J/ApJ/884/59 GRB X-ray flare temporal and spectral properties (Liu+, 2019)
GRB X-ray flare properties among different GRB subclasses.
Liu C., Mao J.
<Astrophys. J., 884, 59-59 (2019)>
=2019ApJ...884...59L 2019ApJ...884...59L (SIMBAD/NED BibCode)
ADC_Keywords: GRB; X-ray sources; Redshifts
Keywords: gamma rays: general; radiation mechanisms: non-thermal
Abstract:
Gamma-ray bursts (GRBs) can be divided into three subclasses: X-ray
flash (XRF), X-ray rich (XRR), and classical GRB (C-GRB). An X-ray
flare is the rebrightening emission shown in the early X-ray afterglow
of some GRBs. In this paper, we comprehensively examine the X-ray
flare properties among XRF, XRR, and C-GRB subclasses. We utilize the
XRF, XRR, and C-GRB subclass samples obtained from the Swift-BAT3
catalog, and the X-ray flare observational properties are collected
from Falcone+ (2007ApJ...671.1921F 2007ApJ...671.1921F), Chincarini+ (2010MNRAS.406.2113C 2010MNRAS.406.2113C),
and Yi+ (2016, J/ApJS/224/20). We find that XRFs and XRRs have more
bright X-ray flares than C-GRBs. The ratio of the X-ray flare fluence
to the prompt emission fluence has different distributions between XRF
and C-GRB subclasses. The linear correlation between the duration and
the peak time of the X-ray flares is also different between XRF and
C-GRB subclasses. We are inclined to identify the GRBs with the bright
X-ray flares as XRFs or XRRs. We discuss some issues that are related
to the XRF/XRR/C-GRB classification. We also caution the selection
effects and the instrument bias in our investigation. Large samples
are required in the future to further confirm our results.
Description:
We utilize the GRB X-ray flare temporal data from both
Chincarini+ (2010MNRAS.406.2113C 2010MNRAS.406.2113C) and Yi+ (2016, J/ApJS/224/20). The
X-ray flares presented by Chincarini+ were observed from 2005 April to
2008 March, while those of Yi+ were observed from 2005 April to 2015
March. The two samples cover the same observational period, from 2005
April to 2008 March.
We also consider the spectral properties of the X-ray flares among
X-ray flash (XRF), X-ray rich (XRR), and classical GRB (C-GRB)
subclasses. We utilize the data from Falcone+ (2007ApJ...671.1921F 2007ApJ...671.1921F).
Thirty-three GRBs were observed from 2005 February to 2006 January,
and 77 X-ray flares with the spectral analysis are included in the
sample.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 236 582 Temporal properties of X-ray flares among X-ray
flash (XRF), X-ray rich (XRR) and
classical GRB (C-GRB)
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See also:
B/swift : Swift Master Catalog (HEASARC, 2004-)
J/ApJS/126/19 : BATSE gamma-ray burst spectral catalog. I. (Preece+, 2000)
J/ApJS/224/20 : 10yr of Swift/XRT obs. of GRBs (Yi+, 2016)
J/ApJ/866/97 : Swift X-ray flash & rich gamma-ray bursts in BAT3 (Bi+, 2018)
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]
5- 11 A7 --- GRB GRB Name (YYMMDDA)
13- 17 A5 --- Type GRB Type (1)
19- 22 A4 --- Int GRB belongs to an intermediate class
24- 30 F7.5 --- z [0.25/8.3]? Redshift (2)
32- 36 F5.1 s T90 [0.3/811]? Burst duration time (2)
38- 43 F6.2 s e_T90 [0.03/560]? Uncertainty in T90 (2)
45- 50 F6.3 10+2keV Epa [0.018/26]? GRB peak energy (2)
52- 60 F9.6 10+2keV e_Epa [5e-5/14.5]? Uncertainty in Epa (2)
62- 64 F3.1 --- alphaPL [0.9/2.6]? Power-law model fit slope (2)
66- 70 F5.3 --- e_alphaPL [0.02/0.5]? Uncertainty in alphaPL (2)
72- 78 F7.4 --- alphaCPL [-0.7/2.5]? Cut-off power-law model fit
slope (2)
80- 85 F6.3 --- e_alphaCPL [0.019/3.6]? Uncertainty in alphaCPL (2)
87- 91 F5.1 10-3J/m2 Sp25 [0.9/898]? GRB prompt emission,
Sp(25-50keV) (2)
93- 96 F4.1 10-3J/m2 e_Sp25 [0.2/18]? Uncertainty in Sp25 (2)
98- 106 F9.4 10-3J/m2 Sp50 [1/1300]? GRB prompt emission,
Sp(50-100keV) (2)
108- 111 F4.1 10-3J/m2 e_Sp50 [0.3/27.1]? Uncertainty in Sp50 (2)
113- 118 F6.1 10-3J/m2 Spf15 [4.5/8500]? Fluence, GRB prompt emission,
Spf(15-350keV) (2)
120- 124 F5.1 10-3J/m2 e_Spf15 [1.5/307]? Uncertainty in Spf15 (2)
126- 133 F8.1 s tbp [59.7/810000]? Peak time of the X-ray
flare
135- 146 F12.1 s e_tbp [0.2/2.5e+9]? Uncertainty in tbp
148- 157 F10.1 s wc [6.2/1.3e+7]? Duration of the X-ray flare
159- 169 F11.1 s e_wc [0.7/2e+8]? Uncertainty in wc
171- 175 F5.1 10-3J/m2 Sid0.2 [0/959]? Fluence, single X-ray flare,
Sid(0.2-10keV)
177- 184 F8.1 10-3J/m2 e_Sid0.2 [0.1/300000]? Uncertainty in Sid0.2
186- 192 F7.2 10-3J/m2 Ste0.2 [0.04/1800]? Total fluence of all X-ray
flares in one GRB, Ste(0.2-10keV) (2)
194- 201 F8.1 10-3J/m2 e_Ste0.2 [0.1/300000]? Uncertainty in Ste0.2 (2)
203- 210 F8.6 --- rgi [5.2e-5/3.5]? S(0.2-10keV)/Sp(15-350keV)
212- 219 F8.6 --- rht [5.2e-5/6.7]? St(0.2-10keV)/Sp(15-350keV)
(2)
221- 225 A5 --- ri Ratio of individual flare >0.2
(check=True)
227- 231 A5 --- rt Ratio of total flare >0.2 (check=True) (2)
233- 236 A4 --- Ref Sample Reference (3)
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Note (1): GRB type as follows:
XRF = X-ray flash (49 occurrences)
C-GRB = Classical GRB (199 occurrences)
XRR = X-ray rich (334 occurrences)
Note (2): Individual GRB properties and total flare properties are only
provided on the first row listed for each GRB. Other rows for that GRB
contain column data for individual X-ray flare properties.
Note (3): Reference as follows:
Ch10 = Chincarini+ (2010MNRAS.406.2113C 2010MNRAS.406.2113C ; 57 occurrences)
Yi16 = Yi+ (2016, J/ApJS/224/20 ; 200 occurrences)
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 17-Mar-2021