The spectacular ionized interstellar medium of NGC 55

Details The spectacular ionized interstellar medium of NGC 55 The spectacular ionized interstellar medium of NGC 55

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aipc..393..469f&link_type=abstract

The seventh astrophysical conference: Star formation, near and far. AIP Conference Proceedings, Volume 393, pp. 469-472 (1997).

Astronomy and Astrophysics

Astrophysics

Hii Regions, Emission And Reflection Nebulae, Origin, Formation, Evolution, Age, And Star Formation, Atomic, Molecular, Chemical, And Grain Processes, Star Formation

Scientific paper

We present deep Hα+[NII], [SII] (λλ 6716,6731 Å) and [OII] (λλ 3726,3729 Å) images of the highly inclined, actively star-forming SBm galaxy NGC 55, located in the nearby Sculptor Group. Due to its proximity, NGC 55 provides a unique opportunity to study the disk-halo interface in a late-type galaxy with unprecedented spatial resolution. Our images reveal a spectacular variety of ionized gas features, ranging from giant HII region complexes, to supergiant filamentary and shell features, to patches of very faint diffuse emission. Many of these features protrude well above the plane of the galaxy, including a very faint fragmented shell of emission which is projected at 2.6 kpc above the disk. Emission-line ratios ([OII]/Hα+[NII],[SII]/Hα+[NII]) increase smoothly in value from the cores of HII regions, through the haloes of HII regions, into the diffuse ionized gas. Such a continuous trend is predicted by models in which the diffuse gas is photoionized by distant OB stars.

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