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 0.6 ^ { \circ } by 0.4 ^ { \circ } .
Most notably , the centroid of the VHE emission is centered near the peak of the coincident ^ { 12 } CO ( J=1-0 ) emission , 0.4 ^ { \circ } 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 \pm 0.33 _ { stat } \pm 0.30 _ { sys } and a flux of N _ { 0 } = ( 1.15 \pm 0.27 _ { stat } \pm 0.35 _ { sys } ) \times 10 ^ { -13 } cm ^ { -2 } s ^ { -1 } TeV ^ { -1 } .
The integral flux above 1 TeV corresponds to \sim 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 .