Abstract
IC 1470 (S156) is a compact H II region associated with an extensive molecular cloud in the Perseus arm. The central star of IC 1470 was observed by Chopinet et al. (1973) who suggest that the exciting star is of spectral type O7. The present investigation is concerned with additional optical data with high spatial resolution and accurate emission line velocities across the nebula. A quantitative comparison is conducted of representative emission line strengths of IC 1470 and M8. It is concluded that IC 1470 has a nebular spectrum similar to M8 and appears to be an H II region excited by a single O7 star. It represents an object formed close to the edge of a molecular cloud, and its ionizing radiation is penetrating the intercloud gas, producing a 'blister' on its edge.
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