Neutral hydrogen (H I) is a magnificent tool when studying the structure of the interstellar medium (ISM) as it is relatively easily observable and can be mapped at good spatial and velocity resolution with modern instruments. Moreover, it traces the cool (~ 100 K) and warm (~ 5000 K) neutral gas which together make up about 60%, or the bulk, of the ISM. The currently accepted picture is that stellar winds and subsequent supernovae are the origin for the clearly defined holes or bubbles within the more or less smooth neutral medium. The H I can therefore serve indirectly as a tracer of the hot interstellar medium (HIM)left behind after the most massive stars within an OB association have gone off as supernovae. A splendid example is the dwarf galaxy IC 2574 for which we discuss H I, optical and X-ray observations.
|Title of host publication||Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies|
|Editors||K A van der Hucht, G Koenigsberger, P R J Eenens|
|Publisher||The International Astronomical Union|
|Publication status||Published - 1999|
|Name||Procs IAU Symposium|