NGC5367 is a member of a class of unusual high Galactic latitude
 molecular clouds with distinctive comet-like appearances. The origin
 of this cometary cloud remains a mystery. Studies of star formation
 in cometary globules near the Gum Nebula indicate that some owe their
 shapes to ionization fronts from nearby OB stars. The Draco cloud has
 been described in terms of ablative mass shedding as the cloud
 passes through the ISM. A detailed study of G110-13 has found evidence
 suggesting that cloud-cloud collisions could also be an important,
 shape-determining mechanism for some cometary clouds.
   NGC 5367 is unique among these high-latitude cometary clouds in
 that it is exceptionally bright at far-IR wavelengths. It is
 relatively nearby (d = 300 pc), has a low mass ( 50 Msun) and size
 ( 2 pc). More significantly, it also contains two embedded B-stars
 for an estimated star forming efficiency of at least 25 percent.
 The coma of NGC 5367 is completely dominated by the scattered light
 from the two B-type stars at optical wavelengths. Two young stellar
 objects were identified in the leading edge of the cloud coincident
 with a dark bar of optical obscurration.
   ISO observations of this cloud will provide  major new insights into
the star formation history of this cloud, and a substantial test of
whether shocks of any kind have played a role in determining its shape.
ISO will be used to measure the OI lines at 63 and 145 microns, and the
CII line at 157 microns. The line fluxes are a sensitive measure of the
presence of photodissociation regions and will be used to descriminate
between low and high-energy shock histories for this cloud. Spectro-
photometry between 3 to 12 microns will identify PAH differences
between the coma and the tail regions which should also be present if
shock processing of dust grain material has occurred. We will also
image the new YSO cluster in the dark bar region to identify additional
YSOs and improve estimates of the cloud's star formation efficiency.