![\begin{figure}
\par\includegraphics[width=17cm,clip]{Fl222_f1.eps}
\end{figure}](/articles/aa/full/2004/11/aafl222/img5.gif) |
Figure 1:
Observed FUSE spectrum of HD 76534. For the sake of
clarity, the spectrum has been binned by 5 pixels and
smoothed. As expected for a B2.5 star such as HD 76534, the stellar
continuum is detected down to 930 Å. The principal broad
absorption lines of H2 are indicated throughout the
spectrum. Airglow lines are labeled with 
symbol. Note
the presence of the absorption line due to the C III
multiplet UV 4 at 1175 Å. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[angle=90,width=8.4cm,clip]{Fl222_f2.eps}
\end{figure}](/articles/aa/full/2004/11/aafl222/img21.gif) |
Figure 2: Example of fit of H2 lines obtained with the O WENS profile fitting procedure in the observed FUSE spectrum of HD 76534. Stellar continuum: dashed line; Intrinsic line profile: dotted line; Resulting profile: thick line. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par {\includegraphics[width=8.7cm,clip]{Fl222_f3.eps} }
\end{figure}](/articles/aa/full/2004/11/aafl222/img41.gif) |
Figure 3: Excitation diagram for H2 in HD 76534. The slope for the column densities of the low J-levels (J=0-3) is much steeper than for the higher (v=0, J=4-8) levels and vibrationally excited levels. This reveals both cold and warm components with three different kinetic temperatures (see text). |
| Open with DEXTER | |
In the text