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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