The ability of intermediate-band Strömgren photometry to correctly identify dwarf, subgiant, and giant stars and provide stellar metallicities and surface gravities

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Volume 521 (October 2010)

A&A, 521 (2010) A40

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Table 2:

Metallicity calibrations evaluated in Sect. 4.
Reference	(b-y)₀		[Fe/H]		$\langle$ [Fe/H]-[M/H] $\rangle$ $\pm$ $\sigma$	Comment
	min	max	min	max	$\langle$ [Fe/H]-[M/H] $\rangle$ $\pm$ $\sigma$	Comment
Olsen (1984)	0.29	1.00	-2.60	0.39	0.11 $\pm$ 0.34	Their Eq. (15)
	0.514	1.000	-2.60	0.39	0.04 $\pm$ 0.39	Their Eq. (15)
	0.514	1.000	-0.25	0.60	0.02 $\pm$ 0.17	Their Eq. (16)
Schuster & Nissen (1989b)	0.22	0.38	-3.5	0.2	0.06 $\pm$ 0.16	F-type dwarfs
	0.37	0.59	-2.6	0.4	0.06 $\pm$ 0.16	G-type dwarfs
Haywood (2002)	0.22	0.59	-2.0	0.5	0.00 $\pm$ 0.18
Martell & Laughlin (2002)	0.288	0.591	-2.0	0.5	0.05 $\pm$ 0.13
Martell & Smith (2004)	0.288	0.591	-2.0	0.5	0.06 $\pm$ 0.21
Nordström et al. (2004)	0.18	0.38	-2.0	0.8	-0.17 $\pm$ 0.52
	0.44	0.59	-2.0	0.8	0.13 $\pm$ 0.08
Ramírez & Meléndez (2005a)	0.19	0.35	-3.5	0.4	0.04 $\pm$ 0.14	F-type dwarfs
	0.35	0.80	-2.5	0.4	0.04 $\pm$ 0.14	G-type dwarfs
Holmberg et al. (2007)	0.24	0.63	-1.00	0.37	0.08 $\pm$ 0.16
Önehag et al. (2008)	0.22	0.59	-3.5	0.4	0.33 $\pm$ 0.30

Notes. Column 1 lists the reference for the calibration. In Cols. 2 to 5 we quote the ranges, for for (b-y)₀ and [Fe/H], within which the calibrations is valid. Column 6 gives the mean difference between [Fe/H] and [M/H] and the associated $\sigma$ . Column 7 provides additional comments.

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