Deep H \alpha images of a faint emission complex 4.0 \arcdeg \times 5.5 \arcdeg in angular extent and located far off the Galactic plane at l = 70.0 \arcdeg , b = -21.5 \arcdeg reveal numerous thin filaments suggestive of a supernova remnant ’ s shock emission .
Low dispersion optical spectra covering the wavelength range 4500 - 7500 Å show only Balmer line emissions for one filament while three others show a Balmer dominated spectrum along with weak [ N i ] 5198 , 5200 Å , [ O i ] 6300 , 6364 Å , [ N ii ] 6583 Å , [ S ii ] 6716 , 6731 Å and in one case [ O iii ] 5007 Å line emission .
Many of the brighter H \alpha filaments are visible in near UV GALEX images presumably due to C iii ] 1909 Å line emission . ROSAT All Sky Survey images of this region show a faint crescent shaped X-ray emission nebula coincident with the portion of the H \alpha nebulosity closest to the Galactic plane .
The presence of long , thin Balmer dominated emission filaments with associated UV emission and coincident X-ray emission suggests this nebula is a high latitude Galactic supernova remnant despite a lack of known associated nonthermal radio emission .
Relative line intensities of the optical lines in some filaments differ from commonly observed [ S ii ] /H \alpha \geq 0.4 radiative shocked filaments and typical Balmer filaments in supernova remnants .
We discuss possible causes for the unusual optical SNR spectra .