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Table 4

Measured abundances for the program stars.

SPM [Fe/H] [C/Fe] [N/Fe] [O/Fe] C/O 12C/13C A(Li) A(Li) A(Li)NLTEa A(Li)NLTEa v sin i
670.8 nm 610.3 nm 670.8 nm 610.3 nm km   s-1

Sun 7.50 8.49 7.95 8.83

142 173  −0.69 +0.02 +0.02 +0.20 +0.30  > 15 2.80 2.52 2.73 2.72 2.2 ± 0.7
171 877  −0.77  −0.23 +0.42 +0.34 +0.12  > 15 2.49 2.29 2.46 2.52  < 1.8
225 245  −0.99  −0.44 +0.54 +0.08 +0.14 8 2.90 2.71 2.83 2.93  < 1.1
313 132 +0.01 +0.07 +0.01  −0.07 +0.63 13 3.45 3.35 3.37 3.56 3.3 ± 0.5
343 555  −0.62 +0.09  −0.08 +0.19 +0.36  > 10 1.79  < 1.94 1.94  < 2.11 2.5 ± 0.8

HD 787b +0.00  −0.24 +0.33 +0.02 0.21 15 2.03 2.14 2.09 2.40
HD 787 +0.04  −0.38 +0.09  −0.22 0.27 15 1.77 2.12 1.98 2.40

Notes. The measured stellar rotational velocities are also indicated.

(a)

NLTE corrections are calculated according to Lind et al. (2009). Owing to the grid boundaries, we assume: ξ = 2.0 km   s-1 for all stars; Teff = 4000 K for #171877, #225245, and HD 787 (2nd instance); log    g = 1.0 for #225245 and HD 787 (2nd instance); [Fe/H] = 0.0 for #313132 and HD 787 (2nd instance).

(b)

Atmospheric parameters are assumed from Castilho et al. (2000); C, N and O abundances are taken from Meléndez et al. (2008). Carbon isotopic ratio is taken from da Silva et al. (1995).

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