Table 1: Literature determinations of atmospheric parameters for $\alpha $ Cen  A and B.
$\alpha $ Centauri A
Reference Atmospheric parameter   Method used
  $T_{\rm eff}$ (K) $\log g$ $\xi _t$ (km s-1) $\rm [Fe/H]$   $T_{\rm eff}$  $\log g$
French & Powell (1971) 5770 - - +0.22   a -
Soderblom (1986) 5770 - - -   b -
England (1980) 5750 4.38 1.0 +0.28   b,c,d c,d
Bessell (1981) 5820 4.25 1.7 -0.01   a,e e
Smith et al. (1986) 5820 4.40 1.54 +0.20   a,e d
Gratton & Sneden (1987) 5750 4.38 1.2 +0.11   f c,e
Abia et al. (1988) 5770 4.5 1.0 +0.22   b f
Edvardsson (1988) - 4.42 - +0.28   - d
Furenlid & Meylan (1990) 5710 4.27 1.0 +0.12   a,e e
Chmielewski et al. (1992) 5800 4.31 - +0.22   b c
Neuforge-Verheecke & Magain (1997) 5830 4.34 1.09 +0.25   a ce
Allende-Prieto et al. (2004) 5519 4.26 1.04 +0.12   f c
Doyle et al. (2005) 5784 4.28 1.08 +0.12   direct direct
Santos et al. (2005) 5844 4.30 1.18 +0.28   a a
del Peloso et al. (2005a) 5813 4.30 1.23 +0.26   b,f c
Valenti & Fischer (2005) 5802 4.33 - +0.23   a e
This work 5824 4.34 1.46 +0.24   a,b,e,f c,e
$\alpha $ Centauri B
Reference Atmospheric parameter   Method used
  $T_{\rm eff}$ (K) $\log g$ $\xi _t$ (km s-1) $\rm [Fe/H]$   $T_{\rm eff}$  $\log g$
French & Powell (1971) 5340 - - +0.12   a -
Soderblom (1986) 5350 - - -   b -
England (1980) 5260 4.73 1.1 +0.38   b,c,e c,e
Bessell (1981) 5350 4.5 1.0 -0.05   a,e e
Smith et al. (1986) 5280 4.65 1.35 +0.20   a,e d
Gratton & Sneden (1987) 5250 4.50 1.0 +0.08   f c,e
Abia et al. (1988) 5300 4.5 1.5 +0.14   b f
Edvardsson (1988) - 4.65 - +0.32   - d
Chmielewski et al. (1992) 5325 4.58 - +0.26   b c
Neuforge-Verheecke & Magain (1997) 5255 4.51 1.00 +0.24   a c,e
Allende-Prieto et al. (2004) 4970 4.59 0.81 +0.18   f c
Santos et al. (2005) 5199 4.37 1.05 +0.19   a a
Valenti & Fischer (2005) 5178 4.56 - +0.22   a e
This work 5223 4.44 1.28 +0.25   a,b,e,f c,e
The notation used from Cols. 6 to 7 stands for: a excitation equilibrium; b wings of Balmer lines; c trigonometric parallax; d wings of strong lines; e ionization equilibrium; f photometric color indexes; direct directly-measured luminosity, mass and radius. Note that, generally, the microturbulence velocities have not the same zero point and cannot be directly compared. Typical errors, respectively, in $T_{\rm eff}$, $\log g$, and [Fe/H] are $\leq$100 K, $\leq$0.2 dex, and $\leq$0.1 dex, but note that these estimates usually do not include systematic uncertainties, and that not all authors provide error determinations, or labor under the same definitions for them.

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