Table 4
List of the strongest emission or absorption lines.
| Feature names | Wavelength (Å) | Type |
|
|
||
| Lyα | 1215 | Absorption/Emission |
| Fe II | 2600 | Intervening |
| Mg II | 2796 | Intervening/Emission |
| 2803 | Intervening/Emission | |
| [OII] | 3727 | Emission |
| 3729 | Emission | |
| Ca K | 3933.7 | Absorption |
| Ca H | 3968.5 | Absorption |
| Hδ | 4101.7 | Absorption |
| Ca I G | 4304.4 | Absorption |
| Hβ | 4861.3 | Absorption/Emission |
| [OIII] | 4959 | Emission |
| 5007 | Emission | |
| Mgb | 5174 | Absorption |
| CaI+FeI | 5269 | Absorption |
| Na I D | 5892.5 | Absorption |
| [NII] | 6548.1 | Emission |
| Hα | 6562.8 | Absorption/Emission |
| [NII] | 6583.6 | Emission |
| Ca triplet | 8498 | Absorption |
| 8542 | Absorption | |
| 8662 | Absorption | |
Notes. The columns give the names of the strongest expected absorption and emission lines, their wavelength in the rest frame in Å, and their nature, which indicate if they appears as absorption or emission lines from the host galaxy, or if they come from an intervening system. For Fe II and Mg II, which are multiplets, only the strongest lines are reported.
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