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The extended supernova remnant G 116.5+1.1 was observed in the opticalemission lines of Halpha+[N II], [S II] and [O III]; deep long-slit spectrawere also obtained. The morphology of the remnant's observed emission is mainlydiffuse and patchy in contrast to the known filamentary emission seen along thewestern limb. The bulk of the detected emission in the region appears unrelatedto the remnant but there is one area of emission in the south-east which ischaracterized by a [S II]/Halpha ratio of ~0.5, implying a possible relation toG 116.5+1.1. If this is actually the case, it would imply a more extendedremnant than previously realized. Emission in the [O III] 5007 A line image isnot detected, excluding moderate or fast velocity shocks running into ionizedinterstellar clouds. Our current estimate of the distance to G 116.5+1.1 of ~3kpc is in agreement with earlier estimates and implies a very extended remnant(69 pc x 45 pc). Observations further to the north-east of G 116.5+1.1 revealeda network of filamentary structures prominent in Halpha+[N II] and [S II] butfailed to detect [O III] line emission. Long-slit spectra in a number ofpositions provide strong evidence that this newly detected emission arises fromshock heated gas. Typical Halpha fluxes lie in the range of 9 to 17 x10^{-17}erg/s/cm^2/ arcsec^2, while low electron densities are implied by theintensities of the sulfur lines. Weak emission from the medium ionization lineat 5007 A is detected in only one spectrum. Cool dust emission at 60 and 100microns may be correlated with the optical emission in a limited number ofpositions. Surpisingly, radio emission is not detected in published surveyssuggesting that the new candidate remnant may belong to the class of "radioquiet" supernova remnants.Comment: 10 pages, 5 figures, accepted for publication in A&

The faint supernova remnant G 116.5+1.1 and the detection of a new candidate remnant