Extended VHE gamma-ray emission towards SGR1806-20, LBV1806-20, and stellar cluster Cl*1806-20
Creators: name: Abdalla, H.
name: Abramowski, A.
name: Aharonian, F.
name: Benkhali, F. Ait
name: Akhperjanian, A. G.
name: Angüner, E. O.
name: Arrieta, M.
name: Aubert, P.
name: Backes, M.
name: Balzer, A.
name: Barnard, M.
name: Becherini, Y.
name: Tjus, J. Becker
name: Berge, D.
name: Bernhard, S.
name: Bernlöhr, K.
name: Birsin, E.
name: Blackwell, R.
name: Böttcher, M.
name: Boisson, C.
name: Bolmont, J.
name: Bordas, P.
name: Bregeon, J.
name: Brun, F.
name: Brun, P.
name: Bryan, M.
name: Bulik, T.
name: Capasso, M.
name: Carr, J.
name: Casanova, S.
name: Chakraborty, N.
name: Chalme-Calvet, R.
name: Chaves, R. C. G.
name: Chen, A.
name: Chevalier, J.
name: Chrétien, M.
name: Colafrancesco, S.
name: Cologna, G.
name: Condon, B.
name: Conrad, J.
name: Couturier, C.
name: Cui, Y.
name: Davids, I. D.
name: Degrange, B.
name: Deil, C.
name: deWilt, P.
name: Djannati-Ataï, A.
name: Domainko, W.
name: Donath, A.
name: Drury, L. O'C.
name: Dubus, G.
name: Dutson, K.
name: Dyks, J.
name: Dyrda, M.
name: Edwards, T.
name: Egberts, K.
name: Eger, P.
name: Ernenwein, J. -P.
name: Eschbach, S.
name: Farnier, C.
name: Fegan, S.
name: Fernandes, M. V.
name: Fiasson, A.
name: Fontaine, G.
name: Förster, A.
name: Funk, S.
name: Füßling, M.
name: Gabici, S.
name: Gajdus, M.
name: Gallant, Y. A.
name: Garrigoux, T.
name: Giavitto, G.
name: Giebels, B.
name: Glicenstein, J. F.
name: Gottschall, D.
name: Goyal, A.
name: Grondin, M. -H.
name: Grudzińska, M.
name: Hadasch, D.
name: Hahn, J.
name: Hawkes, J.
name: Heinzelmann, G.
name: Henri, G.
name: Hermann, G.
name: Hervet, O.
name: Hillert, A.
name: Hinton, J. A.
name: Hofmann, W.
name: Hoischen, C.
name: Holler, M.
name: Horns, D.
name: Ivascenko, A.
name: Jacholkowska, A.
name: Jamrozy, M.
name: Janiak, M.
name: Jankowsky, D.
name: Jankowsky, F.
name: Jingo, M.
name: Jogler, T.
name: Jouvin, L .
name: Jung-Richardt, I.
name: Kastendieck, M. A.
name: Katarzyński, K.
name: Katz, U.
name: Kerszberg, D.
name: Khélifi, B.
name: Kieffer, M.
name: King, J.
name: Klepser, S.
name: Klochkov, D.
name: Kluźniak, W.
name: Kolitzus, D.
name: Komin, Nu.
name: Kosack, K.
name: Krakau, S.
name: Kraus, M.
name: Krayzel, F.
name: Krüger, P. P.
name: Laffon, H.
name: Lamanna, G.
name: Lau, J.
name: Lees, J. -P.
name: Lefaucheur, J.
name: Lefranc, V.
name: Lemière, A.
name: Lemoine-Goumard, M.
name: Lenain, J. -P.
name: Leser, E.
name: Lohse, T.
name: Lorentz, M.
name: Liu, R.
name: Lypova, I.
name: Marandon, V.
name: Marcowith, A.
name: Mariaud, C.
name: Marx, R.
name: Maurin, G.
name: Maxted, N.
name: Mayer, M.
name: Meintjes, P. J.
name: Menzler, U.
name: Meyer, M.
name: Mitchell, A. M. W.
name: Moderski, R.
name: Mohamed, M.
name: Morå, K.
name: Moulin, E.
name: Murach, T.
name: de Naurois, M.
name: Niederwanger, F.
name: Niemiec, J.
name: Oakes, L.
name: Odaka, H.
name: Öttl, S.
name: Ohm, S.
name: Ostrowski, M.
