Continuous optical monitoring   during the prompt emission of GRB 060111B

Klotz, A.; Gendre, B.; Stratta, G.; Atteia, J. L.; Boër, M.; Malacrino, F.; Damerdji, Y.; Behrend, R.

doi:10.1051/0004-6361:20065158

Cited by 52 publications

(65 citation statements)

References 15 publications

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“…In Stratta et al (2009) we presented the results of a multiwavelength campaing performed up to several months after the burst trigger for GRB 060111B, for which a prompt optical emission was observed with the robotic telescope TAROT (Klotz et al 2006). From the analysis of the detected host galaxy and from the early afterglow temporal and spectral properties, we estimated a redshift of about z ∼ 2 and found that a reverse shock origin of the prompt optical emission is consistent with the observations.…”

Section: Introductionsupporting

confidence: 65%

“…At z ∼ 2, the rest frame peak time is t p < 9 s after the BAT trigger (Klotz et al 2006). At the same time, the brightness of this burst in optic (m R ∼ 13.8 mag), although a non negligible dust extinction may affect this burst (see Stratta et al 2009), is relatively moderate if compared with other prompt optical emissions at similar epochs.…”

Section: Analysis and Resultsmentioning

confidence: 79%

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The origin of the prompt optical emission in GRB 060111B

Stratta¹,

Pozanenko

Atteia³

et al. 2011

Advances in Space Research

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Section: Introductionsupporting

confidence: 65%

Section: Analysis and Resultsmentioning

confidence: 79%

The origin of the prompt optical emission in GRB 060111B

Stratta¹,

Pozanenko

Atteia³

et al. 2011

Advances in Space Research

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“…The first Swift-BAT position notice of GRB 060111B was distributed at 20:16:03 UT, 20 s after the trigger, allowing the TAROT and ROTSE III robotic telescopes to observe during prompt emission (Klotz et al 2006;Yost et al 2006;Rykoff et al 2009). TAROT Calern (France) started observing at 20:16:11 UT (28 s after trigger) and detected a bright optical emission with R ∼ 13.7, fading as t −2.4±0.1 until 80 s (Klotz et al 2006).…”

Section: Introductionmentioning

confidence: 99%

A multiwavelength study of Swift GRB 060111B constraining the origin of its prompt optical emission

Stratta¹,

Pozanenko

Atteia

et al. 2009

A&A

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Context. The detection of bright optical emission measured with good temporal resolution during the prompt phase of GRB 060111B makes this GRB a rare event that is especially useful for constraining theories of the prompt emission. Aims. For this reason an extended multi-wavelength campaign was performed to further constrain the physical interpretation of the observations. Methods. In this work, we present the results obtained from our multi-wavelength campaign, as well as from the public Swift/BAT, XRT, and UVOT data. Results. We identified the host galaxy at R ∼ 25 mag from deep R-band exposures taken 5 months after the trigger. Its featureless spectrum and brightness, as well as the non-detection of any associated supernova 16 days after the trigger, enabled us to constrain the distance scale of GRB 060111B within 0.4 ≤ z ≤ 3 in the most conservative case. The host galaxy spectral continuum is best fit with a redshift of z ∼ 2, and other independent estimates converge to z ∼ 1-2. From the analysis of the early afterglow SED, we find that non-negligible host galaxy dust extinction, in addition to the Galactic one, affects the observed flux in the optical regime. The extinction-corrected optical-to-gamma-ray SED during the prompt emission shows a flux density ratio F γ /F opt = 10 −2 -10 −4 with spectral index β γ,opt > β γ , strongly suggesting a separate origin of the optical and gamma-ray components. This result is supported by the lack of correlated behavior in the prompt emission light curves observed in the two energy domains. The temporal properties of the prompt optical emission observed during GRB 060111B and their similarities to other rapidly-observed events favor interpretation of this optical light as radiation from the reverse shock. Observations are in good agreement with theoretical expectations for a thick shell limit in slow cooling regime. The expected peak flux is consistent with the observed one corrected for the host extinction, likely indicating that the starting time of the TAROT observations is very near to or coincident with the peak time. The estimated fireball initial Lorentz factor is Γ ≥ 260-360 at z = 1-2, similar to the Lorentz factors obtained from other GRBs. GRB 060111B is a rare case of a GRB with both a bright, well-observed optical counterpart and a "canonical" early X-ray light curve, thus providing a good test case of the reverse shock emission mechanism in both energy ranges.

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“…The early-time multiwavelength observations are also very useful in constraining the afterglow models, and hence the nature of the possible progenitors and the ambient media surrounding the GRBs (Castro-Tirado et al 1999;Piran 1999). Among the well-known examples of early observations in the pre-Swift era are GRB 990123 (Akerlof et al 1999) and GRB 041219 (Vestrand et al 2005) whereas GRB 050820A (Vestrand et al 2006), GRB 060111B (Klotz et al 2006), GRB 060210 (Stanek et al 2007) and GRB 071010B are good examples in the post-Swift era. The statistics of these examples of long-duration GRBs with very early-time Article published by EDP Sciences afterglow observations have improved because of the precise onboard localization by Swift and co-ordinated observations with the ground-based robotic optical telescopes (Gehrels et al 2004;Gomboc et al 2006).…”

Section: Introductionmentioning

confidence: 99%

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

Castro-Tirado

Jelínek

Kamble

et al. 2009

A&A

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Context. We present observations of the GRB 080319B afterglow at optical, mm, and radio frequencies between a few hours and 67 days after the burst. Aims. We attempt to understand the nature of this extraordinarily bright explosion based on the observed properties and its comparison with afterglow models. Methods. Our observations and other published multiwavelength data were used to reconstruct the light curves and spectral energy distributions of the burst afterglow. Results. Our results indicate that the observed features of the afterglow agrees equally well with the inter stellar matter and the stellar wind density profiles of the circumburst medium. In the case of both density profiles, the maximum synchrotron frequency ν m is below optical value and the cooling break frequency ν c is below X-rays, ∼10 4 s after the burst. The derived value of the Lorentz factor at the time of naked-eye brightness is also ∼300 for a corresponding blast-wave size of ∼10 18 cm. Conclusions. The numerical fit to the multiwavelength afterglow data constraints the values of physical parameters and the emission mechanism of the burst.

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Continuous optical monitoring during the prompt emission of GRB 060111B

Cited by 52 publications

References 15 publications

The origin of the prompt optical emission in GRB 060111B

The origin of the prompt optical emission in GRB 060111B

A multiwavelength study of Swift GRB 060111B constraining the origin of its prompt optical emission

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

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