Details

Autor(en) / Beteiligte

• Aharonian, F.
• Akhperjanian, A.
• Beilicke, M.
• Bernlöhr, K.
• Börst, H.-G.
• Bojahr, H.
• Bolz, O.
• Coarasa, T.
• Contreras, J. L.
• Cortina, J.
• Denninghoff, S.
• Fonseca, M. V.
• Girma, M.
• Götting, N.
• Heinzelmann, G.
• Hermann, G.
• Heusler, A.
• Hofmann, W.
• Horns, D.
• Jung, I.
• Kankanyan, R.
• Kestel, M.
• Kohnle, A.
• Konopelko, A.
• Kornmeyer, H.
• Kranich, D.
• Lampeitl, H.
• Lopez, M.
• Lorenz, E.
• Lucarelli, F.
• Mang, O.
• Meyer, H.
• Mirzoyan, R.
• Moralejo, A.
• Ona-Wilhelmi, E.
• Panter, M.
• Plyasheshnikov, A.
• Pühlhofer, G.
• R. de los Reyes
• Rhode, W.
• Ripken, J.
• Robrade, J.
• Rowell, G.
• Sahakian, V.
• Samorski, M.
• Schilling, M.
• Siems, M.
• Sobzynska, D.
• Stamm, W.
• Tluczykont, M.
• Vitale, V.
• Völk, H. J.
• Wiedner, C. A.
• Wittek, W.

Titel

Detection of TeV gamma-rays from the BL Lac 1ES 1959+650 in its low states and during a major outburst in 2002

Ist Teil von

• Astronomy and astrophysics (Berlin), 2003-07, Vol.406 (1), p.L9-L13

Ort / Verlag

EDP Sciences

Erscheinungsjahr

2003

Link zum Volltext

Quelle

Electronic Journals Library

Beschreibungen/Notizen

• TeV γ-rays from the BL Lac object 1ES 1959+650  have been measured during the years 2000 and 2001 with a significance of 5.2 σ at a value of 5.3% of the Crab flux and in May 2002 during strong outbursts with >$23\,\sigma$ at a flux level of up to 2.2 Crab, making 1ES 1959+650  the TeV Blazar with the third best event statistics. The deep observation of 197.4 h has been performed with the HEGRA stereoscopic system of 5 imaging atmospheric Cherenkov telescopes (IACT system). 1ES 1959+650  is located at a redshift of $z = 0.047$, providing an intermediate distance between the nearby Blazars Mkn 421 and Mkn 501, and the much more distant object H1426+428. This makes 1ES 1959+650  an important member of the class of TeV Blazars in view of the absorption of TeV photons by the diffuse extragalactic background radiation (DEBRA). The differential energy spectrum of 1ES 1959+650  during the flares can be fitted by a power law with a spectral index of $2.83 \pm 0.14_{\mbox{\tiny stat}} \pm 0.08_{\mbox{\tiny sys}}$ or by a power law with an exponential cut-off at $(4.2^{+0.8}_{-0.6~{\mbox{\tiny stat}}} \pm 0.9_{\mbox{\tiny sys}})$ TeV and a spectral index of $1.83 \pm 0.15_{\mbox{\tiny stat}} \pm 0.08_{\mbox{\tiny sys}}$. The low state differential energy spectrum obtained with lower statistics can be described by a pure power law with a spectral index of $3.18 \pm 0.17_{\mbox{\tiny stat}} \pm 0.08_{\mbox{\tiny sys}}$.