The following document lists the file abstract/MMALKAN_PG_DUST.abs
from catalogue VI/111.
A plain copy of the file
(without headers/trailers) may be downloaded.
Current understanding of the evolutionary history of young, high-z galaxies is severely limited by lack of data on their dust content, and its effects in absorption and emission. The powerful long-wavelength capabilities of ISOCAM make it possible for the first time to measure directly dust in the brightest known normal star-forming galaxies at z>2. These objects are newly discovered, and were unknown before ISO's launch. We will combine accurate ground-based L-band measurements of the stellar flux with 6, 12 and 15 micron ISOCAM images to calculate the thermal emission from dust (the "infrared excess") and determine accurately the fraction of stellar light absorbed. By measuring the re-emitted thermal spectrum, we will compare the temperature distribution of dust with what is observed in starburst galaxies at the current epoch. These observations will also be applicable to other cosmological problems, such as measuring the Cosmic IR Background.