V. A. Acciari et al 2009 ApJ 698 L133 doi:10.1088/0004-637X/698/2/L133
V. A. Acciari1, E. Aliu2, T. Arlen3, T. Aune4, M. Bautista5, M. Beilicke6, W. Benbow1, S. M. Bradbury7, J. H. Buckley6, V. Bugaev6, Y. Butt8, K. Byrum9, A. Cannon10, O. Celik3,29, A. Cesarini11, Y. C. Chow3, L. Ciupik12, P. Cogan5, P. Colin13, W. Cui14, M. K. Daniel7,30, R. Dickherber6, C. Duke15, V. V. Dwarkadas16, T. Ergin8, S. J. Fegan3,31, J. P. Finley14, G. Finnegan13, P. Fortin17,31, L. Fortson12, A. Furniss4, D. Gall14, K. Gibbs1, G. H. Gillanders11, S. Godambe13, J. Grube10, R. Guenette5, G. Gyuk12, D. Hanna5, E. Hays18, J. Holder2, D. Horan19, C. M. Hui13, T. B. Humensky20,32, A. Imran21, P. Kaaret22, N. Karlsson12, M. Kertzman23, D. Kieda13, J. Kildea1, A. Konopelko24, H. Krawczynski6, F. Krennrich21, M. J. Lang11, S. LeBohec13, G. Maier5, A. McCann5, M. McCutcheon5, J. Millis25, P. Moriarty26, R. A. Ong3, A. N. Otte4, D. Pandel22, J. S. Perkins1, M. Pohl21, J. Quinn10, K. Ragan5, L. C. Reyes27, P. T. Reynolds28, E. Roache1, H. J. Rose7, M. Schroedter21, G. H. Sembroski14, A. W. Smith9, D. Steele12, S. P. Swordy20, M. Theiling1, J. A. Toner11, L. Valcarcel5, A. Varlotta14, V. V. Vassiliev3, S. Vincent13, R. G. Wagner9, S. P. Wakely20, J. E. Ward10, T. C. Weekes1, A. Weinstein3, T. Weisgarber20, D. A. Williams4, S. Wissel20, M. Wood3 and B. Zitzer14
Show affiliationsWe present evidence that the very high energy (VHE, E > 100 GeV) gamma-ray emission coincident with the supernova remnant IC 443 is extended. IC 443 contains one of the best studied sites of supernova remnant/molecular cloud interaction and the pulsar wind nebula CXOU J061705.3+222127, both of which are important targets for VHE observations. VERITAS observed IC 443 for 37.9 hr during 2007 and detected emission above 300 GeV with an excess of 247 events, resulting in a significance of 8.3 standard deviations (σ) before trials and 7.5σ after trials in a point-source search. The emission is centered at 6h16m51s + 22°30'11'' (J2000) ±0
03stat ± 0
08sys, with an intrinsic extension of 0
16 ± 0
03stat ± 0
04sys. The VHE spectrum is well fit by a power law (dN/dE = N 0 × (E/TeV)–Γ) with a photon index of 2.99 ± 0.38stat ± 0.3sys and an integral flux above 300 GeV of (4.63 ± 0.90stat ± 0.93sys) × 10–12 cm–2 s–1. These results are discussed in the context of existing models for gamma-ray production in IC 443.
gamma rays: observations; ISM: individual (IC 443 = VER J0616.9+2230, = MAGIC J0616+225)
98.58.Db Molecular clouds, H2 clouds, dense clouds, and dark clouds
Issue 2 (2009 June 20)
Received 2009 April 16, accepted for publication 2009 May 19
Published 2009 June 1
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