Table 9: Compilation of high-resolution studies on open clusters. The first panel shows the results of the abundance analyses, while the second one summarises dataset and clusters' properties, showing, in the given order, the number of stars used, the reference (i.e. number in the bibliography and ``PPF'' for the present study; some of the cited references for the abundances are compilations of the results obtained by the same group), the spectral resolution power, the instrument and/or the telescope employed, clusters' Galactocentric distances and ages. The two latter values are flagged with a letter according to the reference used: F for Friel & Janes (1993), B for Bragaglia & Tosi (2006), C for Carraro & Chiosi (1994) and W for the WEBDA database.
Cluster [Fe/H] [O/Fe] [Al/Fe] [Ni/Fe] [Na/Fe] [Si/Fe] [Ca/Fe] [Ti/Fe]
$\alpha$ Per -0.06 $\pm $ 0.05 - - - - - - -
Be 17 -0.10 $\pm $ 0.09 0.00 $\pm $ 0.05 0.25 $\pm $ 0.09 0.02 $\pm $ 0.09 0.37 $\pm $ 0.08 0.30 $\pm $ 0.05 -0.04 $\pm $ 0.03 -0.1 $\pm $ 0.08
Be 20 -0.45 $\pm $ 0.05 0.18 $\pm $ 0.05 0.18 $\pm $ 0.01 -0.02 $\pm $ 0.02 0.2 $\pm $ 0.1 0.05 $\pm $ 0.03 0.08 $\pm $ 0.01 0.38 $\pm $ 0.06
Be 22 -0.32 $\pm $ 0.19 - 0.28 $\pm $ 0.05 0.04 $\pm $ 0.01 0.04 $\pm $ 0.05 -0.04 $\pm $ 0.1 -0.08 $\pm $ 0.02 0.11 $\pm $ 0.1
Be 29 -0.49 $\pm $ 0.05 0.21 $\pm $ 0.02 0.23 $\pm $ 0.03 0.05 $\pm $ 0.06 0.38 $\pm $ 0.01 0.20 $\pm $ 0.02 0.06 $\pm $ 0.04 0.18 $\pm $ 0.16
Be 31 -0.57 $\pm $ 0.23 0.24 $\pm $ 0.08 0.22 $\pm $ 0.13 0.11 $\pm $ 0.12 0.27 $\pm $ 0.10 0.20 $\pm $ 0.14 0.13 $\pm $ 0.05 0.08 $\pm $ 0.09
Be 32 -0.29 $\pm $ 0.04 - 0.11 $\pm $ 0.10 0.00 $\pm $ 0.04 0.12 $\pm $ 0.07 0.12 $\pm $ 0.04 0.07 $\pm $ 0.04 0.02 $\pm $ 0.06
Be 66 -0.48 $\pm $ 0.24 - 0.00 $\pm $ 0.2 0.24 $\pm $ 0.25 0.15 $\pm $ 0.2 - -0.05 $\pm $ 0.2 0.43 $\pm $ 0.2
Blanco 1 0.04 $\pm $ 0.02 0.02 $\pm $ 0.11 - -0.18 $\pm $ 0.01 - -0.09 $\pm $ 0.02 -0.09 $\pm $ 0.02 -0.10 $\pm $ 0.03
Collinder 261 -0.12 $\pm $ 0.09 -0.15 $\pm $ 0.05 0.25 $\pm $ 0.13 0.04 $\pm $ 0.02 0.41 $\pm $ 0.07 0.23 $\pm $ 0.01 -0.01 $\pm $ 0.02 -0.09 $\pm $ 0.02
Coma Ber -0.05 $\pm $ 0.03 - - - - - - -
