A Unified Jet Model of X‐Ray Flashes, X‐Ray–rich Gamma‐Ray Bursts, and Gamma‐Ray Bursts. I. Power‐Law–shaped Universal and Top‐Hat–shaped Variable Opening Angle Jet Models

Lamb, D. Q.; Donaghy, T.; Graziani, C.

doi:10.1086/426099

Cited by 133 publications

(179 citation statements)

References 47 publications

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“…iso relation (Amati relation) discovered in conventional GRBs (Amati et al 2002), which also extends to some previously observed X-ray flash (XRFs) (Lamb et al 2005). Here, E p is the cosmological rest frame spectral peak energy and E iso is the isotropic g-ray energy.…”

Section: Amati Et Al (Submitted) Demonstrated That Grb(xrf) 060218 Wsupporting

confidence: 74%

Messages from GRB 060218

Zhang

Liang

Gupta

et al. 2007

Phil. Trans. R. Soc. A.

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GRB 060218 is a watershed event. Statistically, its detection suggests that there is likely a distinct low-luminosity (LL) population of gamma-ray bursts (GRBs) whose event rate is much higher than that of conventional high-luminosity GRBs. This LL population may give significant contribution to the diffuse neutrino background flux at energies higher than 10 16 eV. The spectral lag of this burst is very long, and roughly follows the luminosity-lag relation of normal GRBs. This, along with the fact that it follows the E p -E iso relation as well, suggests that X-ray flashes (XRFs) are natural extension of GRBs in the softer regime and that GRBs and XRFs share the same radiation physics. We discuss how the broadband data pose strong constraints on possible models of the prompt emission of this GRB.

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Section: Amati Et Al (Submitted) Demonstrated That Grb(xrf) 060218 Wsupporting

confidence: 74%

Messages from GRB 060218

Zhang

Liang

Gupta

et al. 2007

Phil. Trans. R. Soc. A.

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“…Relative to other Swift detected GRBs, GRB 051117A is rather unremarkable, with a BAT fluence placing it at the mean of the brightness distribution, while its spectral characteristics place it at the soft end of the burst population. In fact based on Lamb's definition (Lamb et al 2005), GRB 051117A qualifies as an X-ray Rich Burst.…”

Section: Grb 051117amentioning

confidence: 99%

Swift multi-wavelength observations of the bright flaring burst GRB 051117A

Goad

Page

Godet

et al. 2007

A&A

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We report on the temporal and spectral characteristics of the early X-ray emission from the Gamma Ray Burst 051117A as observed by Swift. The superb quality of the early X-ray light-curve and spectra of this source, one of the brightest seen by the X-ray Telescope at such early times, allows an unprecedented look at the spectral and temporal evolution of the prompt and early afterglow emission for this GRB and allows us to place stringent limits on the detection of lines. GRB 051117A displays a highly complex light-curve, with an apparent initial slow decline of slope α = 0.77 ± 0.07 ( f (t) ∝ t −α ) dominated by numerous superposed flares of varying amplitude and duration. Between orbits 2 and 3, the X-ray light-curve drops abruptly, highlighting the dominance of flaring activity at early times, and indicating that the central engine for this burst remains active for several kiloseconds after the initial explosion. The late time slope (t > 10 4 s) also decays relatively slowly with a powerlaw index of α = 0.66, breaking to a steeper slope of 1.1, 170 ks after the BAT trigger. The X-ray light-curve at early times is characteristic of a noise process, consisting of random shots superposed on an underlying powerlaw decay, with individual shots well-modelled by a fast-rise and exponential decay spanning a broad range in rise-times and decay rates. A temporal spectral analysis of the early light-curve shows that the photon index and source intensity are highly correlated with the spectrum being significantly harder when brighter, consistent with the movement of the peak of the Band function to lower energies following individual flares. The high quality spectrum obtained from the first orbit of WT mode data, enables us to place a 3σ upper limit on the strength of any emission line features of EW < 15 eV, assuming a narrow emission-line of 100 eV at the peak of the effective area.

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“…The number of events detected by SPI-ACS and HETE-2 is relatively low compared to the total number of GRBs detected by HETE-2 during the INTEGRAL mission time. This is not surprising; it is the result of the low sensitivity of SPI-ACS to X-ray flashes and X-ray rich bursts, which constitute approximately 2/3 of the HETE-2 GRB sample (Lamb et al 2005). These events are characterized by an E p <80 keV and thus have their emission maximum below the SPI-ACS energy range.…”

Section: Sample Selectionmentioning

confidence: 99%

The 1st INTEGRAL SPI-ACS gamma-ray burst catalogue

Rau¹,

Kienlin²,

Hurley³

et al. 2005

A&A

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Abstract. We present the sample of gamma-ray bursts detected with the anti-coincidence shield ACS of the spectrometer SPI on-board INTEGRAL for the first 26.5 months of mission operation (up to Jan. 2005). SPI-ACS works as a nearly omnidirectional gamma-ray burst detector above ∼80 keV but lacks spatial and spectral information. In this catalogue, the properties derived from the 50 ms light curves (e.g., T 90 , C max , C int , variability, V/V max ) are given for each candidate burst in the sample. A strong excess of very short events with durations <0.25 s is found. This population is shown to be significantly different from the short-and long-duration burst sample by means of the intensity distribution and V/V max test and is certainly connected with cosmic ray hits in the detector. A rate of 0.3 true gamma-ray bursts per day is observed.

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A Unified Jet Model of X‐Ray Flashes, X‐Ray–rich Gamma‐Ray Bursts, and Gamma‐Ray Bursts. I. Power‐Law–shaped Universal and Top‐Hat–shaped Variable Opening Angle Jet Models

Cited by 133 publications

References 47 publications

Messages from GRB 060218

Messages from GRB 060218

Swift multi-wavelength observations of the bright flaring burst GRB 051117A

The 1st INTEGRAL SPI-ACS gamma-ray burst catalogue

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