We investigate the distribution of the interstellar matter in the environs of the H ii  region Sh2-205 , based on neutral hydrogen 21–cm line data and radio continuum images at 408 and 1420 MHz obtained from the CGPS , ^ { 12 } CO ( J=1 \rightarrow 0 ) observations , high resolution IRAS data ( HIRES ) , and MSX data . 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 three regions are detected both at 408 and 1420 MHz .
The derived spectral indices show the thermal nature of SH 148.83–0.67 and LBN 148.11–0.45 . LBN 148.11–0.45 is a classical H ii  region surrounded by an H i  shell .
The associated neutral atomic and ionized masses are 65 M _ { \odot } Â and 70 M _ { \odot } , respectively .
Dust and molecular gas ( \approx 6 \times 10 ^ { 4 } M _ { \odot } ) are found related to this ionized region .
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 M _ { \odot } Â and 300 M _ { \odot } , respectively .
The emission of SH 149.25–0.0 is too faint to derive the dust and gas parameters . An H i  shell centered at ( l , b ) = ( 149°0′ , –1°30′ ) was also identified .
It correlates morphologically with molecular gas emission .
The neutral atomic and molecular masses are 1600 M _ { \odot } Â and 2.6 \times 10 ^ { 4 } M _ { \odot } , respectively .
The open cluster NGC 1444 is the most probable responsible for shaping this H i  structure .