Table 2
Log of MUSE NFM observations.
| Name | Prog. ID | Observing date | tDIT × nDIT (a) | On-source time | Derotation | Frames per rot. |
|---|---|---|---|---|---|---|
| (s) | (degree) | |||||
| PDS 70 | 60.A-9100(K) | 2018-06-20 | 300 × 6 | 1800 | 90 | 2 |
| J1850-3147 | 60.A-9482(A) | 2018-09-06 | 30 × 6 | 180 | 90 | 3 |
| 2018-09-08(b) | 30 × 6 | 180 | 90 | 3 | ||
| V1094 Sco | 0103.C-0399(A) | 2019-04-14 | 300 × 8 | 2400 | 90 | 2 |
| HD 100546 | 0103.C-0399(A) | 2019-04-28 | 1 × 4 | 4 | 0 | 4 |
| 2019-04-28 | 4 × 40 | 160 | 45 | 8 | ||
| HD 163296 | 0103.C-0399(A) | 2019-04-29 | 2 × 4 | 8 | 0 | 4 |
| 2019-04-29 | 8 × 40 | 320 | 45 | 8 | ||
| 2019-04-29 | 250 × 2 | 500 | 0 | 2 |
Notes. (a) tDIT is exposure time per image frame and nDIT is the number of image frames. (b)We found some Hα residuals at 60 mas from the star center in the data observed on Sept. 8 after we analyzed the data obtained on two nights separately. The dataset is a 3 min snapshot and has a few bad spaxels in the region of the Hα residuals. Therefore, we excluded the data observed on the night of Sept. 8 to minimize the influence of possible instrumental artifacts.
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