Hyades 0.13 $\pm $ 0.05 - - - 0.01 $\pm $ 0.09 0.05 $\pm $ 0.05 0.07 $\pm $ 0.07 0.03 $\pm $ 0.05
IC 2391 0.06 $\pm $ 0.06 - - - - - - -
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
IC 4665 -0.03 $\pm $ 0.04 - - 0.05 $\pm $ 0.13 - 0.09 $\pm $ 0.19 0.03 $\pm $ 0.14 0.21 $\pm $ 0.17
M 35 -0.21 $\pm $ 0.10 - - - - - - -
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
NGC 188 -0.12 $\pm $ 0.16 - - - - - - -
NGC 2141 -0.18 $\pm $ 0.15 0.00 $\pm $ 0.06 0.18 $\pm $ 0.07 0.04 $\pm $ 0.11 0.41 $\pm $ 0.04 0.05 $\pm $ 0.19 0.10 $\pm $ 0.04 0.24 $\pm $ 0.11
NGC 2324 -0.17 $\pm $ 0.05 - 0.00 $\pm $ 0.08 -0.09 $\pm $ 0.02 0.31 $\pm $ 0.10 0.06 $\pm $ 0.11 0.15 $\pm $ 0.05 -0.08 $\pm $ 0.03
NGC 2477 0.07 $\pm $ 0.03 - -0.01$\pm $0.04 0.00 $\pm $ 0.04 0.12 $\pm $ 0.03 0.05 $\pm $ 0.03 -0.01 $\pm $ 0.01 0.01 $\pm $ 0.06
NGC 2506 -0.20 $\pm $ 0.01 - - - - - - -
NGC 2660 0.04 $\pm $ 0.04 - -0.08 $\pm $ 0.10 -0.03 $\pm $ 0.02 0.12 $\pm $ 0.04 0.00 $\pm $ 0.03 0.04 $\pm $ 0.05 0.00 $\pm $ 0.03
NGC 3680 -0.04 $\pm $ 0.03 0.2  $\pm $ 0.05 -0.08 $\pm $ 0.04 -0.05 $\pm $ 0.03 0.01 $\pm $ 0.08 -0.01 $\pm $ 0.04 0.04 $\pm $ 0.06 0.04 $\pm $ 0.07
NGC 3960 0.02 $\pm $ 0.04 - -0.06 $\pm $ 0.06 -0.01 $\pm $ 0.03 0.09 $\pm $ 0.03 0.04 $\pm $ 0.05 0.02 $\pm $ 0.03 -0.04 $\pm $ 0.02
NGC 6134 0.15 $\pm $ 0.03 - - - - - - -
NGC 6253 0.41 $\pm $ 0.05 -0.18 $\pm $ 0.06 -0.08 $\pm $ 0.12 -0.01 $\pm $ 0.06 0.21 $\pm $ 0.02 0.05 $\pm $ 0.03 -0.03 $\pm $ 0.01 -0.1  $\pm $ 0.1
NGC 6791 0.47 $\pm $ 0.07 -0.31 $\pm $ 0.08 -0.21 $\pm $ 0.09 -0.07 $\pm $ 0.07 0.13 $\pm $ 0.21 -0.01 $\pm $ 0.10 -0.15 $\pm $ 0.08 0.03 $\pm $ 0.09
NGC 6819 0.09 $\pm $ 0.03 - -0.07 $\pm $ 0.07 0.01 $\pm $ 0.02 0.47 $\pm $ 0.07 0.18 $\pm $ 0.04 -0.04 $\pm $ 0.06 -0.01 $\pm $ 0.04
NGC 7789 -0.04 $\pm $ 0.05 -0.07 $\pm $ 0.09 0.18 $\pm $ 0.08 -0.02 $\pm $ 0.05 0.28 $\pm $ 0.07 0.14 $\pm $ 0.05 - -0.03 $\pm $ 0.07
Pleiades -0.03 $\pm $ 0.02 - - - - - - -
Praesepe 0.27 $\pm $ 0.10 -0.4 $\pm $ 0.2 -0.05 $\pm $ 0.12 -0.02 $\pm $ 0.1 -0.04 $\pm $ 0.12 -0.01 $\pm $ 0.12 0.00 $\pm $ 0.11 -0.04 $\pm $ 0.12
