  We report the first detection of optical emission from the shell-type
Galactic supernova remnant (SNR) G108.2$-$0.6. We obtained H$\alpha$ images and
long-slit spectra using the 1.5-m RTT150 telescope to examine the morphological
and spectral characteristics of the SNR. We detected several filaments along
its north and south regions, which is consistent with its SNR nature. The
spectra exhibit [SII]/H$\alpha$ ratios in the range of 0.4$-$1.1, indicating
emission from shock-heated gas. The oxygen doublet emission lines
[OI]$\lambda$6300, $\lambda$6363 detected in the south region also support the
indicator of the presence of shocks. We estimate the electron density using the
[SII] 6716/6731 ratio ranging from 15 to 1800 cm$^{-3}$. The spectra show a
relatively low shock velocity of $V_{\rm s}$ $\sim$ 80 km s$^{-1}$ with the
pre-shock cloud density of $n_{\rm c}$ $\sim$18$-$57 cm$^{-3}$. The
H$\alpha$/H$\beta$ ratios show significant variation across the observed
regions with extinction $E(B-V)$ ranging from 0.22 to 1.65. We also analyzed
the 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.
