Earliest Detection of the Optical Afterglow of GRB 030329 and Its Variability

Sato, Rie; Kawai, N.; Suzuki, M.; Yatsu, Yoichi; Kataoka, J.; Takagi, Ryo; Yanagisawa, K.; Yamaoka, H.

doi:10.1086/381157

Cited by 26 publications

(34 citation statements)

References 21 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Yost et al (2005) interpret the break as the passage of the cooling frequency ν c through the R band. We note that Zeh et al (2006) found a similarly sharp break for the cooling frequency passage of the afterglow of GRB 030329 (Sato et al 2003). Also, that break was a bit stronger (Δα = 0.33 ± 0.01) than the theoretical prediction Δα = 0.25 , similar to this case (Δα = 0.31 ± 0.03).…”

Section: B2 Details On the Swift-era Golden Samplesupporting

confidence: 73%

THE AFTERGLOWS OFSWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFTANDSWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

Канн

Klose

Zhang

et al. 2010

ApJ

289

356

View full text Add to dashboard Cite

15131514 KANN ET AL.Vol. 720 ABSTRACT We have gathered optical photometry data from the literature on a large sample of Swift-era gamma-ray burst (GRB) afterglows including GRBs up to 2009 September, for a total of 76 GRBs, and present an additional three pre-Swift GRBs not included in an earlier sample. Furthermore, we publish 840 additional new photometry data points on a total of 42 GRB afterglows, including large data sets for GRBs 050319, 050408, 050802, 050820A, 050922C, 060418, 080413A, and 080810. We analyzed the light curves of all GRBs in the sample and derived spectral energy distributions for the sample with the best data quality, allowing us to estimate the host-galaxy extinction. We transformed the afterglow light curves into an extinction-corrected z = 1 system and compared their luminosities with a sample of pre-Swift afterglows. The results of a former study, which showed that GRB afterglows clustered and exhibited a bimodal distribution in luminosity space, are weakened by the larger sample. We found that the luminosity distribution of the two afterglow samples (Swift-era and pre-Swift) is very similar, and that a subsample for which we were not able to estimate the extinction, which is fainter than the main sample, can be explained by assuming a moderate amount of line-of-sight host extinction. We derived bolometric isotropic energies for all GRBs in our sample, and found only a tentative correlation between the prompt energy release and the optical afterglow luminosity at 1 day after the GRB in the z = 1 system. A comparative study of the optical luminosities of GRB afterglows with echelle spectra (which show a high number of foreground absorbing systems) and those without, reveals no indication that the former are statistically significantly more luminous. Furthermore, we propose the existence of an upper ceiling on afterglow luminosities and study the luminosity distribution at early times, which was not accessible before the advent of the Swift satellite. Most GRBs feature afterglows that are dominated by the forward shock from early times on. Finally, we present the first indications of a class of long GRBs, which form a bridge between the typical highluminosity, high-redshift events and nearby low-luminosity events (which are also associated with spectroscopic supernovae) in terms of energetics and observed redshift distribution, indicating a continuous distribution overall.

show abstract

Section: B2 Details On the Swift-era Golden Samplesupporting

confidence: 73%

THE AFTERGLOWS OFSWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFTANDSWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

Канн

Klose

Zhang

et al. 2010

ApJ

289

356

View full text Add to dashboard Cite

show abstract

“…Rykoff et al 2003, Sato et al 2003. These data should be calibrated properly to be compared with our observations.…”

Section: Photometrymentioning

confidence: 78%

The first hours of the optical afterglow from the cosmic gamma-ray burst 030329

et al. 2003

View full text Add to dashboard Cite

We present the first results of the observations of the extremely bright optical afterglow of gamma-ray burst (GRB) 030329 with the 1.5m Russian-Turkish telescope RTT150 (TÜBITAK National Observatory, Bakyrlytepe, Turkey). RTT150 was one of the first 1.5m-class telescopes pointed to the afterglow. Observations were started approximately 6 hours after the burst. During the first 5 hours of our observations the afterglow faded exactly as a power law with index −1.19 ± 0.01 in each of the BVRI Bessel filters. After that, in all BVRI filters simultaneously we observe a steepening of the power law light curve. The power law decay index smoothly approaches the value ≈ −1.9, observed by other observatories later. This power law break occurs at t − t 0 ≈ 0.57 days and lasts for ≈ ±0.1 days. We observe no variability above the gradual fading with the upper limits 10-1% on time scales 0.1-1000 s. Spectral flux distribution in four BVRI filters corresponds to the power law spectrum with spectral index α = 0.66 ± 0.01. The change of the power law decay index in the end of our observations can be interpreted as a signature of collimated ultrarelativistic jet. The afterglow flux distribution in radio, optical and x-rays is consistent with synchrotron spectrum. We continue our observations of this unique object with RTT150.

show abstract

“…9). Several authors Sato et al 2003) suggested that this additional break (with a change in the temporal slope of Á $ 0:3) may represent the so-called cooling break, predicted in the context of relativistic fireball models (Sari, Piran, & Narayan 1998) to occur as the cooling-break frequency, c , passes through the optical band (with Á ¼ 0:25). As seen in Figure 9, the combination of an early cooling break at day 0.25 and a jet break at day 0.5 allows a fair representation of the early optical data.…”

Section: Early Breaksmentioning

confidence: 98%

“…In particular, the data presented by Uemura et al (2003), , and Sato et al (2003) require at least one additional break to occur around day $0.25. Our compilation clearly elucidates this (Fig.…”

Section: Early Breaksmentioning

confidence: 99%

The Detailed Optical Light Curve of GRB 030329

Lipkin

Ofek

Gal‐Yam

et al. 2004

ApJ

133

128

View full text Add to dashboard Cite

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.

show abstract

Earliest Detection of the Optical Afterglow of GRB 030329 and Its Variability

Cited by 26 publications

References 21 publications

THE AFTERGLOWS OFSWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFTANDSWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

THE AFTERGLOWS OFSWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFTANDSWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

The first hours of the optical afterglow from the cosmic gamma-ray burst 030329

The Detailed Optical Light Curve of GRB 030329

Contact Info

Product

Resources

About