  We present the first results from an imaging and a spectroscopic survey of
the optical emission associated with supernova remnant (SNR) G107.5$-$1.5. We
discovered optical diffuse and filamentary emission from G107.5$-$1.5 using the
1.5-m and 1-m telescopes. The optical emission from the North East (NE) and
North West (NW) regions show the diffuse structure, while the South East (SE)
and East (E) regions show filamentary structure. From long-slit spectra, we
found [SII]/H$\alpha$ $>$ 0.5 for the SE and E regions, which supports the
origin of the emission being from shock-heated gas. The average [SII]/H$\alpha$
ratio is found to be $\sim$0.4 and $\sim$0.3 for the NW and NE regions,
respectively, indicating that the optical emission is coming from ionized gas
in an HII region. From the ratios of [SII]$\lambda\lambda$ 6716/6731, we
estimate an average electron density of $\sim$2400 cm$^{-3}$ for the NW region,
which can be attributed to the dense ionized gas. The average
[SII]$\lambda\lambda$ 6716/6731 ratios are $\sim$1.25 and $\sim$1.15 for the SE
and E regions, respectively, which are indicative of low electron density.
