  We present a study of the HII region Sh2-205 and its environs, based on data
obtained from the CGPS, 12CO observations, and MSX data. We find that Sh2-205
can be separated in three independent optical structures: SH 149.25-0.0, SH
148.83-0.67, and LBN 148.11-0.45. The derived spectral indices show the thermal
nature of SH 148.83-0.67 and LBN 148.11-0.45. The morphology of SH 148.83-0.67,
both in the optical and radio data, along with the energetic requ irements
indicate that this feature is an interstellar bubble powered by the UV photons
of HD 24431 (O9 III). LBN 148.11-0.45 has the morphology of a classic al HII
region and their ionizing sources remain uncertain. Dust and molecular gas are
found related to LBN 148.11-0.45.Particularly, a photodissociation region is
detected at the interface between the ionized and molecular regions. If the
proposed exciting star HD 24094 were an O8--O9 type star, as suggested by its
near-infrared colors, its UV photon flux would be enough to explain the
ionization of the nebula. The optical, radio continuum, and 21-cm line data
allow us to conclude that SH 148.83-0.67 is an interstellar bubble powered by
the energetic action of HD 24431. The associated neutral atomic and ionized
masses are 180 Mo and 300 Mo, respectively. The emission of SH 149.25-0.0 is
too faint to derive the dust and gas parameters. An HI shell centered at (l,b)
= (149.0, 1.5) was also identified. It correlates morphologically with
molecular gas emission. The neutral atomic and molecular masses are 1600 Mo and
2.6 x 10^4 Mo, respectively. The open cluster NGC 1444 is the most probable
responsible for shaping this HI structure.
