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<!-- DOI: 10.1051/0004-6361/200912042 -->

<h2 class="sec">Online Material</h2>

<p></p><p><A NAME="observaciones_espectros"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/table1.html"><span class="bold">Table 1:</span></a>&#160;&#160;Journal of the
intermediate-resolution long-slit spectroscopy observations, carried
out using the 2.5&nbsp;m INT, 2.56&nbsp;m NOT and 4.2&nbsp;m WHT
telescopes and with the instrumentation as explained in text.</p>
<p></p><p></p><p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="haro15espectros"></A><!-- end Label--><A NAME="3398"></A><A NAME="figure2551" HREF="img236.png"><IMG SRC="Timg236.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm,clip]{12042f01.eps}
\end{figure}" HEIGHT="68" WIDTH="98"></A><!-- HTML Figure number: 10 -->
</td>
<td class="img-txt"><span class="bold">Figure 1:</span><p>
IDS&nbsp;INT spectra for regions&nbsp;C, A, and&nbsp;B of Haro&nbsp;15.
Fluxes are not corrected for reddening. The most important emission
lines have been labeled. See Fig.&nbsp;3 in Paper&nbsp;I for the
identification of the regions.
</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=10&DOI=10.1051/0004-6361/200912042" target="DEXTER">Open with DEXTER</a></td></tr>

</table></div> 

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<table>
<tr><td><!-- init Label --><A NAME="haro15espectros2"></A><!-- end Label--><A NAME="3399"></A><A NAME="figure2556" HREF="img237.png"><IMG SRC="Timg237.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm,clip]{12042f02.eps}
\end{figure}" HEIGHT="64" WIDTH="97"></A><!-- HTML Figure number: 11 -->
</td>
<td class="img-txt"><span class="bold">Figure 2:</span><p>
<i> Lower panels</i>: zoom of the spectra of regions&nbsp;C (<i> center</i>), A,  and B of Haro&nbsp;15 (<i> bottom</i>). Fluxes are not corrected for  
reddening. <i> Upper panels</i>: spatial distribution of the relative flux of [O  <small>II</small>] <IMG SRC="img5.png" ALT="$\lambda $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">3727 (<i> upper, 
right</i>) and [O  <small>III</small>] <IMG SRC="img5.png" ALT="$\lambda $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">5007 (<i> upper, left</i>) emission lines along the slit of PA 117<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">.
</td>
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</table></div> 

