  We performed deep optical observations of the area of the new supernova
remnant G 69.4+1.2 in the emission lines of [O III], Halpha+[N II] and [S II].
The low ionization images reveal diffuse and filamentary emission in the
central and south, south-west areas of our field. Estimates of the [S
II]/Halpha ratio suggest that the detected emission in these areas originates
from shock heated gas, while the strong extended source in the north must be an
HII region. The medium ionization image of [O III] shows a single filament
close to the field center. Emission from [O III] is not detected elsewhere in
the field but only in the north from LBN 069.96+01.35. Deep long-slit spectra
taken at the position of the [O III] filament suggest shock velocities ~120
km/s, while in other areas velocities around 50 km/s are expected. The sulfur
lines ratio indicates electron densities less than 120 cm^{-3}. The absolute
Halpha flux is ~5 x 10^{-17} erg s^{-1} cm^{-2} arcsec^{-2}. The optical
emission is very well correlated with the radio emission, especially in the
south west. The soft X-ray emission detected in the ROSAT All-Sky survey shows
a satisfactory degree of correlation with the optical data in the south-west
suggesting their association.
