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We observed 51 positions in the OH 1667 MHz main line transitions in thetranslucent, high latitude cloud MBM40. We detected OH emission in 8 out of 8positions in the molecular core of the cloud and 24 out of 43 in thesurrounding, lower extinction envelope and periphery of the cloud. Using alinear relationship between the integrated OH line intensity and E(B-V), weestimate the mass in the core, the envelope, and the periphery of the cloud tobe 4, 8, and 5 solar masses. As much as a third of the total cloud mass may befound in the in the periphery (E(B-V) $<$ 0.12 mag) and about a half in theenvelope (0.12 $\le$ E(B-V) $\le$ 0.17 mag). If these results are applicable toother translucent clouds the OH 1667 MHz line is an excellent tracer of gas invery low extinction regions and high-sensitivity mapping of the envelopes ofmolecular clouds may reveal the presence of significant quantities of molecularmass.

Hydroxyl as a Tracer of H2 in the Envelope of MBM40