The vertical extent and kinematics of the HI in NGC 2403

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dc.creatorSchaap, W. E.
dc.creatorSancisi, R.
dc.creatorSwaters, R. A.
dc.date2000-03-13
dc.date.accessioned2026-07-07T01:52:42Z
dc.date.available2026-07-07T01:52:42Z
dc.descriptionThe 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.
dc.description4 pages, 2 figures, accepted for publication in Astronomy and Astrophysics Letters
dc.identifierhttps://arxiv.org/abs/astro-ph/0003165
dc.identifierhttp://arxiv.org/abs/astro-ph/0003165
dc.identifierAstronomy and Astrophysics, 2000, 356, L49-L52
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/710
dc.subjectAstrophysics
dc.titleThe vertical extent and kinematics of the HI in NGC 2403
dc.typetext

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