All Figures

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{aa10604f1a.eps}\hspace*{2m... ...i1c.ps}\hspace*{4mm} \includegraphics[width=6.5cm,clip]{0604fi1d.ps}\end{figure}$ Figure 1: Example of multiband images and profiles: NGC 4051. Top-left: i band; top-right: H ${\alpha }$ ; bottom-left: CO; bottom-right: surface brightness profiles. $\Sigma _{\rm sfr}$ (red) in $M_\odot$ pc^-2 Gyr^-1; $\Sigma _{\rm HI}$ (magenta), $\Sigma _{{\rm H}_2}$ (blue) and $\Sigma _{\rm star}$ (green) in $M_\odot$ pc^-2. The arrow indicates r₂₅ as in Col. 10, Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0604fi2a.ps}\hspace*{0.6cm} \includegraphics[width=7cm,clip]{0604fi2b.ps}\end{figure}$ Figure 2: The local Schmidt law for the entire sample, separately for the molecular ( left panel) and the total gas ( right panel). Profiles are normalized to the maximum values for each galaxy. The dashed line in the left panel represents the index n=1, in the right panel n=1.4.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0604fi3a.ps}\hspace*{7mm} \includegraphics[width=7cm,clip]{0604fi3b.ps}\end{figure}$ Figure 3: The Schmidt law for integrated quantities, separately for the molecular ( left panel) and the total hydrogen ( right panel). Filled circles are for our measurements, while empty circles are data from Kennicutt (1998), for the galaxies we have in common. Uncertainties are 0.2 dex for SFR and up to 1 dex for H₂ and for the total gas.
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In the text

$\begin{figure} \par\includegraphics[width=7.15cm,clip]{0604fi4a.ps}\hspace*{0.6cm} \includegraphics[width=7cm,clip]{0604fi4b.ps}\end{figure}$ Figure 4: The relationship between ${\rm def}_{\rm HI}$ and color residuals $({\rm H}_2-{\rm sta})_R$ ( right panel) and $({\rm sfr-sta})_R$ ( left panel). Correlation coefficients are respectively r=0.60 and r=0.65. Uncertainties are discussed in the text.
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In the text

$\begin{figure} \par\includegraphics[width=5.4cm,clip]{0604fi5a.ps}\hspace*{0.4cm... ...b.ps}\hspace*{0.4cm} \includegraphics[width=5.4cm,clip]{0604fi5c.ps}\end{figure}$ Figure 5: Comparison between the mean $\rm sfr-sta$ profile for deficient (dashed lines) and non deficient (continuous lines) galaxies; from left to right, deficiency threshold is set to be ${\rm def}_{\rm HI}\geq 0.4$ , ${\rm def}_{\rm HI}\geq 0.65$ and ${\rm def}_{\rm HI}\geq 0.9$ . Non deficient galaxies are always considered for ${\rm def}_{\rm HI}<0.4$ .
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In the text

$\begin{figure} \par\includegraphics[width=5.3cm,clip]{0604fi6a.ps}\hspace*{0.5cm... ...b.ps}\hspace*{0.5cm} \includegraphics[width=5.3cm,clip]{0604fi6c.ps}\end{figure}$ Figure 6: Comparison between the mean ${\rm H}_2-{\rm sta}$ profile for deficient (dashed lines) and non deficient (continuous lines) galaxies; from left to right, deficiency threshold is set to be ${\rm def}_{\rm HI}\geq 0.4$ , ${\rm def}_{\rm HI}\geq 0.65$ and ${\rm def}_{\rm HI}\geq 0.9$ . Non deficient galaxies are always considered for ${\rm def}_{\rm HI}<0.4$ .
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0604fi7.ps}\end{figure}$ Figure 7: The relationship between $\rm def_{HI}$ and the HI isophotal radius at 5 $\times$ 10¹⁹ cm^-2, normalized to the r₂₅. Correlation coefficient is r=0.81. The dashed lines emphasize that $r_{\rm HI}> r_{25}$ for $\rm def_{HI}>0.9$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{0604fi8a.ps}\vspace*{3mm} \par\includegraphics[width=6.8cm,clip]{0604fi8b.ps}\end{figure}$ Figure 8: Mean radial gradients for the outer part of the $\rm sfr-sta$ ( top panel) and $\rm H_2-sta$ ( bottom panel) colour profiles, in four bins of deficiency (0-0.4, 0.4-0.65, 0.65-0.90, >0.90). Error bars are the uncertainties on the mean values in each bin.
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In the text