V. A. Acciari et al 2009 ApJ 703 L6 doi:10.1088/0004-637X/703/1/L6
V. A. Acciari1, E. Aliu2,27, T. Arlen3, T. Aune4, M. Bautista5, M. Beilicke6, W. Benbow1, D. Boltuch2, S. M. Bradbury7, J. H. Buckley6, V. Bugaev6, Y. Butt8, K. Byrum9, A. Cannon10, A. Cesarini11, Y. C. Chow3, L. Ciupik12, P. Cogan5, W. Cui13, R. Dickherber6, T. Ergin8, S. J. Fegan3, J. P. Finley13, P. Fortin14, L. Fortson12, A. Furniss4, D. Gall13, G. H. Gillanders11, E. V. Gotthelf15, J. Grube10, R. Guenette5, G. Gyuk12, D. Hanna5, J. Holder2, D. Horan16, C. M. Hui17, T. B. Humensky18, P. Kaaret19, N. Karlsson12, M. Kertzman20, D. Kieda17, A. Konopelko21, H. Krawczynski6, F. Krennrich22, M. J. Lang11, S. LeBohec17, G. Maier5, A. McCann5, M. McCutcheon5, J. Millis23, P. Moriarty24, R. Mukherjee14, R. A. Ong3, A. N. Otte4, D. Pandel19, J. S. Perkins1, M. Pohl22, J. Quinn10, K. Ragan5, L. C. Reyes25, P. T. Reynolds26, E. Roache1, H. J. Rose7, M. Schroedter22, G. H. Sembroski13, A. W. Smith9, D. Steele12, S. P. Swordy18, M. Theiling1, J. A. Toner11, V. V. Vassiliev3, S. Vincent17, R. G. Wagner9, S. P. Wakely18,27, J. E. Ward10, T. C. Weekes1, A. Weinstein3, T. Weisgarber18, D. A. Williams4, S. Wissel18, M. Wood3 and B. Zitzer13
Show affiliationsWe report the detection of very-high-energy (VHE) gamma-ray emission from supernova remnant (SNR) G106.3+2.7. Observations performed in 2008 with the VERITAS atmospheric Cherenkov gamma-ray telescope resolve extended emission overlapping the elongated radio SNR. The 7.3σ (pre-trials) detection has a full angular extent of roughly 0
6 by 0
4. Most notably, the centroid of the VHE emission is centered near the peak of the coincident 12CO (J = 1-0) emission, 0
4 away from the pulsar PSR J2229+6114, situated at the northern end of the SNR. Evidently the current-epoch particles from the pulsar wind nebula are not participating in the gamma-ray production. The VHE energy spectrum measured with VERITAS is well characterized by a power law dN/dE = N 0(E/3 TeV)–Γ with a differential index of Γ = 2.29 ± 0.33stat ± 0.30sys and a flux of N 0 = (1.15 ± 0.27stat ± 0.35sys) × 10–13 cm–2 s–1 TeV–1. The integral flux above 1 TeV corresponds to ~5 percent of the steady Crab Nebula emission above the same energy. We describe the observations and analysis of the object and briefly discuss the implications of the detection in a multiwavelength context.
gamma rays: observations; ISM: individual (G106.3+2.7=VER J2227+608); pulsars: individual (J2229+6114); supernova remnants
Issue 1 (2009 September 20)
Received 2009 June 19, accepted for publication 2009 August 10
Published 2009 August 25
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