Table 7: 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.
$\lambda_{{\rm air}}$ (nm) $\log gf$   Object Ref. Remark
  This work Previous Ref.      
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. 6a)
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. 7)
        Sun (3, 8) Clean line (Fig. 6b)
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 mÅ), 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 mÅ)
(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. 2003)
        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. 2003)
        Sun (3, 8) Separation from SmII (442.0526) is sufficient to constrain the abundance (Fig. 6c)
(455.0410) - -0.71 b Sun (3) Very weak solar line ( $W_{\lambda}$ = 0.4 mÅ)
(463.1828) - -1.19 b Sun (3) Very weak solar line ( $W_{\lambda}$ = 0.1 mÅ)
a: Corliss & Bozman (1962) b: Kwiatkowski et al. (1984) c: Ivarsson et al. (2003).
(1) Sneden et al. (1998); (2) Cowan et al. (2002); (3) Kwiatkowski et al. (1984); (4) Sneden et al. (1996); (5) Ivarsson et al. (2003); (6) Sneden et al. (2003); (7) Hill et al. (2002); (8) This work.

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