\begin{table}%t7
\caption{Os I lines previously observed in the Sun and the stars. Lines between parentheses turn out to be unsuitable for Os abundance determination, because they are either too weak or heavily blended in the sun or in metal-poor stars.}\label{table:fulloslines}
%\centerline
{
\begin{tabular}{c c c cccp{6cm}}
\hline\hline
$\lambda_{\rm air}$ (nm)&  \multicolumn{2}{c}{$\log gf$}  &     &Object &Ref.     & Remark\\
\cline{2-4}
&This work&Previous &Ref.&  &&\\
\hline
283.8622    &   $-$0.02&     0.11&    a, b&     Metal-poor stars&        (1, 2)  &     \\
301.8036 &  $-$0.79 &  $-$0.72 &a, b& Metal-poor stars &(2)& In the wing of a strong line\\
&&&&Sun& & In the wing of the strong lines Fe I 302.0491, 302.0639 and 302.1073~nm. Unidentified feature at 301.8025~nm\\
305.8660 &  $-$0.41&  $-$0.43, $-$0.45&   b, c&    Metal-poor stars  &(1, 2, 5, 6)    &In wing of stronger unidentified line at  305.8706~nm\\
&&&&Sun&(3) &In wing of the strong Fe I 305.9054~nm and an unidentified line at 305.8706~nm \\
326.7945 &  $-$1.09&  $-$1.08   &b  &Metal-poor stars & (2, 5, 6) &\\
&&&&Sun&(3, 8) & Blend with too strong Fe I 326.7992~nm (Fig.~\ref{FigOsSun}a)\\
326.9204 &  $-$1.00   &  $-$1.070  &c  &Metal-poor stars & (5) & \\
&&&&Sun&  & Very weak, in the wing of Fe I 426.9232~nm\\
330.1559&   $-$0.74 & $-$0.75, $-$0.743    &b, c    &Metal-poor stars  &    (2, 5, 6, 8)   &(Fig.~\ref{FigCH}) \\
&&&&Sun&(3, 8)& Clean line (Fig.~\ref{FigOsSun}b)\\
350.4662 &  $-$     & $-$1.636  &c  &Metal-poor stars & (5) &\\
&&&&Sun&  & Strong unidentified features (e.g. 350.468~nm)\\
352.8602 &  $-$     & $-$1.740  &c  &Metal-poor stars & (5, 6)   &\\
&&&&Sun&  & Bad fit of the synthetic spectrum\\
(375.2524)  &$-$0.98& $-$0.99&  b&  Sun&    (3) &Nd II at 375.249 is the principal contributor to the feature\\
(397.7231)  &  $-$1.94&   $-$1.59, $-$1.77 &b, c&   Sun     &(3)&   Very weak solar line ($W_{\lambda}$ = 0.7 m\AA), blend with Fe I 397.7166~nm and Co I 397.7177~nm \\
(409.1817)   &  $-$   &$-$1.66& b&  Sun &   (3)&    Very weak solar line ($W_{\lambda}$ = 0.6 m\AA) \\
(413.5774)  &$-$1.24& $-$1.26, $-$1.35 &a, b, c& Metal-poor stars    &(4, 5, 7)&   Blend with Zr I (413.5656), Fe I (413.5755), Sm II (413.5142); this line yields a 0.4 dex too high Os abundance in CS 31082-001 (Ivarsson et~al. \cite{Ivars03}) \\
&&&&Sun& & idem\\
426.0848    &$-$1.43  &$-$1.44, $-$1.47    &a, b, c &    Metal-poor stars&   (4, 5, 7)&    \\
&&&&Sun& & In the wing of FeI (426.0486) and an unidentified line \\
442.0468&   $-$1.20 & $-$1.53   &b  &Metal-poor stars   &(4)    & Very high resolution is necessary to disentangle from SmII (442.0526); this line yields a 0.3 dex too high Os abundance in CS 31082-001 (Ivarsson et~al. \cite{Ivars03})  \\
&&&&Sun&(3, 8) & Separation from SmII (442.0526) is sufficient to constrain the abundance (Fig.~\ref{FigOsSun}c) \\
(455.0410)    &      $-$& $-$0.71   &b& Sun     &(3)&   Very weak  solar line ($W_{\lambda}$ = 0.4 m\AA) \\
(463.1828)  &   $-$   &$-$1.19& b&  Sun     &(3)&   Very weak  solar line ($W_{\lambda}$ = 0.1 m\AA)\\
\hline        
\end{tabular}}
\medskip
a: Corliss \& Bozman (\cite{Corli62})
b: Kwiatkowski et~al. (\cite{Kwiat84})
c: Ivarsson et~al. (\cite{Ivars03}). \\
(1) Sneden et~al. (\cite{Sned98});
(2) Cowan et~al. (\cite{Cowa02});
(3) Kwiatkowski et~al. (\cite{Kwiat84});
(4) Sneden et~al. (\cite{Sned96});
(5) Ivarsson et~al. (\cite{Ivars03});
(6) Sneden et~al. (\cite{Sned03});
(7) Hill et~al. (\cite{Hil02});
(8) This work.
\end{table}