GRB 190114C 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 ∼50 s (i.e., before the MAGIC detection) can hold valuable information. We analyze the spectral evolution of the emission of GRB 190114C as detected by the Fermi Gamma-Ray Burst Monitor (GBM) in the 10 keV-40 MeV energy range up 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 ∼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-40 MeV flux of the power-law component peaks at ∼6 s; it reaches a value of 1.7  ×  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 Γ0 is about 500, depending on the assumed circum-burst density.

Ravasio, M., Oganesyan, G., Salafia, O., Ghirlanda, G., Ghisellini, G., Branchesi, M., et al. (2019). GRB 190114C: From prompt to afterglow. ASTRONOMY & ASTROPHYSICS, 626 [10.1051/0004-6361/201935214].

GRB 190114C: From prompt to afterglow

RAVASIO, MARIA EDVIGE
Primo
;
Salafia, O. S.;Ghirlanda, G.;Ghisellini, G.;
2019

Abstract

GRB 190114C 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 ∼50 s (i.e., before the MAGIC detection) can hold valuable information. We analyze the spectral evolution of the emission of GRB 190114C as detected by the Fermi Gamma-Ray Burst Monitor (GBM) in the 10 keV-40 MeV energy range up 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 ∼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-40 MeV flux of the power-law component peaks at ∼6 s; it reaches a value of 1.7  ×  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 Γ0 is about 500, depending on the assumed circum-burst density.
Articolo in rivista - Articolo scientifico
Gamma-ray burst: general; Gamma-ray burst: individual: GRB 190114C; Radiation mechanisms: non-thermal;
radiation mechanisms: non-thermal; gamma-ray burst: individual: GRB 190114C; gamma-ray burst: general; astro-ph.HE; astro-ph.HE
English
5-giu-2019
2019
626
A12
open
Ravasio, M., Oganesyan, G., Salafia, O., Ghirlanda, G., Ghisellini, G., Branchesi, M., et al. (2019). GRB 190114C: From prompt to afterglow. ASTRONOMY & ASTROPHYSICS, 626 [10.1051/0004-6361/201935214].
File in questo prodotto:
File Dimensione Formato  
aa35214-19.pdf

accesso aperto

Descrizione: Articolo principale
Tipologia di allegato: Publisher’s Version (Version of Record, VoR)
Dimensione 340.1 kB
Formato Adobe PDF
340.1 kB Adobe PDF Visualizza/Apri

I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.

Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10281/268149
Citazioni
  • Scopus 32
  • ???jsp.display-item.citation.isi??? 30
Social impact