<p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="haro15curvas"></A><!-- end Label--><A NAME="3400"></A><A NAME="figure2572" HREF="img238.png"><IMG SRC="Timg238.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f03.eps}
\end{figure}" HEIGHT="67" WIDTH="98"></A><!-- HTML Figure number: 12 -->
</td>
<td class="img-txt"><span class="bold">Figure 3:</span><p>
Position-velocity diagrams for the two slit positions observed in Haro 15. Both the H<IMG SRC="img4.png" ALT="$\alpha $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">
and the [O  <small>III</small>] <IMG SRC="img5.png" ALT="$\lambda $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">5007
profiles have been analyzed. East is at the top in both diagrams. See
Fig.&nbsp;3 in Paper&nbsp;I for the identification of the regions.
</td>
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<table>
<tr><td><!-- init Label --><A NAME="mkn1199espectros"></A><!-- end Label--><A NAME="3401"></A><A NAME="figure2579" HREF="img239.png"><IMG SRC="Timg239.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f04.eps}
\end{figure}" HEIGHT="47" WIDTH="99"></A><!-- HTML Figure number: 13 -->
</td>
<td class="img-txt"><span class="bold">Figure 4:</span><p>
IDS INT spectra for the center of Mkn 1199 and the dwarf companion
galaxy at its NE. Fluxes are not corrected for reddening. The most
important emission lines have been labeled. See Fig.&nbsp;5 in
Paper&nbsp;I for the identification of the regions.
</td>
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<tr><td><!-- init Label --><A NAME="mkn1199curvas"></A><!-- end Label--><A NAME="3402"></A><A NAME="figure2586" HREF="img240.png"><IMG SRC="Timg240.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f06.eps}
\end{figure}" HEIGHT="66" WIDTH="99"></A><!-- HTML Figure number: 14 -->
</td>
<td class="img-txt"><span class="bold">Figure 6:</span><p>
Position-velocity diagrams for the two slit positions observed in Mkn 1199 using the H<IMG SRC="img4.png" ALT="$\alpha $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">
profiles. NE is up in both diagrams. See Fig.&nbsp;5 in Paper&nbsp;I for the identification of the regions.
</td>
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<table>
<tr><td><!-- init Label --><A NAME="mkn5espectros"></A><!-- end Label--><A NAME="3403"></A><A NAME="figure2591" HREF="img241.png"><IMG SRC="Timg241.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f07.eps}
\end{figure}" HEIGHT="47" WIDTH="99"></A><!-- HTML Figure number: 15 -->
</td>
<td class="img-txt"><span class="bold">Figure 7:</span><p>
Spectra for the region A of Mkn&nbsp;5 obtained using IDS at the INT (PA 
<!-- MATH: $349^{\circ}$ -->
<IMG SRC="img10.png" ALT="$349^{\circ }$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="29">)
and ISIS at the WHT (PA 
<!-- MATH: $354^{\circ}$ -->
<IMG SRC="img11.png" ALT="$354^{\circ }$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="30">).
Fluxes are not corrected for reddening. The most important emission
lines have been labeled. See Fig.&nbsp;7 in Paper&nbsp;I for the
identification of the regions.
</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=15&DOI=10.1051/0004-6361/200912042" target="DEXTER">Open with DEXTER</a></td></tr>

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<tr><td><!-- init Label --><A NAME="mkn5curvas"></A><!-- end Label--><A NAME="3404"></A><A NAME="figure2598" HREF="img242.png"><IMG SRC="Timg242.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm,clip]{12042f08.eps}
\end{figure}" HEIGHT="47" WIDTH="98"></A><!-- HTML Figure number: 16 -->
</td>
<td class="img-txt"><span class="bold">Figure 8:</span><p>
Position-velocity diagrams for the slit positions observed in Mkn&nbsp;5 using the [O  <small>III</small>] <IMG SRC="img5.png" ALT="$\lambda $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">5007 profile. N is up in 
all diagrams. See Fig.&nbsp;7 in Paper&nbsp;I for the identification of the regions.
</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=16&DOI=10.1051/0004-6361/200912042" target="DEXTER">Open with DEXTER</a></td></tr>

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<table>
<tr><td><!-- init Label --><A NAME="iras08208espectros"></A><!-- end Label--><A NAME="3405"></A><A NAME="figure2605" HREF="img243.png"><IMG SRC="Timg243.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f09.eps}
\end{figure}" HEIGHT="49" WIDTH="100"></A><!-- HTML Figure number: 17 -->
</td>
<td class="img-txt"><span class="bold">Figure 9:</span><p>
IDS INT spectra for the center of IRAS 0828+2816 and knot #8. Fluxes
are not corrected for reddening. The most important emission lines have
been labeled. See Fig.&nbsp;9 in Paper&nbsp;I for the identification of
the regions.
</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=17&DOI=10.1051/0004-6361/200912042" target="DEXTER">Open with DEXTER</a></td></tr>

