N. S. P. Sabalisck , M. Rozas, J. E. Beckman , J. H. Knapen, PASA, 15 (1), 161
The html and gzipped postscript versions of this paper are in preprint form.
To access the final published version, download the pdf file.
Next Section: Interpretation Title/Abstract Page: THE INTERNAL KINEMATICS OF Previous Section: Observations | Contents Page: Volume 15, Number 1 |
Results
Figure 1 (Right) shows a set of spectra from individual H II regions: intensity v. radial velocity. From spectra of this type we computed the internal velocity dispersions of the principal components in intensity of all the regions measured (the brightest 200 out of 2000 identified in M100). These are shown plotted against H luminosity in figure 1 (Left). We can see a broad scatter, but the upper envelope is clearly linear in the log-log plot. Its slope is
, which agrees with the slope of L versus
found by Arsenault et al. (1990) for the regions of M100 with highest surface brightness. There is a 10% random error in each specific
value and a basic systematic error of about 2.5 Km s
.
Next Section: Interpretation Title/Abstract Page: THE INTERNAL KINEMATICS OF Previous Section: Observations | Contents Page: Volume 15, Number 1 |
![Welcome...](/pasa/welcome.gif)
![About Electronic PASA...](/pasa/about.gif)
![Instructions to Authors](/pasa/authors.gif)
![ASA Home Page...](/pasa/asa_home.gif)
![CSIRO Publishing PASA](/pasa/csiro_pub.gif)
![Browse Articles](/pasa/articles.gif)
![HOME](/pasa/home.gif)
![Search Articles](/pasa/search.gif)
ASKAP
Public