are given up to 7 degrees projected separation from Coma and A1367 in Fig. 10 a and b respectively. Points are coded according to $\rm L_H$ to stress once more the inverse proportionality between SFR and mass. Except for a marginal increase of the dispersion near the center of A1367, the only apparent pattern is a relatively large fraction of faint (Log $\rm L_H~\leq$ 10.0) galaxies with large $\rm H\alpha$ E.W. in the shell contained between 1 and 2 degrees of projected radii around Coma. However, we suggest that this effect is due to a mass segregation instead of a real enhancement of the SFR. In fact if we remove, to the first order, the luminosity (mass) dependence, by multiplying $\rm H\alpha$ E.W. by the corresponding $\rm L_H$ (as derived in three intervals in section 5.1), any evidence for radial gradients is canceled. (See Fig. 10 c and d).

Discussion and Conclusions
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The main results of the present work can be summarized as follows: i) The present SFR properties of spiral galaxies, as derived from a representative sample of the local Universe, increase with increasing Hubble type.ii) These properties do not show a significant dependence on the explored range 