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<table>
<tr><td><!-- init Label --><A NAME="iras08208curvas"></A><!-- end Label--><A NAME="3406"></A><A NAME="figure2610" HREF="img244.png"><IMG SRC="Timg244.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f10.eps}
\end{figure}" HEIGHT="48" WIDTH="99"></A><!-- HTML Figure number: 18 -->
</td>
<td class="img-txt"><span class="bold">Figure 10:</span><p>
Position-velocity diagrams for the three slit positions observed of IRAS 08208+2816 using the [O  <small>III</small>] <IMG SRC="img5.png" ALT="$\lambda $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">5007
profile. N is up in all diagrams. We have included the position of the
regions (see Fig.&nbsp;9 in Paper&nbsp;I for their identification),
emphasizing those analyzed by spectroscopy. Notice that the lacking of
data at the southern edge of the southern tail in the diagrams with
PA&nbsp;345<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
and 355<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
is because of the contamination by a bright star.
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<table>
<tr><td><!-- init Label --><A NAME="pox4curvas"></A><!-- end Label--><A NAME="3407"></A><A NAME="figure2621" HREF="img245.png"><IMG SRC="Timg245.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f12.eps}
\end{figure}" HEIGHT="75" WIDTH="97"></A><!-- HTML Figure number: 19 -->
</td>
<td class="img-txt"><span class="bold">Figure 12:</span><p>
Position-velocity diagram for the slit position observed in POX&nbsp;4 using the [O  <small>III</small>] <IMG SRC="img5.png" ALT="$\lambda $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">5007 profile. NE is up. 
See Fig.&nbsp;11 in Paper&nbsp;I for the identification of the regions.
</td>
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<table>
<tr><td><!-- init Label --><A NAME="um420espectros"></A><!-- end Label--><A NAME="3408"></A><A NAME="figure2628" HREF="img246.png"><IMG SRC="Timg246.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f13.eps}
\end{figure}" HEIGHT="48" WIDTH="98"></A><!-- HTML Figure number: 20 -->
</td>
<td class="img-txt"><span class="bold">Figure 13:</span><p>
ISIS 4.2&nbsp;m WHT spectrum for the center of UM&nbsp;420 (<EM>top</EM>) and the galaxy UGC&nbsp;1809 (<EM>bottom</EM>). Fluxes are not corrected for reddening. The most important emission lines have been labeled.
</td>
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<table>
<tr><td><!-- init Label --><A NAME="um420curvas"></A><!-- end Label--><A NAME="3409"></A><A NAME="figure2637" HREF="img247.png"><IMG SRC="Timg247.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f15.eps}
\end{figure}" HEIGHT="76" WIDTH="98"></A><!-- HTML Figure number: 21 -->
</td>
<td class="img-txt"><span class="bold">Figure 15:</span><p>
Position-velocity diagram for the slit position observed in UM 420 using both the H<IMG SRC="img4.png" ALT="$\alpha $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">
and H<IMG SRC="img1.png" ALT="$\beta $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">
profiles. W is up.
</td>
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<table>
<tr><td><!-- init Label --><A NAME="sbs0926espectros"></A><!-- end Label--><A NAME="3410"></A><A NAME="figure2642" HREF="img248.png"><IMG SRC="Timg248.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f16.eps}
\end{figure}" HEIGHT="47" WIDTH="98"></A><!-- HTML Figure number: 22 -->
</td>
<td class="img-txt"><span class="bold">Figure 16:</span><p>
ISIS 4.2&nbsp;m WHT spectrum for SBS 0926+606&nbsp;A. Fluxes are not
corrected for reddening. The most important emission lines have been
labeled. See Fig.&nbsp;15 in Paper&nbsp;I for the identification of
this region.
</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=22&DOI=10.1051/0004-6361/200912042" target="DEXTER">Open with DEXTER</a></td></tr>

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<table>
<tr><td><!-- init Label --><A NAME="sbs0926curvas"></A><!-- end Label--><A NAME="3411"></A><A NAME="figure2647" HREF="img249.png"><IMG SRC="Timg249.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f17.eps}
\end{figure}" HEIGHT="74" WIDTH="98"></A><!-- HTML Figure number: 23 -->
</td>
<td class="img-txt"><span class="bold">Figure 17:</span><p>
Position-velocity diagram for the slit position with PA&nbsp;14<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
observed in SBS&nbsp;0926+606 using the H<IMG SRC="img4.png" ALT="$\alpha $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">
profile.  Notice that the <i>y</i>-axis is broken. NE is up. See Fig.&nbsp;15 in Paper&nbsp;I for the identification of the regions.
</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=23&DOI=10.1051/0004-6361/200912042" target="DEXTER">Open with DEXTER</a></td></tr>

