J/A+A/588/A135 Fermi/GBM GRB time-resolved spectral catalog (Yu+, 2016)
The Fermi GBM gamma-ray burst time-resolved spectral catalog:
brightest bursts in the first four years.
Yu H.-F., Preece R.D., Greiner J., Bhat P.N., Bissaldi, E., Briggs M.S.,
Cleveland W.H., Connaughton V., Goldstein A., von Kienlin, A.,
Kouveliotou C., Mailyan B., Meegan C.A., Paciesas W.S., Rau A.,
Roberts O.J., Veres P., Wilson-Hodge C., Zhang B.-B., van Eerten H.J.
<Astron. Astrophys. 588, A135 (2016)>
=2016A&A...588A.135Y 2016A&A...588A.135Y (SIMBAD/NED BibCode)
ADC_Keywords: Gamma rays
Keywords: gamma rays: stars - gamma-ray burst: general - methods: data analysis
Abstract:
We aim to obtain high-quality time-resolved spectral fits of gamma-ray
bursts (GRBs) observed by the Gamma-ray Burst Monitor (GBM) on board
the Fermi Gamma-ray Space Telescope. We perform time-resolved spectral
analysis with high temporal and spectral resolution of the brightest
bursts observed by Fermi GBM in its first 4 years of mission. We
present the complete catalog containing 1,491 spectra from 81 bursts
with high spectral and temporal resolution. Distributions of
parameters, statistics of the parameter populations,
parameter-parameter and parameter-uncertainty correlations, and their
exact values are obtained and presented as main results in this
catalog. We report a criterion that is robust enough to automatically
distinguish between different spectral evolutionary trends between
bursts. We also search for plausible blackbody emission components and
find that only 3 bursts (36 spectra in total) show evidence of a pure
Planck function. It is observed that the averaged time-resolved
low-energy power-law index and peak energy are slightly harder than
the time-integrated values. Time-resolved spectroscopic results should
be used when interpreting physics from the observed spectra, instead
of the time-integrated results.
Description:
Time-resolved spectral analysis results of BEST models: for each
spectrum GRB name using the Fermi GBM trigger designation, spectrum
number within individual burst, start time T_start and end time T_stop
for the time bin, BEST model, best-fit parameters of the BEST model,
value of CSTAT per degrees of freedom, 10keV-1MeV photon and
energy flux are given.
Ep evolutionary trends: for each burst GRB name, number of spectra
with E_p, Spearman's Rank Correlation Coefficients between Ep and
photon flux and 90%, 95%, and 99% confidence intervals, Spearman's
Rank Correlation Coefficients between Ep and energy flux and 90%,
95%, and 99% confidence intervals, Spearman's Rank Correlation
Coefficient between Ep and time and 90%, 95%, and 99% confidence
intervals, trends as determined by computer for 90%, 95%, and 99%
confidence intervals, trends as determined by human eyes are given.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 158 1802 BEST model parameters for 1802 spectra
tableb1.dat 258 81 Ep evolutionary trends for 81 bursts
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See also:
J/ApJ/756/112 : Fermi/GBM GRB time-resolved spectral analysis (Lu+, 2012)
J/ApJ/763/15 : Fermi GRB analysis. III. T90 distributions (Qin+, 2013)
J/ApJS/211/13 : The second Fermi/GBM GRB catalog (4yr) (von Kienlin+, 2014)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- TID GBM trigger name of GRB
11- 12 I2 --- SpecNo Spectrum number in burst
14- 21 F8.3 s Tstart Start time of spectrum
23- 30 F8.3 s Tstop End time of spectrum
32- 35 A4 --- BEST BEST model of spectrum
37- 42 F6.4 10000/s/m2/keV Norm ? Normalization factor
44- 49 F6.4 10000/s/m2/keV e_Norm ? Error of normalization factor
51- 56 F6.3 --- alpha ? Low energy photon spectral index
58- 62 F5.3 --- e_alpha ? Error of alpha
64- 69 F6.3 --- beta ? High energy photon spectral index
71- 75 F5.3 --- e_beta ? Error of beta
77- 83 F7.2 keV Ep ? Peak energy
