Table 1.
All observations were performed with SPHERE/IFS (PI: J. Beuzit).
| Object name | ESO ID | Date | DIT [s] × Ntot, λ | Δt [min] | Δα [°] | λ [μm] | Seeing [″] |
|---|---|---|---|---|---|---|---|
| β Pictoris | 096.C-0241(B) | 2015-11-30 | 4 × 760 | 50.7 | 41.1 | 0.95−1.35 | ≈1 |
| HR 8799 | 095.C-0298(D) | 2015-09-28 | 16 × 256 | 68.3 | 23.8 | 0.95−1.68 | ≈1 |
| 51 Eridani | 198.C-0209(J) | 2017-09-28 | 32 × 154 | 83.1 | 52.0 | 0.95−1.68 | < 0.8 |
Notes. Here, DIT stands for detector integration time and Ntot, λ is the total number of images taken per wavelength. Each image contains 39 wavelength frames equally spread over the wavelength range λ. Each dataset has a field rotation of Δα. The atmospheric seeing is given as the approximate value for the atmospheric distortions during the whole observation.
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