Table 2.
Line flux measurements for the most prominent nebular emission lines JWST-PRIMAL sample.
| zspec | [O II] λ3727 | [Ne III] λ3870 + | Hδ | Hγ + | Hβ | [O III] λ5008 | Hα + | [S II] 6725 |
|---|---|---|---|---|---|---|---|---|
| He Iλ3889 | [O III] λ4363 | [N II] λ6585 | ||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) |
| 5.0019 | 424.9 ± 30.6 | 246.9 ± 41.6 | 88.6 ± 22.7 | 105.0 ± 24.7 | 329.9 ± 19.1 | 2072.9 ± 33.9 | 1004.5 ± 21.8 | 76.4 ± 12.7 |
| 5.0049 | 146.5 ± 15.7 | < 40.1 | < 22.9 | < 26.0 | 59.8 ± 8.4 | 249.1 ± 9.5 | 367.4 ± 9.4 | 49.1 ± 6.3 |
| 5.0151 | < 39.6 | < 52.8 | < 29.6 | 52.0 ± 16.6 | 22.2 ± 10.1 | 119.3 ± 9.7 | 121.6 ± 8.6 | < 14.2 |
| 5.0175 | < 108.0 | < 142.6 | < 83.4 | < 97.4 | 65.0 ± 28.9 | 290.6 ± 30.1 | 212.2 ± 26.1 | < 48.4 |
| 5.0212 | 137.9 ± 23.6 | 109.4 ± 31.1 | 54.4 ± 17.5 | 76.9 ± 19.4 | 138.5 ± 13.2 | 797.5 ± 21.5 | 409.4 ± 15.3 | < 21.4 |
| ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | |||
| 11.4906 | 17.0 ± 5.0 | < 36.0, < 36.0 | < 36.0 | < 45.0 | − | − | − | − |
| 11.7060 | < 8.7 | 7.3 ± 2.3, < 9.6 | < 11.0 | − | − | − | − | − |
| 12.5119 | 9.1 ± 2.7 | 9.3 ± 3.1, < 11 | − | − | − | − | − | |
| 12.7822 | < 10.0 | 18 ± 6, < 10.0 | − | − | − | − | − | − |
| 13.3606 | 6.0 ± 2.0 | − | − | − | − | − | − | − |
Notes. All measurements are reported in units of 10−20 erg s−1 cm−2. Uncertainties on measurements are stated at 1σ standard deviations and upper limits at 2σ confidence limits. Column (1): Spectroscopic redshift. Column (2): Unresolved [O II] λ3726, 3729 doublet line flux. Column (3): Unresolved [Ne III] λ3870 + He Iλ3889 line flux measurements, except for the highest redshift sources (z > 10). Column (4): Balmer Hδ. Column (5): Unresolved Balmer Hγ + auroral [O III] λ4363 line flux measurements, except for the highest redshift sources (z > 9.5). Column (6): Balmer Hβ. Column (7): [O III] λ5008 line flux, where [O III] λ4960 is assumed to be 1/3 of this. Column (8): Unresolved Balmer Hα+[N II] λ6585. Column (9): Unresolved [S II] λλ6718, 6732 doublet line flux. A full version of this table, including an expanded set of emission line identifications and measurements, can be found online.
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