Evidence for hot gaseous coronae around the Magellanic Clouds

Journal Article · Thu May 15 04:00:00 EDT 1980 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/157960· OSTI ID:5020168

de Boer, K S; Savage, B D

High-dispersion EUE 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 i, 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, we argue that we have probably detected regions of hot halo gas 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. A cloud detected in the line of sight of HD 5980 in the SMC at V/sub LSR/=300 km s/sup -1/ is of unknown origin.

• Research Organization: Washburn Observatory, University of Wisconsin, Madison
• OSTI ID: 5020168
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 238:1; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640105* -- Astrophysics & Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ABSORPTION SPECTRA
CHARGED PARTICLES
COSMIC GASES
COSMIC RADIO SOURCES
FLUIDS
GALAXIES
GASES
H2 REGIONS
INTERSTELLAR SPACE
IONS
MAGELLANIC CLOUDS
MILKY WAY
RADIAL VELOCITY
SPACE
SPECTRA
ULTRAVIOLET SPECTRA
VELOCITY