The Vela supernova remnant (SNR) is a complex region containing a number of sources of non-thermal radiation. The inner section of this SNR, within 2 degrees of the pulsar PSR B0833-45, has been observed by the HESS γ-ray atmospheric Cherenkov detector in 2004 and 2005. A strong signal is seen from an extended region to the south of the pulsar, within an integration region of radius 0.8° around the position (α = 08h35 m00s, δ = -45°36′ J2000.0). The excess coincides with a region of hard X-ray emission seen by the ROSAT and ASCA satellites. The observed energy spectrum of the source between 550 GeV and 65 TeV is well fit by a power law function with photon index Γ = 1.45 ± 0.09stat ± 0.2sys and an exponential cutoff at an energy of 13.8 ± 2.3stat ± 4.1 sys TeV. The integral flux above 1 TeV is (1.28 ± 0.17 stat ± 0.38sys) × 10-11 cm -2 s-1. This result is the first clear measurement of a peak in the spectral energy distribution from a VHE γ-ray source, likely related to inverse Compton emission. A fit of an Inverse Compton model to the HESS spectral energy distribution gives a total energy in non-thermal electrons of ∼2 × 1045 erg between 5 TeV and 100 TeV, assuming a distance of 290 parsec to the pulsar. The best fit electron power law index is 2.0, with a spectral break at 67 TeV.
|Original language||English (US)|
|Journal||Astronomy and Astrophysics|
|State||Published - Mar 2006|
Bibliographical noteFunding Information:
The authors gratefully acknowledge the generous funding from (1) the National Research Foundation (NRF) Singapore under the Competitive Research Programme (CRP) Funding Scheme (R-265-000-466-281), (2) the National Research Foundation Singapore under its Campus for Research Excellence and Technological Enterprise (CREATE) programme and (3) the China Scholarship Council (CSC).
- Gamma rays: observations
- Ism: plerions