HII Supergiant Shell in the Large Magellanic Cloud

Details HII Supergiant Shell in the Large Magellanic Cloud HII Supergiant Shell in the Large Magellanic Cloud

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006rmxac..26..162o&link_type=abstract

XI IAU Regional Latin American Meeting of Astronomy (Eds. L. Infante & M. Rubio) Revista Mexicana de Astronomía y Astrofísica (S

Astronomy and Astrophysics

Astronomy

Scientific paper

We present kinematical results obtained by using Fabry-Perot Interferometry about The SuperGiant Shell LMC9 in the LMC. That shell, composed by N204, N206, N200, N198, N205 molecular complexes, was analysed with the aim of establishing its characteristics and to test whether it belongs to a major kinematical structure. The obtained radial velocity field presents a main component with a well defined profile, and a minor component, which could reveal the presence of a high velocity stream. It could also be indicative of a layer of gas at a greater distance. In some regions the perturbation of the ISM is due to stellar winds arising from stars which lie inside the nebulosities; in other regions the observed profile could correspond either to supernovae explosions or to very strong stellar winds coming from WR stars. In most of the complexes the bubbles rim seems well defined, with regular gaussian profiles, and could be represented by a single systemic radial velocity. In general the widths of the gaussians are quite variable for the distinct complexes, probably revealing different conditions in the medium in which the ionised gas is embedded. In particular we find small molecular clouds in the CO lines in agreement with the position of the complexes. We also observed a remarkable coincidence between the position of CO concentrations and the HII regions with narrower profiles. So it seems that dense molecular clouds would block the expansion of ionised hydrogen.

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