The Ultra-Long Gamma-Ray Burst 111209a: The Collapse of a Blue Supergiant?

Gendre, B.; Stratta, G.; Atteia, J. L.; Basa, S.; Boër, M.; Coward, D. M.; Cutini, S.; D’Elia, V.; Howell, E. J.; Klotz, A.; Piro, L.

doi:10.1088/0004-637x/766/1/30

Cited by 192 publications

(268 citation statements)

References 71 publications

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“…It might be wondered whether this holds for so-called ultralong events (Levan et al 2014;Gendre et al 2013;Stratta et al 2013;Virgili et al 2013;Zhang et al 2014;Boer et al 2015). We therefore report our results on 130925A (Evans et al 2014;Piro et al 2014), although Swift-BAT data do not cover it in its entirety.…”

Section: Dominant Timescale Vs Durationmentioning

confidence: 93%

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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Section: Dominant Timescale Vs Durationmentioning

confidence: 93%

Individual power density spectra ofSwiftgamma-ray bursts

Guidorzi

Dichiara

Amati

2016

A&A

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“…Within these detections, 7 GRBs are previously classified as ultralong GRBs, which are GRB121027A, GRB111215A, GRB111209A, GRB101225A, GRB100316D, GRB 090417B, GRB060218 (e.g., Gendre et al 2013;Virgili et al 2013;Levan et al 2014;Boër et al 2015). Studies usually refer "ultra-long GRBs" to bursts with durations  kiloseconds (e.g., Gendre et al 2013;Stratta et al 2013;Evans et al 2014;Levan et al 2014;Boër et al 2015), however, no unified definition has been adopted. In this paper, an ultra-long GRB is referred to those events with observed durations longer than 1000 s in BAT energy band.…”

Section: False-detection Rate: Searching For Weak Emissionmentioning

confidence: 99%

The Third Swift Burst Alert Telescope Gamma-Ray Burst Catalog

Lien

Sakamoto

Barthelmy

et al. 2016

ApJ

301

320

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To date, the Burst Alert Telescope (BAT) onboard Swift has detected ∼1000 gamma-ray bursts (GRBs), of which ∼360 GRBs have redshift measurements, ranging from z=0.03 to z=9.38. We present the analyses of the BATdetected GRBs for the past ∼11 years up through GRB151027B. We report summaries of both the temporal and spectral analyses of the GRB characteristics using event data (i.e., data for each photon within approximately 250 s before and 950 s after the BAT trigger time), and discuss the instrumental sensitivity and selection effects of GRB detections. We also explore the GRB properties with redshift when possible. The result summaries and data products are available at http://swift.gsfc.nasa.gov/results/batgrbcat/index.html. In addition, we perform searches for GRB emissions before or after the event data using the BAT survey data. We estimate the false detection rate to be only one false detection in this sample. There are 15 ultra-long GRBs (∼2% of the BAT GRBs) in this search with confirmed emission beyond ∼1000 s of event data, and only two GRBs (GRB100316D and GRB101024A) with detections in the survey data prior to the starting of event data.

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“…We collect all GRBs with information of redshift, fluence, peak energy, and photon indices from GCN Circulars Archive 1 Cucchiara et al (2011) and Gendre et al (2013) (Band et al 1993),…”

Section: Updated Grb Samplementioning

confidence: 99%

Measuring dark energy with theE_iso–E_pcorrelation of gamma-ray bursts using model-independent methods

Wang

Cheng

et al. 2015

A&A

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We use two model-independent methods to standardize long gamma-ray bursts (GRBs) using the E iso − E p correlation (log E iso = a + b log E p ), where E iso is the isotropic-equivalent gamma-ray energy and E p is the spectral peak energy. We update 42 long GRBs and attempt to constrain the cosmological parameters. The full sample contains 151 long GRBs with redshifts from 0.0331 to 8.2. The first method is the simultaneous fitting method. We take the extrinsic scatter σ ext into account and assign it to the parameter E iso . The best-fitting values are a = 49.15 ± 0.26, b = 1.42 ± 0.11, σ ext = 0.34 ± 0.03 and Ω m = 0.79 in the flat ΛCDM model. The constraint on Ω m is 0.55 < Ω m < 1 at the 1σ confidence level. If reduced χ 2 method is used, the best-fit results are a = 48.96 ± 0.18, b = 1.52 ± 0.08, and Ω m = 0.50 ± 0.12. The second method uses type Ia supernovae (SNe Ia) to calibrate the E iso − E p correlation. We calibrate 90 high-redshift GRBs in the redshift range from 1.44 to 8.1. The cosmological constraints from these 90 GRBs are Ω m = 0.23 +0.06 −0.04 for flat ΛCDM and Ω m = 0.18 ± 0.11 and Ω Λ = 0.46 ± 0.51 for non-flat ΛCDM. For the combination of GRB and SNe Ia sample, we obtain Ω m = 0.271 ± 0.019 and h = 0.701 ± 0.002 for the flat ΛCDM and the non-flat ΛCDM, and the results are Ω m = 0.225 ± 0.044, Ω Λ = 0.640 ± 0.082, and h = 0.698 ± 0.004. These results from calibrated GRBs are consistent with that of SNe Ia. Meanwhile, the combined data can improve cosmological constraints significantly, compared to SNe Ia alone. Our results show that the E iso − E p correlation is promising to probe the high-redshift Universe.

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The Ultra-Long Gamma-Ray Burst 111209a: The Collapse of a Blue Supergiant?

Cited by 192 publications

References 71 publications

Individual power density spectra ofSwiftgamma-ray bursts

Individual power density spectra ofSwiftgamma-ray bursts

The Third Swift Burst Alert Telescope Gamma-Ray Burst Catalog

Measuring dark energy with theE_iso–E_pcorrelation of gamma-ray bursts using model-independent methods

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The Ultra-Long Gamma-Ray Burst 111209a: The Collapse of a Blue Supergiant?

Cited by 192 publications

References 71 publications

Individual power density spectra ofSwiftgamma-ray bursts

Individual power density spectra ofSwiftgamma-ray bursts

The Third Swift Burst Alert Telescope Gamma-Ray Burst Catalog

Measuring dark energy with theEiso–Epcorrelation of gamma-ray bursts using model-independent methods

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Product

Resources

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Measuring dark energy with theE_iso–E_pcorrelation of gamma-ray bursts using model-independent methods