Abstract
The Large Magellanic Cloud (LMC) is one of the only two galaxies in which the 104 - 106 K ionized interstellar gas and its underlying massive stellar population can be studied with a sub-parsec resolution over the entire galaxy. Our ability to study the hot ionized gas in the LMC has been enhanced by the availability of the space-based ROSAT, ASCA, EST, and IUE observatories. Existing UV interstellar absorption line studies of the LMC confirm the existence of 105 K gas in large superbubbles and supergiant shells, but cannot conclude on the existence of a continuous hot gaseous halo of the LMC. Recent ROSAT X-ray observations of the LMC show 10 6 K gas in large shell structures as well as in regions not associated with any interstellar structures. The relationship among the 10 4, 105, and 106 K components is discussed for interstellar structures at various scale sizes.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 153-160 |
| Number of pages | 8 |
| Journal | Revista Mexicana de Astronomia y Astrofisica: Serie de Conferencias |
| Volume | 3 |
| State | Published - 1995 |
| Event | 5th Mexico-Texas Conference on Astrophysics: Gaseous Nebulae and Star Formation - Tequesquitengo, Mor, Mexico Duration: Apr 3 1995 → Apr 5 1995 |
Keywords
- H II regions
- ISM: bubbles
- ISM: supernova remnants X-rays: interstellar
- Magellanic clouds
ASJC Scopus subject areas
- Space and Planetary Science
- Astronomy and Astrophysics