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<tr><td><!-- init Label --><A NAME="sbs0948espectro"></A><!-- end Label--><A NAME="3412"></A><A NAME="figure2653" HREF="img250.png"><IMG SRC="Timg250.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f18.eps}
\end{figure}" HEIGHT="47" WIDTH="99"></A><!-- HTML Figure number: 24 -->
</td>
<td class="img-txt"><span class="bold">Figure 18:</span><p>
ISIS 4.2&nbsp;m WHT spectrum for SBS 0948+532 using a slit with PA 114<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">.
Fluxes are not corrected for reddening. The most important emission lines have been labeled.
</td>
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<tr><td><!-- init Label --><A NAME="sbs0948curvas"></A><!-- end Label--><A NAME="3413"></A><A NAME="figure2659" HREF="img251.png"><IMG SRC="Timg251.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f19.eps}
\end{figure}" HEIGHT="75" WIDTH="98"></A><!-- HTML Figure number: 25 -->
</td>
<td class="img-txt"><span class="bold">Figure 19:</span><p>
Position-velocity diagram for the slit position with PA 114<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
observed in SBS 0948+532 using the [O  <small>III</small>] <IMG SRC="img5.png" ALT="$\lambda $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">5007 profile. NW is up (see Fig.&nbsp;17 in Paper&nbsp;I).
</td>
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<table>
<tr><td><!-- init Label --><A NAME="sbs1054espectro"></A><!-- end Label--><A NAME="3414"></A><A NAME="figure2667" HREF="img252.png"><IMG SRC="Timg252.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm,clip]{12042f20.eps}
\end{figure}" HEIGHT="26" WIDTH="99"></A><!-- HTML Figure number: 26 -->
</td>
<td class="img-txt"><span class="bold">Figure 20:</span><p>
IDS 2.5&nbsp;m INT spectrum for SBS&nbsp;1054+364 using a slit with PA&nbsp;55<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">.
Fluxes are not corrected for reddening. The most 
important emission lines have been labeled. See Fig.&nbsp;19 in Paper&nbsp;I for identification of the region.
</td>
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<tr><td><!-- init Label --><A NAME="sbs1054curvas"></A><!-- end Label--><A NAME="3415"></A><A NAME="figure2673" HREF="img253.png"><IMG SRC="Timg253.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f21.eps}
\end{figure}" HEIGHT="74" WIDTH="98"></A><!-- HTML Figure number: 27 -->
</td>
<td class="img-txt"><span class="bold">Figure 21:</span><p>
Position-velocity diagram for the slit position observed in SBS&nbsp;1054+365 using the H<IMG SRC="img4.png" ALT="$\alpha $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">
profile. NE is up. See Fig.&nbsp;19 in 
Paper&nbsp;I for identification of the regions.
</td>
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<tr><td><!-- init Label --><A NAME="sbs1211espectros"></A><!-- end Label--><A NAME="3416"></A><A NAME="figure2678" HREF="img254.png"><IMG SRC="Timg254.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f22.eps}
\end{figure}" HEIGHT="47" WIDTH="99"></A><!-- HTML Figure number: 28 -->
</td>
<td class="img-txt"><span class="bold">Figure 22:</span><p>
ISIS 4.2&nbsp;m WHT spectrum for SBS&nbsp;1211+540 using a slit with PA 138<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">.
Fluxes are not corrected for reddening. The most 
important emission lines have been labeled. See Fig.&nbsp;21 in Paper&nbsp;I for identification of the region.
</td>
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<tr><td><!-- init Label --><A NAME="sbs1211curvas"></A><!-- end Label--><A NAME="3417"></A><A NAME="figure2684" HREF="img255.png"><IMG SRC="Timg255.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f23.eps}
\end{figure}" HEIGHT="76" WIDTH="98"></A><!-- HTML Figure number: 29 -->
</td>
<td class="img-txt"><span class="bold">Figure 23:</span><p>
Position-velocity diagram for the slit position with PA&nbsp;138<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
observed in SBS&nbsp;1211+532 using the [O  <small>III</small>] 
<IMG SRC="img5.png" ALT="$\lambda $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">5007 profile. NW is up. See Fig.&nbsp;21 in Paper&nbsp;I for identification of the regions.
</td>
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<tr><td><!-- init Label --><A NAME="sbs1319espectros"></A><!-- end Label--><A NAME="3418"></A><A NAME="figure2692" HREF="img256.png"><IMG SRC="Timg256.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f24.eps}
\end{figure}" HEIGHT="48" WIDTH="100"></A><!-- HTML Figure number: 30 -->
</td>
<td class="img-txt"><span class="bold">Figure 24:</span><p>
ISIS 4.2&nbsp;m WHT spectrum for regions A (<EM>top</EM>) and C (<EM>bottom</EM>) of SBS 1319+579 obtained with a slit with PA&nbsp;49<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">.
Fluxes are not corrected for reddening. The most important emission
lines have been labeled. See Fig.&nbsp;23 in Paper&nbsp;I for
identification of the regions.
</td>
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<tr><td><!-- init Label --><A NAME="sbs1319curvas"></A><!-- end Label--><A NAME="3419"></A><A NAME="figure2700" HREF="img257.png"><IMG SRC="Timg257.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f25.eps}
\end{figure}" HEIGHT="58" WIDTH="98"></A><!-- HTML Figure number: 31 -->
</td>
<td class="img-txt"><span class="bold">Figure 25:</span><p>
Position-velocity diagram for the slit position observed in SBS&nbsp;1319+579 using the H<IMG SRC="img4.png" ALT="$\alpha $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">
profile. The relative intensity of the  H<IMG SRC="img4.png" ALT="$\alpha $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">
emission along the spatial direction is also shown, identifying all
observed regions. NE is up. See Fig.&nbsp;23 in Paper&nbsp;I for
identification of the regions.
</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=31&DOI=10.1051/0004-6361/200912042" target="DEXTER">Open with DEXTER</a></td></tr>

