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VERITAS Observations of a Very High Energy Gamma-ray Flare from the Blazar 3C 66A

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arxiv 0901.4527 v2 pith:TM3IMKHQ submitted 2009-01-28 astro-ph.HE astro-ph.CO

VERITAS Observations of a Very High Energy Gamma-ray Flare from the Blazar 3C 66A

VERITAS Collaboration: V. A. Acciari , E. Aliu , T. Arlen , M. Beilicke , W. Benbow , M. Bottcher , S. M. Bradbury , J. H. Buckley
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V. Bugaev Y. Butt K. Byrum A. Cannon O. Celik A. Cesarini Y. C. Chow L. Ciupik P. Cogan W. Cui M. K. Daniel R. Dickherber T. Ergin A. Falcone S. J. Fegan J. P. Finley P. Fortin L. Fortson A. Furniss D. Gall K. Gibbs G. H. Gillanders S. Godambe J. Grube R. Guenette G. Gyuk D. Hanna E. Hays J. Holder D. Horan C. M. Hui T. B. Humensky A. Imran P. Kaaret N. Karlsson M. Kertzman D. Kieda J. Kildea A. Konopelko H. Krawczynski F. Krennrich M. J. Lang S. LeBohec G. Maier A. McCann M. McCutcheon J. Millis P. Moriarty R. Mukherjee T. Nagai R. A. Ong A. N. Otte D. Pandel J. S. Perkins D. Petry F. Pizlo M. Pohl J. Quinn K. Ragan L. C. Reyes P. T. Reynolds E. Roache H. J. Rose M. Schroedter G. H. Sembroski A. W. Smith D. Steele S. P. Swordy M. Theiling J. A. Toner A. Varlotta V. V. Vassiliev R. G. Wagner S. P. Wakely J. E. Ward T. C. Weekes A. Weinstein D. A. Williams S. Wissel M. Wood B. Zitzer
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classification astro-ph.HE astro-ph.CO
keywords energydetectedfluxhighobservationsveritasveryabove
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The intermediate-frequency peaked BL Lacertae (IBL) object 3C 66A is detected during 2007 - 2008 in VHE (very high energy: E > 100 GeV) gamma-rays with the VERITAS stereoscopic array of imaging atmospheric Cherenkov telescopes. An excess of 1791 events is detected, corresponding to a significance of 21.2 standard deviations (sigma), in these observations (32.8 hours live time). The observed integral flux above 200 GeV is 6% of the Crab Nebula's flux and shows evidence for variability on the time-scale of days. The measured energy spectrum is characterized by a soft power law with photon index Gamma = 4.1 +- 0.4_stat +- 0.6_sys. The radio galaxy 3C 66B is excluded as a possible source of the VHE emission.

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