Table 2
Summary of the observations with VLT/UVES and VLT/CRIRES.
| Star | Total integration time | S/N a | ||||
| Visual | H | K | Visual | H | K | |
|
|
||||||
| B3-b1 | 6h 10 m | 40 m | 52 m | 20 | 55 | 44 |
| B3-b7 | 6h 10 m | 1h 10 m | 20 m | 38 | 31 | 37 |
| B3-b8 | 6h 10 m | 1h 04 m | 1h 20 m | 65 | 80 | 79 |
| B3-f3 | 11h 50 m | ... | 56 m | 31 | ... | 35 |
| BW-f6 | 6h 25 m | 1h 20 m | 1h 20 m | 34 | 46 | 38 |
| B6-b8 | 8h 30 m | 1h 04 m | 1h 20 m | 55 | 35 | 44 |
| B6-f1 | 5h 15 m | 32 m | 40 m | 75 | 33 | 28 |
| B6-f7 | 5h 15 m | 32 m | 1h 20 m | 30 | 42 | 36 |
Notes.
Signal-to-noise ratio per datapoint in the reduced spectra (0.017 Å per datapoint for the visual spectra, 0.075 Å per datapoint for the H-band spectra, and 0.11 Å per datapoint for the K-band spectra) as measured by the IDL-routine der_snr.pro, see http://www.stecf.org/software/ASTROsoft/DER_SNR
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