Gamma‐Ray Burst Energetics and the Gamma‐Ray Burst Hubble Diagram: Promises and Limitations

Bloom, J.; Frail, D. A.; Kulkarni, S. R.

doi:10.1086/377125

Cited by 391 publications

(673 citation statements)

References 91 publications

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“…For this reason we have investigated whether the deduced SN luminosity is correlated with the corresponding energy release in the gamma-ray band (as given in Bloom et al 2003). No such correlation was found.…”

Section: Sn Properties Vv Ersus Aftergg Low Parametersmentioning

confidence: 99%

A Systematic Analysis of Supernova Light in Gamma‐Ray Burst Afterglows

Zeh

Klose

Hartmann

2004

ApJ

184

242

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We systematically reanalyzed all gamma-ray burst (GRB) afterglow data published through the end of 2002 in an attempt to detect the predicted supernova light component and to gain statistical insight into its phenomenological properties. We fit the observed photometric light curves as the sum of an afterglow, an underlying host galaxy, and a supernova component. The latter is modeled using published multicolor light curves of SN 1998bw as a template. The total sample of afterglows with established redshifts contains 21 bursts (GRB 970228-GRB 021211). For nine of these GRBs a weak supernova excess (scaled to SN 1998bw) was found, which is what makes this one of the first samples of high-z core-collapse supernovae. Among this sample are all bursts with redshifts less than $0.7. These results strongly support the notion that in fact all afterglows of longduration GRBs contain light from an associated supernova. A statistics of the physical parameters of these GRBsupernovae shows that SN 1998bw was at the bright end of its class, while it was not special with respect to its light-curve shape. Finally, we have searched for a potential correlation of the supernova luminosities with the properties of the corresponding bursts and optical afterglows, but we have not found such a relation.

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Section: Sn Properties Vv Ersus Aftergg Low Parametersmentioning

confidence: 99%

A Systematic Analysis of Supernova Light in Gamma‐Ray Burst Afterglows

Zeh

Klose

Hartmann

2004

ApJ

184

242

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“…Bursts are thought to radiate anisotropically, but we sample their radiation field in only one direction. Therefore, L B and E iso are calculated from the observed flux as if the emissions were isotropic; corrections for the anisotropy are based on models of the relativistic jets that emit the observed gamma rays (see Bloom et al 2003). The values L B and E iso are both bolometric quantities in the burst frame; L B is the maximum value of the luminosity, while E iso is the total energy emitted over the duration of the burst (without correcting for the anisotropic emission).…”

Section: Introductionmentioning

confidence: 99%

Gamma‐Ray Burst Intensity Distributions

Band

Norris

Bonnell³

2004

ApJ

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We use the lag-luminosity relation to calculate self-consistently the redshifts, apparent peak bolometric luminosities L B , and isotropic energies E iso for a large sample of BATSE gamma-ray bursts. We consider two different forms of the lag-luminosity relation; for both forms the median redshift for our burst database is 1.6. We model the resulting E iso sample with power-law and Gaussian probability distributions without redshift evolution, both of which are reasonable models. The power-law model has an index of E ¼ 1:76 AE 0:05 (95% confidence), where p(E iso ) / E À E iso . The simple universal jet profile model suggested but did not require E ¼ 2, and subsequent physically reasonable refinements to this model permit greater diversity in E , as well as deviations from a power law; therefore, our observed E iso probability distribution does not disprove the universal jet model.

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“…But the observed energies of GRBs span a wide range. After considering the collimation effect, Frail et al (2001) found that the collimated energies of GRBs clustered around 5 × 10 50 erg, which was confirmed by Bloom et al (2003). Meanwhile, the collimated jet predicts that the appearance of an achromatic break in the afterglow light curve of GRBs (Rhoads 1997;Sari 1999), which is important to standardize the energetic of GRBs.…”

Section: The Luminosity Correlations Of Grbs and Dark Energymentioning

confidence: 82%

GRBs and Fundamental Physics

Petitjean

Wang

et al. 2016

Space Sci Rev

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Gamma-ray bursts (GRBs) are short and intense flashes at the cosmological distances, which are the most luminous explosions in the Universe. The high luminosities of GRBs make them detectable out to the edge of the visible universe. So, they are unique tools to probe the properties of high-redshift universe: including the cosmic expansion and dark energy, star formation rate, the reionization epoch and the metal evolution of the Universe. First, they can be used to constrain the history of cosmic acceleration and the evolution of dark energy in a redshift range hardly achievable by other cosmological probes. Second, long GRBs are believed to be formed by collapse of massive stars. So they can be used to derive the high-redshift star formation rate, which can not be probed by current observations. Moreover, the use of GRBs as cosmological tools could unveil the reionization history and metal evolution of the Universe, the intergalactic medium (IGM) properties and the nature of first stars in the early universe. But beyond that, the GRB high-energy photons can be applied to constrain Lorentz invariance violation (LIV) and to test Einstein's Equivalence Principle (EEP). In this paper, we review the progress on the GRB cosmology and fundamental physics probed by GRBs.

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Gamma‐Ray Burst Energetics and the Gamma‐Ray Burst Hubble Diagram: Promises and Limitations

Cited by 391 publications

References 91 publications

A Systematic Analysis of Supernova Light in Gamma‐Ray Burst Afterglows

A Systematic Analysis of Supernova Light in Gamma‐Ray Burst Afterglows

Gamma‐Ray Burst Intensity Distributions

GRBs and Fundamental Physics

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