Gamma-Ray Burst Peak Duration as a Function of Energy

Fenimore, E. E.; Zand, J. J. M. in ’t; Norris, J. P.; Bonnell, J. T.; Nemiroff, Robert J.

doi:10.1086/309603

Cited by 230 publications

(286 citation statements)

References 8 publications

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“…It shows that there is no significant time dilation of the faint GRBs. We note here that because the widths of the peaks in the time histories of GRBs -and the durations of GRBsare shorter at higher energies (e.g., Fenimore et al 1995 ), this partly (but only partly) compensates for the time dilation due to the cosmological redshift. GRB durations go approximately like E −0.4 , so that this effect shortens the observed durations of GRBs at a redshift z = 10 relative to the durations of GRBs at a redshift z = 1 by a factor of about [(1+10)/(1+1)] 0.4 = 2.…”

Section: X-ray Rich Grbs and The Hardness-intensity Correlationmentioning

confidence: 78%

Spectral analysis of 35 GRBs/XRFs observed with HETE-2/FREGATE

Barraud¹,

Olive²,

Lestrade³

et al. 2003

A&A

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112

101

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Abstract. We present a spectral analysis of 35 GRBs detected with the HETE-2 gamma-ray detectors (the FREGATE instrument) in the energy range 7-400 keV. The GRB sample analyzed is made of GRBs localized with the Wide Field X-ray Monitor onboard HETE-2 or with the GRB Interplanetary Network. We derive the spectral parameters of the time-integrated spectra, and present the distribution of the low-energy photon index, alpha, and of the peak energy, E p . We then discuss the existence and nature of the recently discovered X-Ray Flashes and their relationship with classical GRBs.

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Section: X-ray Rich Grbs and The Hardness-intensity Correlationmentioning

confidence: 78%

Spectral analysis of 35 GRBs/XRFs observed with HETE-2/FREGATE

Barraud¹,

Olive²,

Lestrade³

et al. 2003

A&A

Self Cite

112

101

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“…For this subset we could study the analogous relation in the GRB source rest frame. The corresponding intrinsic quantities, denoted with subscript i, were calculated as follows: τ i = τ/(1 + z) 0.6 , which combines the cosmological dilation and the narrowing of pulses with energy as modelled by Fenimore et al (1995); T 90,i = T 90 /(1 + z). In the latter case we did not apply the narrowing of pulses to the overall duration of the burst: this is correct especially in the presence of waiting times.…”

Section: Dominant Timescale Vs Durationmentioning

confidence: 99%

Individual power density spectra ofSwiftgamma-ray bursts

Guidorzi

Dichiara

Amati

2016

A&A

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Context. Timing analysis can be a powerful tool with which to shed light on the still obscure emission physics and geometry of the prompt emission of gamma-ray bursts (GRBs). Fourier power density spectra (PDS) characterise time series as stochastic processes and can be used to search for coherent pulsations and, more in general, to investigate the dominant variability timescales in astrophysical sources. Because of the limited duration and of the statistical properties involved, modelling the PDS of individual GRBs is challenging, and only average PDS of large samples have been discussed in the literature thus far. Aims. We aim at characterising the individual PDS of GRBs to describe their variability in terms of a stochastic process, to explore their variety, and to carry out for the first time a systematic search for periodic signals and for a link between PDS properties and other GRB observables.Methods. We present a Bayesian procedure that uses a Markov chain Monte Carlo technique and apply it to study the individual PDS of 215 bright long GRBs detected with the Swift Burst Alert Telescope in the 15−150 keV band from January 2005 to May 2015. The PDS are modelled with a power-law either with or without a break. Results. Two classes of GRBs emerge: with or without a unique dominant timescale. A comparison with active galactic nuclei (AGNs) reveals similar distributions of PDS slopes. Unexpectedly, GRBs with subsecond-dominant timescales and duration longer than a few tens of seconds in the source frame appear to be either very rare or altogether absent. Three GRBs are found with possible evidence for a periodic signal at 3.0-3.2σ (Gaussian) significance, corresponding to a multi-trial chance probability of ∼1%. Thus, we found no compelling evidence for periodic signal in GRBs. Conclusions. The analogy between the PDS of GRBs and of AGNs could tentatively indicate similar stochastic processes that rule BH accretion across different BH mass scales and objects. In addition, we find evidence that short dominant timescales and duration are not completely independent of each other, in contrast with commonly accepted paradigms.

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“…We have an assumed functional form for g(z) with one unknown constant c . This constant can be calculated using the dependence of on energy bands (Fenimore et al 1995). These equations can be evaluated for the sensitivity of calculated quantities such as z and L B on observables such as P ph and hEi (which in turn depends on the spectral parameters).…”

Section: Calculatinggredshiftsmentioning

confidence: 99%

Gamma‐Ray Burst Intensity Distributions

Band

Norris

Bonnell³

2004

ApJ

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We use the lag-luminosity relation to calculate self-consistently the redshifts, apparent peak bolometric luminosities L B , and isotropic energies E iso for a large sample of BATSE gamma-ray bursts. We consider two different forms of the lag-luminosity relation; for both forms the median redshift for our burst database is 1.6. We model the resulting E iso sample with power-law and Gaussian probability distributions without redshift evolution, both of which are reasonable models. The power-law model has an index of E ¼ 1:76 AE 0:05 (95% confidence), where p(E iso ) / E À E iso . The simple universal jet profile model suggested but did not require E ¼ 2, and subsequent physically reasonable refinements to this model permit greater diversity in E , as well as deviations from a power law; therefore, our observed E iso probability distribution does not disprove the universal jet model.

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Gamma-Ray Burst Peak Duration as a Function of Energy

Cited by 230 publications

References 8 publications

Spectral analysis of 35 GRBs/XRFs observed with HETE-2/FREGATE

Spectral analysis of 35 GRBs/XRFs observed with HETE-2/FREGATE

Individual power density spectra ofSwiftgamma-ray bursts

Gamma‐Ray Burst Intensity Distributions

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