H.E.S.S. observations of RX J1713.7-3946 with improved angular and spectral resolution; evidence for gamma-ray emission extending beyond the X-ray emitting shell
- H.E.S.S. Collaboration
- Abdalla, H.
- Aubert, P.
- Jankowsky, F.
- Jingo, M.
- Jogler, T.
- Jouvin, L.
- Jung-Richardt, I.
- Kastendieck, M. A.
- Katarzyński, K.
- Katz, U.
- Kerszberg, D.
- Khélifi, B.
- Backes, M.
- Kieffer, M.
- King, J.
- Klepser, S.
- Klochkov, D.
- Kluźniak, W.
- Kolitzus, D.
- Komin, Nu.
- Kosack, K.
- Krakau, S.
- Kraus, M.
- Balzer, A.
- Krüger, P. P.
- Laffon, H.
- Lamanna, G.
- Lau, J.
- Lees, J. -P.
- Lefaucheur, J.
- Lefranc, V.
- Lemière, A.
- Lemoine-Goumard, M.
- Lenain, J. -P.
- Barnard, M.
- Leser, E.
- Lohse, T.
- Lorentz, M.
- Liu, R.
- López-Coto, R.
- Lypova, I.
- Mar, V.
- Marcowith, A.
- Mariaud, C.
- Marx, R.
- Becherini, Y.
- Maurin, G.
- Maxted, N.
- Mayer, M.
- Meintjes, P. J.
- Meyer, M.
- Mitchell, A. M. W.
- Moderski, R.
- Mohamed, M.
- Mohrmann, L.
- Morå, K.
- Tjus, J. Becker
- Moulin, E.
- Murach, T.
- de Naurois, M.
- Niederwanger, F.
- Niemiec, J.
- Oakes, L.
- O'Brien, P.
- Odaka, H.
- Öttl, S.
- Ohm, S.
- Berge, D.
- Ostrowski, M.
- Oya, I.
- Padovani, M.
- Panter, M.
- Parsons, R. D.
- Pekeur, N. W.
- Pelletier, G.
- Perennes, C.
- Petrucci, P. -O.
- Peyaud, B.
- Bernhard, S.
- Piel, Q.
- Pita, S.
- Poon, H.
- Prokhorov, D.
- Prokoph, H.
- Pühlhofer, G.
- Punch, M.
- Quirrenbach, A.
- Raab, S.
- Reimer, A.
- Bernlöhr, K.
- Reimer, O.
- Renaud, M.
- Reyes, R. de los
- Rieger, F.
- Romoli, C.
- Rowell, G.
- Rudak, B.
- Rulten, C. B.
- Sahakian, V.
- Salek, D.
- Blackwell, R.
- Sanchez, D. A.
- Santangelo, A.
- Sasaki, M.
- Schlickeiser, R.
- Schüssler, F.
- Schulz, A.
- Schwanke, U.
- Schwemmer, S.
- Seglar-Arroyo, L.
- Settimo, M.
- Abdalla, H.
- Böttcher, M.
- Seyffert, A. S.
- Shafi, N.
- Shilon, I.
- Simoni, R.
- Sol, H.
- Spanier, F.
- Spengler, G.
- Spies, F.
- Stawarz, Ł.
- Steenkamp, R.
- Boisson, C.
- Stegmann, C.
- Stycz, K.
- Sushch, I.
- Tavernet, J. -P.
- Tavernier, T.
- Taylor, A. M.
- Terrier, R.
- Tibaldo, L.
- Tiziani, D.
- Tluczykont, M.
- Bolmont, J.
- Trichard, C.
- Tuffs, R.
- Uchiyama, Y.
- van der Walt, D. J.
- van Eldik, C.
- van Rensburg, C.
- van Soelen, B.
- Vasileiadis, G.
- Veh, J.
- Venter, C.
- Bordas, P.
- Viana, A.
- Vincent, P.
- Vink, J.
- Voisin, F.
- Völk, H. J.
- Vuillaume, T.
- Wadiasingh, Z.
- Wagner, S. J.
- Wagner, P.
- Wagner, R. M.
- Bregeon, J.
- White, R.
- Wierzcholska, A.
- Willmann, P.
- Wörnlein, A.
- Wouters, D.
- Yang, R.
- Zabalza, V.
- Zaborov, D.
- Zacharias, M.
- Zanin, R.
- Brun, F.
- Zdziarski, A. A.
- Zech, A.
- Zefi, F.
- Ziegler, A.
- Żywucka, N.
- Brun, P.
- Bryan, M.
- Büchele, M.
- Bulik, T.
- Abramowski, A.
- Capasso, M.
- Carr, J.
- Casanova, S.
- Cerruti, M.
- Chakraborty, N.
- Chalme-Calvet, R.
- Chaves, R. C. G.
- Chen, A.
- Chevalier, J.
- Chrétien, M.
- Aharonian, F.
- Coffaro, M.
- Colafrancesco, S.
- Cologna, G.
- Condon, B.
- Conrad, J.
- Cui, Y.
- Davids, I. D.
- Decock, J.
- Degrange, B.
- Deil, C.
- Benkhali, F. Ait
- Devin, J.
- deWilt, P.
- Dirson, L.
- Djannati-Ataï, A.
- Domainko, W.
- Donath, A.
- Drury, L. O'C.
- Dutson, K.
- Dyks, J.
- Edwards, T.
- Akhperjanian, A. G.
- Egberts, K.
- Eger, P.
- Ernenwein, J. -P.
- Eschbach, S.
- Farnier, C.
- Fegan, S.
- Fern, M. V.
- Fiasson, A.
- Fontaine, G.
- Förster, A.
- Andersson, T.
- Funk, S.
- Füßling, M.
- Gabici, S.
- Gajdus, M.
- Gallant, Y. A.
- Garrigoux, T.
- Giavitto, G.
- Giebels, B.
- Glicenstein, J. F.
- Gottschall, D.
- Angüner, E. O.
- Goyal, A.
- Grondin, M. -H.
- Hadasch, D.
- Hahn, J.
- Haupt, M.
- Hawkes, J.
- Heinzelmann, G.
- Henri, G.
- Hermann, G.
- Hervet, O.
- Arrieta, M.
- Hinton, J. A.
- Hofmann, W.
- Hoischen, C.
- Holler, M.
- Horns, D.
- Ivascenko, A.
- Jacholkowska, A.
- Jamrozy, M.
- Janiak, M.
- Jankowsky, D.
Publication date
January 2016
DOIAbstract
Supernova remnants exhibit shock fronts (shells) that can accelerate charged particles up to very high energies. In the past decade, measurements of a handful of shell-type supernova remnants in very-high-energy gamma rays have provided unique insights into the acceleration process. Among those objects, RX$~$J1713.7-3946 (also known as G347.3-0.5) has the largest surface brightness, allowing us in the past to perform the most comprehensive study of morphology and spatially resolved spectra of any such very-high-energy gamma-ray source. Here we present extensive new H.E.S.S. measurements of RX$~$J1713.7-3946, almost doubling the observation time compared to our previous publication. Combined with new improved analysis tools, the previous sen...
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