The H2 1-0 S(1) emission line in the vicinity of the OH maser source W75N(OH) was observed to determine whether H2 line emission in certain star-forming regions might be linked to OH masers. The region was selected because the OH maser source has been well observed and because of its similarity to Orion. Like Orion, it contains IR sources, H20 masers, H II regions and OH maser spots. The spectrum of the H2 line is plotted and it is noted that the line is unresolved by the Fabry-Perot (FWHM = 120 km/s) and has a flux of (4.3 plus or minus 0.8) x 10 to the -20th W per square centimeter in an 18-arcsec beam. OH masers may prove to be important indicators of the presence of the type of activity associated with H2 line sources.