J/A+A/589/A97 GRBs Ep and Fourier PDS slope correlation (Dichiara+, 2016)
Correlation between peak energy and Fourier power density spectrum slope in
gamma-ray bursts.
Dichiara S., Guidorzi C., Amati L., Frontera F., Margutti R.
<Astron. Astrophys. 589, A97 (2016)>
=2016A&A...589A..97D 2016A&A...589A..97D (SIMBAD/NED BibCode)
ADC_Keywords: Gamma rays ; Combined data
Keywords: gamma-ray burst: general - methods: statistical
Abstract:
The origin of the gamma-ray burst (GRB) prompt emission still defies
explanation, in spite of recent progress made, for example, on the
occasional presence of a thermal component in the spectrum along with
the ubiquitous non-thermal component that is modelled with a Band
function. The combination of finite duration and aperiodic modulations
make GRBs hard to characterise temporally. Although correlations
between GRB luminosity and spectral hardness on one side and time
variability on the other side have long been known, the loose and
often arbitrary definition of the latter makes the interpretation
uncertain.
We characterise the temporal variability in an objective way and
search for a connection with rest-frame spectral properties for a
number of well-observed GRBs.
We studied the individual power density spectra (PDS) of 123 long GRBs
with measured redshift, rest-frame peak energy Ep,i of the
time-averaged νFν spectrum, and well-constrained PDS slope
α detected with Swift, Fermi and past spacecraft. The PDS were
modelled with a power law either with or without a break adopting a
Bayesian Markov chain Monte Carlo technique.
Description:
We report in the table the parameters resulting from the power density
spectrum analysis of a sample of 123 long GRBs with measure of
redshift. The PDS best-fit parameters are listed together with the
isotropic-equivalent energy and spectral rest-frame peak energy
values. Uncertainties are 1 sigma confidence.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 92 143 PDS parameters of a sample of 123 long GRBs
refs.dat 75 104 References
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See also:
J/ApJ/777/132 : A search for progenitors of short GRBs (Dichiara+, 2013)
J/A+A/589/A98 : Swift GRBs individual power density spectra (Guidorzi+, 2016)
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 (YYMMNNA)
9- 15 A7 --- Exp Experiment use for detection and
spectroscopy (1)
17- 22 F6.4 --- z Redshift
24- 29 F6.3 [10+45J] log(E52) logarithmic value of Eiso
(isotropic-equivalent radiated energy)
(in 1052erg)
31- 35 F5.3 [10+45J] e_log(E52) logarithmic error related to Log(E52)
(in 1052erg)
37- 41 F5.3 [keV] log(Epi) logarithmic value of Ep,i
(peak energy of the nuFnu spectrum)
43- 47 F5.3 [keV] e_log(Epi) logarithmic error related to Log(Epi)
49- 54 F6.1 s tstart Time interval used for the PDS extraction:
start time (2)
56- 60 F5.1 s tstop Time interval used for the PDS extraction:
stop time (2)
62- 66 F5.3 --- alpha PDS power-law index
68- 72 F5.3 --- e_alpha alpha error
74- 79 F6.3 [Hz] logfb ? logarithmic break frequency of PDS (3)
81- 85 F5.3 [Hz] e_logfb ? logarithmic error related to logfb
87- 88 I2 --- r_z [1-70]? References for redshift values,
in refs.dat file
90- 92 I3 --- r_log(Epi) [71-104]? References for Ep,i values,
in refs.dat file
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Note (1): Fer+Swi indicates that both Fermi and Swift data gave acceptable
results for that GRB. The values are reported in two consecutive lines,
referring to Fermi and Swift, respectively.
Note (2): Times (in seconds) are referred to the trigger time.
Note (3): Only for the GRBs whose PDS are best fit with a bent power-law model.
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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 ocde
5- 23 A19 --- BibCode BibCode
25- 48 A24 --- aut Atuhor's name
51- 75 A25 --- Com Comments
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Acknowledgements:
Simone Dichiara, dichiara(at)fe.infn.it
(End) Simone Dichiara [Univ. Ferrara], Patricia Vannier [CDS] 17-Mar-2016