Table 6: Literature data about high-resolution spectroscopic studies of clusters that have more than one high-resolution entry. Errors refer to the rms dispersion between stellar values, or half of the full spread when only two or three stars are studied. From Cols. 1 to 8 we indicate the abundance measurements. In Col. 9, the number of stars used is given; in Col. 10, the reference, in Cols. 11 and 12, we indicate, respectively, the spectral resolution and the instrument and/or the observatory.
[Fe/H] [O/Fe] [Al/Fe] [Ni/Fe] [Na/Fe] [Si/Fe] [Ca/Fe] [Ti/Fe] N Ref. R Instr/OBS
IC 4651
0.12 $\pm $ 0.05 - -0.10 $\pm $ 0.06 -0.02 $\pm $ 0.08 -0.03 $\pm $ 0.07 -0.02 $\pm $ 0.05 0.04 $\pm $ 0.06 -0.02 $\pm $ 0.07 4 1 100 K UVES/VLT
0.11 $\pm $ 0.01 - - - - - - - 5 4 48 K FEROS/1.5 m
0.10 $\pm $ 0.03 - 0.01 $\pm $ 0.07 0.05 $\pm $ 0.05 0.02 $\pm $ 0.16 0.07 $\pm $ 0.03 0.02 $\pm $ 0.04 0.09 $\pm $ 0.04 22 10 100 K UVES/VLT
 
Praesepe
0.27 $\pm $ 0.10 -0.4 $\pm $ 0.2 -0.05 $\pm $ 0.12 -0.02 $\pm $ 0.10 -0.04 $\pm $ 0.12 -0.01 $\pm $ 0.12 0.00 $\pm $ 0.11 -0.04 $\pm $ 0.12 7 1 100 K UVES/VLT
0.04 $\pm $ 0.04 - - - - - - - 7 7 60 & 30 K CFHT & Hale
0.11 $\pm $ 0.03 - - - - - - - 4 2 55 K MIKE/MagCl
 
M 67
0.03 $\pm $ 0.04 -0.07 $\pm $ 0.08 -0.03 $\pm $ 0.11 -0.02 $\pm $ 0.07 -0.02 $\pm $ 0.07 -0.03 $\pm $ 0.06 0.03 $\pm $ 0.07 -0.02 $\pm $ 0.11 6 1 100 K UVES/VLT
0.02 $\pm $ 0.14 0.07 $\pm $ 0.03 0.17 $\pm $ 0.05 0.08 $\pm $ 0.10 0.30 $\pm $ 0.10 0.09 $\pm $ 0.11 0.07 $\pm $ 0.06 0.12 $\pm $ 0.07 3 14 28 K KPNO & CTIO
0.03 $\pm $ 0.03 0.01 $\pm $ 0.03 -0.05 $\pm $ 0.04 -0.02 $\pm $ 0.04 0.05 $\pm $ 0.07 0.02 $\pm $ 0.04 0.05 $\pm $ 0.04 -0.02 $\pm $ 0.04 10 11 45 K UVES/VLT
-0.03 $\pm $ 0.03 0.02 $\pm $ 0.04 0.14 $\pm $ 0.06 0.04 $\pm $ 0.06 0.19 $\pm $ 0.07 0.10 $\pm $ 0.04 0.04 $\pm $ 0.08 0.04 $\pm $ 0.10 12 13 60 & 30 K SOFIN/NOT
0.02 $\pm $ 0.12 - - - - - - - 3 7 60 K CFHT
-0.04 $\pm $ 0.12 - - - - - - - 8 9 34 K KPNO
 
Collinder 261
-0.03 $\pm $ 0.03 -0.2 $\pm $ 0.1 0.12 $\pm $ 0.08 0.06 $\pm $ 0.08 0.33 $\pm $ 0.06 0.24 $\pm $ 0.05 0.01 $\pm $ 0.05 -0.12 $\pm $ 0.09 6 5 48 K FEROS/1.5 m
-0.22 $\pm $ 0.11 -0.1  $\pm $ 0.15 0.39 $\pm $ 0.12 0.02 $\pm $ 0.04 0.48 $\pm $ 0.22 0.22 $\pm $ 0.09 -0.04 $\pm $ 0.10 -0.07 $\pm $ 0.09 7 8 25 K CTIO
 
Be 29
-0.54 $\pm $ 0.02 0.23 $\pm $ 0.03 0.26 $\pm $ 0.01 -0.02 $\pm $ 0.02 0.36 $\pm $ 0.01 0.18 $\pm $ 0.02 0.02 $\pm $ 0.02 0.33 $\pm $ 0.04 2 14 28 K KPNO & CTIO
-0.44 $\pm $ 0.18 0.18 $\pm $ 0.02 0.20 $\pm $ 0.03 0.11 $\pm $ 0.06 0.39 $\pm $ 0.08 0.22 $\pm $ 0.03 0.10 $\pm $ 0.06 0.02 $\pm $ 0.01 2 3 34 K HIRES/KECK
 
NGC 6253
0.46 $\pm $ 0.03 -0.18 $\pm $ 0.06 -0.08 $\pm $ 0.12 -0.05 $\pm $ 0.01 0.21 $\pm $ 0.02 0.09 $\pm $ 0.06 -0.02 $\pm $ 0.12 -0.19 $\pm $ 0.10 4 6 43 K UVES/VLT
0.36 $\pm $ 0.07 - - 0.08 $\pm $ 0.07 - 0.02 $\pm $ 0.08 -0.04 $\pm $ 0.12 -0.01 $\pm $ 0.14 5 12 47 K UVES/VLT
References: (1) Present study; (2) An et al. (2007); (3) Carraro et al. (2004); (4) Carretta et al. (2004); (5) Carretta et al. (2005); (6) Carretta et al. (2007); (7) Friel & Boesgaard (1992); (8) Friel et al. (2003); (9) Hobbs & Thorburn (1991); (10) Pasquini et al. (2004); (11) Randich et al. (2006); (12) Sestito et al. (2007); (13) Tautvaisiene et al. (2000); (14) Yong et al. (2005).


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