Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682)

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Volume 511 (February 2010)

A&A, 511 (2010) A56

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Table 11:

Literature abundance determinations for M 67 based on high resolution spectroscopy.
	Here	T00^a	S00^b	Y05^c	R06^d	P08^e	S09^f
$R=\lambda/\delta\lambda$	30 000	30-60 000	30 000	28 000	45 000	100 000	50 000
S/N	50-100	$\geq$ 100	40-70	30-100	90-180	$\simeq$ 80	100-300
[Fe/H]	+0.05 $\pm$ 0.02( $\pm$ 0.10)	-0.03 $\pm$ 0.04	-0.05 $\pm$ 0.01	+0.02 $\pm$ 0.01	+0.03 $\pm$ 0.01	+0.03 $\pm$ 0.04	0.00 $\pm$ 0.01
[Al/Fe]	+0.03 $\pm$ 0.02( $\pm$ 0.05)	+0.14 $\pm$ 0.07	-	+0.17 $\pm$ 0.01	-0.06 $\pm$ 0.04	-0.03 $\pm$ 0.11	-
[Ba/Fe]	+0.25 $\pm$ 0.02( $\pm$ 0.06)	+0.07 $\pm$ 0.12	+0.21 $\pm$ 0.20	-0.02 $\pm$ 0.03	-	-	-
[Ca/Fe]	-0.16 $\pm$ 0.03( $\pm$ 0.03)	+0.05 $\pm$ 0.09	-0.02 $\pm$ 0.03	+0.07 $\pm$ 0.02	+0.05 $\pm$ 0.04	+0.03 $\pm$ 0.07	-
[Co/Fe]	+0.08 $\pm$ 0.06( $\pm$ 0.06)	+0.08 $\pm$ 0.07	-	-	-	-	-
[Cr/Fe]	+0.01 $\pm$ 0.03( $\pm$ 0.06)	+0.10 $\pm$ 0.09	-	-	-0.01 $\pm$ 0.04	+0.03 $\pm$ 0.09	-
[La/Fe]	+0.05 $\pm$ 0.06( $\pm$ 0.09)	+0.13 $\pm$ 0.10	-	+0.11 $\pm$ 0.02	-	-	-
[Mg/Fe]	+0.27 $\pm$ 0.04( $\pm$ 0.10)	+0.10 $\pm$ 0.06	-0.11 $\pm$ 0.08	+0.16 $\pm$ 0.02	-0.01 $\pm$ 0.03	-	-
[Na/Fe]	+0.08 $\pm$ 0.09( $\pm$ 0.04)	+0.19 $\pm$ 0.08	-0.05 $\pm$ 0.05	+0.30 $\pm$ 0.03	+0.04 $\pm$ 0.07	-0.02 $\pm$ 0.07	-
[Ni/Fe]	+0.05 $\pm$ 0.01( $\pm$ 0.10)	+0.04 $\pm$ 0.08	+0.04 $\pm$ 0.06	+0.08 $\pm$ 0.02	-0.01 $\pm$ 0.04	-0.02 $\pm$ 0.07	-
[O/Fe]	+0.04 $\pm$ 0.10( $\pm$ 0.03)	+0.02 $\pm$ 0.06	-0.02 $\pm$ 0.08	+0.07 $\pm$ 0.02	-0.04 $\pm$ 0.01	-0.07 $\pm$ 0.09	-
[Sc/Fe]	-0.03 $\pm$ 0.04( $\pm$ 0.08)	+0.10 $\pm$ 0.06	-	-	-	-	-
[Si/Fe]	+0.10 $\pm$ 0.02( $\pm$ 0.07)	+0.10 $\pm$ 0.05	-	+0.09 $\pm$ 0.03	+0.03 $\pm$ 0.04	-0.03 $\pm$ 0.06	-
[Ti/Fe]	-0.04 $\pm$ 0.06( $\pm$ 0.06)	+0.04 $\pm$ 0.13	-	+0.12 $\pm$ 0.02	-0.03 $\pm$ 0.04	-0.02 $\pm$ 0.11	-
[V/Fe]	+0.15 $\pm$ 0.13( $\pm$ 0.14)	+0.15 $\pm$ 0.16	-	-	-	-	-
[Y/Fe]	-0.05 $\pm$ 0.04( $\pm$ 0.12)	+0.01 $\pm$ 0.14	-	-	-	-	-

Notes. ^(a) Tautvaisiene (2000), from 6 red clump stars. ^(b) Shetrone & Sandquist (2000), from 4 turn-off stars (we ignored blue stragglers). ^(c) Yong et al. (2005), from 3 red clump stars. ^(d) Randich et al. (2006), from 8 dwarfs and 2 slightly evolved stars. ^(e) Pace et al. (2008), from 6 main-sequence stars. ^(f) Santos et al. (2009), from 3 red clump giants and 6 dwarfs.

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