Table 1
Spectrographs implemented in this study.
| Spectrograph | Observatory | Spectral res. | vrad | Δλ | N⋆ | Nsp |
|---|---|---|---|---|---|---|
| R = λ∕dλ | precision (a) | |||||
| (m s−1) | ||||||
| HARPS | ESO La Silla, 3.6 m telescope | ~115 000 (b) | 0.5 | Green | 36 | 429 |
| FEROS | ESO La Silla, 2.2 m telescope | ~48 000 | 21 | Green, red | 25 | 93 |
| UVES | ESO VLT, UT2 (c) 8 m telescope | ~70 000 | 25 | Blue, red | 24 | 2331 |
| CORALIE | La Silla (d), Euler 1.2 m telescope | ~55 000 | 3 | Green | 22 | 483 |
| SOPHIE | OHP (e), 1.93 m telescope | ~75 000 (b) | 5 | Green | 30 | 370 |
| HARPS-North | Roque (f), TNG (g) 3.6 m telescope | ~115 000 | 0.5 | Green | 1 | 103 |
| HERMES | Roque (f), Mercator 1.2 m telescope | ~85 000 | 2.5 | Green, red | 3 | 110 |
Notes. Column 3 gives the spectral resolution R and Col. 4 the instrumental (systematic)vrad uncertainty. Column 5 gives the wavelength range(s) Δλ on which westandardised and reduced the spectra (see text). Columns 6 and 7 give the number of observed Cepheids N⋆ and the total number of acquired spectra Nsp for each instrument. (a)According to the literature. (b)When used in high-resolution mode. (c)Unitary Telescope 2 (Kueyen) at ESO Very Large Telescope Observatory (Cerro Paranal, Chile). (d) Swiss Observatory at Cerro La Silla, Chile. (e) Observatoire de Haute-Provence, France. (f) Observatorio del Roque de los Muchachos, La Palma, Canary Islands. (g)Telescopio Nazionale Galileo.
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