FORS2/VLT survey of Milky Way globular clusters - II. Fe and Mg abundances of 51 Milky Way globular clusters on a homogeneous scale

B. Dias; B. Barbuy; I. Saviane; E. V. Held; G. S. Da Costa; S. Ortolani; M. Gullieuszik; S. Vásquez

doi:10.1051/0004-6361/201526765

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Volume 590 (June 2016)

A&A, 590 (2016) A9

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Table 3

Summary of the properties of the current and previous metallicity scales.

Scale	Total	Avg. stars	λλ	R	[Fe/H]	Common	σ	r ²	Polyn.
	clusters	per cluster	(nm)		range	clusters			order

This work	51	16	456–586	2000	[–2.4, 0.0]	–	–	–	–

Carretta et al. (2009a)	19	100	560–680	20 000–40 000	[–2.4, –0.4]	13	0.07	0.99	1
Zinn & West (1984)	56¹	–⁽¹⁾	360–570	775	[–2.4, –0.1]	19	0.18	0.93	2
Rutledge et al. (1997)	52	19	725–900	2000	[–2.3, –0.1]	17	0.13	0.97	2
Kraft & Ivans (2003)	11+5²	13	614–652	45 000–60 000	[–2.3, –0.7]	10	0.11	0.94	1
Saviane et al. (2012a)	14+20³	19	770–950	2440	[–2.3, –0.1]	14	0.12	0.97	2

Notes.The fit parameters of previous metallicity scales against ours are presented. We also give the characteristics of our metallicity scale for comparison.

⁽¹⁾

They observed integrated spectra of 60 clusters; however, their Table 5 only presents metallicities for 56 objects.

⁽²⁾

They analysed spectra of different sources.

⁽³⁾

Observations and analysis are homogeneous, and 14 clusters were used for calibration.

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