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<!-- DOI: 10.1051/0004-6361/200809925 -->

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

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<tr><td><!-- init Label --><A NAME="f_spec">&#160;</A><!-- end Label--><A NAME="1911"></A><A NAME="figure727"
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<td class="img-txt"><span class="bold">Figure 1:</span><p>
Comparison of the spectra for a subset of 
nitrogen rich and nitrogen normal LMC stars. The spectral region containing the
N  <SMALL>II</SMALL>&nbsp;3995&nbsp;&#197; line is expanded (<I> left panel</I>) and the line is 
indicated. The spectral type, surface gravity, nitrogen abundance and 
projected rotational velocity of these stars are indicated in the panels.
Other than the strength of the nitrogen lines there are no systematic 
differences between
the spectra of stars of the same spectral type, surface gravity and projected
rotational velocity. </p></td>
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<td class="img-txt"><span class="bold">Figure 1:</span><p>
continued.</p></td>
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<td class="img-txt"><span class="bold">Figure 1:</span><p>
continued.</p></td>
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<A NAME="tab1"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/12/aa09925-08/table1.html"><span class="bold">Table 1:</span></a>&#160;&#160;
Equivalent width measurements and derived abundances for the metal lines observed in the spectra of our sample stars.</p>
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<p>
<A NAME="t_results"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/12/aa09925-08/table2.html"><span class="bold">Table 2:</span></a>&#160;&#160;
Atmospheric parameters, projected rotational velocities and chemical
compositions of the sample.</p>  

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