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<p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="sbs1415espectros"></A><!-- end Label--><A NAME="3420"></A><A NAME="figure2705" HREF="img258.png"><IMG SRC="Timg258.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f26.eps}
\end{figure}" HEIGHT="48" WIDTH="100"></A><!-- HTML Figure number: 32 -->
</td>
<td class="img-txt"><span class="bold">Figure 26:</span><p>
ISIS 4.2&nbsp;m WHT spectrum for regions&nbsp;C (<EM>top</EM>) and A (<EM>bottom</EM>) of SBS&nbsp;1415+437 using a slit with PA 20<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">.
Fluxes are not corrected for reddening. The most important emission
lines have been labeled. See Fig.&nbsp;25 in Paper&nbsp;I for
identification of the regions.
</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=32&DOI=10.1051/0004-6361/200912042" target="DEXTER">Open with DEXTER</a></td></tr>

</table></div>
<p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="sbs1415curvas"></A><!-- end Label--><A NAME="3421"></A><A NAME="figure2713" HREF="img259.png"><IMG SRC="Timg259.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f27.eps}
\end{figure}" HEIGHT="74" WIDTH="98"></A><!-- HTML Figure number: 33 -->
</td>
<td class="img-txt"><span class="bold">Figure 27:</span><p>
Position-velocity diagram for the slit position with PA&nbsp;20<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
observed in SBS&nbsp;1415+437 using the H<IMG SRC="img4.png" ALT="$\alpha $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">
profile. NE is up. See Fig.&nbsp;25 in Paper&nbsp;I for identification of the regions.
</td>
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</table></div>
<p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="iiizw107espectros"></A><!-- end Label--><A NAME="3422"></A><A NAME="figure2719" HREF="img260.png"><IMG SRC="Timg260.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f28.eps}
\end{figure}" HEIGHT="47" WIDTH="99"></A><!-- HTML Figure number: 34 -->
</td>
<td class="img-txt"><span class="bold">Figure 28:</span><p>
IDS INT spectra for the regions A (<EM>bottom</EM>) and&nbsp;B (<EM>top</EM>)
of IRAS&nbsp;III&nbsp;Zw&nbsp;107. Fluxes are not corrected for
reddening. The most important emission lines have been labeled. See
Fig.&nbsp;27 in Paper&nbsp;I for identification of the regions.
</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=34&DOI=10.1051/0004-6361/200912042" target="DEXTER">Open with DEXTER</a></td></tr>

