Table 1.
VLT/MUSE data employed.
| Name | Program ID/P.I. | texp × nexp = Texp [s] (a) |
 ×  [s] (b) |
|---|---|---|---|
| IC 5063 | 60.A-9339/Marconi/Hawthorn/Salvato | 600 × 4 = 2400 | 60 × 2 |
| NGC 5643 | 095.B-0532/Carollo | 900 × 4 = 3600 | 120 × 2 |
| 60.A-9339/Marconi/Hawthorn/Salvato | 500 × 4 = 2000 (c) | 100 × 4 | |
| NGC 1068 | 094.B-0321/Marconi | 500 × 4 + 100 × 8 = 2800 (d) | 100 × 4 + 100 × 8 |
| NGC 1386 | 094.B-0321/Marconi | 500 × 8 = 4000 | 100 × 8 |
Notes.
Total exposure time on object Texp, given by the combination of the single nexp-times repeated exposures having duration of texp each.
After comparing the two datasets from program 60.A-9339 and 095.B-0532 for NGC 5643, we employed the observations from program 095.B-0532 here because their seeing is superior to that from program 60.A-9339.
The first OB was in the central spaxels affected by emission lines that were saturated or in the non-linear response regime of the instrument. The second observing block (OB) was then acquired with shorter exposure times (100 s instead of 500 s), and only this second OB was adopted in the central spaxels.
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