We report the detection of TeV γ-rays from the shell-type supernova remnant RX J0852.0-4622 with data of 3.2 h of live time recorded with HESS in February 2004. An excess of (700 ± 60) events from the whole remnant with a significance of 12 σ was found. The observed emission region is clearly extended with a radius of the order of 1° and the spatial distribution of the signal correlates with X-ray observations. The spectrum in the energy range between 500 GeV and 15 TeV is well described by a power law with a photon index of Γ = 2.1 ± 0.1stat ± 0.2syst and a differential flux at 1 TeV of ϕ1 TeV = (2.1 ± 0.2stat ± 0.6syst) × 10-11 cm-2 s-1 TeV-1. The integral flux above 1 TeV was measured to be Φ(E>1 TeV) = (1.9 ± 0.3stat ± 0.6syst) × 10-11 cm-2 s-1, which is at the level of the flux of the Crab nebula at these energies. More data are needed to draw firm conclusions on the magnetic field in the remnant and the type of the particle population creating the TeV γ-rays.
Detection of TeV γ-ray emission from the shell-type supernova remnant RX J0852.0-4622 with HESS
- F. Aharonian et al. (H.E.S.S. Collaboration)
- Astronomy & Astrophysics 437, L7-L10 (2005)
- 2005
Abstract
Auxiliary informations
H.E.S.S. data points for Figure 3
Energy interval Mean energy Flux Flux Error [TeV] [TeV] [/TeV cm^2 s] 0.4 0.7 0.53 3.8e-11 2.3e-11 0.7 1.0 0.79 2.96e-11 7.8e-12 1.0 1.4 1.18 1.98e-11 3.2e-12 1.4 2.1 1.7 8.4e-12 1.4e-12 2.1 3.1 2.5 2.64e-12 6.7e-13 3.1 4.5 3.8 1.27e-12 3.6e-13 4.5 6.6 5.4 7.0e-13 2.2e-13 6.6 9.7 8 1.58e-13 9.3e-14 9.7 14 12 9.0e-14 6.9e-14
Remarks: Statistical errors only. Systematic error on energy scale estimated to 30%. See paper for details.
H.E.S.S. sky plot of Figure 2
Remarks: The plot is smoothed with a Gaussian (0.1°) according to the instrument’s point spread function. See paper for details.
