JET BREAKS AND ENERGETICS OF<i>Swift</i>GAMMA-RAY BURST X-RAY AFTERGLOWS

Racusin, J. L.; Liang, En‐Wei; Burrows, D. N.; Falcone, A.; Sakamoto, T.; Zhang, Bingbing; Evans, P. A.; Osborne, J. P.

doi:10.1088/0004-637x/698/1/43

Cited by 309 publications

(447 citation statements)

References 111 publications

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“…The optical/NIR temporal index α = −0.73 ± 0.01 of the segment a is consistent within 3σ errors with the closure relations (Granot & Sari 2002;Dai & Cheng 2001;Zhang & Mészáros 2004;Racusin et al 2009) for a normal decay in the ν m < ν < ν c regime, where the jet is interacting with a homogeneous ISM and is in the slow cooling phase. The corresponding power-law index of electron energy distribution p = 1.44 ± 0.16 is very hard.…”

Section: Closure Relationssupporting

confidence: 80%

The two-component jet of GRB 080413B

Filgas

Krühler

Greiner

et al. 2011

A&A

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Aims. The quick and precise localization of GRBs by the Swift telescope allows the early evolution of the afterglow light curve to be captured by ground-based telescopes. With GROND measurements we can investigate the optical/near-infrared light curve of the afterglow of gamma-ray burst 080413B in the context of late rebrightening. Methods. Multi-wavelength follow-up observations were performed on the afterglow of GRB 080413B. X-ray emission was detected by the X-ray telescope onboard the Swift satellite and obtained from the public archive. Optical and near-infrared photometry was performed with the seven-channel imager GROND mounted at the MPG/ESO 2.2 m telescope and additionally with the REM telescope, both in La Silla, Chile. The light curve model was constructed using the obtained broad-band data. Results. The broad-band light curve of the afterglow of GRB 080413B is well fitted with an on-axis two-component jet model. The narrow ultra-relativistic jet is responsible for the initial decay, while the rise of the moderately relativistic wider jet near its deceleration time is the cause of the rebrightening of the light curve. The later evolution of the optical/NIR light curve is then dominated by the wide component, the signature of which is almost negligible in the X-ray wavelengths. These components have opening angles of θ n ∼ 1.7 • and θ w ∼ 9 • , and Lorentz factors of Γ n > 188 and Γ w ∼ 18.5. We calculated the beaming-corrected energy release to be E γ = 7.9 × 10 48 erg.

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Section: Closure Relationssupporting

confidence: 80%

The two-component jet of GRB 080413B

Filgas

Krühler

Greiner

et al. 2011

A&A

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“…Since Dainotti, Cardone & Capozziello (2008) have shown a correlation between the luminosity at the end of the X-ray plateau with the time the plateau phase ceases, we examined whether the plateau phase plays a role in our correlation. In our sample we find 35 GRBs that have a plateau following the criteria of Racusin et al (2009). Repeating the Spearman rank correlation for log LX,200s − αX,>200s for these GRBs, we find a coefficient of -0.73 at a confidence of 4.97σ, indicating a strong correlation.…”

Section: Observational Resultssupporting

confidence: 56%

“…In order to compare the afterglow properties with the prompt emission properties we determined the isotropic γ-ray energy Eiso and peak energy, E peak from the γ-ray emission, following Racusin et al (2009). The BAT fluence was converted to Eiso at a rest-frame bandpass of 10 to 10000 keV using equation 4 from Bloom, Frail & Sari (2001).…”

Section: Grb Afterglow Samplementioning

confidence: 99%

Exploring the canonical behaviour of long gamma-ray bursts using an intrinsic multiwavelength afterglow correlation

Oates

Racusin

Pasquale

et al. 2015

Mon. Not. R. Astron. Soc.

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In this paper we further investigate the relationship, reported by Oates et al. (2012), between the optical/UV afterglow luminosity (measured at restframe 200 s) and average afterglow decay rate (measured from restframe 200 s onwards) of long duration Gamma-ray Bursts (GRBs). We extend the analysis by examining the X-ray light curves, finding a consistent correlation. We therefore explore how the parameters of these correlations relate to the prompt emission phase and, using a Monte Carlo simulation, explore whether these correlations are consistent with predictions of the standard afterglow model. We find significant correlations between: log L O,200s and log L X,200s ; α O,>200s and α X,>200s , consistent with simulations. The model also predicts relationships between log E iso and log L 200,s , however, while we find such relationships in the observed sample, the slope of the linear regression is shallower than that simulated and inconsistent at 3σ. Simulations also do not agree with correlations observed between log L 200s and α >200s , or log E iso and α >200s . Overall, these observed correlations are consistent with a common underlying physical mechanism producing GRBs and their afterglows regardless of their detailed temporal behaviour. However, a basic afterglow model has difficulty explaining all the observed correlations. This leads us to briefly discuss alternative more complex models.

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“…3, given the wide range of measurements determined from slope changes in LGRB afterglow light curves (see, e.g., Racusin et al 2009). Unfortunately, recent simulations have shown that this change in the afterglow light curve may occur at much later times than currently thought, and therefore, the change in the light curve that we currently observe is not in fact due the result of the jet opening angle (van Eerten & MacFadyen 2012).…”

Section: Model Limitationsmentioning

confidence: 99%

The First Billion Years project: gamma-ray bursts at z > 5

Elliott

Khochfar

Greiner

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Long gamma-ray burst's (LGRB's) association to the death of massive stars suggest they could be used to probe the cosmic star formation history (CSFH) with high accuracy, due to their high luminosities. We utilise cosmological simulations from the First Billion Years project to investigate the biases between the CSFH and the LGRB rate at z > 5, assuming various different models and constraints on the progenitors of LGRBs. We populate LGRBs using a selection based on environmental properties and demonstrate that the LGRB rate should trace the CSFH to high redshifts. The measured LGRB rate suggests that LGRBs have opening angles of θ jet = 0.1 • , although the degeneracy with the progenitor model cannot rule out an underlying bias. We demonstrate that proxies that relate the LGRB rate with global LGRB host properties do not reflect the underlying LGRB environment, and are in fact a result of the host galaxy's spatial properties, such that LGRBs can exist in galaxies of solar metallicity. However, we find a class of host galaxies that have low stellar mass and are metal-rich, and that their metallicity dispersions would not allow low-metallicity environments. Detection of hosts with this set of properties would directly reflect the progenitor's environment. We predict that 10% of LGRBs per year are associated with this set of galaxies that would have forbidden line emission that could be detected by instruments on the James Webb Space Telescope. Such a discovery would place strong constraints on the collapsar model and suggest other avenues to be investigated.

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JET BREAKS AND ENERGETICS OFSwiftGAMMA-RAY BURST X-RAY AFTERGLOWS

Cited by 309 publications

References 111 publications

The two-component jet of GRB 080413B

The two-component jet of GRB 080413B

Exploring the canonical behaviour of long gamma-ray bursts using an intrinsic multiwavelength afterglow correlation

The First Billion Years project: gamma-ray bursts at z > 5

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