Saurer 1 -0.38 $\pm $ 0.14 0.47 $\pm $ 0.13 0.33 $\pm $ 0.02 0.20 $\pm $ 0.05 0.44 $\pm $ 0.05 0.38 $\pm $ 0.1 0.20 $\pm $ 0.04 0.12 $\pm $ 0.12

Cluster N Ref. R Instr/OBS $R_{\rm GC}$ [kpc] Age [Gyr]
$\alpha$ Per 6 9 60 & 30 K CFHT & Hale 8.2 W 0.07 W
Be 17 3 10 25 K KPNO 10.7 W 12 W
Be 20 2 18 28 K KPNO & CTIO 15.9 W 6.0 W
Be 22 2 17 34 K HIRES/KECK 14.02 B 2.40 B
Be 29 See Table 6 20.81 B 3.70 B
Be 31 1 18 28 K KPNO & CTIO 15.8 W 2.0 W
Be 32 9 4, 13 47 K UVES/VLT 11.30 B 6.5 B
Be 66 1 17 34 K HIRES/KECK 12.4 W 5.0 W
Blanco 1 8 8 50 K Anglo/Aus 8.0 W 0.62 W
Collinder 261 See Table 6 6.96 B 6 B
Coma Ber 14 9 60 K CFHT 8.0 W 0.4 W
Hyades 98 12 60 K HIRES/KECK 8.0 W 0.8 W
IC 2391 66 14 50 K FEROS/2.2m MPG-ESO 8.0 W 0.05 W
IC 4651 4 1 100 K UVES/VLT 7.8 L 1.6 C
IC 4665 18 15 60 K HIRES/KECK 7.7 W 0.43 W
M 35 9 2 20 K WIYN/HYDRA 8.91 B 0.18 B
M 67 6 1 100 K UVES/VLT 9.1 F 4.8 C
NGC 188 7 11 34 K KPNO 9.2 W 4.3 W
NGC 2141 1 18 28 K KPNO & CTIO 12.6 F 4 F
NGC 2324 7 4 47 K UVES/VLT 11.4 W 0.4 W
NGC 2477 6 4 47 K UVES/VLT 8.4 W 0.7 W
NGC 2506 2 6 48 K FEROS/1.5m 10.38 B 1.70 B
NGC 2660 5 4, 13 47 K UVES/VLT 8.69 B 0.95 B
NGC 3680 2 1 100 K UVES/VLT 8.3 F 1.8 C
NGC 3960 6 4, 13 47 K UVES/VLT 7.80 B 1.2 B
NGC 6134 6 6 48 K & 43 K FEROS/1.5 m & UVES/VLT 7.2 W 0.93 W
NGC 6253 See Table 6 6.6 B 3 B
NGC 6791 5 7 43 K UVES/VLT 8.4 F 4.4 W
NGC 6819 3 3 40 K SARG/TNG 7.71 B 2 B
NGC 7789 9 16 30 K SOFI/NOT 9.4 F 2 F
Pleiades 13 9 60 & 30 K CFHT & Hale 8.1 W 0.1 W
Praesepe 7 1 100 K UVES/VLT 8.1 W 0.7 W
Saurer 1 2 5 34 K HIRES/KECK 9.7 W 7.1 W
References: (1) Present study; (2) Barrado y Navascués et al. (2001); (3) Bragaglia et al. (2001); (4) Bragaglia et al. (2008); (5) Carraro et al. (2004); (6) Carretta et al. (2004); (7) Carretta et al. (2007); (8) Ford et al. (2005); (9) Friel & Boesgaard (1992); (10) Friel et al. (2005); (11) Hobbs et al. (1990); (12) Paulson et al. (2003); (13) Sestito et al. (2006); (14) Platais et al. (2007); (15) Shen et al. (2005); (16) Tautvaisiene et al. (2005); (17) Villanova et al. (2005); (18) Yong et al. (2005).


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