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<!-- DOI: 10.1051/0004-6361/201015071 -->

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<td class="img-txt"><span class="bold">Figure 2:</span><p>
Larger version of Fig.&nbsp;<a href="/articles/aa/full_html/2010/13/aa15071-10/aa15071-10.html#fig:spec">2</a>.  <EM> Top</EM>: HIFI spectral scan of Orion KL in Band 4b. <EM> Bottom</EM>:
HIFI spectral scan of Orion KL in Band 1a. Strong lines in both spectra
are identified. At the bottom of each panel we give the continuum level
seen in the data at the ends of the bands. We made use of the myXCLASS
program (<a href="http://www.astro.uni-koeln.de/projects/schilke/XCLASS" TARGET="_blank">http://www.astro.uni-koeln.de/projects/schilke/XCLASS</a>) which accesses
  the CDMS (<a name="tex2html34" href="/articles/aa/full_html/2010/13/aa15071-10/aa15071-10.html#muller05">M&#xfc;ller et&nbsp;al.  2005</a>,<a name="tex2html35" href="/articles/aa/full_html/2010/13/aa15071-10/aa15071-10.html#muller01">2001</a>, <a href="http://www.cdms.de" TARGET="_blank">http://www.cdms.de</a>) and JPL
  (<a href="/articles/aa/full_html/2010/13/aa15071-10/aa15071-10.html#pickett98">Pickett et&nbsp;al.  1998</a>, <a href="http://spec.jpl.nasa.gov" TARGET="_blank">http://spec.jpl.nasa.gov</a>) molecular data bases for line assignment.
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