2002A&A...385.1042B

Deep optical CCD images of the supernova remnant G 17.4-2.3 were obtained and faint emission has been discovered therein. The images, taken in the emission lines of Hα+[NII], [S II] and [OIII], reveal filamentary structures in the east, south-east area, while diffuse emission in the south and central regions of the remnant is also present. The radio emission in the same area is found to be well correlated with the brightest optical filament. The flux calibrated images suggest that the optical filamentary emission originates from shock-heated gas ([S II]/Hα>0.4), while the diffuse emission seems to originate from an HII region ([S II]/Hα<0.3). Furthermore, deep long-slit spectra were taken at the bright [OIII] filament and clearly show that the emission originates from shock heated gas. The [OIII] flux suggests shock velocities into the interstellar ``clouds'' greater than 100km/s, while the [SII]λ 6716/6731 ratio indicates electron densities ∼240cm^–3. Finally, the Hα emission has been measured to be between 7 to 20x10^–17erg/s/cm²/arcsec².