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The hypothesis of the VESUVIO survey coming out from the meeting in Napoli was: a medium-deep (r’<24 S/N=10) survey in a region of about 100 square degrees of Horologium supercluster; a deep (r’<25, S/N=10) survey on Hercules supercluster (10 square degrees); a deep (r’<25, S/N=10) survey on a distant (z=0.2-0.4) supercluster. We estimated that, assuming “consistent” depths in the other wavebands, the total time needed to complete the surveys was in the range 100-120 VST/OmegaCam nights. Given the main science goals of the survey, i.e. to obtain detailed characterisation of galaxies in the full range of cosmic environments, we clearly stated that the optical part of the survey has to be fine-tuned with the X-ray survey, with the radio survey, and with the redshift survey. This is without any doubts the crucial step towards the definition of survey as a whole.  For a number of reasons, it was not possible to discuss the present notes with all WG members. The content should thus be considered as very preliminary. *+-Ÿ Ą¤Ľ§ACDŞŹŽś¸ş& &"&|*~*€*÷č÷áŮŃÉÂżÉáÉáÉáÉáÉCJ j0JU5CJ(OJQJ>*CJOJQJ>*CJ(OJQJ CJOJQJj0J5CJ OJQJU5CJ OJQJ& &"&~*€*ýűýű,-/č4y@™šœŸ Ą˘Ł¤§ABCDü÷ňíćÜŇÍČĂžš´ŻŞĽ ›–‘‘]ü˙˙^ü˙˙_ü˙˙`ü˙˙aü˙˙cü˙˙dü˙˙fü˙˙gü˙˙Ŕü˙˙âý˙˙ăý˙˙‡ţ˙˙Ěţ˙˙  ˙˙˙   ˙˙˙ Ń˙˙˙Ó˙˙˙Ô˙˙˙The immediate objective of opticalobservations is to obtain, for a statistically controlled sample of galaxies: accurate surface photometry; a consistent (within the survey) morphological classification; colour gradients; colour profiles (for a subsample).*+-Ÿ Ą¤Ľ§ACDŞŹŽś¸ş& &"&÷č÷áŮŃÉÂżÉáÉáÉáÉCJ j0JU5CJ(OJQJ>*CJOJQJ>*CJ(OJQJ CJOJQJj0J5CJ OJQJU5CJ OJQJśÚ ŹŽŕ˜ź¸ş0ŽŇzl n Ô!Z"D#F#â$ä$&&&úúřööúúúúřööúúúööööęęöööööö  & F„¤ Ćh¤ & F This objective, being the more demanding, will ensure to obtain integrated quantities for a deeper (typically by 2-4 mag) sample to study luminosity functions and colour-magnitude diagrams as a function of environment. The immediate objective of opticalobservations is to obtain, for a statistically controlled sample of galaxies accurate surface photometry, leading to: a consistent (within the survey) morphological classification; colour gradients; colour profiles (for a subsample). A WG on surface photometry has been established. This objective, being the more demanding, will ensure to obtain integrated quantities for a deeper (typically by 2-4 mag) sample to study luminosity functions and colour-magnitude diagrams (relations, where applicable) as a function of environment. In the present phase, a thorough discussion with the theory WG group is essential in order to distribute efforts in the most effective way. Feedback from the theory WG is needed: to better constrain the accuracy of the quantities to be measured; to plan the observing strategy in order to optimise (in time and quality) the scientific outcome the imaging survey. For what the non-optical parts of the survey are concerned, we need to go deeper into the discussion on how X-ray, and especially radio observations have to be combined (in terms of strategy) with imaging. A very critical item to be discussed is that of redshifts. 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