Detection of Extended VHE Gamma Ray Emission from G106.3+2.7 with VERITAS

Details Detection of Extended VHE Gamma Ray Emission from G106.3+2.7 with VERITAS Detection of Extended VHE Gamma Ray Emission from G106.3+2.7 with VERITAS

2009-11-24

arxiv.org/abs/0911.4695v1

ApJL 703:L6-L9 (2009)

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

5 pages, 2 figures

Scientific paper

10.1088/0004-637X/703/1/L6

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.

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