Aleksić, J. 2010 MAGIC对GRB 080430余辉的高能辐射的观测

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没看到。给了个上限：5.5 × 10^-11 erg cm^-2 s^-1

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Title:		MAGIC observation of the GRB 080430 afterglow
Authors:		Aleksić, J.; Anderhub, H.; Antonelli, L. A.;  et al.
Affiliation:
Publication:		Astronomy and Astrophysics, Volume 517, id.A5 (A&A Homepage)
Publication Date:		07/2010
Origin:		EDP Sciences
Keywords:		radiation mechanisms: non-thermal, gamma-ray burst: individual: GRB 080430
DOI:		10.1051/0004-6361/200913461
Bibliographic Code:		2010A&A...517A...5A

Abstract

Context. Gamma-ray bursts are cosmological sources emitting radiation from the gamma-rays to the radio band. Substantial observational efforts have been devoted to the study of gamma-ray bursts during the prompt phase, i.e. the initial burst of high-energy radiation, and during the long-lasting afterglows. In spite of many successes in interpreting these phenomena, there are still several open key questions about the fundamental emission processes, their energetics and the environment.
Aims: Independently of specific gamma-ray burst theoretical recipes, spectra in the GeV/TeV range are predicted to be remarkably simple, being satisfactorily modeled with power-laws, and therefore offer a very valuable tool to probe the extragalactic background light distribution. Furthermore, the simple detection of a component at very-high energies, i.e. at ~100 GeV, would solve the ambiguity about the importance of various possible emission processes, which provide barely distinguishable scenarios at lower energies.
Methods: We used the results of the MAGIC telescope observation of the moderate resdhift (z ~ 0.76) GRB 080430 at energies above about 80 GeV, to evaluate the perspective for late-afterglow observations with ground based GeV/TeV telescopes.
Results: We obtained an upper limit of F_{95% CL} = 5.5 × 10^-11 erg cm^-2 s^-1 for the very-high energy emission of GRB 080430, which cannot set further constraints on the theoretical scenarios proposed for this object also due to the difficulties in modeling the low-energy afterglow. Nonetheless, our observations show that Cherenkov telescopes have already reached the required sensitivity to detect the GeV/TeV emission of GRBs at moderate redshift (z ≲ 0.8), provided the observations are carried out at early times, close to the onset of their afterglow phase.

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