Evidence for hot gaseous coronae around the Magellanic Clouds

Details Evidence for hot gaseous coronae around the Magellanic Clouds Evidence for hot gaseous coronae around the Magellanic Clouds

May 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...238...86d&link_type=abstract

Astrophysical Journal, Part 1, vol. 238, May 15, 1980, p. 86-92.

Astronomy and Astrophysics

Astronomy

84

Coronas, High Temperature Gases, Intergalactic Media, Magellanic Clouds, Astronomical Spectroscopy, H I Regions, Iue, Line Spectra, Ultraviolet Astronomy

Scientific paper

High-dispersion IUE far-UV spectra were obtained for five stars in the LMC and two stars in the SMC. At Magellanic Cloud velocities, all the spectra exhibit very strong interstellar lines of Al III, Si IV, and C IV, in addition to the usual lower ionization stage lines associated with H I region absorption. In two stars interstellar N V is also detected at the 50 mA level. From a consideration of the strength, width, and radial velocity of these high ionization stage lines, it is argued that regions of hot halo gas have probably been detected in front of the Magellanic Clouds. The regions detected exhibit absorption characteristics very similar to that of the Milky Way corona described previously by Savage and de Boer (1979). A cloud detected in the line of sight to HD 5980 in the SMC at a radial velocity of 300 km/s is of unknown origin.

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