Peak Luminosity–Spectral Lag Relation Caused by the Viewing Angle of the Collimated Gamma-Ray Bursts

Ioka, Kunihito; Nakamura, Takashi

doi:10.1086/321717

Cited by 169 publications

(210 citation statements)

References 35 publications

(50 reference statements)

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“…Another explanation for the spectral-lag-luminosity relation is based purely on kinematic effects (Salmonson 2000;Salmonson & Galama 2002;Ioka & Nakamura 2001;Dermer 2004;Shen et al 2005;Lu et al 2006), where the peak luminosity L pk and spectral lag τ depend on a single kinematic variable…”

Section: Discussionmentioning

confidence: 99%

“…So, for example, Salmonson (2000) showed that the lag-luminosity relation is due only to a variation in the line-of-sight Γ among bursts, with high Γ bursts having smaller spectral lags and low Γ bursts exhibiting longer ones. On the other hand, Ioka & Nakamura (2001) showed that the lag-luminosity relation can be explained by variation in the observer angle, θ v , from the axis of the jet, using a simple jet in which Γ = const. for θ < θ j , and zero emission for θ > θ j , where θ j is the opening angle of the jet.…”

Section: Discussionmentioning

confidence: 99%

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Luminosity Correlations for Gamma-Ray Bursts and Implications for Their Prompt and Afterglow Emission Mechanisms

Sultana

Kazanas

Fukumura

2012

ApJ

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We present the relation between the (z-and k-corrected) spectral lags, τ , for the standard Swift energy bands 50-100 keV and 100-200 keV and the peak isotropic luminosity, L iso (a relation reported first by Norris et al.), for a subset of 12 long Swift gamma-ray bursts (GRBs) taken from a recent study of this relation by Ukwatta et al. The chosen GRBs are also a subset of the Dainotti et al. sample, a set of Swift GRBs of known redshift, employed in establishing a relation between the (GRB frame) luminosity, L X , of the shallow (or constant) flux portion of the typical X-Ray Telescope GRB-afterglow light curve and the (GRB frame) time of transition to the normal decay rate, T brk . We also present the L X -T brk relation using only the bursts common in the two samples. The two relations exhibit a significant degree of correlation (ρ = −0.65 for the L iso -τ and ρ = −0.88 for the L X -T brk relation) and have surprisingly similar best-fit power-law indices (−1.19 ± 0.17 for L iso -τ and −1.10 ± 0.03 for L X -T brk ). Even more surprisingly, we noted that although τ and T brk represent different GRB time variables, it appears that the first relation (L iso -τ ) extrapolates into the second one for timescales τ T brk . This fact suggests that these two relations have a common origin, which we conjecture to be kinematic. This relation adds to the recently discovered relations between properties of the prompt and afterglow GRB phases, indicating a much more intimate relation between these two phases than hitherto considered.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Luminosity Correlations for Gamma-Ray Bursts and Implications for Their Prompt and Afterglow Emission Mechanisms

Sultana

Kazanas

Fukumura

2012

ApJ

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“…We address first the problem of an instantaneous emission from a very thin shell located at a radius r and propagating with a Lorentz factor (this problem or related ones were considered by Fenimore, Madras, & Nayakshin 1996;Kumar & Panaitescu 2000;Ioka & Nakamura 2001;Ryde & Petrosian 2002 and others). Because of the relativistic beaming, the observer receives mainly photons emitted up to an angle of ¼ 1= relative to the line of sight.…”

Section: The Blandford-mckee Light Curvementioning

confidence: 99%

Modeling Fluctuations in Gamma‐Ray Burst Afterglow Light Curves

Nakar

Piran

2003

ApJ

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The fluctuations observed in the light curves of some gamma-ray burst (GRB) afterglows (such as GRB 021004) provide a useful tool to probe the circumburst density profile and to probe the variations in the energy of the blast wave with time. We present a general formalism that reduces the calculation of the observed light curve from a Blandford-McKee blast wave to the evaluation of a one-dimensional integral. Using this formalism we obtain a simple approximation to the general light curve that arises in more complex situations where the afterglow's energy or the external density varies. The solution is valid for spherically symmetric profiles, and it takes full consideration of angular time delay effects. We present the light curves of several external density profiles and demonstrate the effects of density variations on the light curve. We also revisit the afterglow of GRB 021004 and find that the steep decay after the first bump ($4000 s) cannot result from a spherically symmetric density variation or from the passage of the synchrotron frequency through the optical band. This suggests that an angular structure is responsible for some of the observed features in the light curve. This may be the first evidence that an angular structure is important in the early stages of the afterglow.

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“…Therefore, we cannot use a simple color selection technique for the high-z GRBs. Spectroscopic observations to detect the Lyα break feature , Fe line (Mészáros & Rees 2003) or empirical methods by using only the γ-ray data (Fenimore & Ramirez-Ruiz 2000;Norris et al 2000;Ioka & Nakamura 2001;Amati et al 2002;Atteia 2003;Murakami et al 2003;Yonetoku et al 2003) are required.…”

Section: Comment On Lyman Break Techniquementioning

confidence: 99%

“…In order to investigate the reionization history using our photometric method, we need to determine redshifts of GRBs by other ways, e.g., detections of iron lines in X-ray afterglow spectra (Mészáros & Rees 2003) and of the Lyα break in NIR spectra, or empirical methods by using only the γ-ray data (Fenimore & Ramirez-Ruiz 2000;Norris et al 2000;Ioka & Nakamura 2001;Amati et al 2002;Atteia 2003;Murakami et al 2003;Yonetoku et al 2003). Even if redshifts of GRBs are unknown prior to follow-up observations, it is worth performing NIR photometry as early phase as possible since ∼ 10% of GRBs are expected to be located at z 10 (Bromm & Loeb 2002).…”

Section: Introductionmentioning

confidence: 99%

Near-Infrared Colors of Gamma-Ray Burst Afterglows and Cosmic Reionization History

Inoue

Yamazaki

Nakamura

2004

AIP Conference Proceedings

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Using the near-infrared (NIR) observations of the afterglows of the high redshift (5 z 25) gammaray bursts (GRBs) that will be detected by the Swift satellite, we discuss a way to study the cosmic reionization history. In principle the details of the cosmic reionization history are well imprinted in the NIR spectra of the GRB afterglows. However the spectroscopy with a space telescope is required to obtain such an information for a very high redshift (z 15) unless the neutral fraction of the highz universe is less than 10 −6 . The broad-band photometry has the higher sensitivity than that of the spectroscopy, so that the NIR photometric follow-up of the GRB afterglows is very promising to examine the cosmic reionization history. A few minutes exposure with a 8-m class ground-based telescope of the afterglow of the high-z GRBs will reveal how many times the reionization occurred in the universe.

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Peak Luminosity–Spectral Lag Relation Caused by the Viewing Angle of the Collimated Gamma-Ray Bursts

Cited by 169 publications

References 35 publications

Luminosity Correlations for Gamma-Ray Bursts and Implications for Their Prompt and Afterglow Emission Mechanisms

Luminosity Correlations for Gamma-Ray Bursts and Implications for Their Prompt and Afterglow Emission Mechanisms

Modeling Fluctuations in Gamma‐Ray Burst Afterglow Light Curves

Near-Infrared Colors of Gamma-Ray Burst Afterglows and Cosmic Reionization History

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