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===================================================================== Time for this proposal is to be transferred from MROWANRO.SURVEY_1 S ===================================================================== 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.