All Figures

$\begin{figure} \par\includegraphics[angle=90,width=13cm,clip]{1457fig1.eps}\end{figure}$ Figure 1: Deep optical image of Mkn 1087 and its surrounding in R filter. Mkn 1087, KPG 103a, the north companion galaxy (N) and the rest of the surrounding objects are labeled. The background cluster of galaxies is indicated with a circle.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1457fig2.eps}\end{figure}$ Figure 2: Detailed images in R band of Mkn 1087 ( up) and KPG 103a ( bottom). The brightest knots inside both galaxies are labeled, as well as the external objects #2, #3 and #12. A weak plume at the east of KPG 103a, that curves toward the south, is also barely observed (it is indicated by an arrow).
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In the text

$\begin{figure} \par\includegraphics[width=17.4cm,clip]{1457fig3.eps}\end{figure}$ Figure 3: Logarithmic contour maps in B and J filters of Mkn 1087. M indicates the main body of Mkn 1087, C the center of it, K the nearby galaxy KPG 103a and N the north companion galaxy. The contours are 3 $\sigma$ , 10 $\sigma$ , 20 $\sigma$ , 50 $\sigma$ and 100 $\sigma$ over the sky level for both maps. The slit positions used for spectroscopy are also shown over the B image, indicating with ticks the center of the different zones from which we have extracted the one-dimensional spectra.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{1457fig4.eps}\end{figure}$ Figure 4: ISIS WHT spectra of the center of Mkn 1087, the intense knot #7 and its north companion object. The most important emission lines are labeled in the upper spectrum. All the spectra have been scaled down in flux in order to distinguish the faint lines. Note the high continuum level and the H I absorptions due to the underlying stellar population in the spectrum of the center of Mkn 1087. All spectra are redshift-corrected.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{1457fig5.eps}\end{figure}$ Figure 5: a), b), c) and d): position-velocity diagrams for the four slit positions observed with INT, analysed in 1.6 arcsec bins. The horizontal bars represent the uncertainty of the Gaussian fitting for each point. The location and extension of the different galaxy members are also indicated. North is up in all the diagrams.
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1457fig6.eps}\end{figure}$ Figure 6: Position-velocity diagram for the single slit position observed in Mkn 1087 with WHT, analysed in 1.2 arcsec bins. The horizontal bars represent the uncertainty of the Gaussian fitting for each point. The location and extension of the different galaxy members are also indicated. North is up.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1457fig7a.eps}\hspace*{6mm} \includegraphics[width=8.4cm,clip]{1457fig7b.eps}\end{figure}$ Figure 7: a) (V-R) versus (U-B) values of the knots and STARBURST99 (Leitherer et al. 1999) predictions for an instantaneous burst with a Salpeter IMF and $Z/Z_\odot$ = 1 and 0.4. The age of the bursts decrease from left to right. M represents the values for Mkn 1087 main body, whereas K represents the values for the galaxy KPG 103a. b) W(H $\alpha$ ) versus (U-B) for knots in Mkn 1087 and STARBURST99 (Leitherer et al. 1999) predictions. Some ages of the $Z/Z_\odot$ = 1 model are marked, showing the temporal evolution of the burst. The W(H $\alpha$ ) of the north companion object is indicated with an horizontal arrow because there is not U-B color available for it.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1457fig8.eps}\end{figure}$ Figure 8: F([O III] $\lambda$ 5007) versus W (H $\beta$ ). Models by Stasinska et al. (2001). Tracks correspond to sequences of different metallicities and electronic densities. Each symbol marks the position of the models at 1 Myr interval, starting in the upper-right corner of the diagram with an age of 1 Myr.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1457fig9a.eps}\vspace*{4mm} \includegraphics[width=8.6cm,clip]{1457fig9b.eps}\end{figure}$ Figure 9: Surface brightness and B, V and R color profiles for Mkn 1087 ( up) and KPG 103a ( down). The line in the surface brightness diagrams is an exponential law fitting to the B profile. The dotted horizontal line in the color profile diagrams indicates the average color derived for each system.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1457fig10.eps}\end{figure}$ Figure 10: Surface brightness and color profiles for the north companion object and knot #3. We follow the same notation than in Fig. 9. Note that knot #3 has not an underlying component.