Table 1.
Setups used for GIRAFFE and UVES observation of open clusters.
| Setup | λλ | R1 | R2 | No | Stars and clusters on which | Prominent lines and elements |
|---|---|---|---|---|---|---|
| (nm) | fibres | the setup is mainly used | ||||
| UVES | ||||||
| 520 | 414-621 | 47000 | 6 | early type stars | Hγ, β; and see below the case of blue setups | |
| 580 | 476-684 | 47000 | 8 | late type stars | Hα; Fe I, II; Fe-peak; α-el.; Na; [O I]; Al; n-capt.; Li | |
| GIRAFFE | ||||||
| HR03 | 403.3-420.1 | 24800 | 31400 | 130 | early-type st., massive young cl. | Hδ; He I; Si II; IV; O II; [Si II] |
| HR04 | 418.8-439.2 | 24000 | 130 | early-type st., massive young cl. | Hγ; He I; He II; Si IV; N II | |
| HR05a | 434.0-458.7 | 18470 | 20250 | 130 | early-type st., massive young cl. | He I, II, Si III; Mg II; N II; III; O II |
| HR06 | 453.8-475.9 | 20350 | 24300 | 130 | early-type st., massive young cl. | He I, II; Si IV; C III; N II and N III; O II |
| HR09b | 514.3-535.6 | 25900 | 31750 | 130 | early-type st. | Mg b; Fe I, Fe II; Ti II; Cr I, Cr II; S II; Mn II |
| HR14a | 630.8-670.1 | 17740 | 18000 | 130 | early-type st., massive young cl. | Hα; He I, II; Si II; C II; Ti I; Ba II; TiO |
| HR15n | 647.0-679.0 | 17000 | 19200 | 130 | late-type st., all cl. | Hα; He I,II, Li; Fe I; Ca; Si; Mg; Ti I; Ba II; |
| [S II]; [N II]; TiO; CaH | ||||||
Notes. R1, R2 are the resolution before and after the GIRAFFE upgrade in February 2015, respectively (no change for UVES). The HR04 setup was used only after the upgrade. The number of allocated stars are less than the fibres, since some (≥1 for UVES, ≳15 for GIRAFFE) are dedicated to sky positions. We define here stars of O, B, and A spectral type as ‘early’ and stars of F, G, K, and M spectral type as ‘late’. We note that some A-type stars have been observed using UVES 580. For a few clusters used as cross-survey calibrators, also HR10 (533.9–561.9 nm) and HR21 (848.4–900.1 nm) exposures of a fraction of the targets are acquired.
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