Contents of: VI/111/./abstract/FHAMMER_HIZ_GAL2.abs

The following document lists the file abstract/FHAMMER_HIZ_GAL2.abs from catalogue VI/111.
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We propose to complete deep ISO integrations of CFRS fields which have
already been widely studied by the largest spectroscopic survey of faint
galaxies available up to date. Deep imagery/photometry are available in
B, V, I and K bands while about 50% of the I=22.1 galaxies have been
spectroscopically measured. Moreover a significant part (30%) of these
fields have been covered by deep HST imagery. The ISO observations
of two additional fields (CFRS2215+00 and CFRS2215+00) combined with the
already planned observations of CFRS1414+52 and of CFRS0300+00 (PROPID:
HIZ_GAL), would provide an unique sample of about 100 ISO sources with
spectroscopy, deep imagery (including K-band) and detailed morphology
from HST. This program will also be used as a template to the deep surveys
on blank fields planned in the core program.
Our aim is to investigate the infrared properties of field galaxies
including (1) the evolution of the dust properties in field galaxies
up to z=1 and the consequence on to the estimation of the global star formation
rate and its evolution; (2) the faint population of AGNs which dominates the
microJy radio counts and represents a significant fraction of the overabundant
population of faint blue galaxies.
We intend to carry out deep observations in 4 wavelength ranges, at
5-8/12-18 microns with ISOCAM and 60/90 microns with ISOPHOT. Our goal
is to get a better understanding of the dust emission in distant normal
galaxies as well as in AGNs and its link with optical and radio emission.
Several broad band measurements are required to understand the relative
influence of hot/cold dust in galaxies as well as to disentangle dust
emission from non thermal emissions in AGNs.
We believe that using fields where a considerable amount of work has
already been done will put us in a good position to rapidly provide new
and fascinating results just after the ISO observations.



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