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|
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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