The following document lists the file abstract/GMILEY_HZDUST2.abs
from catalogue VI/111.
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===================================================================== ==> In this proposal, more time is being requested for GMILEY.DUSTHZRG ===================================================================== The detection of dust emission from high-z galaxies is one of the most exciting possibilities of CAM and PHOT. Given in-flight experience, this goal seems now more challenging than thought before launch, but feasible with observing modes that allow optimum deglitching, flatfielding, rejection of spurious sources, and correction of long-term and short-term drifts. We thus propose to expand our programme GMILEY.DUSTHZRG to make a dedicated effort at deep, confusion-limited imaging of only a SMALL number (5) of high-z radio galaxies, using the available time to optimize the observing modes. PHOT will be used at 90 and 160 micron, and CAM at 15 micron to investigate the spectral energy distributions (SEDs) of radio galaxies at redshifts greater than 3. The SEDs will provide insight into the nature of the far-IR emission of the most distant known galaxies, when the universe was only 10 percent of its present age. The SEDs will allow us to study the ubiquity of processed material in these young objects, the luminosity of the dust emission and the temperatures of the emitting dust components. Derived color temperatures will allow an assessment of the relative importance of an active nucleus and starbursts in producing the emission. The results will have consequences for heavy element production, the early evolution and formation of galaxies, and the role of starbursts in the early universe. The CAM observations will probe hot dust associated with an obscured quasar nucleus predicted to exist by unified models of active nuclei. ISO provides the only way of probing the temperature-sensitive Wien part of the blackbody curve. Measurements to be obtained with the new SCUBA bolometer array at the JCMT will complement the SEDs at long wavelengths. We have the largest sample of distant radio galaxies available, from which we have selected the best candidate sources. The data will provide a unique view of the neutral interstellar (and probably star forming) interstellar medium in the most distant galaxies known to us.