Table 1
Datasets are made of a number of exposure files, which are acquired over the “Time Span” interval.
| Dataset name | UT-MR-NoFT | AT-MR-FT | AT-LR-FT |
|
|
|||
| Date | 2011/01/16 | 2012/02/22 | 2012/10/09 |
| Telescopes | UTs 1-2-4 | ATs D0-I1-H0 | ATs |
| Objects (Kmag) | HD 15694 | various | HD 197635 |
| Kmag | 2.5 | 2.04 <K< 3.4 | 2.8 |
| Nb of files | 2 | 40 | 37 |
| Time Span | 0.2 h | 5.7 h | 3.5 h |
| Nb frames per file | 970 | 37 | 1000 |
| DIT (s) | 0.19 | 2.0 | 0.026 |
| Frames sampling (s) | 0.42 | 2.5 | 0.06 |
| Spectral Res. | Medium | Medium | Low |
| Spectral Band | K | K | K |
| Fringe Tracker | OFF | ON | ON |
| Seeing (arcsec) | 0.9, 1.0, 1.0 | 0.6, 0.9, 1.4 | 0.5,0.6,0.8, |
| (min., avg., max.) | |||
| τ0 (ms) | 5.2, 8.4, 12.8 | 3.3, 3.5, 3.7 | 1.9, 2.4, 3.0 |
| (min., avg., max.) | |||
Notes. Each file contains a number of individual frames with each of them exposed during a digital integration time (DIT) and separated by the “Frame sampling” interval. The medium and low spectral resolutions of AMBER are, respectively, 1500 and 35. Atmospheric seeing is given in arcsec and coherence time τ0 in milliseconds.
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