Table A.4.
Spectroscopic identification of our targets.
| ID | zphot | zspec |  |
p a |  |
Balmer | Emission | σν d |
|---|---|---|---|---|---|---|---|---|
| abs.b | linesc | km s−1 | ||||||
| Robust zspec | ||||||||
| ZF-COS-20032 | 
|
 |
1.6 | 96% | 1.0 | – | [O I]6300 Hα [N II]λλ | 217 ± 161 |
| ZF-COS-20115 | 
|
|
−0.9 | 100% | 1.0 | Yes | – | – |
| ZF-COS-20133 | 
|
|
0.6 | 100% | 1.0 | – | Hβ [O III]λλ | 60 ± 26 |
| 3D-EGS-18996 | 
|
|
−8.3 | 100% | 1.0 | Yes | [O III]λλ | 530 ± 199 |
| 3D-EGS-26047 | 
|
|
0.0 | 99% | 1.0 | – | [O II]λλ Hβ [O III]λλ | 530 ± 263 |
| 3D-EGS-40032 | 
|
|
−0.0 | 100% | 1.0 | Yes | [O II]λλ | 582 ± 236 |
| ZF-UDS-8197 | 
|
|
−1.2 | 99% | 1.0 | – | [O III]λλ | 530 ± 53 |
| 3D-UDS-27939 | 
|
|
4.5 | 100% | 1.0 | – | [O I]6300 Hα [N II]λλ [S II]λλ | 154 ± 7 |
| Uncertain zspec | ||||||||
| ZF-COS-17779 | 
|
|
1.4 | 77% | 1.0 | – | Hβ [O III]λλ | 60 ± 26 |
| ZF-COS-18842 | 
|
|
−4.5 | 75% | 1.1 | – | [O III]λλ | 60 ± 279 |
| ZF-COS-19589 | 
|
|
0.1 | 32% | 0.9 | – | – | – |
| 3D-EGS-31322 | 
|
|
0.5 | 84% | 1.0 | Yes | – | – |
| Rejected zspec | ||||||||
| ZF-COS-10559 | 
|
|
0.4 | 2% | 0.9 | – | – | – |
| ZF-COS-14907 | 
|
|
−23.1 | 63% | 1.2 | – | – | – |
| 3D-EGS-27584 | 
|
|
4.3 | 9% | 1.0 | – | – | – |
| 3D-EGS-34322 | 
|
|
0.1 | 18% | 0.9 | – | – | – |
| ZF-UDS-3651 | 
|
|
2.7 | 33% | 1.1 | – | – | – |
| ZF-UDS-4347 | 
|
|
0.5 | 39% | 0.9 | – | – | – |
| ZF-UDS-6496 | 
|
|
1.3 | 33% | 1.0 | – | – | – |
| ZF-UDS-7329 | 
|
|
−0.1 | 25% | 1.0 | – | – | – |
| ZF-UDS-7542 | 
|
|
−0.6 | 35% | 1.0 | – | – | – |
| 3D-UDS-35168 | 
|
|
−0.5 | 4% | 1.0 | – | – | – |
| 3D-UDS-39102 | 
|
|
0.2 | 4% | 1.0 | – | – | – |
| 3D-UDS-41232 | 
|
|
0.2 | 25% | 1.0 | – | – | – |
Notes. This table is also available in electronic format at the CDS.
Indicates galaxies for which the redshift could be determined with p > 50% from the continuum emission alone, using Balmer absorption lines.
List of emission lines detected with a significance of at least 2σ. Line doublets names are shortened as in Table A.5.
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