Table 2
Stellar libraries used to simulate BP/RP and RVS spectra.
| Name | N | Teff / K | log g / dex | [Fe/H] / dex | Ref. | Notes | ||
|
|
||||||||
| OB stars | 1296 | 15 000−55 000 | 1.75−4.75 | 0.0−0.6 | 1 | TLUSTY code; NLTE, mass loss, vmicro | ||
| Ap/Bp stars | 36 | 7000−16000 | 4.0 | 0.0 | 2 | LLmodels code, chemical peculiarities | ||
| A stars | 1450 | 6000−16 000 | 2.5−4.5 | 0.0 | 3 | LLmodels code, [α/Fe] = 0.0, +0.4 | ||
| MARCS | 1792 | 2800−8000 | −0.5−5.5 | −5.0−1.0 | 4 | Galactic enrichment law for [α/Fe] | ||
| Phoenix | 4575 | 3000−10 000 | −0.5−5.5 | −2.5−0.5 | 5 | ΔTeff = 100 K | ||
| UCD | 2560 | 400−4000 | −0.5−5.5 | −2.5−0.5 | 6 | various dust models | ||
| C stars MARCS | 428 | 4000−8000 | 0.0−5.0 | −5.0−0.0 | 7 | [C/Fe] depends on [Fe/H] | ||
| Be | 174 | 15 000−25 000 | 4.0 | 0.0 | 8 | range of envelope to stellar radius ratios | ||
| WR | 43 | 25 000−51 000 | 2.8−4.0 | 0.0 | 9 | range of mass loss rates | ||
| WD | 187 | 6000−90 000 | 7.0−9.0 | 0.0 | 10 | WDA & WDB | ||
| MARCS NLTE | 33 | 4000−6000 | 4.5−5.5 | 0.0 | 11 | NLTE line profiles | ||
| MARCS RVS | 146 394 | 2800−8000 | −0.5−5.5 | −5.0−1.0 | 12 | variations in individual elements abundances | ||
| 3D models | 13 | 4500−6500 | 2.0−5.0 | −2.0−0.0 | 13 | StaggerCode models and Optim3D code | ||
| SDSS stars | 50 000 | 3750−10 000 | 0.0−5.5 | −2.5−0.5 | 14 | semi-empirical library | ||
| Emission line stars | 1620 | − | − | − | 15 | semi-empirical library (see Sect. 5.4) | ||
Notes. N is the number of spectra in the library. Ap/Bp are peculiar stars; UCD are ultracool dwarfs; WR are Wolf Rayet stars; WD are white dwarfs.
Reference. 1) Bouret et al. (2008); 2) Kochukhov & Shulyak (2008); 3) Shulyak et al. (2004); 4) Gustafsson et al. (2008); 5) Brott & Hauschildt (2005); 6) Allard et al. (2001); 7) Masseron, priv. comm.; 8), 9) Martayan et al. (2008); 10) Castanheira et al. (2006); 11) Korn et al., priv. comm.; 12) Recio-Blanco et al., priv. comm.; 13) Chiavassa et al. (2011); 14) Tsalmantza & Bailer-Jones (2010b); 15) Lobel et al. (2010).
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