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A standard parametric maximum-likelihood technique is used to determine boththe probability distribution over total HI mass $M_{\rm HI}$ and the regressionof this quantity on the linear optical diameter $D_{\rm o}$ for field giantspirals (Sa-Sc) from a complete HI-flux-limited data set of these objects.Gaussian and Schechter parametrizations of the HI mass function are explored.We find that the available data are equally well described by both models, andthat the different morphological classes of giant spirals have HI massfunctions which, in general, agree well within the errors. The largestdiscrepancy corresponds to the Sb-type systems which exhibit a deficit of lowHI-mass objects relative to the other types. Using a straightforwardgeneralization of the gaussian model, we have also investigated the lineardependence of $M_{\rm HI}$ on $D_{\rm o}$. We confirm that the HI content ofspirals is much better predicted by the size of their optical disks than bytheir morphological types alone. The inferred correlations imply a considerabledecrease of the ratio $M_{\rm HI}/D_{\rm o}^2$ with increasing galaxy size fortypes earlier than Sc.Comment: 23 pages, uuencoded gzipped postscript; 3 Tables and 12 Figures  available upon request from josepm@faess0.am.ub.e

The H i Content of Spirals. I. Field Galaxy H i Mass Functions and H i Mass--Optical Size Regressions