85- 91 F7.2 keV e_Ep ? Error of peak energy
93- 99 F7.2 keV Eb ? Break energy
101-106 F6.2 keV e_Eb ? Error of break energy
108-115 F8.2 --- CSTAT ? CSTAT value
117-119 I3 --- dof ? Degrees of freedom
121-130 F10.5 10000/s/m2 phFl ? Photon flux
131-136 F6.2 10000/s/m2 e_phFl ? Error of photon flux
141-150 E10.4 mW/m2 EnFl ? Energy flux
152-158 E7.2 mW/m2 e_EnFl ? Error of energy flux
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- TID GBM trigger name of GRB
11- 12 I2 --- Nspec Number of spectra with measured Ep
14- 19 F6.3 --- rhoEpph90 ? Spearman's Rank Correlation Coefficients
between Ep and the photon flux and the 90%
confidence interval rho(Ep-phfl, 90%)
21 A1 --- --- [+]
22- 26 F5.3 --- E_rhoEpph90 ? Upper error of rho(Ep-phfl, 90%)
28 A1 --- --- [-]
29- 33 F5.3 --- e_rhoEpph90 ? Lower error of rho(Ep-phfl, 90%)
35- 40 F6.3 --- rhoEpen90 ? Spearman's Rank Correlation Coefficients
between Ep and the energy flux and the 90%
confidence interval rho(Ep-enfl, 90%)
42 A1 --- --- [+]
43- 47 F5.3 --- E_rhoEpen90 ? Upper error of rho(Ep-enfl, 90%)
49 A1 --- --- [-]
50- 54 F5.3 --- e_rhoEpen90 ? Lower error of rho(Ep-enfl, 90%)
56- 61 F6.3 --- rhoEpt90 ? Spearman's Rank Correlation Coefficients
between Ep and the time and the 90%
confidence interval rho(E_p-time, 90%)
63 A1 --- --- [+]
64- 68 F5.3 --- E_rhoEpt90 ? Upper error of rho(E_p-time, 90%)
70 A1 --- --- [-]
71- 75 F5.3 --- e_rhoEpt90 ? Lower error of rho(E_p-time, 90%)
77- 85 A9 --- Trend90 Trend as determined by the computer for
90% confidence level
87- 92 F6.3 --- rhoEpph95 ? Spearman's Rank Correlation Coefficients
between Ep and the photon flux and the 95%
confidence interval rho rho(Ep-phfl, 95%)
94 A1 --- --- [+]
95- 99 F5.3 --- E_rhoEpph95 ? Upper error of rho(Ep-phfl, 95%)
101 A1 --- --- [-]
102-106 F5.3 --- e_rhoEpph95 ? Lower error of rho(Ep-phfl, 95%)
108-113 F6.3 --- rhoEpen95 ? Spearman's Rank Correlation Coefficients
between Ep and the energy flux and the 95%
confidence interval rho(Ep-enfl, 95%)
115 A1 --- --- [+]
116-120 F5.3 --- E_rhoEpen95 ? Upper error of rho(Ep-enfl, 95%)
122 A1 --- --- [-]
123-127 F5.3 --- e_rhoEpen95 ? Lower error of rho(Ep-enfl, 95%)
129-134 F6.3 --- rhoEpt95 ? Spearman's Rank Correlation Coefficients
between Ep and the time and the 95%
confidence interval rho(E_p-time, 95%)
136 A1 --- --- [+]
137-141 F5.3 --- E_rhoEpt95 ? Upper error of rho(E_p-time, 95%)
143 A1 --- --- [-]
144-148 F5.3 --- e_rhoEpt95 ? Lower error of rho(E_p-time, 95%)
150-158 A9 --- Trend95 Trend as determined by the computer for 95%
confidence level
160-165 F6.3 --- rhoEpph99 ? Spearman's Rank Correlation Coefficients
between Ep and the photon flux and the 99%
confidence interval rho rho(Ep-phfl, 99%)
167 A1 --- --- [+]
168-172 F5.3 --- E_rhoEpph99 ? Upper error of rho(Ep-phfl, 99%)
174 A1 --- --- [-]
175-179 F5.3 --- e_rhoEpph99 ? Lower error of rho(Ep-phfl, 99%)
181-186 F6.3 --- rhoEpen99 ? Spearman's Rank Correlation Coefficients
between Ep and the energy flux and the 99%
confidence interval rho(Ep-enfl, 99%)
188 A1 --- --- [+]
189-193 F5.3 --- E_rhoEpen99 ? Upper error of rho(Ep-enfl, 99%)
195 A1 --- --- [-]
196-200 F5.3 --- e_rhoEpen99 ? Lower error of rho(Ep-enfl, 99%)
202-207 F6.3 --- rhoEpt99 ? Spearman's Rank Correlation Coefficients
between Ep and the time and the 99%
confidence interval rho(E_p-time, 99%)
209 A1 --- --- [+]
210-214 F5.3 --- E_rhoEpt99 ? Upper error of rho(E_p-time, 99%)
216 A1 --- --- [-]
217-221 F5.3 --- e_rhoEpt99 ? Lower error of rho(E_p-time, 99%)
223-231 A9 --- Trend99 Trend as determined by the computer for 99%
confidence level
233-258 A26 --- TrendEye Trend determined by human eyes
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Acknowledgements:
Hoi-Fung Yu, sptfung(at)mpe.mpg.de
(End) Hoi-Fung Yu [MPE, Germany], Patricia Vannier [CDS] 22-Jan-2016