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DETECTION OF EXTENDED VHE GAMMA RAY EMISSION FROM G106.3+2.7 WITH VERITAS

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2009-09-20
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, Tülün
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.
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 7.3 sigma (pre-trials) detection has a full angular extent of roughly 0 degrees.6 by 0 degrees.4. Most notably, the centroid of the VHE emission is centered near the peak of the coincident (CO)-C-12 (J = 1-0) emission, 0 degrees.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)(-Gamma) with a differential index of Gamma = 2.29 +/- 0.33(stat) +/- 0.30(sys) and a flux of N-0 = (1.15 +/- 0.27(stat) +/- 0.35(sys)) x 10(-13) cm(-2) s(-1) TeV-1. The integral flux above 1 TeV corresponds to similar 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.