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<p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="iiizw107curvas"></A><!-- end Label--><A NAME="3423"></A><A NAME="figure2726" HREF="img261.png"><IMG SRC="Timg261.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f29.eps}
\end{figure}" HEIGHT="74" WIDTH="99"></A><!-- HTML Figure number: 35 -->
</td>
<td class="img-txt"><span class="bold">Figure 29:</span><p>
Position-velocity diagram for the slit position with PA&nbsp;0<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
observed in III&nbsp;Zw&nbsp;107 using the H<IMG SRC="img4.png" ALT="$\alpha $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">
profile. N is up. See Fig.&nbsp;27 in Paper&nbsp;I for identification of the regions.
</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=35&DOI=10.1051/0004-6361/200912042" target="DEXTER">Open with DEXTER</a></td></tr>

</table></div>
<p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="tol9espectros"></A><!-- end Label--><A NAME="3424"></A><A NAME="figure2732" HREF="img262.png"><IMG SRC="Timg262.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f30.eps}
\end{figure}" HEIGHT="49" WIDTH="99"></A><!-- HTML Figure number: 36 -->
</td>
<td class="img-txt"><span class="bold">Figure 30:</span><p>
IDS INT spectrum  (<EM>bottom</EM>) using a slit with PA&nbsp;49<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
and ALFOSC 2.56&nbsp;m NOT spectrum (<EM>top</EM>) using a slit of PA 109<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
of Tol 9. Fluxes are not been corrected for reddening. The most
important emission lines have been labeled. See Figs.&nbsp;29 and 30 in
Paper&nbsp;I for identification of the regions.
</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=36&DOI=10.1051/0004-6361/200912042" target="DEXTER">Open with DEXTER</a></td></tr>

</table></div>
<p></p><p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="tol1457espectros"></A><!-- end Label--><A NAME="3425"></A><A NAME="figure2743" HREF="img263.png"><IMG SRC="Timg263.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f32.eps}
\end{figure}" HEIGHT="69" WIDTH="100"></A><!-- HTML Figure number: 37 -->
</td>
<td class="img-txt"><span class="bold">Figure 32:</span><p>
ALFOSC 2.56&nbsp;m NOT spectra of the regions analyzed in
Tol&nbsp;1457-262. Fluxes are not corrected for reddening. The most
important emission lines have been labeled. See Fig.&nbsp;31 in
Paper&nbsp;I for identification of the regions.
</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=37&DOI=10.1051/0004-6361/200912042" target="DEXTER">Open with DEXTER</a></td></tr>

</table></div>
<p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="tol1457curvas"></A><!-- end Label--><A NAME="3426"></A><A NAME="figure2748" HREF="img264.png"><IMG SRC="Timg264.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f33.eps}
\end{figure}" HEIGHT="59" WIDTH="98"></A><!-- HTML Figure number: 38 -->
</td>
<td class="img-txt"><span class="bold">Figure 33:</span><p>
Position-velocity diagram for the slit position observed in <EM>Object&nbsp;1</EM> of Tol 1457-262 using the H<IMG SRC="img4.png" ALT="$\alpha $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">
profile. The 
relative intensity of the H<IMG SRC="img4.png" ALT="$\alpha $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">
emission along the spatial direction is also shown, identifying all
observed regions. NW is up. See Fig.&nbsp;31 in Paper&nbsp;I for
identification of the regions.
</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=38&DOI=10.1051/0004-6361/200912042" target="DEXTER">Open with DEXTER</a></td></tr>

