Table 15
Overview of the WG13 nodes.
| Node | Teff range | Technique | Parameters determined | Abundances | # spectra |
|---|---|---|---|---|---|
| ROBGrid | 3000 – 50 000 K | χ2 minimisation with grid Of theoretical spectra | Teff, log ɡ, [M/H], vrad, v sin i(a) | − | 8667 |
| ROB | 6000 – 12000 K | Fe−Fe+ ionisation balance Of diagnostic photospheric lines | Teff, log ɡ, [Fe/H], ξ, v sin i(a) | C, O, Mg, Al, Sc, Fe | 517 |
| MGNDU | 5000 – 15 000 K | PCA and SIR | Teff, log ɡ, [M/H], vrad, v sin i | − | 186 |
| Liège | 10 000 – 32000 K | χ2 minimisation with grid | Teff, log ɡ, vrad, v sin i(a) | He, C, N, Ne, Mg, Si | 696 |
| ON | 14000 – 33 000K | Non-LTE synthesis and Si ionisation balance | Teff, log ɡ, v sin i(a) | C, O, Si | 184 |
| IAC | 22000 – 55 000K | χ2 minimisation with grid of FASTWIND models | Teff, log ɡ, v sin i, vmacro | He | 268 |
| Mntp | 30 000 – 45 000 K | χ2 minimisation with grid of CMFGEN models | Teff, log ɡ, v sin i, vmacro | − | 55 |
| LiègeO | 20 000 – 45 000 K | CMFGEN | Teff, log ɡ v sin i, vmacro | He, C, N | 293 |
Notes. Listed are the effective temperature range covered by the node, the spectral analysis technique used, the stellar parameters that are determined, the elements for which abundances are determined, and the number of spectra processed. (a)What is listed here as v sin i is actually the total line-broadening parameter, which can include other effects, such as macroturbulence.
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.