The vertical extent and kinematics of the HI in NGC 2403

Details The vertical extent and kinematics of the HI in NGC 2403 The vertical extent and kinematics of the HI in NGC 2403

2000-03-13

arxiv.org/abs/astro-ph/0003165v1

Astronomy and Astrophysics, 2000, 356, L49-L52

Astronomy and Astrophysics

Astrophysics

4 pages, 2 figures, accepted for publication in Astronomy and Astrophysics Letters

Scientific paper

The neutral hydrogen line profiles along the major axis of the nearby spiral galaxy NGC 2403 show a wing towards the sytemic velocity. This asymmetry can be explained with the presence of an abnormally thick HI disk (FWHM ~ 5 kpc) or with a two-component structure: a thin disk and a slowly rotating, thicker (1-3 kpc) HI layer. The latter model gives a better representation of the observations. These results throw a new light on the disk-halo connection. In particular, the decrease of rotational velocity with height above the plane may be the result of a galactic fountain flow. A vertically extended, slowly rotating HI layer may be common among spiral galaxies with high levels of star formation.

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