Iron-peak elements Sc, V, Mn, Cu, and Zn in Galactic bulge globular clusters

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Table 5

Sensitivity of abundances to changes of ΔT_eff = 100 K, Δlog g = +0.20, and Δv_t = 0.20 km s⁻¹.

Species	ΔT	Δ log g	Δv_t	(∑ x²)^1∕2([X/Fe]_sp)	(∑ x²)^1∕2([X/Fe])
	(100 K)	(+0.20 dex)	(+0.20 kms⁻¹)		(+0.10 dex)
(1)	(2)	(3)	(4)	(5)	(6)
HP 1 : 2115

ScII	−0.02	+0.10	−0.01	+0.10	+0.10
VI	+0.15	+0.01	−0.01	+0.15	+0.15
MnI	+0.01	+0.01	−0.02	+0.02	+0.03
CuI	+0.10	+0.02	−0.10	+0.14	+0.14
ZnI	−0.05	+0.10	−0.01	+0.12	+0.12

NGC 6528 : I–36

ScII	−0.02	+0.10	−0.05	+0.11	+0.12
VI	+0.05	+0.01	−0.12	+0.13	+0.13
MnI	+0.01	+0.01	−0.10	+0.10	+0.10
CuI	+0.02	+0.01	−0.12	+0.12	+0.12
ZnI	+0.07	+0.07	−0.15	+0.18	+0.19

Notes. Error estimation usually take into account only these three stellar parameters, [X/Fe]_sp, as given in column (5). The error in Δ[Fe/H] = 0.1 dex is added in the last column, warning that this is an over estimation.

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