Table 2.
Physical parameters characterizing the starburst in GN-z11 and high-z galaxies in the early Universe.
| Galaxy | Redshift | Metallicity | SFR | log(M*) | Re | ΣSFR | Σ* | C5 |
|---|---|---|---|---|---|---|---|---|
| 12 + log(O/H) | (M⊙ yr−1) | (M⊙) | (pc) | (103 M⊙ yr−1 kpc−2) | (104 M⊙ pc−2) | (105 M⊙ pc−1) | ||
| GN-z11 | 10.6 | 7.91 | 24 | 8.96 | 64 | 0.933 | 3.6 | 85 |
| GN-z8-LAE | 8.3 | 7.85 | 11.3 | 7.66 | 143 | 0.088 | 0.036 | 2 |
| CEERS-1019A | 8.7 | 7.70 | 148 | 8.76 | 112 | 1.86 | 0.72 | 30 |
| CEERS-1019B | 8.7 | 7.70 | 83 | 8.66 | 145 | 0.645 | 0.355 | 19 |
| MACSJ1149-JD1 | 9.1 | 7.88 | 0.4 | 7.15 | < 25 | > 0.10 | > 0.36 | > 3 |
| GN-z9p4 | 9.4 | 7.35 | 64 | 8.7 | 118 | 0.732 | 0.573 | 25 |
| RXJ2129-z95 | 9.5 | 7.48 | 1.7 | 7.63 | 16.2 | 1.03 | 2.6 | 16 |
| MACS0647-JD1 | 10.2 | 7.79 | 5.0 | 8.62 | 70 | 0.162 | 1.35 | 35 |
| MACS0647-JD1A | 10.2 | 7.79 | 1 | 8 | 70 | 0.033 | 0.325 | 8 |
| MACS0647-JD1B | 10.2 | 7.79 | 0.6 | 7.8 | 20 | 0.239 | 2.5 | 19 |
| GHz2 | 12.3 | 7.40 | 9 | 8.91 | 34–105 | 0.1–1.0 | 1–10 | 45–141 |
| GS-z14-0 | 14.3 | 6.9 | 25 | 8.7 | 260 | 0.059 | 0.12 | 11 |
Notes. GN-z11: Metallicity and SFR are from this work, the stellar mass is a mean of the values presented in Bunker et al. (2023) and Tacchella et al. (2023), and effective radius Tacchella et al. (2023). GN-z8-LAE: Navarro-Carrera et al. (2024); CEERS-1019: Marques-Chaves et al. (2024a); MACS1149-JD1: Metallicity (Stiavelli et al. 2023), size, and stellar mass for clump 2 (Bradač et al. 2024); GN-z9p4: Schaerer et al. (2024); RXJ2129: Williams et al. (2023); MACS0647-JD: stellar mass (Hsiao et al. 2023), metallicity (Hsiao et al. 2024b,a), SFR (Hsiao et al. 2024a). GHz2: Metallicity and SFR (Zavala et al. 2024), size, stellar mass, SFR, and stellar mass surface brightness (Calabro et al. 2024). GS-z14-0: Helton et al. (2024). The SFR and stellar mass surface densities were derived from the corresponding quantities divided by 2πRe2. The compactness index (C5) is defined as C5 = (M*/105 M⊙)/Rhm[pc] with Rhm = 1.7 × Re as the half-mass radius, (Krause et al. 2016). The uncertainties in the different parameters are given in the references.
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