GRB190114C: from prompt to afterglow?

被引：38

作者：

Ravasio, M. E. ^{[1
,2
]}

Oganesyan, G. ^{[3
,4
]}

Salafia, O. S. ^{[1
,2
]}

Ghirlanda, G. ^{[1
,2
]}

Ghisellini, G. ^{[1
]}

Branchesi, M. ^{[3
,4
]}

Campana, S. ^{[1
]}

Covino, S. ^{[1
]}

Salvaterra, R. ^{[5
]}

机构：

[1] INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy

[2] Univ Milano Bicocca, Dipartimento Fis G Occhialini, Piazza Sci 3, I-20126 Milan, Italy

[3] Gran Sasso Sci Inst, Viale F Crispi 7, I-67100 Laquila, Italy

[4] Ist Nazl Fis Nucl, Lab Nazl Gran Sasso, I-67100 Laquila, Italy

[5] INAF, Ist Astrofis Spaziale & Fis Cosm, Via E Bassini 15, I-20133 Milan, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2019年 / 626卷

关键词：

radiation mechanisms: non-thermal; gamma-ray burst: individual: GRB 190114C; gamma-ray burst: general; GAMMA-RAY BURST; HIGH-ENERGY EMISSION; FERMI OBSERVATIONS; AGILE DETECTION; LORENTZ FACTOR; BLAST WAVES; SPECTRA; CONSTRAINTS; RADIATION; COMPONENT;

D O I：

10.1051/0004-6361/201935214

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

GRB190114C is the first gamma-ray burst detected at very high energies (VHE, i.e., >300 GeV) by the MAGIC Cherenkov telescope. The analysis of the emission detected by the Fermi satellite at lower energies, in the 10 keV-100 GeV energy range, up to similar to 50 s (i.e., before the MAGIC detection) can hold valuable information. We analyze the spectral evolution of the emission of GRB190114C as detected by the Fermi Gamma-Ray Burst Monitor (GBM) in the 10 keV-40MeV energy range up to similar to 60 s. The first 4 s of the burst feature a typical prompt emission spectrum, which can be fit by a smoothly broken power-law function with typical parameters. Starting on similar to 4 s post-trigger, we find an additional nonthermal component that can be fit by a power law. This component rises and decays quickly. The 10 keV-40MeV flux of the power-law component peaks at similar to 6 s; it reaches a value of 1.7 x 10(-5) erg cm(-2) s(-1). The time of the peak coincides with the emission peak detected by the Large Area Telescope (LAT) on board Fermi. The power-law spectral slope that we find in the GBM data is remarkably similar to that of the LAT spectrum, and the GBM+LAT spectral energy distribution seems to be consistent with a single component. This suggests that the LAT emission and the power-law component that we find in the GBM data belong to the same emission component, which we interpret as due to the afterglow of the burst. The onset time allows us to estimate that the initial jet bulk Lorentz factor Gamma(0) is about 500, depending on the assumed circum-burst density.

引用

页数：6

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