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

The following document lists the file abstract/PANDREAN_PROP_A.abs from catalogue VI/111.
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 A complete sample of 29 galaxies, selected from the IRAS Point Source
 Catalogue at a limiting flux of 2 Jy at 60 micron in the sky region
 delimited by the equatorial coordinates 21h < alpha < 5h and -22.5deg
 < delta < -26.5deg, has been already observed from the ground in the
 continuum at 1.3mm, spectroscopically at 115 GHz (CO (1-0)) and at
 21 cm. With such an amount of FIR-mm information, it is to our knowledge
 the best available infrared sample for an ISO investigation.
 We propose to use PHOT and LWS to take FIR photometry and spectra of
 CII emission line for all the objects of the sample to address the
 following issues: (1) the total amount of dust present in the
 interstellar medium (ISM), (2) the global star formation activity and the
 relative contributions of the molecular and atomic phases in the formation
 of the CII line, (3) the luminosity function and evolution of IR galaxies.
 In order to constrain the dust properties the entire spectrum from
 the IR down to 1mm should be taken. Indeed, there is evidence from 1 mm
 data that a large amount of dust lies at cold temperatures so that IRAS
 data are not sufficient to correctly estimate it. The current uncertainties
 in the broad-band FIR spectrum of galaxies seriously affect, in particular,
 our knowledge of: (a) the spatial distribution of dust in galaxy discs;
 (b) the total amount of dust and the gas-to-dust ratio; (c) the effect of
 dust on the extinction of the optical light. A comparison between CO and HI
 data and spectra of CII will allow to probe the photon-dominated regions
 associated with massive star formation and the diffuse atomic phase of the
 interstellar medium. The FIR/submm data for such a complete sample will also
 allow us to estimate the luminosity functions of galaxies in all the FIR
 domain and better constrain their contribution to the background radiation.
 PHOT and LWS offer a unique possibility to complement the IRAS/mm, CO and HI
 data on our galaxy sample, hence allowing a very significantly improvement in
 our knowledge of the physical processes occuring inside them.

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