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<!-- DOI: 10.1051/0004-6361/200810841 -->

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

<p>

<A NAME="t2"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/24/aa10841-08/table2.html"><span class="bold">Table 2:</span></a>&#160;&#160;
Logarithmic extinction C at  HH<IMG
 WIDTH="10" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img4.png"
 ALT="$\beta $">
and dereddened line intensities 
  on the scale H<IMG
 WIDTH="48" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img13.png"
 ALT="$\beta =100$">.</p>
<p>

<A NAME="t3"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/24/aa10841-08/table3.html"><span class="bold">Table 3:</span></a>&#160;&#160;
Plasma parameters and abundances. The first row for each PN gives
 parameters computed from the nominal values of the observational data. The
 second and third row give the upper and lower limits respectively of these
 parameters. Column&nbsp;(1) gives the PNG number; Col.&nbsp;(2) usual name; Col.&nbsp;(3) electron density deduced from [S&nbsp; <SMALL>II</SMALL>]&nbsp;<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img1.png"
 ALT="$\lambda $">6731/6716; Cols.&nbsp;(4) and&nbsp;(5) 
 electron temperatures from [O&nbsp; <SMALL>III</SMALL>]&nbsp;<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img1.png"
 ALT="$\lambda $">4363/5007 and [N&nbsp; <SMALL>II</SMALL>]&nbsp;<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img1.png"
 ALT="$\lambda $">5755/6584 respectively (the
 value of <IMG
 WIDTH="17" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img3.png"
 ALT="$T_{\rm e}$">(N&nbsp; <SMALL>II</SMALL>) is in parenthesis if <IMG
 WIDTH="17" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img3.png"
 ALT="$T_{\rm e}$">(O&nbsp; <SMALL>III</SMALL>) was chosen
 for all ions). Columns&nbsp;(6) to&nbsp;(12) give the
 He/H, N/H, O/H, Ne/H, S/H, Ar/H, Cl/H ratios, respectively. Column&nbsp;(13) gives the
 logarithmic extinction C at  HH<IMG
 WIDTH="10" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img4.png"
 ALT="$\beta $">
derived from our spectra.
</p>
<p>

<p>
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<tr><td><!-- init Label --><A NAME="oppo_abund">&#160;</A><!-- end Label--><A NAME="2270"></A><A NAME="figure2085"
 HREF="img86.png"><IMG
 WIDTH="195" HEIGHT="251" SRC="Timg86.png"
 ALT="\begin{figure}
\par\includegraphics[width=5.5cm,clip]{0841f21a.eps}\hspace*{2.5m...
...s}\hspace*{2.5mm}
\includegraphics[width=5.5cm,clip]{0841f21l.eps}
\end{figure}"></A><!-- HTML Figure number: 24 --></td>
<td class="img-txt"><span class="bold">Figure 21:</span><p>
The relation of different abundance ratios with ionization parameter
  O<sup>++</sup>/O<sup>+</sup>+O<sup>++</sup> for Galactic bulge PNe: [WR]&nbsp;PNe -
  magenta triangles; WEL&nbsp;PNe - blue squares; VL&nbsp;PNe - 
  green circles; normal PNe - 
  black or grey
  diamonds. Filled symbols mark objects with best quality data. PNe with a
  quality of the derived abundance ratio above the adopted rejection limit
  (i.e. error &gt;0.3&nbsp;dex) are represented with open thin-line symbols.</p></td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=24&DOI=10.1051/0004-6361/200810841" target="DEXTER">Open with DEXTER</a></td></tr>

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<table>
<tr><td><!-- init Label --><A NAME="hepphe_abund">&#160;</A><!-- end Label--><A NAME="2271"></A><A NAME="figure2112"
 HREF="img87.png"><IMG
 WIDTH="195" HEIGHT="242" SRC="Timg87.png"
 ALT="\begin{figure}
\par\includegraphics[width=5.5cm,clip]{0841f22a.eps}\hspace*{2.5m...
...ps}\hspace*{2.5mm}
\includegraphics[width=5.5cm,clip]{0841f22l.eps}
\end{figure}"></A><!-- HTML Figure number: 25 --></td>
<td class="img-txt"><span class="bold">Figure 22:</span><p>
The relation of different abundance ratios with ionization parameter
  He<sup>++</sup>/He<sup>+</sup>+He<sup>++</sup> for Galactic bulge PNe. The same notation as in
  Fig.&nbsp;<a href="/articles/aa/full_html/2009/24/aa10841-08/aa10841-08.html#oppo_abund">21</a>.</p></td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=25&DOI=10.1051/0004-6361/200810841" target="DEXTER">Open with DEXTER</a></td></tr>

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