%0 Journal Article
%T HESS J1818-154, a new composite supernova remnant discovered in TeV gamma rays and X-rays
%+ Laboratoire Univers et Théories (LUTH (UMR_8102))
%+ Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU)
%+ Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE)
%+ Laboratoire Leprince-Ringuet (LLR)
%+ AstroParticule et Cosmologie (APC (UMR_7164))
%+ Laboratoire d'Annecy de Physique des Particules (LAPP)
%+ Laboratoire Univers et Particules de Montpellier (LUPM)
%+ Astroparticules (ASTRO)
%A Abramowski, A.
%A Aharonian, F.
%A Benkhali, F. Ait
%A Akhperjanian, A. G.
%A Angüner, E.
%A Anton, G.
%A Balenderan, S.
%A Balzer, Agnès
%A Barnacka, A.
%A Becherini, Y.
%A Tjus, J. Becker
%A Bernlöhr, K.
%A Birsin, E.
%A Bissaldi, E.
%A Biteau, J.
%A Böttcher, M.
%A Boisson, C.
%A Bolmont, J.
%A Bordas, P.
%A Brucker, J.
%A Brun, F.
%A Brun, P.
%A Bulik, T.
%A Carrigan, S.
%A Casanova, S.
%A Cerruti, M.
%A Chadwick, P. M.
%A Chalme-Calvet, R.
%A Chaves, R. C. G.
%A Cheesebrough, A.
%A Chrétien, M.
%A Colafrancesco, S.
%A Cologna, G.
%A Conrad, J.
%A Couturier, C.
%A Cui, Y.
%A Dalton, M.
%A Daniel, M. K.
%A Davids, I. D.
%A Degrange, B.
%A Deil, C.
%A de Wilt, P.
%A Dickinson, H. J.
%A Djannati-Ataï, A.
%A Domainko, W.
%A Drury, L. O'C.
%A Dubus, G.
%A Dutson, K.
%A Dyks, J.
%A Dyrda, M.
%A Edwards, T.
%A Egberts, K.
%A Eger, P.
%A Espigat, P.
%A Farnier, C.
%A Fegan, S.
%A Feinstein, F.
%A Fernandes, M. V.
%A Fernandez, D.
%A Fiasson, A.
%A Fontaine, G.
%A Förster, A.
%A Füssling, M.
%A Gajdus, M.
%A Gallant, Y. A.
%A Garrigoux, T.
%A Giavitto, G.
%A Giebels, B.
%A Glicenstein, J. F.
%A Grondin, M. -H.
%A Grudzińska, M.
%A Häffner, S.
%A Hahn, J.
%A Harris, J.
%A Heinzelmann, G.
%A Henri, G.
%A Hermann, G.
%A Hervet, O.
%A Hillert, A.
%A Hinton, J. A.
%A Hofmann, W.
%A Hofverberg, P.
%A Holler, M.
%A Horns, D.
%A Jacholkowska, A.
%A Jahn, C.
%A Jamrozy, M.
%A Janiak, M.
%A Jankowsky, F.
%A Jung, I.
%A Kastendieck, M. A.
%A Katarzynski, K.
%A Katz, U.
%A Kaufmann, S.
%A Khélifi, B.
%A Kieffer, Michel
%A Klepser, S.
%A Klochkov, D.
%A Kluźniak, W.
%A Kneiske, T.
%A Kolitzus, D.
%A Komin, Nu.
%A Kosack, K.
%A Krakau, S.
%A Krayzel, F.
%A Krüger, P. P.
%A Laffon, H.
%A Lamanna, G.
%A Lefaucheur, J.
%A Lemière, A.
%A Lemoine-Goumard, M.
%A Lenain, J. -P.
%A Lennarz, D.
%A Lohse, T.
%A Lopatin, A.
%A Lu, C. -C.
%A Marandon, V.
%A Marcowith, A.
%A Marx, R.
%A Maurin, G.
%A Maxted, N.
%A Mayer, M.
%A Mccomb, T. J. L.
%A Méhault, J.
%A Meintjes, P. J.
%A Menzler, U.
%A Meyer, M.
%A Moderski, R.
%A Mohamed, M.
%A Moulin, Emmanuel
%A Murach, T.
%A Naumann, C. L.
%A de Naurois, M.
%A Niemiec, J.
%A Nolan, S. J.
%A Oakes, L.
%A Ohm, S.
%A Wilhelmi, E. de Ona
%A Opitz, B.
%A Ostrowski, M.
%A Oya, I.
%A Panter, M.
%A Parsons, R. D.
%A Arribas, M. Paz
%A Pekeur, N. W.
