We present NOT optical observations of a clump ( l = 127 \aas@@fstack { \circ } 9435 , b = + 1 \aas@@fstack { \circ } 8298 ) , embedded in an extended , irregularly shaped , diffuse optical nebula . This condensation shows an emission-line spectrum typical of classic H ii regions . Although its location on the sky coincides with a nearby extended photoionized region recently identified by ( ) in radio data from the Canadian Galactic Plane Survey ( CGPS ) , the systemic velocity of this \approx 1′-sized H ii region , V _ { LSR } = - 71 \pm 12 km s ^ { -1 } , poses it far out in the Galaxy , beyond the Perseus arm . The location of this region in the Galaxy is supported by H i structures visible at comparable radial velocity on CGPS data . We argue that this H ii region might belong to an outer Galactic arm . The emission line ratios of the surrounding extended nebula , whose radial velocity is consistent with that of the small H ii region , are typical of photoionized gas in the low density limit . Smaller clumps of comparable surface brightness are visible within the optical boundaries of the extended , faint nebula . After comparison of the optical data with far infrared and radio observations , we conclude that this nebula is an H ii region , \sim 70 pc in size , probably photoionized by an association of OB stars and surrounded by a ring of neutral hydrogen .