Discovery of very high energy gamma-ray emission from the blazar 1ES 1727+502 with the MAGIC Telescopes
Creators: name: MAGIC Collaboration
name: Aleksić, J.
name: Antonelli, L. A.
name: Antoranz, P.
name: Asensio, M.
name: Backes, M.
name: de Almeida, U. Barres
name: Barrio, J. A.
name: González, J. Becerra
name: Bednarek, W.
name: Berger, K.
name: Bernardini, E.
name: Biland, A.
name: Blanch, O.
name: Bock, R. K.
name: Boller, A.
name: Bonnefoy, S.
name: Bonnoli, G.
name: Tridon, D. Borla
name: Borracci, F.
name: Bretz, T.
name: Carmona, E.
name: Carosi, A.
name: Fidalgo, D. Carreto
name: Colin, P.
name: Colombo, E.
name: Contreras, J. L.
name: Cortina, J.
name: Cossio, L.
name: Covino, S.
name: Da Vela, P.
name: Dazzi, F.
name: De Angelis, A.
name: De Caneva, G.
name: De Lotto, B.
name: Mendez, C. Delgado
name: Doert, M.
name: Domínguez, A.
name: Prester, D. Dominis
name: Dorner, D.
name: Doro, M.
name: Eisenacher, D.
name: Elsaesser, D.
name: Farina, E.
name: Ferenc, D.
name: Fonseca, M. V.
name: Font, L.
name: Fruck, C.
name: López, R. J. García
name: Garczarczyk, M.
name: Terrats, D. Garrido
name: Gaug, M.
name: Giavitto, G.
name: Godinović, N.
name: Muñoz, A. González
name: Gozzini, S. R.
name: Hadamek, A.
name: Hadasch, D.
name: Häfner, D.
name: Herrero, A.
name: Hose, J.
name: Hrupec, D.
name: Idec, W.
name: Jankowski, F.
name: Kadenius, V.
name: Klepser, S.
name: Knoetig, M. L.
name: Krähenbühl, T.
name: Krause, J.
name: Kushida, J.
name: La Barbera, A.
name: Lelas, D.
name: Lewandowska, N.
name: Lindfors, E.
name: Lombardi, S.
name: López, M.
name: López-Coto, R.
name: López-Oramas, A.
name: Lorenz, E.
name: Lozano, I.
name: Makariev, M.
name: Mallot, K.
name: Maneva, G.
name: Mankuzhiyil, N.
name: Mannheim, K.
name: Maraschi, L.
name: Marcote, B.
name: Mariotti, M.
name: Martínez, M.
name: Masbou, J.
name: Mazin, D.
name: Meucci, M.
name: Miranda, J. M.
name: Mirzoyan, R.
name: Moldón, J.
name: Moralejo, A.
name: Munar-Adrover, P.
name: Nakajima, D.
name: Niedzwiecki, A.
name: Nilsson, K.
name: Nowak, N.
name: Orito, R.
name: Paiano, S.
name: Palatiello, M.
name: Paneque, D.
name: Paoletti, R.
name: Paredes, J. M.
name: Partini, S.
name: Persic, M.
name: Prada, F.
name: Moroni, P. G. Prada
name: Prandini, E.
name: Puljak, I.
name: Reichardt, I.
name: Reinthal, R.
name: Rhode, W.
name: Ribó, M.
name: Rico, J.
name: Rügamer, S.
name: Saggion, A.
name: Saito, K.
name: Saito, T. Y.
name: Salvati, M.
name: Satalecka, K.
name: Scalzotto, V.
name: Scapin, V.
name: Schultz, C.
name: Schweizer, T.
name: Shore, S. N.
name: Sillanpää, A.
name: Sitarek, J.
name: Snidaric, I.
name: Sobczynska, D.
name: Spanier, F.
name: Spiro, S.
name: Stamatescu, V.
name: Stamerra, A.
name: Steinke, B.
name: Storz, J.
name: Sun, S.
name: Surić, T.
name: Takalo, L.
name: Takami, H.
name: Tavecchio, F.
name: Temnikov, P.
name: Terzić, T.
name: Tescaro, D.
name: Teshima, M.
name: Tibolla, O.
name: Torres, D. F.
name: Toyama, T.
name: Treves, A.
name: Uellenbeck, M.
name: Vogler, P.
name: Wagner, R. M.
name: Weitzel, Q.
name: Zandanel, F.
name: Zanin, R.
Publisher: name: arXiv
Year: 2013
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: Motivated by the Costamante &amp; Ghisellini (2002) predictions we investigated if the blazar 1ES 1727+502 (z=0.055) is emitting very high energy (VHE, E&gt;100 GeV) gamma rays. We observed the BL Lac object 1ES 1727+502 in stereoscopic mode with the two MAGIC telescopes during 14 nights between May 6th and June 10th 2011, for a total effective observing time of 12.6 hours. For the study of the multiwavelength spectral energy distribution (SED) we use simultaneous optical R-band data from the KVA telescope, archival UV/optical and X-ray observations by instruments UVOT and XRT on board of the Swift satellite and high energy (HE, 0.1 GeV - 100 GeV) gamma-ray data from the Fermi-LAT instrument. We detect, for the first time, VHE gamma-ray emission from 1ES 1727+502 at a statistical significance of 5.5 sigma. The integral flux above 150 GeV is estimated to be (2.1\pm0.4)% of the Crab Nebula flux and the de-absorbed VHE spectrum has a photon index of (2.7\pm0.5). No significant short-term variability was found in any of the wavebands presented here. We model the SED using a one-zone synchrotron self-Compton model obtaining parameters typical for this class of sources.
description: 7 pages, 5 figures, 2 tables, submitted to A&amp;A