% IMPORTANT: The following is UTF-8 encoded. This means that in the presence % of non-ASCII characters, it will not work with BibTeX 0.99 or older. % Instead, you should use an up-to-date BibTeX implementation like “bibtex8” or % “biber”. @ARTICLE{Abdalla:418010, author = {Abdalla, H. and Abramowski, A. and Aharonian, F. and Ait Benkhali, F. and Akhperjanian, A. G. and Andersson, T. and Angüner, E. O. and Arrieta, M. and Aubert, P. and Backes, M. and Balzer, A. and Barnard, M. and Becherini, Y. and Becker Tjus, J. and Berge, D. and Bernhard, S. and Bernlöhr, K. and Blackwell, R. and Böttcher, M. and Boisson, C. and Bolmont, J. and Bordas, P. and Bregeon, J. and Brun, F. and Brun, P. and Bryan, M. and Bulik, T. and Capasso, M. and Carr, J. and Casanova, S. and Cerruti, M. and Chakraborty, N. and Chalme-Calvet, R. and Chaves, R. C. G. and Chen, A. and Chevalier, J. and Chrétien, M. and Colafrancesco, S. and Cologna, G. and Condon, B. and Conrad, J. and Cui, Y. and Davids, I. D. and Decock, J. and Degrange, B. and Deil, C. and Devin, J. and deWilt, P. and Dirson, L. and $Djannati-Ata\'i,$ A. and Domainko, W. and Donath, A. and Drury, L. O'C. and Dubus, G. and Dutson, K. and Dyks, J. and Edwards, T. and Egberts, K. and Eger, P. and Ernenwein, J.-P. and Eschbach, S. and Farnier, C. and Fegan, S. and Fernandes, M. V. and Fiasson, A. and Fontaine, G. and Förster, A. and Fukuyama, T. and Funk, S. and Füßling, M. and Gabici, S. and Gajdus, M. and Gallant, Y. A. and Garrigoux, T. and Giavitto, G. and Giebels, B. and Glicenstein, J. F. and Gottschall, D. and Goyal, A. and Grondin, M.-H. and Hadasch, D. and Hahn, J. and Haupt, M. and Hawkes, J. and Heinzelmann, G. and Henri, G. and Hermann, G. and Hervet, O. and Hinton, J. A. and Hofmann, W. and Hoischen, C. and Holler, M. and Horns, D. and Ivascenko, A. and Jacholkowska, A. and Jamrozy, M. and Janiak, M. and Jankowsky, D. and Jankowsky, F. and Jingo, M. and Jogler, T. and Jouvin, L. and Jung-Richardt, I. and Kastendieck, M. A. and Katarzyński, K. and Katz, U. and Kerszberg, D. and Khélifi, B. and Kieffer, M. and King, J. and Klepser, S. and Klochkov, D. and Kluźniak, W. and Kolitzus, D. and Komin, Nu. and Kosack, K. and Krakau, S. and Kraus, M. and Krayzel, F. and Krüger, P. P. and Laffon, H. and Lamanna, G. and Lau, J. and Lees, J.-P. and Lefaucheur, J. and Lefranc, V. and Lemière, A. and Lemoine-Goumard, M. and Lenain, J.-P. and Leser, E. and Lohse, T. and Lorentz, M. and Liu, R. and López-Coto, R. and Lypova, I. and Marandon, V. and Marcowith, A. and Mariaud, C. and Marx, R. and Maurin, G. and Maxted, N. and Mayer, M. and Meintjes, P. J. and Meyer, M. and Mitchell, A. M. W. and Moderski, R. and Mohamed, M. and Mohrmann, L. and Morå, K. and Moulin, E. and Murach, T. and de Naurois, M. and Niederwanger, F. and Niemiec, J. and Oakes, L. and O'Brien, P. and Odaka, H. and Öttl, S. and Ohm, S. and Ostrowski, M. and Oya, I. and Padovani, M. and Panter, M. and Parsons, R. D. and Pekeur, N. W. and Pelletier, G. and Perennes, C. and Petrucci, P.-O. and Peyaud, B. and Piel, Q. and Pita, S. and Poon, H. and Prokhorov, D. and Prokoph, H. and Pühlhofer, G. and Punch, M. and Quirrenbach, A. and Raab, S. and Reimer, A. and Reimer, O. and Renaud, M. and de los Reyes, R. and Rieger, F. and Romoli, C. and Rosier-Lees, S. and Rowell, G. and Rudak, B. and Rulten, C. B. and Sahakian, V. and Salek, D. and Sanchez, D. A. and Santangelo, A. and Sasaki, M. and Schlickeiser, R. and Schüssler, F. and Schulz, Anneli and Schwanke, U. and Schwemmer, S. and Settimo, M. and Seyffert, A. S. and Shafi, N. and Shilon, I. and Simoni, R. and Sol, H. and Spanier, F. and Spengler, G. and Spies, F. and Steenkamp, R. and Stegmann, C. and Stinzing, F. and Stycz, K. and Sushch, I. and Takahashi, T. and Tavernet, J.