Astronomy and Astrophysics – Astronomy
Scientific paper
May 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...499l..87w&link_type=abstract
Astrophysical Journal Letters v.499, p.L87
Astronomy and Astrophysics
Astronomy
19
Ism: Structure, Galaxies: Halos, Galaxies: Ism, Galaxies: Magellanic Clouds, Ultraviolet: Ism
Scientific paper
Based on the detection of C IV absorption in five Large Magellanic Cloud (LMC) stars observed with the Goddard High-Resolution Spectrograph on the Hubble Space Telescope, we present the first unambiguous evidence that C ^{+3} exists in the LMC away from regions where it could have been locally produced. We can exclude that this C ^{+3} is associated with hot early-type stars or active regions. Significant differences between the H alpha and C ^{+3} velocities toward our probes indicate that H ^{+} and C ^{+3} are not cospatial. Large column density variations show that the distribution of C ^{+3} is not uniform. The properties of the LMC C IV lines are similar but not identical to those found for the Milky Way: 45 km s ^{-1} versus 73 km s ^{-1} for the average FWHM, (8-12) x 1013 cm ^{-2} versus (9-16) x 1013 cm ^{-2} for the average column density. The H alpha versus C IV velocity differences and the similarity of the properties of the LMC and Milky Way C IV absorption suggest that at least some of the C ^{+3} in the LMC is in a hot corona and that it has been produced by processes similar to those in the Milky Way. Our results show the feasibility of detecting high-ionization absorption in faint LMC stars, but more observations will be necessary before we can understand the distribution and properties of 105 K gas in the LMC.
Bomans Dominik
Chu Y.-H. Y.-H.
Howk Chris J.
Points Sean D.
Wakker Bart
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