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1457fig11.eps}\end{figure}$ Figure 11: Emission line ratios of knots in Mkn 1087. The solid lines give the limit for ionization by a zero age starburst, following Dopita et al. (2000).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1457fig12.eps}\end{figure}$ Figure 12: Relation between metallicity and distance from the nucleus of Mkn 1087 for all the observed knots. We have considered the oxygen abundances derived using the calibration by Pilyugin (2001).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1457fig13.eps}\end{figure}$ Figure 13: Luminosity-metallicity relation for the observed detached bursts in Mkn 1087 and knot #7. The solid line is the relation for dwarf irregulars found by Richer & McCall (1995), while the dashed line is an extrapolation of it. We have considered the oxygen abundances derived using the calibration by Pilyugin (2001).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=13cm,clip]{1457fig1.eps}\end{figure}$	Figure 1: Deep optical image of Mkn 1087 and its surrounding in R filter. Mkn 1087, KPG 103a, the north companion galaxy (N) and the rest of the surrounding objects are labeled. The background cluster of galaxies is indicated with a circle.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1457fig2.eps}\end{figure}$	Figure 2: Detailed images in R band of Mkn 1087 ( up) and KPG 103a ( bottom). The brightest knots inside both galaxies are labeled, as well as the external objects #2, #3 and #12. A weak plume at the east of KPG 103a, that curves toward the south, is also barely observed (it is indicated by an arrow).
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$\begin{figure} \par\includegraphics[width=15cm,clip]{1457fig5.eps}\end{figure}$	Figure 5: a), b), c) and d): position-velocity diagrams for the four slit positions observed with INT, analysed in 1.6 arcsec bins. The horizontal bars represent the uncertainty of the Gaussian fitting for each point. The location and extension of the different galaxy members are also indicated. North is up in all the diagrams.
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$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1457fig6.eps}\end{figure}$	Figure 6: Position-velocity diagram for the single slit position observed in Mkn 1087 with WHT, analysed in 1.2 arcsec bins. The horizontal bars represent the uncertainty of the Gaussian fitting for each point. The location and extension of the different galaxy members are also indicated. North is up.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1457fig8.eps}\end{figure}$	Figure 8: F([O III] $\lambda$ 5007) versus W (H $\beta$ ). Models by Stasinska et al. (2001). Tracks correspond to sequences of different metallicities and electronic densities. Each symbol marks the position of the models at 1 Myr interval, starting in the upper-right corner of the diagram with an age of 1 Myr.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1457fig9a.eps}\vspace*{4mm} \includegraphics[width=8.6cm,clip]{1457fig9b.eps}\end{figure}$	Figure 9: Surface brightness and B, V and R color profiles for Mkn 1087 ( up) and KPG 103a ( down). The line in the surface brightness diagrams is an exponential law fitting to the B profile. The dotted horizontal line in the color profile diagrams indicates the average color derived for each system.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1457fig10.eps}\end{figure}$	Figure 10: Surface brightness and color profiles for the north companion object and knot #3. We follow the same notation than in Fig. 9. Note that knot #3 has not an underlying component.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1457fig11.eps}\end{figure}$	Figure 11: Emission line ratios of knots in Mkn 1087. The solid lines give the limit for ionization by a zero age starburst, following Dopita et al. (2000).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1457fig12.eps}\end{figure}$	Figure 12: Relation between metallicity and distance from the nucleus of Mkn 1087 for all the observed knots. We have considered the oxygen abundances derived using the calibration by Pilyugin (2001).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1457fig13.eps}\end{figure}$	Figure 13: Luminosity-metallicity relation for the observed detached bursts in Mkn 1087 and knot #7. The solid line is the relation for dwarf irregulars found by Richer & McCall (1995), while the dashed line is an extrapolation of it. We have considered the oxygen abundances derived using the calibration by Pilyugin (2001).
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