J/ApJS/261/25 Optical LC fit parameters for 179 GRBs (Dainotti+, 2022)
The optical two- and three-dimensional fundamental plane correlations for nearly
180 gamma-ray burst afterglows with Swift/UVOT, RATIR, and the Subaru telescope.
Dainotti M.G., Young S., Li L., Levine D., Kalinowski K.K., Kann D.A.,
Tran B., Zambrano-Tapia L., Zambrano-Tapia A., Cenko S.B., Fuentes M.,
Sanchez-Vazquez E.G., Oates S.R., Fraija N., Becerra R.L., Watson A.M.,
Butler N.R., Gonzalez J.J., Kutyrev A.S., Lee W.H., Prochaska J.X.,
Ramirez-Ruiz E., Richer M.G., Zola S.
<Astrophys. J. Suppl. Ser., 261, 25 (2022)>
=2022ApJS..261...25D 2022ApJS..261...25D
ADC_Keywords: GRB; Redshifts; References; Photometry; Optical
Keywords: Gamma-ray bursts
Abstract:
Gamma-ray bursts (GRBs) are fascinating events due to their
panchromatic nature. We study optical plateaus in GRB afterglows via
an extended search into archival data. We comprehensively analyze all
published GRBs with known redshifts and optical plateaus observed by
many ground-based telescopes (e.g., Subaru Telescope, RATIR) around
the world and several space-based observatories such as the Neil
Gehrels Swift Observatory. We fit 500 optical light curves, showing
the existence of the plateau in 179 cases. This sample is 75% larger
than the previous one, and it is the largest compilation so far of
optical plateaus. We discover the 3D fundamental plane relation at
optical wavelengths using this sample. This correlation is between the
rest-frame time at the end of the plateau emission, Topt*, its
optical luminosity, Lopt, and the peak in the optical prompt emission,
Lpeak,opt, thus resembling the three-dimensional (3D) X-ray
fundamental plane (the so-called 3D Dainotti relation). We correct our
sample for redshift evolution and selection effects, discovering that
this correlation is indeed intrinsic to GRB physics. We investigate
the rest-frame end-time distributions in X-rays and optical
(Topt*, TX*), and conclude that the plateau is achromatic only
when selection biases are not considered. We also investigate if the
3D optical correlation may be a new discriminant between optical GRB
classes and find that there is no significant separation between the
classes compared to the Gold sample plane after correcting for
evolution.
Description:
We analyzed 500 GRB optical afterglows with known redshifts, thus
building the most comprehensive sample of optical light curves (LCs)
to date by searching the literature for all GRBs detected between
1997 May and 2021 May by several satellites, e.g., the Swift
Ultraviolet/Optical Telescope (UVOT), and ground-based
telescopes/detectors, e.g., the Subaru Telescope, Gamma-ray Burst
Optical/Near-IR Detector (GROND), Re-ionization and Transients
InfraRed camera/telescope (RATIR), the MITSuME, etc.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 210 179 Fitting parameters for the sample of 179 GRBs
refs.dat 1894 82 References
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See also:
J/A+A/333/231 : O-M stars model atmospheres (Bessell+ 1998)
J/ApJ/654/L25 : Light-curve data for GRB 050319 (Huang+, 2007)
J/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009)
J/ApJ/720/1513 : The afterglows of Swift-era GRBs. I. (Kann+, 2010)
J/ApJ/774/157 : Swift GRBs with X-ray afterglows and z<9.5 (Dainotti+, 2013)
J/A+A/557/A12 : Optical light curves of γ-ray bursts (Zaninoni+, 2013)
J/MNRAS/455/1027 : The afterglow of GRB 130831A photometry (De Pasquale+, 2016)
J/A+A/617/A122 : GRB 111209A GROND and UVOT light curves (Kann+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- GRB GRB Name
9- 14 A6 --- Author Source reference (see refs.dat file)
16- 18 I3 --- Sp Spectrum source (see refs.dat file)
20- 26 F7.5 --- z [0.06/8.23] Redshift
28- 34 F7.2 s T90 [0.3/1088] T90 duration (1)
36- 49 A14 --- Class GRB Class (2)
51- 62 F12.8 [mW/m2] logFa [-15.1/-8.7] log of flux at the end of
the plateau emission, in erg/s/cm2 units
64- 74 F11.9 [mW/m2] e_logFa [0.004/1.2] Uncertainty in logFa
76- 86 F11.9 [s] logTa [1.8/6.6] log of time at the end of
the plateau emission
88- 98 F11.9 [s] e_logTa [0.004/0.61] Uncertainty in logTa
100-110 F11.9 [s] Alpha [0.4/3.3] Slope after the end of the
plateau emission
112-122 F11.9 [s] e_Alpha [0/1.51] Uncertainty in Alpha
124-130 F7.5 [s] beta [0.12/1.8] Optical spectral index
132-138 F7.5 [s] e_beta [0.01/1.15] Uncertainty in beta
140-150 F11.9 --- ktotal [0.29/3.3] K-correction
152-162 F11.9 --- e_ktotal [0.0013/2.51] Uncertainty in ktotal
164-174 F11.9 [s] logTa-re [1.35/6.5] log of rest frame time at the
end of the plateau emission
176-186 F11.9 [s] e_logTa-re [0.004/0.61] Uncertainty in logTa-re
188-198 F11.8 [10-7W] logLumTa [41.99/49.24] log of luminosity at the
end of the plateau emission, in erg/s units
200-210 F11.9 [10-7W] e_logLumTa [0.006/1.15] Uncertainty in logTa-re
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Note (1): T90=90% of the total emitted energy during the prompt emission from
5% to 95% of the total counts.
Note (2): GRB Classes as follows:
A = Hjorth+ (2003Natur.423..847H 2003Natur.423..847H) [2001grba.conf...16H] Class A;
B = Hjorth+ (2003Natur.423..847H 2003Natur.423..847H) [2001grba.conf...16H] Class B;
C = Hjorth+ (2003Natur.423..847H 2003Natur.423..847H) [2001grba.conf...16H] Class C;
D = Hjorth+ (2003Natur.423..847H 2003Natur.423..847H) [2001grba.conf...16H] Class D;
E = Hjorth+ (2003Natur.423..847H 2003Natur.423..847H) [2001grba.conf...16H] Class E;
IS = intrinsically short;
KN = KN;
L = Long;
S = Short;
SEE = SGRBs with extended emission;
SN = associated with SNe Ic, which can be category A, B, C, D, and E;
UL = Ultra-Long;
VL = Very long;
XRF = X-ray flashes;
XRR = X-ray Rich.
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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 A1 --- --- [=]
8-1895 A1888 --- Text Detailed reference(s)
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 26-Sep-2022