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Acciari, VA,Aliu, E,Arlen, T,Aune, T,Bautista, M,Beilicke, M,Benbow, W,Boltuch, D,Bradbury, SM,Buckley, JH,Bugaev, V,Butt, Y,Byrum, K,Cannon, A,Cesarini, A,Chow, YC,Ciupik, L,Cogan, P,Cui, W,Dickherber, R,Ergin, T,Fegan, SJ,Finley, JP,Fortin, P,Fortson, L,Furniss, A,Gall, D,Gillanders, GH,Gotthelf, EV,Grube, J,Guenette, R,Gyuk, G,Hanna, D,Holder, J,Horan, D,Hui, CM,Humensky, TB,Kaaret, P,Karlsson, N,Kertzman, M,Kieda, D,Konopelko, A,Krawczynski, H,Krennrich, F,Lang, MJ,LeBohec, S,Maier, G,McCann, A,McCutcheon, M,Millis, J,Moriarty, P,Mukherjee, R,Ong, RA,Otte, AN,Pandel, D,Perkins, JS,Pohl, M,Quinn, J,Ragan, K,Reyes, LC,Reynolds, PT,Roache, E,Rose, HJ,Schroedter, M,Sembroski, GH,Smith, AW,Steele, D,Swordy, SP,Theiling, M,Toner, JA,Vassiliev, VV,Vincent, S,Wagner, RG,Wakely, SP,Ward, JE,We
2009
September
Astrophysical Journal Letters
DETECTION OF EXTENDED VHE GAMMA RAY EMISSION FROM G106.3+2.7 WITH VERITAS
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()
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gamma rays: observations ISM: individual (G106.3+2.7=VER J2227+608) pulsars: individual (J2229+6114) supernova remnants PULSAR WIND NEBULAE SOURCE 3EG J2227+6122 GALACTIC-PLANE SURVEY SUPERNOVA REMNANT MOLECULAR CLOUDS SOURCE LIST TELESCOPE DISCOVERY ASTRONOMY FIELD
703
6
9
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.
DOI 10.1088/0004-637X/703/1/L6
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