Table C.1.
Priors used in this work.
| Bagpipes | |
| SFR: | |
| log Z/Z⊙ | (0.001, 2.5) |
| log M★, formed/M⊙ | (6, 13) |
| Bin edges [Myr] | (0, 10, 100, 250 |
| 500, 800, 1100)* | |
| AV [mag] | (0, 2) |
| log U | (0, −4) |
| AGN: | |
| αλ | (−2.5, 3) |
| βλ | (−1.5, 2.3) |
| Dense Basis | |
| log M★/M⊙ | (6, 13) |
| Dust prior | Flat |
| sSFR prior | sSFRflat |
| log sSFR | (−12, −7.5) |
Notes. *The bin edges shown in the table were used for the z = 5 sources, namely the tLRD, BBG, SAT1, and C1. For C2, C3, and the fuzz, we included bins at 2500, 5000, and 5500 Myr. We set a Calzetti et al. (2000) dust attenuation law in both codes. The redshifts were set to the zspec (or photo-zs in the absence of spectra).
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