Optical CCD imaging and spectroscopic observations of three supernova remna
nts have been performed for the first time. Filamentary and diffuse emissio
n is discovered from the supernova remnant G 67.7+1.8 located similar to 82
' to the south of CTB 80's pulsar. The Ha: and sulfur emission are almost
equally strong at a level of similar to 20 10(-17) erg s(-1) cm(-2) arcsec(
-2) suggesting shock-heated emission. Electron densities less than 240 cm(-
3) arcsec are estimated, while the weak [OIII] emission suggests shock velo
cities in the range of 60-80 kms(-1). Emission can also be seen in the ROSA
T All Sky Survey data which indicate an extended hard X-ray source. Emissio
n from G 31.5-0.6 is detected only in the H alpha + [NII] image at a typica
l flux level of 35 10(-17) erg s(-1) cm(-2) arcsec(-2). The morphology of t
he observed radiation is diffuse and partially correlated with the non-ther
mal radio emission. Deep long-slit spectra detect sulfur line emission whic
h is not strong enough to identify it as emission from shocked gas. Finally
, optical emission from G 49.2-0.7 is obscured by several dark nebulae whic
h probably give rise to significant X-ray attenuation. The H alpha + [NII]
flux is typically similar to 40 10(-17) erg s(-1) cm(-2) arcsec(-2) while t
he [SII] flux is very weak, not allowing its identification as shock-heated
. However, a small area of similar to3 ' XII emits strong sulfur flux relat
ive to H alpha ([SII]/H alpha similar to 0.6) This area is located in the s
outh-east of G 49.2-0.7, close to the outer boundaries of the X-ray and rad
io emission. However, deep optical spectra would be required to firmly esta
blish the nature of this emission and its association to G 49.2-0.7.