All Figures

Figure 1: The Virgo cluster region considered in the present analysis. The dashed broken line represents the boundary of the VCC catalog and the rectangle the area covered by the HIJASS blind HI survey. Superposed are the X-ray contours from ROSAT (Böhringer et al. 1994). All 355 late-type (Sa-Im-BCD) members of the Virgo cluster with are shown divided into H  I detected (296) and undetected (59). Large symbols refer to objects observed in this work.

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In the text

	Figure 2: H  I spectra of the tentatively detected galaxies in the Virgo cluster.
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In the text

	Figure 3: Comparison of the HI fluxes adopted in this work and those found in the Leda database.
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In the text

	Figure 4: Comparison of the HI masses as derived from this work with those derived in the blind HIJASS H  I survey (Davies et al. 2004) for galaxies in common in the radial velocity interval of 500-2500 km s-1. Open triangles are for undetected HIJASS galaxies.
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In the text

Figure 5: The Virgo cluster H  I mass function (HIMF) as derived from this work using only the detected galaxies (histogram), together with the HIMF derived from the blind HIJASS survey (D04), normalized to our data as described in the text. Error bars represent purely statistical errors. For comparison, the dotted line gives the Field HIMF as derived by Zwaan et al. (2003), normalized arbitrarily in order to match our data at .

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In the text

Figure 6: The dotted histogram is obtained from the late-type galaxies optical luminosity function, as determined in the field by Marzke et al. (1998), transformed into using the relation discussed in the text. It appears consistent with the field HILF of Zwaan et al. (2003) (long dashed line) indicating that most of the HI is contributed to by late-type galaxies. The dashed histogram is obtained from the late-type galaxies optical luminosity function of Virgo (see Fig. 7), transformed into using the same vs.  relation. The continuum histogram is the HIMF actually observed in Virgo (see Fig. 5). The filled dots represent the Montecarlo simulation described in the text aimed at modeling the effects of the H  I deficiency on the HIMF.

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In the text

	Figure 7: The optical luminosity distribution of the 355 late-type galaxies analyzed in this work, divided in Giants and Dwarfs, consistent with the one in Sandage et al. (1985) for mag, accounting for the different assumed distance.
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In the text

	Figure 8: The fractional HI mass function as derived from the detected objects alone (dashed histogram) and including undetected galaxies (continuum histogram).
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In the text