name: Oya, I.
name: Padovani, M.
name: Panter, M.
name: Parsons, R. D.
name: Arribas, M. Paz
name: Pekeur, N. W.
name: Pelletier, G.
name: Petrucci, P. -O.
name: Peyaud, B.
name: Pita, S.
name: Poon, H.
name: Prokhorov, D.
name: Prokoph, H.
name: Pühlhofer, G.
name: Punch, M.
name: Quirrenbach, A.
name: Raab, S.
name: Reimer, A.
name: Reimer, O.
name: Renaud, M.
name: Reyes, R. de los
name: Rieger, F.
name: Romoli, C.
name: Rosier-Lees, S.
name: Rowell, G.
name: Rudak, B.
name: Rulten, C. B.
name: Sahakian, V.
name: Salek, D.
name: Sanchez, D. A.
name: Santangelo, A.
name: Sasaki, M.
name: Schlickeiser, R.
name: Schüssler, F.
name: Schulz, A.
name: Schwanke, U.
name: Schwemmer, S.
name: Seyffert, A. S.
name: Shafi, N.
name: Shilon, I.
name: Simoni, R.
name: Sol, H.
name: Spanier, F.
name: Spengler, G.
name: Spies, F.
name: Stawarz, L.
name: Steenkamp, R.
name: Stegmann, C.
name: Stinzing, F.
name: Stycz, K.
name: Sushch, I.
name: Tavernet, J. -P.
name: Tavernier, T.
name: Taylor, A. M.
name: Terrier, R.
name: Tluczykont, M.
name: Trichard, C.
name: Tuffs, R.
name: van der Walt, J.
name: van Eldik, C.
name: van Soelen, B.
name: Vasileiadis, G.
name: Veh, J.
name: Venter, C.
name: Viana, A.
name: Vincent, P.
name: Vink, J.
name: Voisin, F.
name: Völk, H. J.
name: Vuillaume, T.
name: Wadiasingh, Z.
name: Wagner, S. J.
name: Wagner, P.
name: Wagner, R. M.
name: White, R.
name: Wierzcholska, A.
name: Willmann, P.
name: Wörnlein, A.
name: Wouters, D.
name: Yang, R.
name: Zabalza, V.
name: Zaborov, D.
name: Zacharias, M.
name: Zdziarski, A. A.
name: Zech, A.
name: Zefi, F.
name: Ziegler, A.
name: Zywucka, N.
Publisher: name: arXiv
Year: 2016
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: Using the High Energy Spectroscopic System (H.E.S.S.) telescopes we have discovered a steady and extended very high-energy (VHE) gamma-ray source towards the luminous blue variable candidate LBV1806-20, massive stellar cluster Cl*1806-20, and magnetar SGR1806-20. The new VHE source, HESSJ1808-204, was detected at a statistical significance of &gt;6sigma (post-trial) with a photon flux normalisation $(2.9 \pm 0.4_{\rm stat} \pm 0.5_{\rm sys})\times 10^{-13}$\,ph\,cm$^{-2}$\,s$^{-1}$\,TeV$^{-1}$ at 1TeV and a power-law photon index of $2.3\pm0.2_{\rm stat}\pm 0.3_{\rm sys}$. The luminosity of this source (0.2 to 10 TeV; scaled to distance d=8.7kpc) is $L_{\rm VHE}\sim1.6 \times 10^{34}(d/{8.7kpc})^2$\,erg\,s$^{-1}$. The VHE gamma-ray emission is extended and is well fit by a single Gaussian with statistical standard deviation of $0.095^\circ \pm 0.015^\circ$. This extension is similar to that of the synchrotron radio nebula G10.0-0.3, which is thought to be powered by LBV1806-20. The VHE gamma-ray luminosity could be provided by the stellar wind luminosity of LBV1806-20 by itself and/or the massive star members of Cl*1806-20. Alternatively, magnetic dissipation (e.g. via reconnection) from SGR1806-20 can potentially account for the VHE luminosity. The origin and hadronic and/or leptonic nature of the accelerated particles responsible for HESSJ1808-204 is not yet clear. If associated with SGR1806-20, the potentially young age of the magnetar (650yr) can be used to infer the transport limits of these particles to match the VHE source size. This discovery provides new interest in the potential for high-energy particle acceleration from magnetars, massive stars, and/or stellar clusters.
description: Accepted for publication in A&amp;A (This version reduced some latex in the title and abstract)