Coronal C+3 in the large magellanic cloud: Evidence for a hot halo

Bart Wakker, J. Chris Howk, You Hua Chu, Dominik Bomans, Sean D. Points

Research output: Contribution to journalArticlepeer-review

Abstract

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 Hα 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) × 1013 cm-2 versus (9-16) × 1013 cm-2 for the average column density. The Ha 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.

Original languageEnglish (US)
Pages (from-to)L87-L91
JournalAstrophysical Journal
Volume499
Issue number1 PART II
DOIs
StatePublished - 1998

Keywords

  • Galaxies: ISM
  • Galaxies: halos
  • ISM: structure
  • Magellanic Clouds
  • Ultraviolet: ISM

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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