2009A&A...499..789B

Deep optical CCD images of the supernova remnant G 32.8-0.1 were obtained where filamentary and diffuse emission was discovered. The images were acquired in the emission lines of Hα+[NII] and [SII]. Filamentary and diffuse structures are detected in most areas of the remnant, while no significant [OIII] emission is present. The flux-calibrated images suggest that the optical emission originates from shock-heated gas since the [SII]/Hα ratio is greater than 1.2. The Spitzer images at 8µm and 24µm show a few filamentary structures to be correlated with the optical filaments, while the radio emission at 1.4 GHz in the same area is found to be very well correlated with the brightest optical filaments. The results from deep long-slit spectra also support the origin of the emission being from shock-heated gas ([SII]/Hα>1.5). The absence of [OIII] emission indicates slow shock velocities into the interstellar ``clouds''