Triggered star formation in a molecular shell created by a SNR?

CICHOWOLSKI SILVINA; PINEAULT SERGE; GAMEN ROBERTO; ARNAL E. MARCELO; SUAD LAURA A.; ORTEGA MARTIN E.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

WILEY-BLACKWELL PUBLISHING, INC

Lugar: Londres; Año: 2014 vol. 438 p. 1089 - 1101

0035-8711

We present a study of a new molecular shell, G 126.1-0.8-14, using  available multiwavelength 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. 1, -0. 8), in the velocity range -10.5 to -15.5 km/s. The HI 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 shows that they alone cannot 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  object 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.