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Narrow passband optical images of the large Galactic supernova remnantG179.0+2.6 reveal a faint but nearly complete emission shell dominated bystrong [O III] 4959,5007 A line emission. The remnant's optical emission, whichconsists of both diffuse and filamentary features, is brightest along itssouthern and northeastern limbs. Deep H-alpha images detect little coincidenceemission indicating an unusually high [O III]/H-alpha emission ratio for such alarge and apparently old remnant. Low-dispersion optical spectra of severalregions confirm large [O III]/H-alpha line ratios with typical values around10. The dominance of [O III] emission for the majority of the remnant's opticalfilaments suggests shock velocities above 100 km/s are present throughout mostof the remnant, likely reflecting a relatively low density ambient ISM. Theremnant's unusually strong [O III] emission adds to the remnant's interestingset of properties which include a thick radio emission shell, radialpolarization of its radio emission like that typically seen in young supernovaremnants, and an unusually slow-rotating gamma-ray pulsar with a characteristicspin-down age ~50 kyr.

Optical Emission Associated with the Galactic Supernova Remnant G179.0+2.6