All Tables

Table 1: Details of the absorption lines included in the atomic model used after converged populations were obtained. A total of 11 transitions were treated in detail. Wavelength of absorption line, upper and lower level identification, excitation potential for lower level and oscillator strength are respectively given for each of the transitions included.
Table 2: The IDs, atmospheric parameters (effective temperature, gravity and iron content) and the LTE abundances for oxygen and carbon for the sample of low-metallicity stars from Akerman et al. (2004) are shown in Cols. 1, 2, 3, 4, 5 and 7 respectively. The corresponding LTE [C/O] values are in Col. 10. Our adopted non-LTE abundance corrections for oxygen and carbon (obtained when neglecting collisions with H I atoms) and the resulting [O/H] and [C/O] non-LTE abundance ratios from this study are shown in Cols. 6, 8, 9 and 11 respectively. All values from the Akerman et al. study have been corrected, where appropriate, for our different choice of the carbon and oxygen solar abundances ( $\log\epsilon_{\rm C_\odot}=8.39$ and $\log\epsilon_{\rm O_\odot}=8.66$ ).