SIMBAD references

We investigate the distribution of the interstellar matter in the environs of the HII region Sh2-205, based on neutral hydrogen 21-cm-line data and radio continuum images at 408 and 1420 MHz obtained from the CGPS, ¹²CO (J=1 ⟶0) observations, high-resolution IRAS data (HIRES), and MSX data.

Sh2-205 can be separated into three distinct optical structures: SH149.25-0.0, SH148.83-0.67, and LBN148.11-0.45. The three regions are detected at both 408 and 1420 MHz. The derived spectral indices show the thermal nature of SH148.83-0.67 and LBN148.11-0.45.

LBN148.11-0.45 is a classical HII region surrounded by an HI shell. The associated neutral atomic and ionized masses are 65M_☉ and 70M_☉, respectively. Dust and molecular gas (∼6x10⁴M_☉) related to this ionized region have been found. In particular, a photodissociation region is detected at the interface between the ionized and molecular regions. If the proposed exciting star HD24094 were an O8-O9 type star, as suggested by its near-infrared colours, its UV photon flux would be strong enough to explain the ionization of the nebula.

The optical, radio continuum, and 21-cm-line data allow us to conclude that SH148.83-0.67 is an interstellar bubble powered by the energetic action of HD24431. The associated neutral atomic and ionized masses are 180M_☉ and 300M_☉, respectively. The emission of SH149.25-0.0 is too faint to derive the dust and gas parameters.

An HI shell centred at (l, b) = (149°0', -1°30') was also identified. It correlates morphologically with the molecular gas emission. The neutral atomic and molecular masses of the shell are 1600M_☉ and 2.6x10⁴M_☉, respectively. The open cluster NGC1444 is probably responsible for shaping this HI structure.