We present a study of a new molecular shell , G 126.1–0.8–14 , using available multiwavelegth Galactic plane surveys and optical Gemini observations .
A well defined shell-like structure is observed in the CO ( 1–0 ) line emission at ( l , b ) = ( 126 \aas@@fstack { \circ } 1 , –0 \aas@@fstack { \circ } 8 ) , in the velocity range –10.5 to –15.5 km s ^ { -1 } .
The H i emission shows a region of low emissivity inside G 126.1–0.8–14 , while radio continuum observations reveal faint non-thermal emission possibly related to this shell .
Optical spectra obtained with Gemini South show the existence of B-type stars likely to be associated with G 126.1–0.8–14 .
An estimate of the stellar wind energy injected by these stars show that they alone can not be able to create such a structure .
On the other hand , one supernova explosion would provide enough energy to generate the shell .
Using the MSX , IRAS , and WISE Point Source Catalogues we have found about 30 young stellar objects candidates , whose birth could have been triggered by the expansion of G 126.1–0.8–14 .
In this context , Sh2-187 could be a consequence of the action on its surroundings of the most massive ( and thus most evolve ) of the stars formed by the expanding molecular shell .