A significant quantity of photometric data on spiral galaxies is today available in the literature, but, very often, only measurements in one or two photometric bands (see De Vaucouleurs et al., RC3) are performed, while it would be more useful to have multiband photometry at disposal. From measurements in all the five photometric bands of the Johnson and Kron extended system, it is possible to obtain information on the dust distribution, on the various kinds of stellar populations present, and on their distribution throughout the galaxy. Data obtained in the U and B bands are very dust-sensitive and highlight the emission coming from ionized gas regions and from young stars; data from the V band bring out mainly the emission coming from A-type dwarfs, while the R and I bands are more sensitive to the old stellar population, like that of K-type giants. Moreover, these last two bands are less sensitive than the previous ones to the presence of dust. The study of the surface brightness radial profiles of galaxies allows to distinguish the zones of recent star formation; according to Boroson (Boroson 1981), in fact, when star formation is limited to certain regions of the disk, a departure from an exponential disk profile occurs. This interpretation seems confirmed by the work by Prieto et al. (1992). In their work the authors find that the non exponential behaviour in the bulge to disk transition zone (Freeman II profile) can be ascribed to a young stellar population hidden by dust. According to this work, the presence of dust can be enlightened by reddening and dimming in the light coming from the galactic zone considered. The study of the variation of physical parameters, like the bulge and disk scalelengths, versus wavelength, can help the comprehension of star formation histories of the galaxies. In a recent work, Ryder & Dopita (1994, hereafter RD), have found that, for a sample of 34 spiral galaxy, the V scalelength is longer than the I one. This is due to the fact that each new stellar generation adds a contribution to the scalelength, instead of following the pattern of the old one. On the contrary, if the dust contribution is underestimated, and the Holmerg approximation (Holmberg 1958) is wrong, (i.e. there is much more dust inside the disk), the behaviour of the disk scalelength is dependent on the adopted dust model (see Disney et al. 1989, hereafter DDP). The study of the trend of colour indexes with radius has been used to give an experimental confirmation (see Paper I) to the infall model of Larson & Tinsley (Larson & Tinsley 1978, herafter L&T78). We have acquired, for a sample of seven spiral galaxies, photometric data in five photometric bands U, B, V, R, I of the Johnson and Kron extended system, and we have analyzed the surface brightness radial profiles of the galaxies and the radial trend of colour indexes (B- V), (B-I), (U-B). In the following section we describe the observations, while in Sect. 3 we present the data reduction and analysis with some comments on each galaxy; finally in Sect. 4 we discuss the results obtained.