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2000ApJ...532..221S - Astrophys. J., 532, 221-237 (2000/March-3)
Molecular gas, dust, and star formation in the barred spiral NGC 5383.
SHETH K., REGAN M.W., VOGEL S.N. and TEUBEN P.J.
Abstract (from CDS):
These discrepancies remain for all our simulations which produce offset bar dust lanes and indicate that the model is missing an essential process or component. A small nuclear bar might account for the discrepancy, but we rule this out using a Hubble Space Telescope NICMOS (near-IR camera and multiobject spectrometer) image: this reveals a nuclear trailing spiral, not a bar; we show that coarser resolution (i.e., ground-based images) can produce artifacts that resemble bars or rings. We conclude that the discrepancies in morphology and contrast are due to the omission of star formation from the model; this is supported by the observed high rate of central star formation (7 M☉.yr–1), a rate that can consume most of the accumulating gas.
As is common in similar bars, the star formation rate in the bar between the bar ends and the central region is low (0.5 M☉.yr–1), despite the high gas column density in the bar dust lanes; this is generally attributed to shear and shocks. We note a tendency for the H II regions to be associated with the spurs feeding the main bar dust lanes, but these are located on the leading side of the bar. We propose that stars form in the spurs, which provide a high column density but low shear environment. H II regions can therefore be found even on the leading side of the bar because the ionizing stars pass ballistically through the dust lane.
Abstract Copyright: ∼
Journal keyword(s): galaxies: individual (NGC 5383) - Galaxies: ISM - Galaxies: Kinematics and Dynamics - Galaxies: Starburst - Galaxies: Structure - Methods: Numerical
Nomenclature: Fig.1: [SRV2000] H-R (Nos H-I to H-III), [SRV2000] HP N=1. Fig.3: [SRV2000] C-R (Nos C-I to C-IV).
Simbad objects: 23
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