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Time for this proposal is  to be transferred from MROWANRO.SURVEY_1  S
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ISOPHOT AND ISOCAM are  used to determine  the luminosity functions of
galaxies  through four ISO bands. They  are  absolutely needed for all
statistics on galaxy distributions, in particular to interpret the ISO
deep surveys as ELAIS and the guarantee time Deep Survey (GTDS) or any
others which are   not  redshift-followed up (two  or  more  years are
needed  to do it).   On ~ 0.25  square degree, the  ESO-Sculptor sample
is complete  till R =  20.5, 600  redshifts (Bellanger et  al,  1995) and
spectral types (Galaz et al, 1996) have already been measured from 675
spectra of galaxies  with an ESO key-program (de  Lapparent, 1989).  A
deep optical photometry  limited  to magnitudes B=24.5,   V=24, R=23.5
(Arnouts et al, 1996) is  extended to the K  band photometry at ESO (a
joined programme with VdL and  BRV).  A VLA radio  map of this area is
also scheduled.   That field is one of  the most complete for  such an
area and depth.
Following the OTAC recommendations on the  first proposal, that field
was partly (28' x  28') included in the survey ELAIS, of which BRV is
co-PI. But ELAIS is limited to R= 18, checked by the ELAIS/CAM test.
So that less than 40/600 galaxies of the ESO sample will be detected
on the  SCULPTOR area  target, quite unsufficient for any luminosity
function through ISO bands and loosing a major scientific interest.
The secund ISO call is a  unique opportunity to profit by the multi-
wavelength completude of that reference  survey. Moreover as a second
survey,  it will be useful to confirm the results of the GTDS survey.
Our group  gathers confirmed expertises on  data processing,galaxy
evolution  models, interpretation of faint galaxy counts, correlation
functions and large scale structures.