%A Pelletier, G.
%A Perez, J.
%A Petrucci, P. -O.
%A Peyaud, B.
%A Pita, S.
%A Poon, H.
%A Pühlhofer, G.
%A Punch, M.
%A Quirrenbach, A.
%A Raab, S.
%A Raue, M.
%A Reimer, A.
%A Reimer, O.
%A Renaud, M.
%A Reyes, R. de Los
%A Rieger, F.
%A Rob, L.
%A Romoli, C.
%A Rosier-Lees, S.
%A Rowell, G.
%A Rudak, B.
%A Rulten, C. B.
%A Sahakian, V.
%A Sanchez, D. A.
%A Santangelo, A.
%A Schlickeiser, R.
%A Schüssler, F.
%A Schulz, A.
%A Schwanke, U.
%A Schwarzburg, S.
%A Schwemmer, S.
%A Sol, H.
%A Spengler, G.
%A Spies, F.
%A Stawarz, L.
%A Steenkamp, R.
%A Stegmann, C.
%A Stinzing, F.
%A Stycz, K.
%A Sushch, I.
%A Szostek, A.
%A Tavernet, J. -P.
%A Tavernier, T.
%A Taylor, A. M.
%A Terrier, R.
%A Tluczykont, M.
%A Trichard, C.
%A Valerius, K.
%A van Eldik, C.
%A van Soelen, B.
%A Vasileiadis, G.
%A Venter, C.
%A Viana, A.
%A Vincent, P.
%A Völk, H. J.
%A Volpe, F.
%A Vorster, M.
%A Vuillaume, T.
%A Wagner, S. J.
%A Wagner, P.
%A Ward, M.
%A Weidinger, M.
%A Weitzel, Q.
%A White, R.
%A Wierzcholska, A.
%A Willmann, P.
%A Wörnlein, A.
%A Wouters, D.
%A Zabalza, V.
%A Zacharias, M.
%A Zajczyk, A.
%A Zdziarski, A. A.
%A Zech, A.
%A Zechlin, H. -S.
%< avec comité de lecture
%@ 0004-6361
%J Astronomy and Astrophysics - A&A
%I EDP Sciences
%V 562
%P A40
%8 2014
%D 2014
%Z 1310.6956
%Z 2014A&A...562A..40H
%R 10.1051/0004-6361/201322914
%Z Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE]
%Z Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE]
%Z Physics [physics]
%Z Physics [physics]/Astrophysics [astro-ph]Journal articles
%X Composite supernova remnants (SNRs) constitute a small subclass of remnants of massive stellar explosions where non-thermal radiation is observed from both the expanding shell-like shock front and from a pulsar wind nebula (PWN) located inside of the SNR. These systems represent a unique evolutionary phase of SNRs where observations in the radio, X-ray and gamma-ray regimes allow the study of the co-evolution of both of these energetic phenomena. In this article, we report results from observations of the shell-type SNR G15.4+0.1 performed with the High Energy Stereoscopic System (H.E.S.S.) and XMM-Newton. A compact TeV gamma-ray source, HESSJ1818-154, located in the center and contained within the shell of G15.4+0.1 is detected by H.E.S.S. featuring a spectrum best represented by a power-law model with a spectral index of $-2.3 \pm 0.3_{stat} \pm 0.2_{sys}$ and an integral flux of F$(>0.42\,\mathrm{TeV}$)=($0.9 \pm 0.3_{\mathrm{stat}} \pm 0.2_{\mathrm{sys}}) \times 10^{-12}$ cm$^{-2}$ s$^{-1}$. Furthermore, a recent observation with XMM-Newton reveals extended X-ray emission strongly peaked in the center of G15.4+0.1. The X-ray source shows indications for an energy-dependent morphology featuring a compact core at energies above 4 keV and more extended emission that fills the entire region within the SNR at lower energies. Together, the X-ray and VHE gamma-ray emission provide strong evidence for the existence of a PWN located inside the shell of G15.4+0.1 and this SNR can therefore be classified as a composite based on these observations. The radio, X-ray and gamma-ray emission from the PWN is compatible with a one-zone leptonic model which requires a low average magnetic field inside the emission region. An unambiguous counterpart to the putative pulsar, thought to power the PWN, has not been detected neither in radio nor in X-ray observations of G15.4+0.1.
%G English
%Z HESS
%2 https://hal.in2p3.fr/in2p3-00907620/document
%2 https://hal.in2p3.fr/in2p3-00907620/file/aa22914-13.pdf
%L in2p3-00907620
%U https://hal.in2p3.fr/in2p3-00907620
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