The following document lists the file abstract/DCALZETT_PROP_001.abs
from catalogue VI/111.
A plain copy of the file
(without headers/trailers) may be downloaded.
We plan to investigate the relative importance of the warm and cool dust emission, the dust opacity, and the characteristics of the dust-star geometrical distribution in galaxies by studying multiwavelength spectral energy distributions of a sample of star-forming galaxies. The ultraviolet and optical spectra of our sample galaxies will be complemented by ISOPHOT measurements of the dust emission at 60, 100, 135 and 200 um. Using the spectral energy distribution of the dust emission in the range 40-240 um we will investigate the cool dust emission, heated by the non-ionizing stars, and how it relates to the warm dust emission, heated by the hot, young stars. From the UV and optical spectra we can estimate the amount of ionizing and non-ionizing energy absorbed by dust. This information will be used, in conjunction with the ISO measurements, to study the energy balance between dust absorption of UV and optical starlight and dust emission in the far infrared, and to infer the dust opacity of the galaxies. The long wavelength baseline of ISO is a requirement for the success of the present investigation, since the cool dust emission peaks at wavelengths greater than 100 um. The IRAS fluxes of most of our sample galaxies are known with large uncertainties or are upper limits; ISO, thanks to its high sensitivity, will provide accurate measurements for these objects.