Abstract
The results of follow-up observations of the TeV γ-ray source HESS J1640−465 from 2004 to 2011 with the High Energy Stereoscopic System (HESS) are reported in this work. The spectrum is well described by an exponential cut-off power law with photon index Γ = 2.11 ± 0.09stat ± 0.10sys, and a cut-off energy of |$E_{\rm c} = 6.0^{+2.0}_{-1.2}$| TeV. The TeV emission is significantly extended and overlaps with the northwestern part of the shell of the SNR G338.3−0.0. The new HESS results, a re-analysis of archival XMM–Newton data and multiwavelength observations suggest that a significant part of the γ-ray emission from HESS J1640−465 originates in the supernova remnant shell. In a hadronic scenario, as suggested by the smooth connection of the GeV and TeV spectra, the product of total proton energy and mean target density could be as high as WpnH ∼ 4 × 1052(d/10kpc)2 erg cm−3.
Highlights
Starting in 2004 the Galactic Plane Survey (Aharonian et al 2006b) performed by the H.E.S.S
The detailed H.E.S.S. results presented in this work show that the VHE γ-ray emission from HESS J1640−465 significantly overlaps with the north-western part of the supernova remnants (SNRs) shell of G338.3−0.0
The VHE γ-ray spectrum smoothly connects with the Fermi spectrum and has a high-energy cut-off that implies that particles with tens of TeV energies are present in the acceleration region
Summary
Starting in 2004 the Galactic Plane Survey (Aharonian et al 2006b) performed by the H.E.S.S. Collaboration, using an array of imaging atmospheric Cherenkov telescopes (IACTs), led to the discovery of nearly 70 new sources in the very-high-energy (VHE, E>100 GeV) γ-ray regime (Carrigan et al 2013). Since the original discovery of HESS J1640−465, the available H.E.S.S. exposure towards this source has quadrupled w.r.t the data used in (Aharonian et al 2006b), and advanced analysis methods are available that allow for a much more detailed spectral and morphological study of the VHE γ-ray emission. H.E.S.S. follow-up studies and a re-analysis of XMM-Newton data are presented Both the broadband SED and the TeV morphology reveal evidence for proton acceleration in the SNR shell of G338.3−0.0. All results were cross-checked by an independent analysis and calibration for consistency (de Naurois & Rolland 2009)
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