Gaia FGK benchmark stars: opening the black box of stellar element abundance determination

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Table 6

Summary of tests and uncertainties.

Test	Expected σ	Max σ	Min σ	Comment
	dex	dex	dex

1. Line list	0.05	0.6	0.0	EWs are not affected by position of core of line
				but number of HFS components might be important

2. Continuum	0.3	0.6	0.05	Absolute abundance is very dependent
				but methods should not re-normalise

3. HFS	0.08	0.4	0.0	Differences in abundances between HFS:N and
				HFS:Y are similar for all methods

4. v_mic	0.2	1.2	0.01	Maximum difference corresponds to 1 km s^-1 range in v_mic,
				dependency decreases when HFS is considered.

5. α-enhancement	0.02	0.1	0.001	Cool stars are more affected than
				metal-poor warm stars.

6. Atmosphere model interpolation	0.01	0.04	0.002	Obtained from models with 1% difference in
				temperature and 5–10% difference in gas pressure.

7. Blends	0.02	0.1	0.0	Maximum difference is found for
				EW methods for cool dwarf star.

8.1. Same EWs	0.02	0.06	0.001	Weak lines are more affected.
8.2. Same syntheses	0.07	0.12	0.001	Convolution is more important than the choice of mask.

Notes. For each test, we list the typical (median) uncertainty obtained from all results in a given test (expected σ), as well as the maximum difference (Max σ) and the minimum difference (Min σ).

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