J/A+A/565/A72 Optical and X-ray light curves of BAT6 sample (Melandri+, 2014)
Optical and X-ray rest-frame light curves of the BAT6 sample.
Melandri A., Covino S., Rogantini D., Salvaterra R., Sbarufatti B.,
Bernardini M.G., Campana S., D'Avanzo P., D'Elia V., Fugazza D.,
Ghirlanda G., Ghisellini G., Nava L., Vergani S.D., Tagliaferri G.
<Astron. Astrophys. 565, A72 (2014)>
=2014A&A...565A..72M 2014A&A...565A..72M
ADC_Keywords: Gamma rays - X-ray sources
Keywords: gamma-ray burst: general - gamma rays: general - X-rays: general
Abstract:
We present the rest-frame light curves in the optical and X-ray bands
of an unbiased and complete sample of the Swift long gamma-ray bursts
(GRBs), namely, the BAT6 sample.
The unbiased BAT6 sample (consisting of 58 events) has the highest
level of completeness in redshift (∼95%), allowing us to compute the
rest-frame X-ray and optical light curves for 55 and 47 objects,
respectively. We compute the X-ray and optical luminosities, which
accounte for any possible source of absorption (Galactic and
intrinsic) that could affect the observed fluxes in these two bands.
Description:
We followed the classification scheme described in Margutti et al.
(2013, Cat. J/MNRAS/428/729/) that divided the light curves in four
main classes: class 0 for events decaying with simple power-law; class
Ia (Ib) for a smooth broken power-law that goes from a shallower
(steeper) to a steeper (shallower) decay; class IIa or IIb for events
that display steep-shallow-steep (canonical) or shallow-steep-shallow
decays respectively; and finally, class III for those events that show
a late-time break in their light curves.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 117 55 X-ray light curves fit results
table3.dat 144 55 Optical light curves fit results
bat/* . 51 BAT γ-ray light curves
bat2/* . 3 BAT γ-ray light curves for 3 sources
xrt/* . 55 XRT X-ray light curves
opt/* . 47 Optical light curves
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See also:
J/ApJ/673/96 : BAT X-ray Survey. III (Ajello+, 2008)
J/ApJ/678/102 : BAT X-ray survey. I (Ajello+, 2008)
J/ApJS/175/179 : The BAT1 gamma-ray burst catalog (Sakamoto+, 2008)
J/ApJ/711/495 : Durations of Swift/BAT GRBs (Butler+, 2010)
J/ApJS/195/2 : The second Swift BAT GRB catalog (BAT2) (Sakamoto+, 2011)
J/MNRAS/428/729 : GRB Swift X-ray light curves analysis (Margutti+, 2013)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- GRB Identifier of the GRB name
8 A1 --- fx [a] not fitted (1)
10- 14 F5.2 --- Xalf1 ?=- First X-ray decay index αX,1
16- 19 F4.2 --- e_Xalf1 ? Error of Xalf1
21- 25 F5.2 ks Xtb1 ?=- Time of the first X-ray break tbX,1
27- 30 F4.2 ks e_Xtb1 ? Error of Xtb1
32- 36 F5.2 --- Xalf2 ?=- Second X-ray decay index αX,2
38- 41 F4.2 --- e_Xalf2 ? Error of Xalf2
43- 48 F6.2 ks Xtb2 ?=- Time of the second X-ray break tbX,2
50- 54 F5.2 ks e_Xtb2 ? Error of Xtb2
56- 59 F4.2 --- Xalf3 ?=- Third X-ray decay index αX,3
61- 64 F4.2 --- e_Xalf3 ? Error of Xalf3
66- 72 E7.2 10-7W XNPL ?=- Normalisation of the power-law function
74- 80 E7.2 10-7W e_XNPL ? Error of NPL
83- 89 E7.2 10-7W XNBPL ?=- Normalisation of the broken power-law
function
91- 97 E7.2 10-7W e_XNBPL ? Error of NBPL
100-103 F4.2 --- Xchi Reduced χ2, goodness of the fit
106-109 I4 --- Xdof Degrees of freedom
112-117 A6 --- Xtyp Classification type of the GRB following the
scheme described in section 2 (G1)
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Note (1): a: we did not fit the early time steep exponential decay due to
high latitude emission.
