GRB 991216 Joins the Jet Set: Discovery and Monitoring of Its Optical Afterglow

Halpern, J. P.; Uglesich, R.; Mirabal, N.; Kassin, Susan; Thorstensen, J. R.; Keel, William C.; Diercks, A.; Bloom, J.; Harrison, Fiona A.; Mattox, J. R.; Eracleous, Michael

doi:10.1086/317134

Cited by 94 publications

(124 citation statements)

References 29 publications

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“…3), tends to fall near the isotropic models and along a 1 a 2 the jet models. Well-observed bursts with light-curve breaks are shown : GRB 990123 (Holland et al 2000), GRB 990510 (Stanek et al 1999), GRB 991216 (Garnavich et al 2000a ;Halpern et al 2000), GRB 000301C (Garnavich, Loeb, & Stanek 2000b ;Rhoads & Fruchter 2001), GRB 980519 (Jaunsen et al 2001), GRB 000926 (Price et al 2001a). We do not include GRB 991208 (Castro-Tirado et al 2001), which is well observed until the "" break ÏÏ deÐned by only one point.…”

Section: Discussionmentioning

confidence: 94%

RapidUBVRIFollow‐up of the Highly Collimated Optical Afterglow of GRB 010222

Stanek

Garnavich

Jha

et al. 2001

ApJ

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We present the earliest optical observations of the optical counterpart to the gamma-ray burst (GRB) 010222, obtained with the Fred L. Whipple Observatory 1.2 m telescope in UBV RI passbands, starting 3.64 hr after the burst (0.4 hr after public notiÐcation of the burst localization). We also present late R-band observations of the afterglow obtained with the 1.8 m Vatican Advanced Technology Telescope D25 days after the burst. The temporal analysis of our data joined with published data indicates a steepening decay, independent of wavelength, asymptotically approaching at early times F l P t~0.80B0.05 (t > 1 day) and at late times, with a sharp break at days. This is the F l P t~1.30B0.05 t b \ 0.72^0.10 second earliest observed break of any afterglow (after GRB 980519), which clearly indicates the importance of rapid multiband follow-up for GRB afterglow research. The optical spectral energy distribution, corrected for small Galactic reddening, can be Ðtted fairly well by a single power law with F l P l~1.07B0.09. However, when we Ðt using our BV RI data only, we obtain a shallower slope of [0.88^0.10, in excellent agreement with the slope derived from our low-resolution spectrum ([0.89^0.03). The spectral slope and light-curve decay slopes we derive are not consistent with a jet model despite the presence of a temporal break. SigniÐcant host dust extinction with a starburst reddening law would Ñatten the spectral index to match jet predictions and still be consistent with the observed spectral energy distribution. We derive an opening angle of smaller than any listed in the 2¡ .1, recent compilation of Frail et al. The total beamed energy corrected for the jet geometry is 4 ] 1050 ergs, very close to the "" standard ÏÏ value of 5 ] 1050 ergs found by Frail et al. for a number of other bursts with light-curve breaks.

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Section: Discussionmentioning

confidence: 94%

RapidUBVRIFollow‐up of the Highly Collimated Optical Afterglow of GRB 010222

Stanek

Garnavich

Jha

et al. 2001

ApJ

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“…The optical AG of GRB 000301c is practically unextinct, that of GRB 000926 has strong extinction in the host galaxy (e.g., Fynbo et al 2001) and that of GRB 991216 has strong extinction both in the host galaxy and in ours (e.g., Halpern et al 2000). We discuss GRBs 991208, 000418, 000510, 990123 and 970508 in slightly less detail.…”

Section: Thus the Total Number Of Parameters In Our Broadband Fits Imentioning

confidence: 97%

“…The NIR/optical data for this GRB are from Halpern et al (2000) and Garnavich et al (2000a); the radio data from Frail et al (2000b). In Fig.…”

Section: Grb 991216mentioning

confidence: 99%

On the radio afterglow of gamma ray bursts

Dado

Dar

Rújula

2003

A&A

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Abstract. We use the cannonball (CB) model of gamma ray bursts (GRBs) to predict the spectral and temporal behaviour of their radio afterglows (AGs). A single simple expression describes the AGs at all times and frequencies; its high-frequency limit reproduces the successful CB model predictions for optical and X-ray AGs. We analyze all of the observed radio AGs of GRBs with known redshifts, including those of the exceptionally close-by GRB 980425. We also study in detail the timeevolution of the AGs' spectral index. The agreement between theory and observations is excellent, even though the CB model is extremely frugal in the number of parameters required to explain the radio observations. We propose to use the scintillations in the radio AGs of GRBs to verify and measure the hyperluminal speed of their jetted CBs, whose apparent angular velocity is of the same order of magnitude as that of galactic pulsars, consistently measured directly, or via scintillations.

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“…Left: PCA determination of index for GRB 000115. Right: ASM/PCA/Chandra decay of GRB 991216, reported in Halpern et al [8] four derived from Locburst and one from the ASM; Table 1. In each case celestial positions were promptly reported to the community.…”

Section: Observations Of Afterglows With the Pcamentioning

confidence: 99%

“…• Optical afterglow in GRB 991216 with a break in the decay curve indicating a jet in interstellar medium [8], radio emission [4], and a reported lower-limit to the redshift, z > 1.02 [20].…”

Section: Observations Of Afterglows With the Pcamentioning

confidence: 99%

Observations of Gamma-Ray Bursts with the Rossi X-Ray Timing Explorer

Bradt

Levine

Marshall

et al.

Eso Astrophysics Symposia

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The role of the Rossi X-ray Timing Explorer (RXTE) in the study of Gamma-ray Bursts (GRBs) is reviewed. Through April 2001, the All-Sky Monitor (ASM) and the Proportional Counter Array (PCA) instruments have detected 30 GRBs. In 16 cases, an early celestial position was released to the community, sometimes in conjunction with IPN results. The subsequent optical and radio searches led to the detection of 5 x-ray afterglows, to at least 6 optical or radio afterglows, to 3 of the 17 secure redshifts known at this writing, and to 2 other likely redshifts. The decay curves of early x-ray afterglows have been measured. The rapid determination of the location of GRB 970828 and the absence of optical afterglow at that position gave one of the first indications that GRBs occur in star-forming regions [6]. The location of GRB 000301C led to the determination of a break in the optical decay rate [16] which is evidence for a jet, and to variability in the optical light curve that could represent gravitational lensing [7]. X-ray light curves of GRB from the ASM in conjunction with gamma-ray light curves exhibit striking differences in different bands and may reveal the commencement of the x-ray afterglow [18].

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GRB 991216 Joins the Jet Set: Discovery and Monitoring of Its Optical Afterglow

Cited by 94 publications

References 29 publications

RapidUBVRIFollow‐up of the Highly Collimated Optical Afterglow of GRB 010222

RapidUBVRIFollow‐up of the Highly Collimated Optical Afterglow of GRB 010222

On the radio afterglow of gamma ray bursts

Observations of Gamma-Ray Bursts with the Rossi X-Ray Timing Explorer

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