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We report the first detection of optical emission from the shell-typeGalactic supernova remnant (SNR) G108.2$-$0.6. We obtained H$\alpha$ images andlong-slit spectra using the 1.5-m RTT150 telescope to examine the morphologicaland spectral characteristics of the SNR. We detected several filaments alongits north and south regions, which is consistent with its SNR nature. Thespectra exhibit [SII]/H$\alpha$ ratios in the range of 0.4$-$1.1, indicatingemission from shock-heated gas. The oxygen doublet emission lines[OI]$\lambda$6300, $\lambda$6363 detected in the south region also support theindicator of the presence of shocks. We estimate the electron density using the[SII] 6716/6731 ratio ranging from 15 to 1800 cm$^{-3}$. The spectra show arelatively low shock velocity of $V_{\rm s}$ $\sim$ 80 km s$^{-1}$ with thepre-shock cloud density of $n_{\rm c}$ $\sim$18$-$57 cm$^{-3}$. TheH$\alpha$/H$\beta$ ratios show significant variation across the observedregions with extinction $E(B-V)$ ranging from 0.22 to 1.65. We also analyzedthe archival HI data and estimated the kinematic distance to the SNR of$\sim$0.8 kpc and dynamical age as $\sim$70$\pm$10 kyr of G108.2$-$0.6.

Discovery of optical emission from the supernova remnant G108.2-0.6 and its atomic environment