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Table 3:

Internal zero-point abundances adopted for our giant stars using MARCS and Kurucz models.

Sun Giants
Specie Literaturea This workb MARCSc Kuruczd
(1) (2) (3) (4) (5)

Fe
7.50,7.45,7.56,7.50 $7.49\pm0.04$ 7.53 7.54
O $_{\rm [O~I]}$ 8.83, 8.73.8.71,8.69 $8.74\pm0.04$ 8.83 8.84
Na 6.33, 6.27, 6.27, 6.24 $6.24\pm0.04$ 6.24 6.24
Mg 7.58, 7.54, 7.58, 7.60 $7.56\pm0.04$ 7.65 7.66
Al 6.47, 6.28, 6.47, 6.45 $6.39\pm0.04$ 6.56 6.56
Si 7.55, 7.62, 7.54, 7.51 $7.54\pm0.03$ 7.60 7.63
Ca 6.36, 6.33, 6.36, 6.34 $6.34\pm0.02$ 6.32 6.30
Ti 5.02, 4.90, 4.92, 4.95 $4.94\pm0.05$ 4.83 4.81

Notes. (a) Solar photospheric abundances from Grevesse & Sauval (1998), Reddy et al. (2003), Bensby et al. (2003, 2004) and Asplund et al. (2009); (b) solar abundances based on our previous work (Meléndez et al. 2006a; Meléndez & Ramírez 2007; Meléndez et al. 2009) using different (e.g. McDonald, Keck, Magellan) solar spectra; (c,d) Our internal zero-points for giants represent the thin-disk abundances at [Fe/H] = 0.0. These zero-points are not absolute abundances and should only be used when both our gf-values and analysis techniques are adopted.


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