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