  We present the first calibrated CCD images of the faint supernova remnant G
114.3+0.3 in the emission lines of [OII], [OIII], Halpha+[NII] and [SII]. The
deep low ionization CCD images reveal diffuse emission in the south and central
areas of the remnant. These are correlated with areas of intense radio
emission, while estimates of the [SII]/Halpha ratio suggest that the detected
emission originates from shock heated gas. In the medium ionization image of
[OIII] we discovered a thin filament in the south matching very well the outer
radio contours. This filament is not continuous over its total extent but shows
variations in the intensity, mainly in the south-west suggesting inhomogeneous
interstellar clouds. Deep long-slit spectra were also taken along the [OIII]
filament clearly identifying the observed emission as emission from shock
heated gas. The Halpha emission is a few times 10^(-17) erg s^(-1) cm^(-2)
arcsec^(-2), while the variations seen in the [OIII] flux suggest shock
velocities into the interstellar clouds around or below 100 km/s. The sulfur
line ratio approaches the low density limit implying electron densities less
than ~500 cm^(-3).
