Ultraviolet interstellar absorption toward stars in the Small Magellanic Cloud. III - The structure and kinematics of the Small Magellanic Cloud

Details Ultraviolet interstellar absorption toward stars in the Small Magellanic Cloud. III - The structure and kinematics of the Small Magellanic Cloud Ultraviolet interstellar absorption toward stars in the Small Magellanic Cloud. III - The structure and kinematics of the Small Magellanic Cloud

Sep 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apjs...59...77f&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 59, Sept. 1985, p. 77-93.

Astronomy and Astrophysics

Astrophysics

55

Interstellar Matter, Magellanic Clouds, Nebulae, Ultraviolet Spectra, Absorption Spectra, H I Regions, H Ii Regions, Interstellar Gas, Iue, Line Spectra, Radial Velocity

Scientific paper

The structural and kinematic properties of the Small Magellanic Cloud (SMC) were studied by combining IUE satellite observations of individual bright stars (Sk 159 and HD 5980) with existing optical and radio data. It is shown that the SMC has a complex structure due to gravitational interaction with the Milky Way and the Large Magellanic Cloud (LMC). Stars observed in the southwest regions of the SMC were associated with the 134 km/s H I complex. H II regions in the SMC were distributed according to a rotational velocity of 167 km/s. All IUE high-dispersion targets exhibit ultraviolet absorption near 100 km/s and 200 km/s. It is shown that the absorption arises in the widespread H I complexes at velocities similar to the H II regions. Some possible explanations for the origin of H II and H I regions in the SMC are discussed. The locations of the nine high-dispersion IUE targets in the SMC are given.

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