApJ...859..160W 2018ApJ...859..160W), Yi+ (2017JHEAp..13....1Y 2017JHEAp..13....1Y), and
Goldstein+ (2016, J/ApJ/818/18).
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- Ref Reference code
4- 27 A24 --- Auth First author's name
29- 47 A19 --- BibCode Bibcode of the reference
49- 94 A46 --- Comm Comment
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Global notes:
Note (G1): Flag as follows:
a = The main emission (ME) of the GRBs.
b = GRB 211106A has three possible redshifts.
c = The time resolution of Fp is larger than 64ms.
Note (G2): In this paper, both Eiso and Liso are corrected to the energy band
of 1-104keV in the rest frame. The Eiso is estimated by
Li+ 2016, J/ApJS/227/7 :
Eiso=(4πDL2Sγk)/(1+z)
where DL is the luminosity distance, Sγ is the fluence, and k
is the k-correction factor.
See Section 2.
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 18-Aug-2025