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Astron. Astrophys. 358, 812-818 (2000)
Vertical motions in the disk of NGC 5668 as seen with optical Fabry-Perot spectroscopy *
J. Jiménez-Vicente 1,2 and
E. Battaner 2
1 Kapteyn Institute, Postbus 800, 9700 AV Groningen, The Netherlands
2 Universidad de Granada, Departamento de Física Teórica y del Cosmos, 18071 Granada, Spain
Received 21 October 1999 / Accepted 13 April 2000
Abstract
We have observed the nearly face-on spiral galaxy NGC 5668 with the
TAURUS II Fabry-Perot interferometer at the William Herschel Telescope
using the ![[FORMULA]](img1.gif)
line to study the
kinematics of the ionized gas. From the extracted data cube we
construct intensity, velocity and velocity dispersion maps. We
calculate the rotation curve in the innermost 2 arcmin and we use the
residual velocity field to look for regions with important vertical
motions. By comparing the geometry of these regions in the residual
velocity field with the geometry in the intensity and velocity
dispersion maps we are able to select some regions which are very
likely to be shells or chimneys in the disk. The geometry and size of
these regions are very similar to the shells or chimneys detected in
other galaxies by different means. Moreover, it is worth noting than
this galaxy has been reported to have a population of neutral hydrogen
high velocity clouds (Schulman et al. 1996) which, according to these
observations, could have been originated by chimneys similar to those
reported in this paper.
Key words: ISM: kinematics and
dynamics 
galaxies: individual:
NGC 5668
galaxies: ISM
galaxies: kinematics and
dynamics
galaxies: spiral
* Based on observations made with the William Herschel Telescope operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias
Send offprint requests to: J. Jiménez-Vicente
Correspondence to: jjimenez@astro.rug.nl
Contents
- 1. Introduction
- 2. NGC 5668: general properties
- 3. Observations and data reduction
- 4. The velocity field and the rotation curve
- 5. The residual velocity field and the shell/chimney candidates (HRVR's)
- 6. Some shell/chimney properties
- 7. Conclusions
- References
© European Southern Observatory (ESO) 2000
Online publication: June 20, 2000
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