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26 April 2024

» arxiv » 0911.4695

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Detection of Extended VHE Gamma Ray Emission from G106.3+2.7 with VERITAS
VERITAS Collaboration ; V. A. Acciari ; E. Aliu ; T. Arlen ; T. Aune ; M. Bautista ; M. Beilicke ; W. Benbow ; D. Boltuch ; S. M. Bradbury ; J. H. Buckley ; V. Bugaev ; Y. Butt ; K. Byrum ; A. Cannon ; A. Cesarini ; Y. C. Chow ; L. Ciupik ; P. Cogan ; W. Cui ; R. Dickherber ; T. Ergin ; S. J. Fegan ; J. P. Finley ; P. Fortin ; L. Fortson ; A. Furniss ; D. Gall ; G. H. Gillanders ; E. V. Gotthelf ; J. Grube ; R. Guenette ; G. Gyuk ; D. Hanna ; J. Holder ; D. Horan ; C. M. Hui ; T. B. Humensky ; P. Kaaret ; N. Karlsson ; M. Kertzman ; D. Kieda ; A. Konopelko ; H. Krawczynski ; F. Krennrich ; M. J. Lang ; S. LeBohec ; G. Maier ; A. McCann ; M. McCutcheon ; J. Millis ; P. Moriarty ; R. Mukherjee ; R. A. Ong ; A. N. Otte ; D. Pandel ; J. S. Perkins ; M. Pohl ; J. Quinn ; K. Ragan ; L. C. Reyes ; P. T. Reynolds ; E. Roache ; H. J. Rose ; M. Schroedter ; G. H. Sembroski ; A. W. Smith ; D. Steele ; S. P. Swordy ; M. Theiling ; J. A. Toner ; V. V. Vassiliev ; S. Vincent ; R. G. Wagner ; S. P. Wakely ; J. E. Ward ; T. C. Weekes ; A. Weinstein ; T. Weisgarber ; D. A. Williams ; S. Wissel ; M. Wood ; B. Zitzer ;
Date:	24 Nov 2009
Abstract:	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 0.6deg by 0.4deg. Most notably, the centroid of the VHE emission is centered near the peak of the coincident 12CO (J = 1-0) emission, 0.4deg 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)^{-G} with a differential index of G = 2.29 +/- 0.33stat +/- 0.30sys and a flux of N_0 = (1.15 +/- 0.27stat +/- 0.35sys)x 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.
Source:	arXiv, 0911.4695
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