</table></div>
<p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="eso566espectros"></A><!-- end Label--><A NAME="3427"></A><A NAME="figure2754" HREF="img265.png"><IMG SRC="Timg265.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f34.eps}
\end{figure}" HEIGHT="47" WIDTH="98"></A><!-- HTML Figure number: 39 -->
</td>
<td class="img-txt"><span class="bold">Figure 34:</span><p>
ALFOSC 2.56&nbsp;m NOT spectra for the galaxy pair ESO&nbsp;566-8 (<EM>top</EM>) and ESO&nbsp;566-7 (<EM>bottom</EM>)
that constitute Arp&nbsp;256. Fluxes are not been corrected for
reddening. The most important emission lines have been labeled. See
Fig.&nbsp;34 in Paper&nbsp;I for identification of the galaxies.
</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=39&DOI=10.1051/0004-6361/200912042" target="DEXTER">Open with DEXTER</a></td></tr>

</table></div>
<p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="eso566curvas"></A><!-- end Label--><A NAME="3428"></A><A NAME="figure2761" HREF="img266.png"><IMG SRC="Timg266.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm]{12042f35.eps}
\end{figure}" HEIGHT="74" WIDTH="99"></A><!-- HTML Figure number: 40 -->
</td>
<td class="img-txt"><span class="bold">Figure 35:</span><p>
Position-velocity diagram for the slit position observed in Arp&nbsp;252 using the H<IMG SRC="img4.png" ALT="$\alpha $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">
profile.  Notice that the <i>y</i>-axis is broken  in two parts. N is up. See Fig.&nbsp;34 in Paper&nbsp;I for identification of the galaxies.
</td>
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</table></div>
<p></p><p></p><p></p><h2 class="sec"><a name="SECTION00080000000000000000"></a>
Appendix A: Tables</h2>
<A NAME="haro15lineas"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.1.html"><span class="bold">Table A.1:</span></a>&#160;&#160;
Dereddened line intensity ratios with respect to <i>I</i>(H<IMG SRC="img1.png" ALT="$\beta $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">)&nbsp;=&nbsp;100 for knots analyzed in Haro&nbsp;15.</p>
<p><A NAME="haro15abun"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.2.html"><span class="bold">Table A.2:</span></a>&#160;&#160;
Physical conditions and chemical abundances of the ionized gas of the regions analyzed in Haro&nbsp;15.</p>
<p><A NAME="mkn1199lineas"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.3.html"><span class="bold">Table A.3:</span></a>&#160;&#160;
Dereddened line intensity ratios with respect to <i>I</i>(H<IMG SRC="img1.png" ALT="$\beta $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">)=100 for knots analyzed in Mkn 1199.</p>
<p><A NAME="mkn1199abun"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.4.html"><span class="bold">Table A.4:</span></a>&#160;&#160;
Physical conditions and chemical abundances of the ionized gas of the regions analyzed in Mkn 1199.</p>
<p></p><p><A NAME="mkn5lineas"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.5.html"><span class="bold">Table A.5:</span></a>&#160;&#160;
Dereddened line intensity ratios with respect to <i>I</i>(H<IMG SRC="img1.png" ALT="$\beta $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">)=100 for knots analyzed in Mkn&nbsp;5. Region A was observed using three slit positions with a PA of 0<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
(INT-1), 349<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">&nbsp;=&nbsp;-11<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
(INT-2), and 354<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">&nbsp;=&nbsp;-6<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
(WHT).</p>
<p><A NAME="mkn5abun"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.6.html"><span class="bold">Table A.6:</span></a>&#160;&#160;
Physical conditions and chemical abundances of the ionized gas of the regions analyzed in Mkn 5.</p>
<p><A NAME="iras08208lineas"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.7.html"><span class="bold">Table A.7:</span></a>&#160;&#160;
Dereddened line intensity ratios with respect to <i>I</i>(H<IMG SRC="img1.png" ALT="$\beta $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">)&nbsp;=&nbsp;100 for regions analyzed in IRAS 08208+2816. The slit positions that we used for each knot are: PA&nbsp;345<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
