Free Access
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. vmic | 0.2 | 1.2 | 0.01 | Maximum difference corresponds to 1 km s-1 range in vmic, | |
| 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).
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.