Early optical emission from the γ-ray burst of 4 October 2002

Fox, D. B.; Yost, S. A.; Kulkarni, S. R.; Torii, K.; Katô, Takeo; Yamaoka, H.; Šako, M.; Harrison, Fiona A.; Sari, R.; Price, P. A.; Berger, E.; Söderberg, A. M.; Djorgovski, S. G.; Barth, Aaron J.; Pravdo, S. H.; Frail, D. A.; Gal‐Yam, A.; Lipkin, Y.; Mauch, T.; Harrison, Craig; Buttery, H.

doi:10.1038/nature01504

Cited by 105 publications

(81 citation statements)

References 14 publications

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“…Comparing the available data reported by Tiengo et al (2003) with our optical light curves and assuming that the X-ray and optical flux are correlated, as found by Fox et al (2003) for GRB 021004, we expect the optical-to-X-ray slope index to remain approximately constant. As we have shown in x 4.1, this is indeed the case, especially if the early X-ray point, obtained before the proposed cooling transition, is discarded.…”

Section: Can a Single Broken Power Law Provide A Good Fit To The Data?mentioning

confidence: 84%

“…In particular, for some OTs, a dense temporal sampling of the light curve, sometimes starting shortly (minutes to hours) after the GRB trigger, was carried out by worldwide observing networks. A case to note is the OT of GRB 021004, where multiple bumps and wiggles in the light curve, probably not associated with an SN, were first observed (e.g., Bersier et al 2003;Mirabal et al 2003;Fox et al 2003).…”

Section: Introductionmentioning

confidence: 99%

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The Detailed Optical Light Curve of GRB 030329

Lipkin

Ofek

Gal‐Yam

et al. 2004

ApJ

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133

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We present densely sampled BVRI light curves of the optical transient associated with the gamma-ray burst (GRB) 030329, the result of a coordinated observing campaign conducted at five observatories. Augmented with published observations of this GRB, the compiled optical data set contains 2687 photometric measurements, obtained between 78 minutes and 79 days after the burst. This data set allows us to follow the photometric evolution of the transient with unprecedented detail. We use the data to constrain the light curve of the underlying supernova (SN) 2003dh and show that it evolved faster than and was probably somewhat fainter than the Type Ic SN 1998bw, associated with GRB 980425. We find that our data can be described by a broken power-law decay perturbed by a complex variable component. The early-and late-time decay slopes are determined to be 1 % 1:1 and 2 % 2. Assuming this single-break power-law model, we constrain the break to lie between $3 and $8 days after the burst. This simple, singly broken power-law model, derived only from the analysis of our optical observations, may also account for available multiband data, provided that the break happened $8 days after the burst. The more complex double-jet model of Berger et al. provides a comparable fit to the optical, X-ray, millimeter, and radio observations of this event. The unique early coverage available for this event allows us to trace the color evolution of the afterglow during the first hours after the burst. We detect a significant change in optical colors during the first day. Our color analysis is consistent with a cooling-break frequency sweeping through the optical band during the first day. The light curves of GRB 030329 reveal a rich array of variations, superposed over the mean power-law decay. We find that the early variations (P8 days after the burst) are asymmetric, with a steep rise followed by a relatively slower (by a factor of about 2) decline. The variations maintain a similar timescale during the first 4 days and then get significantly longer. The structure of these variations is similar to those previously detected in the afterglows of several GRBs.

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Section: Can a Single Broken Power Law Provide A Good Fit To The Data?mentioning

confidence: 84%

Section: Introductionmentioning

confidence: 99%

The Detailed Optical Light Curve of GRB 030329

Lipkin

Ofek

Gal‐Yam

et al. 2004

ApJ

Self Cite

133

128

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“…Figure 2 shows the light curves in the visible, NIR and millimetre bands for GRB 021004. The optical/NIR data points are plotted together with other published data (Fox et al 2003;Uemura et al 2003;Pandey et al 2003;Bersier et al 2003;Holland et al 2003;Mirabal et al 2003;Pak et al 2005) in order to show the complexity of the light curves.…”

Section: Brief Description Of the Modellingmentioning

confidence: 99%

GRB 021004 modelled by multiple energy injections

Postigo¹,

Castro-Tirado²,

Gorosabel³

et al. 2005

A&A

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GRB 021004 is one of the best sampled gamma-ray bursts (GRB) to date, although the nature of its light curve is still being debated. Here we present 107 new optical, near-infrared (NIR) and millimetre observations, ranging from 2 h to more than a year after the burst. Fitting the multiband data to a model based on multiple energy injections suggests that at least 7 refreshed shocks took place during the evolution of the afterglow, implying a total energy release (collimated within an angle of 1.• 8) of ∼8 × 10 51 erg. Analysis of the late photometry reveals that the GRB 021004 host is a low extinction (A V ∼ 0.1) starburst galaxy with M B −22.0.

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“…3465,3469,3470,3489,3491,3488,3493,3486,3506. Data for GRB 021004 are from Fox et al (2003a) and GCNCs 1564GCNCs , 1566GCNCs , 1570GCNCs , 1573GCNCs , 1576GCNCs , 1577GCNCs , 1578GCNCs , 1580GCNCs , 1581GCNCs , 1582GCNCs , 1584GCNCs , 1587GCNCs , 1591GCNCs , 1594GCNCs , 1606GCNCs , 1614GCNCs , 1615GCNCs , 1628. Data for GRB 050319 are from Woźniak et al (2005) and GCNCs …”

Section: Early Optical Grb Afterglowsmentioning

confidence: 99%

Early re-brightening of the afterglow of GRB 050525a

Klotz

Boër

Atteia

et al. 2005

A&A

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Abstract. We present time resolved optical data acquired by the TAROT automated observatory on the afterglow of GRB 050525a from 6 to 136 min after the GRB. We find evidence for a rapid re-brightening of 0.65 mag of the afterglow at ∼33 min after the GRB. The decay slope α is 1.14 ± 0.07 in the first part and is 1.23 ± 0.27 after the re-brightening event.The afterglow of GRB 050525a is the third known afterglow that exhibits a re-brightening event beginning at 0.01-0.02 day in the rest time frame.

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Early optical emission from the γ-ray burst of 4 October 2002

Cited by 105 publications

References 14 publications

The Detailed Optical Light Curve of GRB 030329

The Detailed Optical Light Curve of GRB 030329

GRB 021004 modelled by multiple energy injections

Early re-brightening of the afterglow of GRB 050525a

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