-P. and Tavernier, T. and Taylor, A. M. and Terrier, R. and Tibaldo, L. and Tiziani, D. and Tluczykont, M. and Trichard, C. and Tuffs, R. and Uchiyama, Y. and van der Walt, D. J. and van Eldik, C. and van Rensburg, C. and van Soelen, B. and Vasileiadis, G. and Veh, J. and Venter, C. and Viana, A. and Vincent, P. and Vink, J. and Voisin, F. and Völk, H. J. and Volpe, F. and Vuillaume, T. and Wadiasingh, Z. and Wagner, S. J. and Wagner, P. and Wagner, R. M. and White, R. and Wierzcholska, A. and Willmann, P. and Wörnlein, A. and Wouters, D. and Yang, R. and Zabalza, V. and Zaborov, D. and Zacharias, M. and Zdziarski, A. A. and Zech, A. and Zefi, F. and Ziegler, A. and Żywucka, N.}, collaboration = {H. E. S. S.{ Collaboration}}, title = {{H}.{E}.{S}.{S}. observations of {RX} {J}1713.7−3946 with improved angular and spectral resolution: {E}vidence for gamma-ray emission extending beyond the {X}-ray emitting shell}, journal = {Astronomy and astrophysics}, volume = {612}, issn = {1432-0746}, address = {Les Ulis}, publisher = {EDP Sciences}, reportid = {PUBDB-2019-00138, arXiv:1609.08671}, pages = {A6}, year = {2018}, note = {(c) ESO}, abstract = {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 sensitivity is more than doubled. The H.E.S.S. angular resolution of 0.048° (0.036° above 2 TeV) is unprecedented in gamma-ray astronomy and probes physical scales of 0.8 (0.6) parsec at the remnant’s location. The new H.E.S.S. image of RX J1713.7−3946 allows us to reveal clear morphological differences between X-rays and gamma rays. In particular, for the outer edge of the brightest shell region, we find the first ever indication for particles in the process of leaving the acceleration shock region. By studying the broadband energy spectrum, we furthermore extract properties of the parent particle populations, providing new input to the discussion of the leptonic or hadronic nature of the gamma-ray emission mechanism.Key words: acceleration of particles / cosmic rays / ISM: supernova remnants / gamma rays: general / astroparticle physic★ All images (FITS files)are available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/612/A6† Deceased.}, keywords = {gamma ray: emission (INSPIRE) / gamma ray: VHE (INSPIRE) / X-ray: emission (INSPIRE) / HESS (INSPIRE) / acceleration (INSPIRE) / supernova (INSPIRE) / angular resolution (INSPIRE) / charged particle (INSPIRE) / energy spectrum (INSPIRE) / sensitivity (INSPIRE) / brightness (INSPIRE) / resolution (INSPIRE) / spectral (INSPIRE) / doubling (INSPIRE) / surface (INSPIRE)}, cin = {ZEU-HESS}, ddc = {520}, cid = {I:(DE-H253)ZEU-HESS-20140213}, pnm = {613 - Matter and Radiation from the Universe (POF3-613)}, pid = {G:(DE-HGF)POF3-613}, experiment = {EXP:(DE-H253)HESS-20170101}, typ = {PUB:(DE-HGF)29 / PUB:(DE-HGF)16}, eprint = {1609.08671}, howpublished = {arXiv:1609.08671}, archivePrefix = {arXiv}, SLACcitation = {$\%\%CITATION$ = $arXiv:1609.08671;\%\%$}, UT = {WOS:000429404700006}, doi = {10.1051/0004-6361/201629790}, url = {https://bib-pubdb1.desy.de/record/418010}, }