All Figures

$\begin{figure} \par\includegraphics[width=17cm,clip]{8652f1a.eps} \end{figure}$ Figure 1: The H $\alpha$ ( left) and the continuum-subtracted ( right) images of 42 observed galaxies in the CVnI cloud. North and East are indicated by arrows. The size of the images is about 4 $\hbox {$^\prime $ }$ .
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In the text

$\begin{figure}\par\includegraphics[width=17cm]{8652f1b.eps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\par\includegraphics[width=17cm]{8652f1c.eps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\par\includegraphics[width=17cm]{8652f1d.eps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\par\includegraphics[width=17cm]{8652f1e.eps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\par\includegraphics[width=17cm]{8652f1f.eps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\par\includegraphics[width=17cm]{8652f1g.eps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\par\includegraphics[width=17cm]{8652f1h.eps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\par\includegraphics[width=17cm]{8652f1i.eps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\par\includegraphics[width=17cm]{8652f1j.eps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\par\includegraphics[width=17cm]{8652f1k.eps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\par\includegraphics[width=17cm]{8652f1l.eps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\par\includegraphics[width=17cm]{8652f1m.eps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure}\par\includegraphics[width=17cm]{8652f1n.eps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{8652f2.eps} \end{figure}$ Figure 2: Star formation rate versus blue absolute magnitude for 78 galaxies in the Canes Venatici I cloud (circles) and 41 members of the M 81 group (squares). The open symbols indicate the galaxies with only an upper limit of their ${\it SFR}$ . The line corresponds to a constant ${\it SFR}$ per unit luminosity.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{8652f3.eps} \end{figure}$ Figure 3: Star formation rate versus neutral hydrogen mass for galaxies in the CVnI cloud (circles) and the M 81 group (squares). The galaxies with upper limit of ${\it SFR}$ or $M_{\rm HI}$ are indicated by open symbols. The dashed line corresponds to a fixed ${\it SFR}$ per unit hydrogen mass and the solid line traces the relationship ${\it SFR}\propto M_{\rm HI}^{1.5}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{8652f4.eps} \end{figure}$ Figure 4: The CVnI cloud galaxies and the M 81 group members on the evolutional plane ``past-future'': p_* = log $([{\it SFR}]\cdot T_0/L_B)$ and f_* = log $(M_{\rm HI}/[{\it SFR}]\cdot T_0)$ . The galaxies with upper limits of ${\it SFR}$ or $M_{\rm HI}$ are shown by open symbols.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{8652f5a.eps}\hspace*{3mm} \includegraphics[width=8.3cm,clip]{8652f5b.eps} \end{figure}$ Figure 5: The specific star formation rate ( left) and the time of exhaustion of the available reserves of gas ( right) versus the tidal index for the CVnI cloud (circles) and the M 81 group galaxies (squares). The open symbols indicate the galaxies with upper limits of ${\it SFR}$ or $M_{\rm HI}$ . The solid and dashed regression lines correspond to the filled only and to the filled plus open symbols, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{8652f1a.eps} \end{figure}$	Figure 1: The H $\alpha$ ( left) and the continuum-subtracted ( right) images of 42 observed galaxies in the CVnI cloud. North and East are indicated by arrows. The size of the images is about 4 $\hbox {$^\prime $ }$ .
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$\begin{figure}\par\includegraphics[width=17cm]{8652f1b.eps} \end{figure}$	Figure 1: continued.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{8652f2.eps} \end{figure}$	Figure 2: Star formation rate versus blue absolute magnitude for 78 galaxies in the Canes Venatici I cloud (circles) and 41 members of the M 81 group (squares). The open symbols indicate the galaxies with only an upper limit of their ${\it SFR}$ . The line corresponds to a constant ${\it SFR}$ per unit luminosity.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{8652f3.eps} \end{figure}$	Figure 3: Star formation rate versus neutral hydrogen mass for galaxies in the CVnI cloud (circles) and the M 81 group (squares). The galaxies with upper limit of ${\it SFR}$ or $M_{\rm HI}$ are indicated by open symbols. The dashed line corresponds to a fixed ${\it SFR}$ per unit hydrogen mass and the solid line traces the relationship ${\it SFR}\propto M_{\rm HI}^{1.5}$ .
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{8652f4.eps} \end{figure}$	Figure 4: The CVnI cloud galaxies and the M 81 group members on the evolutional plane ``past-future'': p_* = log $([{\it SFR}]\cdot T_0/L_B)$ and f_* = log $(M_{\rm HI}/[{\it SFR}]\cdot T_0)$ . The galaxies with upper limits of ${\it SFR}$ or $M_{\rm HI}$ are shown by open symbols.
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