  We present a study of the compact blister HII region BFS 10 and its highly
filamentary molecular cloud. We utilize 12CO observations from the Five College
Radio Astronomy Observatory to determine the distance, size, mass, and velocity
structure of the molecular cloud. Infrared observations obtained from the UKIRT
Infrared Deep Sky Survey and the Spitzer Infrared Array Camera, as well as
radio continuum observations from the Canadian Galactic Plane Survey, are used
to extract information about the central HII region. This includes properties
such as the ionizing photon rate and infrared luminosity, as well as
identifying a rich embedded star cluster associated with the central O9 V star.
Time-scales regarding the expansion rate of the HII region and lifetime of the
ionizing star reveal a high likelihood that BFS 10 will develop into a bipolar
HII region. Although the region is expected to become bipolar, we conclude from
the clouds velocity structure that there is no evidence to support the idea
that star formation at the location of BFS 10 was triggered by two colliding
clouds. A search for embedded young stellar objects (YSOs) within the molecular
cloud was performed. Two distinct regions of YSOs were identified; one region
associated with the rich embedded cluster and another sparse group associated
with an intermediate mass YSO.
