Open Access
Table B.1
Core TARDIS/PPXF configuration adopted in this work.
| Block | Parameter | Value |
|---|---|---|
| Global | vsys | 2035 km s−1 |
| Foreground E(B–V) | 0.01 | |
| LSF treatment | Templates convolved to the wavelength-dependent MUSE LSF (E22) | |
| Binning | Target S/N | 35 (also 60 and 90 for robustness) |
| S/N window | 5300–5500 Å | |
| Kinematics | Templates | 40-grid |
| λ range | 4800–7000 Å | |
| Moments | V, σ, h3, h4 | |
| Polynomials | additive / multiplicative = 12/0 (as E22) | |
| Attenuation | Templates | 40-grid |
| λ range | 4800–7000 Å | |
| RV | 3.41 (LMC-like) | |
| Polynomials | additive / multiplicative = 0/0 | |
| Populations | Templates | 117-grid (as E22) |
| λ range | 4760–9350 Å (masked windows; Fig. A.1) | |
| Regularisation | none | |
| MC realizations | 20 | |
| Polynomials | additive / multiplicative = 0/12 (as E22) | |
| Emission lines | λ range | 4760–9350 Å; brightest observed-frame sky lines masked using the UVES atlas (Hanuschik 2003) |
| Kinematic tying | 3 families (H recombination, low-ionization, high-ionization; see Belfiore et al. 2019) | |
| Detection | robust if not fully compromised by masking and S/N> 5 in at least one bin, with S/N≡ Fline/σ(Fline) (E22) | |
| Derived | E(B–V)gas | Balmer decrement (case B) with a Calzetti-type curve (C00) evaluated at RV = 3.41 |
| SFR | Hα calibration from Kennicutt & Evans (2012) | |
Notes. The fitting sequence follows E22, but the stellar-template grids are extended to lower metallicity. The main masked regions are indicated in Fig. A.1.
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