All Figures

$\begin{figure} \par\resizebox{12cm}{!}{\includegraphics[clip]{0158f1ac.ps}}\par\resizebox{12cm}{!}{\includegraphics[clip]{0158f1bc.ps}} \end{figure}$ Figure 1: Positions of 146 spiral (triangles) and 61 elliptical (circles) galaxies in the Virgo field (within $9^\circ$ from M 87) as a function of Declination and distance (assumed correct, top) and radial velocity (bottom). H I-deficient galaxies (deviating more than $3\sigma$ from normalcy) are shown as filled triangles - with the ones apparently outside the cluster (Table 7, below) shown as surrounded filled triangles (red triangles in the electronic version of the Journal), while Messier ellipticals (see Table 2) are shown as filled circles, with M 49 to the South, and M 59, M 89, M 60, M 87, M 86 and M 84 at increasing distances (top plot) and M 89, M 59, M 84, M 60 and M 87 at increasing radial velocities (bottom plot, M 86 has v < 0).
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{0158f2c.ps} \end{figure}$ Figure 2: Simulated and observed velocity-distance diagrams. The observer is at (0,0) and sees a cone of angular radius $9^\circ$ . Dots represent the velocity field traced by the particles (1 in 50 for clarity) in the cosmological N-body simulation in the direction of the most massive halo, for which distances and velocities have been rescaled (Eqs. (8) and (9)) incorporating a Hubble flow with $H_{0}=66.7~\rm km~s^{-1}~Mpc^{-1}$ , as in the simulation. Superposed are galaxies of the Virgo cluster. Circles and triangles represent early-type and late-type galaxies, respectively. The size of the triangles informs about the H I-deficiency of the spiral galaxies measured in units of the mean standard deviation for field objects (=0.24). H I-deficient galaxies deviating more than $3\sigma$ from normalcy apparently outside the cluster (Table 7, below) are shown as surrounded filled triangles (red triangles in the electronic version of the Journal). Squares represent additional spiral galaxies with no H I-deficiency data. Open symbols indicate galaxies with uncertain distances (with distance errors greater than 5 Mpc or spirals with only one distance estimate). Dashed lines show the unperturbed Hubble flow with H₀ = 66.7 and $70 ~\rm km ~s^{-1} ~Mpc^{-1}$ , respectively (going upwards). The locations of the vertical spikes of simulated particles away from the Virgo cluster (assumed to lie at 16.8 Mpc) are not meaningful and should not be compared to the measured galaxy distances.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{0158f3c.ps} \end{figure}$ Figure 3: Same as Fig. 2, but incorporating Gaussian relative distance errors of $\sigma \ln D = 0.2$ for the dark matter particles.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{0158f4.ps} \end{figure}$ Figure 4: Positions of galaxies within $9^\circ$ of M 87 in 3 distance (left) and velocity (right) bins. Ellipticals and spirals are shown as circles and triangles, respectively. Messier ellipticals are shown as filled circles, while M 49 (NGC 4472) is also highlighted as a thick dotted circle (bottom plots, in green in the electronic version of the journal). H I-deficient (> $3~\sigma$ ) spirals are shown as filled triangles (with the 13 apparently in the outskirts of Virgo (Table 7) in red in the electronic version of the Journal). The large solid circles show the virial radius r₁₀₀ at the different distance bins, while the large dotted circles indicates r₁₀₀ at the distance to M 87.
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In the text

$\begin{figure} \par\resizebox{13cm}{!}{\includegraphics[clip]{0158f5.ps}} \end{figure}$ Figure 5: Color-luminosity diagram for 12 of the 13 H I-deficient galaxies of Table 7 (VCC 1569 was excluded because it is not bright enough to be included in GOLDMine), possibly outside the Virgo cluster (large filled symbols) or placed at the distance of the Virgo cluster (large open symbols). Other Virgo galaxies are shown as small open symbols. Triangles, squares and pentagons (respectively in red, green, and blue in the electronic version of the journal) refer to galaxies of morphological type 1-2, 3-4 and 5-6, respectively. The data is taken from the GOLDMine (Gavazzi et al. 2003) database, and dereddened using the internal and Galactic extinctions from LEDA with the selective extinctions of Cardelli et al. (1989).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{0158f6.ps}} \end{figure}$ Figure 6: Comparison of H I-deficiency estimators. Galaxies possibly located outside the Virgo cluster are shown as filled circles. The vertical and horizontal dashed lines shows the $3~\sigma$ cutoff for DEF₁ and DEF₂, respectively.
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In the text

$\begin{figure} \par\resizebox{17cm}{!}{\includegraphics[clip]{0158f7.ps}} \end{figure}$ Figure 7: POSS I snapshots of the T=1 H I-deficient galaxies of Table 7. The box size is 6' and North points upwards.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{0158f3c.ps} \end{figure}$	Figure 3: Same as Fig. 2, but incorporating Gaussian relative distance errors of $\sigma \ln D = 0.2$ for the dark matter particles.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{0158f6.ps}} \end{figure}$	Figure 6: Comparison of H I-deficiency estimators. Galaxies possibly located outside the Virgo cluster are shown as filled circles. The vertical and horizontal dashed lines shows the $3~\sigma$ cutoff for DEF₁ and DEF₂, respectively.
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$\begin{figure} \par\resizebox{17cm}{!}{\includegraphics[clip]{0158f7.ps}} \end{figure}$	Figure 7: POSS I snapshots of the T=1 H I-deficient galaxies of Table 7. The box size is 6' and North points upwards.
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