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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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