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

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dc.contributor.authorH.E.S.S. Collaboration,
dc.contributor.authorAbramowski, A.
dc.contributor.authorAharonian, F.
dc.contributor.authorAit Benkhali, F.
dc.contributor.authorAkhperjanian, A.
dc.contributor.authorAngüner, E.
dc.contributor.authorBackes, M.
dc.contributor.authorBalenderan, S.
dc.contributor.authorBalzer, A.
dc.contributor.authorBarnacka, A.
dc.contributor.authorBecherini, Y.
dc.contributor.authorBecker Tjus, J.
dc.contributor.authorBerge, D.
dc.contributor.authorBernhard, S.
dc.contributor.authorBernlöhr, K.
dc.contributor.authorBirsin, E.
dc.contributor.authorBiteau, J.
dc.contributor.authorBöttcher, M.
dc.contributor.authorBoisson, C.
dc.contributor.authorBolmont, J.
dc.contributor.authoret al.
dc.date.issued2015
dc.descriptionCorrected by: Erratum: H.E.S.S. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud, in Astronomy and Astrophysics; 580, C1 (2015). The reference to the second corresponding author (C. Trichard) in the published article was missing.
dc.description.abstractG349.7+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 <E< 100 GeV) γ-rays. Radio and infrared observations indicate that the remnant is interacting with a molecular cloud. In this paper, the detection of very high energy (VHE, E> 100 GeV) γ-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 ± 1.1stat ± 1.3syst) × 10−13 ph cm−2 s−1 corresponding to ~0.7% of that of the Crab Nebula and to a luminosity of ~1034 erg s−1 above the same energy threshold, and a steep photon index ΓVHE = 2.8 ± 0.27stat ± 0.20syst 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 ΓHE = 2.2 ± 0.04stat+0.13−0.31 sys. The combined γ-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 Ebr,γ = 55+70−30 GeV, slightly higher than what is usually observed in the HE/VHE γ-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 Ecut,γ = 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 γ-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 nHWp ~ 5 × 1051 erg cm−3.
dc.description.statementofresponsibilityA. Abramowski … P. deWilt ... G. Rowell … et al. (for the H.E.S.S. Collaboration)
dc.identifier.citationAstronomy and Astrophysics: a European journal, 2015; 574:A100-1-A100-7
dc.identifier.doi10.1051/0004-6361/201425070
dc.identifier.issn0004-6361
dc.identifier.issn1432-0746
dc.identifier.urihttp://hdl.handle.net/2440/102391
dc.language.isoen
dc.publisherEDP Sciences
dc.rights© ESO 2015
dc.source.urihttp://www.aanda.org/articles/aa/abs/2015/02/aa25070-14/aa25070-14.html
dc.subjectgamma rays; general – ISM; supernova remnants – ISM; clouds
dc.titleH.E.S.S. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud
dc.typeJournal article
pubs.publication-statusPublished

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