for C, PA 355<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
for #8 and #10, and PA 10<IMG SRC="img3.png" ALT="$^{\circ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="9">
for #3 y #5.</p>
<p><A NAME="iras08208abun"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.8.html"><span class="bold">Table A.8:</span></a>&#160;&#160;
Physical conditions and chemical abundances of the ionized gas of the regions analyzed in IRAS 08208+2816.</p>
<p><A NAME="pox4lineas"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.9.html"><span class="bold">Table A.9:</span></a>&#160;&#160;
Dereddened line intensity ratios with respect to <i>I</i>(H<IMG SRC="img1.png" ALT="$\beta $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">)=100 for regions analyzed in POX&nbsp;4, UM 420, and SBS 0926+606.</p>
<p><A NAME="pox4abun"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.10.html"><span class="bold">Table A.10:</span></a>&#160;&#160;
Physical conditions and chemical abundances of the ionized gas in POX 4, UM 420, and SBS 0926+606.</p>
<p><A NAME="sbs1054lineas"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.11.html"><span class="bold">Table A.11:</span></a>&#160;&#160;
Dereddened line intensity ratios with respect to <i>I</i>(H<IMG SRC="img1.png" ALT="$\beta $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">)&nbsp;=&nbsp;100 for regions analyzed in SBS&nbsp;0948+532, SBS&nbsp;1054+365, and SBS&nbsp;1211+540.</p>
<p><A NAME="sbs1054abun"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.12.html"><span class="bold">Table A.12:</span></a>&#160;&#160;
Physical conditions and chemical abundances of the ionized gas in SBS&nbsp;0948+532, SBS&nbsp;1054+365, and SBS&nbsp;1211+540.</p>
<p><A NAME="a13"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.13.html"><span class="bold">Table A.13:</span></a>&#160;&#160;
Dereddened line intensity ratios with respect to <i>I</i>(H<IMG SRC="img1.png" ALT="$\beta $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">)&nbsp;=&nbsp;100
for knots analyzed in SBS&nbsp;1319+579 (regions&nbsp;A, B, and&nbsp;C)
and SBS&nbsp;1415+457 (regions&nbsp;C and&nbsp;A).</p>
<p><A NAME="sbs1319abun"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.14.html"><span class="bold">Table A.14:</span></a>&#160;&#160;
Physical conditions and chemical abundances of the ionized gas for the regions analyzed in SBS 1319+579 and SBS 1415+437.</p>
<p></p><p><A NAME="iiizw107lineas"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.15.html"><span class="bold">Table A.15:</span></a>&#160;&#160;
Dereddened line intensity ratios with respect to <i>I</i>(H<IMG SRC="img1.png" ALT="$\beta $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">)&nbsp;=&nbsp;100
for knots analyzed in III&nbsp;Zw&nbsp;107 (regions A, B, and C) and
Tol&nbsp;9 (spectra obtained with 2.5&nbsp;m INT and 2.56&nbsp;m NOT).</p>
<p><A NAME="iiizw107abun"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.16.html"><span class="bold">Table A.16:</span></a>&#160;&#160;
Physical conditions and chemical abundances of the ionized gas for the regions analyzed in III&nbsp;Zw&nbsp;107 and Tol&nbsp;9.</p>
<p><A NAME="tol1457lineas"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.17.html"><span class="bold">Table A.17:</span></a>&#160;&#160;
Dereddened line intensity ratios with respect to <i>I</i>(H<IMG SRC="img1.png" ALT="$\beta $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">)&nbsp;=&nbsp;100
for knots analyzed in Tol&nbsp;1457-262 (regions&nbsp;A, B, and&nbsp;C)
and Arp&nbsp;252 (galaxy A, ESO&nbsp;566-8, and galaxy B,
ESO&nbsp;566-7).</p>
<p><A NAME="tol1457abun"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/47/aa12042-09/tableA.18.html"><span class="bold">Table A.18:</span></a>&#160;&#160;
Physical conditions and chemical abundances of the ionized gas for the
regions analyzed in Tol&nbsp;1457-262 and Arp&nbsp;252 (galaxy&nbsp;A,
ESO&nbsp;566-8, and galaxy&nbsp;B, ESO&nbsp;566-7).</p>
<p></p><p></p>

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