  Dwarf galaxies provide a special environment due to their low mass, small
size and generally low metal content. These attributes make them perfect
laboratories for the interaction of massive stars with the interstellar medium
on small and especially large spatial scales. The natural result of the
spatially concentrated energy output from stellar winds and supernovae of an OB
association is an expanding bubble. These bubbles can grow to kpc-size and
become the dominant driver of the chemical and dynamical evolution of dwarf
galaxies. In such low mass systems, bubbles have an enhanced probability of
breaking out of the gaseous disk into the halo of the host galaxy. This may
lead to venting metal enriched hot gas to large distances from the sites of
creation. In this work I review the current observational material on hot gas
inside bubbles, blow-outs, and hot halos of dwarf galaxies and discuss several
conclusions which can be drawn from the observations. I will also present an
analysis of the dwarf galaxy NGC 1705 as a case study, highlighting
observational methods and problems with the current data. Finally I will
comment on some areas where large progress should be possible in the near
future.
