SNR G24.7+0.6 is a 9.5 kyrs radio and γ-ray supernova remnant evolving in a dense medium. In the GeV regime, SNR G24.7+0.6 (3FHL J1834.1-0706e/FGES J1834.1-0706) shows a hard spectral index (Γ ˜ 2) up to 200 GeV, which makes it a good candidate to be observed with Cherenkov telescopes such as MAGIC. We observed the field of view of SNR G24.7+0.6 with the MAGIC telescopes for a total of 31 h. We detect very high-energy γ-ray emission from an extended source located 0.34° away from the centre of the radio SNR. The new source, named MAGIC J1835-069 is detected up to 5 TeV, and its spectrum is well-represented by a power-law function with spectral index of 2.74 ± 0.08. The complexity of the region makes the identification of the origin of the very high-energy emission difficult; however, the spectral agreement with the LAT source and overlapping position at less than 1.5σ point to a common origin. We analysed 8 yr of Fermi-LAT data to extend the spectrum of the source down to 60 MeV. Fermi-LAT and MAGIC spectra overlap within errors and the global broad-band spectrum is described by a power law with exponential cut-off at 1.9 ± 0.5 TeV. The detected γ-ray emission can be interpreted as the results of proton-proton interaction between the supernova and the CO-rich surrounding.

Acciari, V.~., Ansoldi, S., Antonelli, L.~., Arbet Engels, A., Arcaro, C., Baack, D., et al. (2019). Discovery of TeV $gamma$-ray emission from the neighbourhood of the supernova remnant G24.7+0.6 by MAGIC. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 483(4), 4578-4585 [10.1093/mnras/sty3387].

Discovery of TeV $gamma$-ray emission from the neighbourhood of the supernova remnant G24.7+0.6 by MAGIC

Bonnoli, G.
Supervision
;
Da Vela, P.
Membro del Collaboration Group
;
Ninci, D.
Membro del Collaboration Group
;
Paoletti, R.
Data Curation
;
Rugliancich, A.
Membro del Collaboration Group
;
Stamerra, A.
Project Administration
;
2019-01-01

Abstract

SNR G24.7+0.6 is a 9.5 kyrs radio and γ-ray supernova remnant evolving in a dense medium. In the GeV regime, SNR G24.7+0.6 (3FHL J1834.1-0706e/FGES J1834.1-0706) shows a hard spectral index (Γ ˜ 2) up to 200 GeV, which makes it a good candidate to be observed with Cherenkov telescopes such as MAGIC. We observed the field of view of SNR G24.7+0.6 with the MAGIC telescopes for a total of 31 h. We detect very high-energy γ-ray emission from an extended source located 0.34° away from the centre of the radio SNR. The new source, named MAGIC J1835-069 is detected up to 5 TeV, and its spectrum is well-represented by a power-law function with spectral index of 2.74 ± 0.08. The complexity of the region makes the identification of the origin of the very high-energy emission difficult; however, the spectral agreement with the LAT source and overlapping position at less than 1.5σ point to a common origin. We analysed 8 yr of Fermi-LAT data to extend the spectrum of the source down to 60 MeV. Fermi-LAT and MAGIC spectra overlap within errors and the global broad-band spectrum is described by a power law with exponential cut-off at 1.9 ± 0.5 TeV. The detected γ-ray emission can be interpreted as the results of proton-proton interaction between the supernova and the CO-rich surrounding.
2019
Acciari, V.~., Ansoldi, S., Antonelli, L.~., Arbet Engels, A., Arcaro, C., Baack, D., et al. (2019). Discovery of TeV $gamma$-ray emission from the neighbourhood of the supernova remnant G24.7+0.6 by MAGIC. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 483(4), 4578-4585 [10.1093/mnras/sty3387].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11365/1082118