All Figures

$\begin{figure} \par\includegraphics[width=4.4cm,clip]{espsep.eps}\hspace*{2mm} \includegraphics[width=4.3cm,clip]{espdvel.eps} \end{figure}$ Figure 1: Frequency of pair projected separation (Sep) and frequency of radial velocity difference ( $\Delta v$ ) for our sample pairs.
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In the text

$\begin{figure} \par\includegraphics[width=4.3cm,clip]{espp117a.eps}\hspace*{2mm}... ...ps}\hspace*{2mm} \includegraphics[width=4.3cm,clip]{espp437b.eps} \end{figure}$ Figure 2: Peculiar spectra of galaxies.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=4.3cm,clip]{espp422a.eps} \hspac... ...\hspace*{2mm} \includegraphics[width=4.3cm,clip]{espp546a.eps} } \end{figure}$ Figure 3: Spectra of some galaxies.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[width=5.8cm,clip]{altaron.eps}\hspace*{2mm} \includegraphics[width=5.8cm,clip]{halfa.eps} } \end{figure}$ Figure 4: In both figures, open triangles represent our data for galaxies with non-peculiar morphologies; bold triangles, the data for galaxies with peculiar morphology; and starry triangles, the ones for objects with peculiar spectra. Figure 4a presents the variation of EW $\rm {(H_{\alpha } + [N_{II}])}$ with morphological type. In this figure open squares represent field galaxies' integrated spectra data from Kennicutt (1992, hereafter K 92); bold squares, K(92) data for strongly interacting galaxies; and starry squares, K(92) data for Seyfert galaxies. The behavior of field galaxies with $5{-}7~\hbox{\rm \AA}$ resolution integrated spectra from Kennicutt (1992, hereafter K 92) is presented with a broken line. The dotted line shows the behavior of EW $\rm {(H_{\alpha } + [N_{II}])}$ for the integrated spectra of field galaxies from Kennicutt & Kent (1983, hereafter KK 83). The solid line indicates a trial upper limit for our sample galaxies that may not show emission line strength excess. This line is parallel and encompasses the one which represents K92 data of integrated emission because the latter is diluted over a larger region. Figure 4b presents the variation of EW (H $_{\alpha }$ ) with morphological type.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=4.4cm,clip]{wekpc.eps}\hspace*{2mm} \includegraphics[width=4.3cm,clip]{halfakpc.eps} } \end{figure}$ Figure 5: These figures relate EW $\rm {(H_{\alpha } + [N_{II}])}$ and EW (H $_{\alpha }$ ) with projected separation. As before, open triangles represent our data for galaxies with non-peculiar morphologies; bold triangles, the data for galaxies with peculiar morphology; and starry triangles, the ones for objects with peculiar spectra.
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In the text

Full version

$\begin{figure} \par\mbox{\includegraphics[width=5.7cm,clip]{espp24a.eps} \hspace... ...hspace{0.3cm} \includegraphics[width=5.8cm,clip]{espp117b.eps} } \end{figure}$ Figure 3: Spectra of some galaxies.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[width=5.7cm,clip]{espp101a.eps} \hspa... ...hspace{0.3cm} \includegraphics[width=5.8cm,clip]{espp316b.eps} } \end{figure}$ Figure 3: continued.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[width=5.8cm,clip]{espp331a.eps} \hspa... ...ce{0.3cm} \includegraphics[width=5.7cm,clip]{espp363a.eps} } \par\end{figure}$ Figure 3: continued.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{espp373a.eps} \hspace{0.3c... ...hspace{0.3cm} \includegraphics[width=5.7cm,clip]{espp402b.eps} } \end{figure}$ Figure 3: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=5.8cm,clip]{espp416a.eps} \hspac... ...hspace{0.3cm} \includegraphics[width=5.7cm,clip]{espp429b.eps} } \end{figure}$ Figure 3: continued.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[width=5.7cm,clip]{espp457a.eps} \hspa... ...hspace{0.3cm} \includegraphics[width=5.8cm,clip]{espp487b.eps} } \end{figure}$ Figure 3: continued.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[width=5.7cm,clip]{espp490a.eps} \hspa... ...hspace{0.3cm} \includegraphics[width=5.7cm,clip]{espp546b.eps} } \end{figure}$ Figure 3: continued.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=5.7cm,clip]{espp539a.eps} \hspac... ...cs[width=5.8cm,clip]{espp617b.eps} } \par\hbox{\hspace{08cm}} \par\end{figure}$ Figure 3: continued.
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In the text

$\begin{figure} \par\includegraphics[width=4.4cm,clip]{espsep.eps}\hspace*{2mm} \includegraphics[width=4.3cm,clip]{espdvel.eps} \end{figure}$	Figure 1: Frequency of pair projected separation (Sep) and frequency of radial velocity difference ( $\Delta v$ ) for our sample pairs.
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$\begin{figure} \par\includegraphics[width=4.3cm,clip]{espp117a.eps}\hspace{2mm}... ...ps}\hspace{2mm} \includegraphics[width=4.3cm,clip]{espp437b.eps} \end{figure}$	Figure 2: Peculiar spectra of galaxies.
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$\begin{figure} \par\mbox{\includegraphics[width=4.3cm,clip]{espp422a.eps} \hspac... ...\hspace*{2mm} \includegraphics[width=4.3cm,clip]{espp546a.eps} } \end{figure}$	Figure 3: Spectra of some galaxies.
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$\begin{figure} \par\mbox{\includegraphics[width=4.4cm,clip]{wekpc.eps}\hspace*{2mm} \includegraphics[width=4.3cm,clip]{halfakpc.eps} } \end{figure}$	Figure 5: These figures relate EW $\rm {(H_{\alpha } + [N_{II}])}$ and EW (H $_{\alpha }$ ) with projected separation. As before, open triangles represent our data for galaxies with non-peculiar morphologies; bold triangles, the data for galaxies with peculiar morphology; and starry triangles, the ones for objects with peculiar spectra.
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$\begin{figure} \par\mbox{ \includegraphics[width=5.7cm,clip]{espp101a.eps} \hspa... ...hspace{0.3cm} \includegraphics[width=5.8cm,clip]{espp316b.eps} } \end{figure}$	Figure 3: continued.
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