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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- 7 A7 --- GRB Identifier of the GRB name
9 A1 --- fo [a] not fitted (2)
11- 15 F5.2 --- Oalf1 ?=- First decay index αO,1
17- 20 F4.2 --- e_Oalf1 ? Error of Oalf1
22- 27 F6.3 ks Otb1 ?=- Time of the first break tbO,1
29- 34 F6.3 ks e_Otb1 ? Error of Otb1
36- 41 F6.2 --- Oalf2 ?=- Second decay index αO,2
43- 46 F4.2 --- e_Oalf2 ? Error of Oalf2
48- 52 F5.2 ks Otb2 ?=- Time of the second break tbO,1
54- 58 F5.2 ks e_Otb2 ? Error of Otb2
60- 65 F6.2 --- Oalf3 ?=- Third decay index αO,3
67- 70 F4.2 --- e_Oalf3 ? Error of Oalf3
72- 75 F4.2 ks Otb3 ?=- Time of the third break tbO,1
77- 80 F4.2 ks e_Otb3 ? Error of Otb3
81- 85 F5.2 --- Oalf4 ?=- Forth decay index αO,4
87- 90 F4.2 --- e_Oalf4 ? Error of Oalf4
92- 99 F8.2 10-7W ONPL ?=- Normalisation of the power-law function
101-107 F7.2 10-7W e_ONPL ? Error of ONPL
110-116 F7.3 10-7W ONBPL ?=- Normalisation of the broken power-law
function
118-123 F6.3 10-7W e_ONBPL ? Error of ONBPL
125-129 F5.2 --- Ochi ?=- Reduced χ2 goodness of the fit
132-134 I3 --- Odof ?=- Degrees of freedom
136-145 A10 --- Otyp Classification type of the GRB following the
scheme described in section 2 (G1)
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Note (2): a: we did not fit the late time host galaxy and/or supernovae
component
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Byte-by-byte Description of file(#): bat/*
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Bytes Format Units Label Explanations
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2- 15 E14.8 s t Rest-frame time since burst
17- 30 E14.8 s E_t Positive error of t
32- 45 E14.8 s e_t Negative error of t
47- 60 E14.8 10+43W Lum γ-ray luminosity (in 10+50erg/s)
62- 75 E14.8 10+43W E_Lum Positive error of Lg
77- 90 E14.8 10+43W e_Lum Negative error of Lg
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Byte-by-byte Description of file: bat2/*
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Bytes Format Units Label Explanations
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1- 21 F21.18 s t Rest-frame time since burst
25- 44 F20.17 s e_t Error on t
50- 71 E22.18 10+43W Lum γ-ray luminosity (in 10+50erg/s)
74- 94 E21.18 10+43W e_Lum Error on Lg
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Byte-by-byte Description of file(#): xrt/*
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Bytes Format Units Label Explanations
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2- 15 E14.8 s t Rest-frame time since burst
17- 30 E14.8 s E_t Positive error of t
32- 45 E14.8 s e_t Negative error of t
47- 60 E14.8 10+43W Lum X-ray luminosity (in 10+50erg/s)
62- 75 E14.8 10+43W E_Lum Positive error of LX
77- 90 E14.8 10+43W e_Lum Negative error of LX
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Byte-by-byte Description of file: opt/*
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Bytes Format Units Label Explanations
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2- 16 F15.5 s t Rest-frame time since burst
17- 31 F15.8 s e_t Error of t
33- 44 E12.8 10+43W Lum Optical luminosity (in 10+50erg/s):
46- 56 E11.6 10+43W e_Lum Error of Lopt
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Global Notes:
Note (G1):
We followed the classification scheme described in Margutti et al.
(2013, Cat. J/MNRAS/428/729/) that divided the light curves in four
main classes:
* class 0 for events decaying with simple power-law;
* class Ia (Ib) for a smooth broken power-law that goes from a shallower
(steeper) to a steeper (shallower) decay;
* class IIa or IIb for events that display steep-shallow-steep (canonical)
or shallow-steep-shallow decays respectively;
* class III for those events that show a late-time break in their
light curves.
Acknowledgements:
Andrea Melandri, andy.melandri(at)gmail.com
(End) Patricia Vannier [CDS] 10-Mar-2014