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

Abstract

Very high energy (>100 GeV) gamma-ray emission has been detected for the first time from the composite supernova remnant G 0.9+0.1 using the HESS instrument. The source is detected with a significance of ≈13σ, and a photon flux above 200 GeV of (5.7±0.7stat±1.2sys)×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 ∝ E-Γ) with photon index Γ = 2.40±0.11stat±0.20sys. 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.

Astronomy & Astrophysics 432, L25-L29 (2005)
ArXiv pre-print

Auxiliary informations

Data points for Figure 3

80 photoelectron cut (filled circles)

Mean energy  Flux     Flux Error
   [TeV]       [/TeV cm^2 s]
   0.23    2.42e-11   8.60e-12
   0.38    8.20e-12   1.49e-12
   0.67    2.34e-12   3.78e-13
   1.19    6.97e-13   1.20e-13
   2.10    1.28e-13   4.24e-14
   3.93    1.58e-14   1.40e-14
   6.16    9.39e-15   5.99e-15

With 200 photoelectron cut (open circles)

Mean energy  Flux     Flux Error
   [TeV]       [/TeV cm^2 s]
   0.42    6.16e-12   1.63e-12
   0.61    2.79e-12   5.33e-13
   0.92    1.07e-12   2.01e-13
   1.31    4.42e-13   8.83e-14
   1.91    2.66e-13   5.21e-14
   2.88    6.93e-14   2.21e-14
   4.22    2.81e-14   1.31e-14

Remarks: Statistical errors only. Systematic error on energy scale estimated to 20%. See paper for details.

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