Table 4.
Summary of exposure times (in min) for early-type stars.
| Setup | mag range | Exposure time |
|||||
|---|---|---|---|---|---|---|---|
| Original |
Revised (Dec 2013) |
Revised (Dec 2014) |
|||||
| O,early-B | late-B,A | O,early-B | late-B,A | O,early-B | late-B,A | ||
| U520 | 8 < V < 11 | (a) | (a) | (a) | (a) | (a) | (a) |
| HR03 | 10 < V < 13 | — | — | — | — | 36 | — |
| 11 < V < 14 | 34 | — | 87 | — | 90 | — | |
| 12 < V < 15 | 86 | 29 | 110 | 74 | 112 | 58 | |
| 13 < V < 16 | 107 | 73 | — | 93 | — | 75 | |
| 13 < V < 17 | — | 94 | — | — | — | — | |
| HR04, HR05A | 10 < V < 13 | — | — | — | — | 13 | — |
| 11 < V < 14 | 17 | — | 60 | — | 32 | — | |
| 12 < V < 15 | 41 | 12 | 75 | 42 | 40 | 21 | |
| 13 < V < 16 | 51 | 31 | — | 53 | — | 26 | |
| 13 < V < 17 | — | 40 | — | — | — | — | |
| HR06 | 10 < V < 13 | — | — | — | — | 9.3 | — |
| 11 < V < 14 | 14 | — | 46 | — | 23 | — | |
| 12 < V < 15 | 35 | 10 | 58 | 33 | 29 | 15 | |
| 13 < V < 16 | 43 | 25 | — | 41 | — | 19 | |
| 13 < V < 17 | — | 32 | — | 105 | — | 49 | |
| HR09B | 10 < V < 13 | — | — | — | — | 15 | — |
| 11 < V < 14 | 32 | — | 86 | — | 38 | — | |
| 12 < V < 15 | 79 | 21 | 108 | 56 | 47 | 25 | |
| 13 < V < 16 | 99 | 54 | — | 70 | — | 32 | |
| 13 < V < 17 | — | 69 | — | — | — | — | |
| HR14A | 10 < V < 13 | — | — | — | — | 5.6 | — |
| 11 < V < 14 | 14 | — | 19 | — | 14 | — | |
| 12 < V < 15 | 34 | — | 46 | — | 35 | — | |
| 13 < V < 16 | 42 | 22 | 57 | 30 | 44 | 23 | |
| 13 < V < 17 | — | 28 | — | 38 | — | 29 | |
Notes.
Exposure times are set by the corresponding exposure times for GIRAFFE. The original exposure times were based on the GIRAFFE exposure time calculator. However, we experienced problems attaining the required S/N and the integration times were increased in December 2013. With the introduction of updated values in the GIRAFFE exposure time calculator, these were again revised in December 2014. The integration times aim for a S/N > 100 for O,early B, and > 50 for late-B,A spectral types. For fainter stars, we cannot reach these values within a reasonable integration time, so the lower values of S/N > 70 and 35, respectively, are aimed for; these integration times are set in italic. See Blomme et al. (2022) for details.
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