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Acciari, V. A; Aliu, E; Arlen, T; Aune, T; Bautista, M; Beilicke, M; Benbow, W; Boltuch, D; Bradbury, S. M; Buckley, J. H; Bugaev, V; Butt, Y; Byrum, K; Cannon, A; Cesarini, A; Chow, Y. C; Ciupik, L; Cogan, P; Cui, W; Dickherber, R; Ergin, T; Fegan, S. J; Finley, J. P; Fortin, P; Fortson, L; Furniss, A; Gall, D; Gillanders, G. H; Gotthelf, E. V; Grube, J; Guenette, R; Gyuk, G; Hanna, D; Holder, J; Horan, D; Hui, C. M; Humensky, T. B; Kaaret, P; Karlsson, N; Kertzman, M; Kieda, D; Konopelko, A; Krawczynski, H; Krennrich, F; Lang, M. J; LeBohec, S; Maier, G; McCann, A; McCutcheon, M; Millis, J; Moriarty, P; Mukherjee, R; Ong, R. A; Otte, A. N; Pandel, D; Perkins, J. S; Pohl, M; Quinn, J; Ragan, K; Reyes, L. C; Reynolds, P. T; Roache, E; Rose, H. J; Schroedter, M; Sembroski, G. H; Smith, A. W; Steele, D; Swordy, S. P; Theiling, M; Toner, J. A; Vassiliev, V. V; Vincent, S; Wagner, R. G; Wakely, S. P; Ward, J. E; Weekes, T. C; Weinstein, A; Weisgarber, T; Williams, D. A; Wissel, S; Wood, M; Zitzer, B
Astrophysical journal/The Astrophysical journal, 09/2009, Letnik: 703, Številka: 1Journal Article
We 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 7.3sigma (pre-trials) detection has a full angular extent of roughly 0.{sup 0}6 by 0.{sup 0}4. Most notably, the centroid of the VHE emission is centered near the peak of the coincident {sup 12}CO (J = 1-0) emission, 0.{sup 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 {sub 0}(E/3 TeV){sup -G}AMMA with a differential index of GAMMA = 2.29 +- 0.33{sub stat} +- 0.30{sub sys} and a flux of N{sub 0} = (1.15 +- 0.27{sub stat} +- 0.35{sub sys}) x 10{sup -13} cm{sup -2} s{sup -1} TeV{sup -1}. The integral flux above 1 TeV corresponds to {approx}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.
