Other
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6588d&link_type=abstract
HST Proposal ID #6588
Other
Hst Proposal Id #6588 Galaxies &Amp, Clusters
Scientific paper
Observations of the interstellar medium at the disk-halo interface of spiral galaxies provide us with very significant information on the physical state and structure of the interstellar medium {ISM} in a global sense. The nature of disk-halo interaction is particularly important for our understanding of the evolution of galaxies. We propose to study the morphology of diffuse ionized gas and its correlation with dust and other ISM components in the disk- halo interface of several edge-on galaxies. This gas is the extra-galactic analog of the Reynolds layer in the Milky Way. The morphology and vertical extent of this gas seems to vary from object to object and to change even within individual galaxies. Correlations with tracers of star formation strongly indicate that extraplanar gas is indeed correlated with star formation activity in the underlying disk, in agreement with galactic fountain and chimney models of the disk-halo interface. However, while ground-based data begin to resolve the largest filamentary structures and bubbles, the resolution is completely inadequate to characterize the structure of the ionized medium well enough to test specific predictions of these models. In view of the important role that transport of energy and matter from disk to halo and vice versa has in models of galactic evolution, it is crucial to accurately image the diffuse ionized gas layer in different galaxies to better test the theoretical predictions.
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