Multi-wavelength observations of the GRB 080319B afterglow and the modeling constraints

Castro-Tirado, A. J.; Jelínek, M.; Kamble, A.; Gorosabel, J.; Postigo, A. de Ugarte; Prins, S.; Oreiro, R.; Chantry, Virginie; Трушкин, С. А.; Bremer, M.; Winters, J. M.; Pozanenko, A.; Krugly, Yu. N.; Slyusarev, I.; Kornienko, G. I.; Erofeeva, A.; Misra, Kuntal; Ramprakash, A. N.; Mohan, V.; Bhattacharya, Dipankar; Volnova, A.; Plá, J.; Ibrahimov, M.; Im, Myungshin; Volvach, A. E.; Wijers, R. A. M. J.

doi:10.1051/0004-6361/200811135

Cited by 22 publications

(8 citation statements)

References 46 publications

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“…With A = 0.01, e = 0.2, B ∼ 6 × 10 −7 (Racusin et al 2008), we find, using ZP09, 0 < 580. From the optical light curves (Pandey et al 2009), one can estimate the deceleration time of the afterglow to be less than 100 s. Setting the efficiency parameterη = 0.3 and the wind parameter A = 0.01 (Racusin et al 2008), we find, using SP99, 0 > 810.…”

Section: Grb 080319bmentioning

confidence: 97%

Lorentz factor constraint from the very early external shock of the gamma-ray burst ejecta

Zou

Piran

2010

Monthly Notices of the Royal Astronomical Society

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While it is generally agreed that the emitting regions in gamma‐ray bursts move ultra‐relativistically towards the observer, different estimates of the initial Lorentz factors, Γ0, lead to different at times conflicting estimates. We show here that the quiet periods in which the signals goes down below the instrumental thresholds put strong upper limits on the values of Γ0. According to the standard internal–external shock model, an external shock should develop during the prompt stage. This external shock radiates in the hard X‐rays to soft gamma‐rays bands and this emission should be seen as a smooth background signal. The observed deep minima indicate that this contribution is negligible. This limits, in turn, Γ0. We obtain upper limits on Γ0 for several bursts with typical values around hundreds. We compare these values with those obtained by the other methods, which typically yield lower limits. The results are marginally consistent leaving only a narrow range of allowed values for Γ0.

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Section: Grb 080319bmentioning

confidence: 97%

Lorentz factor constraint from the very early external shock of the gamma-ray burst ejecta

Zou

Piran

2010

Monthly Notices of the Royal Astronomical Society

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“…GRB 080319B This is the famous "naked eye" burst. Data in the V were collected from Pandey et al (2009). From Bloom et al (2009) we used data in r band and in the B, V, Rc and Ic bands.…”

Section: Grb 060814mentioning

confidence: 99%

Dust extinctions for an unbiased sample of gamma-ray burst afterglows

Covino¹,

Melandri²,

Salvaterra³

et al. 2013

Monthly Notices of the Royal Astronomical Society

101

123

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In this paper we compute rest-frame extinctions for the afterglows of a sample of Swift γ-ray bursts complete in redshift. The selection criteria of the sample are based on observational high-energy parameters of the prompt emission and therefore our sample should not be biased against dusty sight-lines. It is therefore expected that our inferences hold for the general population of γ-ray bursts. Our main result is that the optical/near-infrared extinction of γ-ray burst afterglows in our sample does not follow a single distribution. 87% of the events are absorbed by less than 2 mag, and 50% suffer from less than 0.3-0.4 mag extinction. The remaining 13% of the afterglows are highly absorbed. The true percentage of γ-ray burst afterglows showing high absorption could be even higher since a fair fraction of the events without reliable redshift measurement are probably part of this class. These events may be due to highly dusty molecular clouds/star forming regions associated with the γ-ray burst progenitor or along the afterglow line of sight, and/or to massive dusty host galaxies.No clear evolution in the dust extinction properties is evident within the redshift range of our sample, although the largest extinctions are at z ∼ 1.5 − 2, close to the expected peak of the star formation rate. Those events classified as dark are characterized, on average, by a higher extinction than typical events in the sample. A correlation between optical/near-infrared extinction and hydrogen-equivalent column density based on X-ray studies is shown although the observed N H appears to be well in excess compared to those observed in the Local Group. Dust extinction does not seem to correlate with GRB energetics or luminosity.

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“…Optical emission rises until around ≈ 20 s after the trigger, then it decays slightly but rises again at around ≈ 45 s after the trigger. Reported rise and decay power-law indices that correspond to the rise of the first peak and the decay of the last peak are α rise = −4.6 ± 0.7 (Pandey et al 2009) and α decay = 6.5 ± 0.9 (Racusin et al 2008), respectively.…”

Section: Sub-samplementioning

confidence: 99%

GRB 090727 and Gamma-Ray Bursts With Early-Time Optical Emission

Kopač

Kobayashi

Gomboc

et al. 2013

ApJ

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We present a multi-wavelength analysis of gamma-ray burst GRB 090727, for which optical emission was detected during the prompt gamma-ray emission by the 2-m autonomous robotic Liverpool Telescope and subsequently monitored for a further two days with the Liverpool and Faulkes telescopes. Within the context of the standard fireball model, we rule out a reverse shock origin for the early time optical emission in GRB 090727 and instead conclude that the early time optical flash likely corresponds to emission from an internal dissipation processes. Putting GRB 090727 into a broader observational and theoretical context, we build a sample of 36 gamma-ray bursts (GRBs) with contemporaneous early time optical and gamma-ray detections. From these GRBs, we extract a sub-sample of 18 GRBs, which show optical peaks during prompt gamma-ray emission, and perform detailed temporal and spectral analysis in gamma-ray, X-ray, and optical bands. We find that in most cases early time optical emission shows sharp and steep behaviour, and notice a rich diversity of spectral properties. Using a simple internal shock dissipation model, we show that the emission during prompt GRB phase can occur at very different frequencies via synchrotron radiation. Based on the results obtained from observations and simulation, we conclude that the standard external shock interpretation for early time optical emission is disfavoured in most cases due to sharp peaks (∆t/t < 1) and steep rise/decay indices, and that internal dissipation can explain the properties of GRBs with optical peaks during gamma-ray emission.

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Multi-wavelength observations of the GRB 080319B afterglow and the modeling constraints

Cited by 22 publications

References 46 publications

Lorentz factor constraint from the very early external shock of the gamma-ray burst ejecta

Lorentz factor constraint from the very early external shock of the gamma-ray burst ejecta

Dust extinctions for an unbiased sample of gamma-ray burst afterglows

GRB 090727 and Gamma-Ray Bursts With Early-Time Optical Emission

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