Home > Publications database > H.E.S.S. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud > print

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005     20250730113843.0
024 7 _ |a 10.1051/0004-6361/201425070
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024 7 _ |a 0004-6361
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024 7 _ |a 1432-0746
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100 1 _ |a H.E.S.S. Collaboration
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245 _ _ |a H.E.S.S. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud
260 _ _ |a Les Ulis
|c 2015
|b EDP Sciences
336 7 _ |a article
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336 7 _ |a ARTICLE
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336 7 _ |a Journal Article
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500 _ _ |a (c) ESO. This article has an erratum (DOI 10.1051/0004-6361/201425070e). The arXiv version includes the changes of the erratum.
520 _ _ |a G349.7+0.2 is a young Galactic supernova remnant (SNR) located at the distance of 11.5 kpc and observed across the entire electromagnetic spectrum from radio to high energy (HE; 0.1 GeV 100 GeV) $\gamma$-ray emission coincident with this SNR with the High Energy Stereoscopic System (H.E.S.S.) is reported. This makes it one of the farthest Galactic SNR ever detected in this domain. An integral flux F(E> 400 GeV) = (6.5 $\pm$ 1.1$_{stat}$ $\pm$ 1.3$_{syst}$) × $10^{−13} ph cm^{−2} s^{−1}$ corresponding to ~0.7% of that of the Crab Nebula and to a luminosity of $~10^{34}$ erg $s^{−1}$ above the same energy threshold, and a steep photon index $Γ_{VHE}$ = 2.8 $\pm$ 0.27$_{stat}$ $\pm$ $0.20_{syst}$ are measured. The analysis of more than 5 yr of Fermi-LAT data towards this source shows a power-law like spectrum with a best-fit photon index $Γ_{HE}$ = 2.2 $\pm$ 0.04$_{stat}$$^{+0.13}_{−0.31}$ $_{sys}$. The combined $\gamma$-ray spectrum of G349.7+0.2 can be described by either a broken power-law (BPL) or a power-law with exponential (or sub-exponential) cutoff (PLC). In the former case, the photon break energy is found at $E_{br, \gamma}$ = $55^{+70}_{−30}$ GeV, slightly higher than what is usually observed in the HE/VHE $\gamma$-ray emitting middle-aged SNRs known to be interacting with molecular clouds. In the latter case, the exponential (respectively sub-exponential) cutoff energy is measured at $E_{cut,\gamma}$ = $1.4^{+1.6}_{−0.55}$ (respectively $0.35^{+0.75}_{−0.21}$) TeV. A pion-decay process resulting from the interaction of the accelerated protons and nuclei with the dense surrounding medium is clearly the preferred scenario to explain the $\gamma$-ray emission. The BPL with a spectral steepening of 0.5−1 and the PLC provide equally good fits to the data. The product of the average gas density and the total energy content of accelerated protons and nuclei amounts to $\mathit{n}_{H}\mathit{W}_{p}$ ~ 5 × $10^{51}$ erg cm$^{−3}$.
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