Table 4
Overview of the WG13 Nodes.
| Sect. | Node | Teff range | Technique | Parameters determined | Abundances |
|---|---|---|---|---|---|
| 3.2 | ROBGrid | 3000–50 000K | χ2 minimisation with grid of theoretical spectra | Teff, log g, [M/H], υrad, υ sin i (a) | … |
| 3.3 | ROB | 6000–12 000K | Fe - Fe+ ionisation balance of diagnostic photospheric lines | Teff, log g, [Fe/H], ξ, υ sin i (a) | C, O, Mg, Al, Sc, Fe |
| 3.4 | MGNDU | 5000–15 000K | Principal Component Analysis and Sliced Inverse Regression | Teff, log g, [M/H], υrad, υ sin i | … |
| 3.5 | Liège | 10 000–32 000K | χ2 minimisation with grid | Teff, log g, υrad, υ sin i (a) | He, C, N, Ne, Mg, Si |
| 3.6 | ON | 14 000–33 000 K | Non-LTE synthesis and Si ionisation balance | Teff, log g, υ sin i (a) | C, O, Si |
| 3.7 | IAC | 22 000–55 000K | χ2 minimisation with grid of FASTWIND models | Teff, log g, υ sin i, υmacro | He |
| 3.8 | Mntp | 30 000–45 000K | χ2 minimisation with grid of CMFGEN models | Teff, log g, υ sin i, υmacro | … |
| 3.9 | LiègeO | 20 000–45 000K | CMFGEN | Teff, log g, υ sin i, υmacro | He, C, N |
| Node | Atomic data for stellar parameters | Atomic data for abundances |
|---|---|---|
| ROBGrid | Bertone et al. (2008); Munari et al. (2005) Coelho et al. (2005); Palacios et al. (2010) Lanz & Hubeny (2003, 2007) and references therein | … |
| ROB | Kurucz (1992); Castelli & Kurucz (2003) and references therein | Laverick et al. (2019) |
| MGNDU | Kurucz (1992); Castelli & Kurucz (2003) Sbordone et al. (2004) and references therein | Gebran et al. (2016) and references therein |
| Liège | Lanz & Hubeny (2007) and references therein | He, N, Mg and Si: Morel et al. (2006) and references therein; Ne: Morel & Butler (2008); C: Nieva & Przybilla (2008) |
| ON | Hubeny & Lanz (1995, 2017); Bragança et al. (2019) | Bragança et al. (2019) |
| IAC | Puls et al. (2005) and references therein | Puls et al. (2005) and references therein |
| Mntp | CMFGEN website (b) | … |
| LiègeO | CMFGEN website (b) | CMFGEN website (b) |
Notes. For each Node the reference is given to the section describing it. Also listed are the effective temperature range covered by the Node, the spectral analysis technique used, the stellar parameters that are determined, and the elements for which abundances are determined. While the formal limit for WG13 is Teff > 7000 K, some Teff ranges extend to lower temperatures to provide an overlap with the other WGs. The second part of the table lists the references to the atomic data used by each of the Nodes. (a)What is listed here as υ sin i is actually the total line-broadening parameter, which can include other effects, such as macroturbulence. See Sect. 4.2 for further details. (b)http://kookaburra.phyast.pitt.edu/hillier/web/CMFGEN.htm
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