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Home All issues Volume 500 / No 3 (June IV 2009) A&A, 500 3 (2009) 1143-1155 Full HTML
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Table 2:

The measured equivalent widths $W_{\lambda }$ (in mÅ) for the C  I  and O  I  features detected in the 15 newly observed halo stars used in this study, together with the S/N near the features of interest.
  C  I C  I C  I C  I C  I C  I   C  I   O  I O  I O  I  
  $\lambda 9061.4$ $\lambda 9062.5$ $\lambda 9078.3$ $\lambda 9088.5$a $\lambda 9094.8$ $\lambda 9111.8$ S/N $\lambda 9405.7$ S/N $\lambda 7771.9$ $\lambda 7774.2$ $\lambda 7775.4$ S/N
$\chi_{\rm exc}$ [eV] 7.48 7.48 7.48 7.48 7.49 7.49   7.69   9.15 9.15 9.15  
log(gf) -0.35 -0.46 -0.58 -0.43 0.15 -0.30   0.29   0.37 0.22 0.00  
ID                          
UVES (2004)                          
CD-24 17504 - - - - 9.5 - 150 10.5 80 1.7b - - 400
CD-71 1234 10.3 - 5.6 13.3 - 11.4 140 23.6 150 8.6 8.0 6.3 160
CS 22943-0095 16.0 16.3 11.0 14.7 48.8 21.7 70 46.3 70 18.4 14.1 9.8 230
G004-037 10.8 6.9 3.8 7.2 26.0 14.1 150 27.5 110 12.4 9.5 5.9 300
G048-029c 8.0 5.9 3.6 3.2 18.2 8.6 200 20.8 100 10.9 5.7 2.5 200
G059-027 27.5 21.6 18.1 22.6 55.9 31.4 150 59.7 70 25.1 20.9 14.9 170
G126-052 13.0 12.4 6.7 13.5 40.2 17.2 150 42.3 150 16.6 9.4 6.9 240
G166-054 6.6 - - - 14.5 7.9 170 - 110 8.0 6.8 4.0 200
HD 84937 17.3 12.7 17.6 15.3 44.0 22.5 220 48.1 170 19.1 14.0 8.9 170
HD 338529 18.0 13.0 - 12.9 48.7 - 220 43.0 150 19.6 12.6 9.2 400
LP635-014 10.8 10.3 11.8 11.8 35.1 17.5 300 38.0 220 14.3 8.0 5.8 230
LP651-004 7.6 6.7 5.1 3.6 16.7 9.1 115 22.4 120 10.3 9.4 5.1 250
MIKE (2003)                          
G041-041 - - - - 18.1 - 80 - 40 7.7d 5.2d 3.3d 250
G048-029c - - - - 19.6 10.3 200 - 40 7.7 4.8 4.5 360
G084-029 - - - 7.1 17.1 - 130 - 40 8.4d 5.8d 3.7d 500
LP831-070 - - - - <8.0 <3.0 130 - 40 <2.0 <2.0 - 380
a Where this C  I  feature was detected, blending with Fe  I  was taken into account in the equivalent width determination. b The oxygen abundance derived with this measurement was confirmed for this star also via synthetic spectrum fitting, as described in the text. c This star was observed in both UVES (2004) and MIKE (2003) runs. d Since equivalent widths for the O  I  IR triplet were measured for these stars also in the 6Li program (Asplund et al. 2006), with typical ${\it S/N}\sim 400$ at the relevant wavelengths, a weighted mean of the determinations was used.


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