The supernova remnant (SNR) G106.3 + 2.7 has a comet-shaped morphology in radio with a head and an elongated tail, and a pulsar PSR J2229 + 6114 is located in the northern boundary of the head. Recently, $\gamma$-rays with energies range from GeV to 500 TeV spatially coincident with the tail region have been detected. We investigate whether the $\gamma$-rays can be produced by the high-energy electrons/positrons in a nebula powered by PSR J2229 + 6114. Using a one-zone model for the multiband emission from the nebula, the detected radio, X-ray and $\gamma$-ray fluxes can be well reproduced with the assumption that a fraction ($\sim 0.12$) of the spin-down luminosity is used to power the leptons in the emission zone. The particle spectrum has a break at the lorentz factor $\gamma >{10}^8$ mainly due to the radiative loss of synchrotron radiation, and the magnetic field strength in the emission zone can be constrained to be $\sim 4\mu$ G. The result shows that the detected $\gamma$-ray spectrum can be well produced via IC scattering of the high-energy electrons/positrons in the nebula which is in the tail region of the remnant.

超新星遗迹（SNR）G106.3 + 2.7在无线电中具有彗星形形态，头部和尾部拉长，脉冲星PSR J2229 + 6114位于头部的北边界。最近，$\gamma$已检测到能量范围从 GeV 到 500 TeV 在空间上与尾部区域重合的 - 射线。我们调查是否$\gamma$由 PSR J2229 + 6114 驱动的星云中的高能电子/正电子可以产生 - 射线。 $\gamma$- 射线通量可以很好地再现，假设一个分数 ($～0.12$) 的自旋下降光度用于为发射区中的轻子提供动力。粒子谱在洛伦兹因子处有中断$\gamma >{10}^8$ 主要是由于同步辐射的辐射损失，发射区的磁场强度可以约束为 $～4\mu$ G. 结果表明检测到 $\gamma$可以通过星云中高能电子/正电子的 IC 散射很好地产生 - 射线光谱，星云位于残余物的尾部区域。