- Very high energy gamma rays from the composite SNR G0.9+0.1 doi link

Author(s): Aharonian F., Akhperjanian A.G., Aye K.-M., Bazer-Bachi A.R., Beilicke M., Berghaus P., Bussons Gordo J., Chounet L.-M., Degrange B., Djannati-Ataï A., Espigat P., Feinstein F., Fleury P., Fontaine G., Gallant Y., Giebels B., Lemière A., Lemoine M., Leroy N., Marcowith A., De Naurois M., Ouchrif M., Pita S., Punch M., Tavernet J.-P., Terrier R., Théoret C.G., Tluczykont M., Vasileiadis G., Vincent P.

(Article) Published: Astronomy & Astrophysics, vol. 432 p.L25-L29 (2005)
Links openAccess full text : arxiv

Ref HAL: in2p3-00023664_v1
Ref Arxiv: astro-ph/0501265
DOI: 10.1051/0004-6361:200500022
Ref. & Cit.: NASA ADS
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Very high energy (> 100 GeV) gamma-ray emission has been detected for the first time from the composite supernova remnant G0.9+0.1 using the H.E.S.S. instrument. The source is detected with a significance of 13 sigma, and a photon flux above 200 GeV of (5.7+/-0.7 stat +/- 1.2 sys) * 10^-12 cm^-2 s^-1, making it one of the weakest sources ever detected at TeV energies. The photon spectrum is compatible with a power law (dN/dE \propto E^-Gamma) with photon index Gamma = 2.40 +/- 0.11 stat +/- 0.20 sys. The gamma-ray emission appears to originate in the plerionic core of the remnant, rather than the shell, and can be plausibly explained as inverse Compton scattering of relativistic electrons.