Volume 384, Number 3, March IV 2002
|Page(s)||866 - 871|
|Section||Cosmology (including clusters of galaxies)|
|Published online||15 March 2002|
The influence of clumping on surface brightness fits of edge-on spiral galaxies
University of Crete, Physics Department, PO Box 2208, 710 03 Heraklion, Creete, Greece
2 Observatoire de Marseille, 2 place Le Verrier, 13248 Marseille Cedex 4, France
3 Max-Planck-Institute für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
4 European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany
5 Max-Planck-Institute für Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching, Germany
6 CNR/Istituto di Radioastronomia – Sezione di Firenze, Largo E. Fermi 5, 50125 Firenze, Italy
Corresponding author: S. Bianchi, email@example.com
Accepted: 16 January 2002
We have used a Monte Carlo radiative transfer code to produce edge-on images of dusty galactic disks, allowing a fraction of the dust to be distributed in clumps. Synthetic images of edge-on galaxies have been constructed for different amounts of dust, distributions of clumps and fractions of dust in clumps, following the formalism of Bianchi et al. ([CITE]). We have also considered models with stellar emission embedded in the clumps. The synthetic images have been fitted with analytical models made with smooth distributions of dust, adopting the procedure developed by Xilouris et al. ([CITE]) to fit optical images of real edge-on galaxies. We have compared the parameters determined by the fit with the input parameters of the models. For the clumping distributions adopted in this paper, the neglect of clumping results in underestimating the amount of dust in a galaxy. However, the underestimation is never larger than 40%.
Key words: radiative transfer / ISM: dust, extinction / galaxies: photometry / galaxies: spiral / galaxies: structure
© ESO, 2002
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