The distribution of the diffuse ionized interstellar medium perpendicular to the disk of the edge-on galaxy NGC 891

Details The distribution of the diffuse ionized interstellar medium perpendicular to the disk of the edge-on galaxy NGC 891 The distribution of the diffuse ionized interstellar medium perpendicular to the disk of the edge-on galaxy NGC 891

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...232l..15d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 232, no. 2, June 1990, p. L15-L18. Research supported by Lowell Observatory.

Astronomy and Astrophysics

Astrophysics

138

Diffuse Radiation, Galactic Structure, Interstellar Gas, Ionized Gases, Absorption Spectra, Emission Spectra, H Alpha Line

Scientific paper

This paper reports the detection of an H-alpha-emitting component of the diffuse ionized interstellar medium with a scale height of up to 1 kpc in the edge-on galaxy NGC 891. The presented data show individual structures out to about 4.5 kpc above the plane. The distribution is very inhomogeneous; three different regions are characterized by the observed scale height and the presence of a filamentary structure. The emitting gas is analogous to the diffuse low-density, 2-3 kpc thick layer of warm ionized gas observed in the Galaxy. In NGC 891, the properties of this gas phase, such as scale height and surface density, are directly related to star-forming processes in the underlying disk. Individual structures are compared with predictions by models of the inerstellar medium driven by multiple supernova events. The estimated total mass of this diffuse component of the ionized gas is 4 x 10 to the 8th solar masses.

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