G 65.3+5.7
The first CCD mosaics of this supernova remnant  in the optical emission lines of [OII] and [OIII] were obtained from
Skinakas Observatory. The new images reveal several diffuse and filamentary structures both inside and outside the extent of the remnant. The medium ionization line of [OIII] 5007 A provides the sharpest view to the system, while the remnant appears less filamentary in the emission line of [OII]3727 A. There are significant morphological differences between the two images strongly suggesting the presence of incomplete shock structures. Long and short scale variations are observed in several areas of the remnant, the shortest ones with a length of ~0.6 light-yera. Deep long--slit spectra were taken at several different positions to study the physical conditions in more detail. All spectra show that the emission originates from shock heated gas, while the majority of them is characterized by large [OIII]/Hbeta ratios. The absolute Ha flux ranges from 0.5--22 x 10^-17 erg/s/cm^2/arcsec^2, while the sulfur line ratios indicate electron densities below ~200 cm^-3. Estimates of the shock velocities and the column densities lie in the range of 90-140 km/s. Finally, the observed variations of the Ha/Hbeta ratios may reflect the presence of intrinsic absorption affecting the optical spectra.
It is believed that this remnants lies at a distance of ~3000 light-years and has an ange of ~26000 years.

[OIII] image of G65.3+5.7

[OII] image of G65.3+5.7