Optical observations of the supernova remnant G 69 . 4 + 1 . 2

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], Hα + [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]/Hα 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 H ii 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. The absolute Hα flux is ∼5 × 10 erg s cm arcsec. 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.