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Table A.1.

SED fitting: Full results.

[Z/H] log(age) log(LHα, int)
Burst
-3.15 +0.77 6.4 13.5 4.01 43.93
-2.15 0.0 6.5 4.33 4.26 43.58
-1.15 +0.86 6.6 6.54 3.87 43.15
-0.85 +1.27 6.6 6.75 10.42 43.13
-0.54 +2.12 6.5 7.28 18.96 43.21
-0.37 +2.61 6.5 6.19 26.44 43.15
-0.24 +3.18 6.5 6.61 29.93 43.20
-0.15 +5.61 6.6 19.94 25.73 43.18
0.00 +5.94 6.5 21.60 24.30 43.03
Cont.
-3.15 +0.45 7.4 11.57 5.81 43.64
-2.15 +0.03 6.9 5.31 4.09 43.64
-1.15 0.0 7.3 3.52 4.67 43.30
-0.85 +0.34 7.3 3.55 7.14 43.26
-0.54 +1.28 7.3 5.10 11.60 43.20
-0.37 +2.04 7.3 7.03 14.48 43.14
-0.24 +2.73 7.3 8.78 17.03 43.10
-0.15 +3.32 7.6 11.58 13.33 42.86
0.00 +4.03 7.3 14.87 16.49 43.08

We list the best-fit model for each stellar metallicity and for a single-burst or continuous star formation that satisfies the additional bounds from the IR photometry (F105W> 25.2 and [4.5]> 25.3). The age is in yr. We list the goodness of fit using the full spectral data relative to the best model for a certain SFH (). The best-fit χ2red, full are 3.00 and 3.17 for the single-burst and continuous star formation models, respectively. We also list when only using wavelength layers around the N V and C IV P Cygni profiles. For each model we also list the intrinsic Hα luminosity in erg s−1.

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