Table 10.
Quasar emission lines found in the Milliquas-based composite spectrum and covering the redshift range 0.052 ≤ z ≤ 4.35 (Fig. 33).
| Emission line | λobs | F/FLyα |
|---|---|---|
| +λlab (nm) | (nm) | |
| Lyϵ λ93.780 | 94.356 ± 1.327 | 0.344(2) |
| Lyδ λ94.974 | ⋯ | ⋯ |
| C III λ97.702 | 98.632 ± 0.237 | 0.393(2) |
| N III λ99.069 | ⋯ | ⋯ |
| Lyβ λ102.572 | 103.423 ± 0.139 | 0.479(2) |
| O VI λ103.383 | ⋯ | ⋯ |
| Fe II λ111.208 (a) | 112.098 ± 0.500 | 0.328(2) |
| Lyα λ121.567 | 122.250 ± 0.033 | 1.000(2) |
| O I λ130.435 | 130.495 ± 0.545 | 0.402(2) |
| Si II λ130.682 | ⋯ | ⋯ |
| Si IV λ139.676 | 139.568 ± 0.098 | 0.427(2) |
| O IV] λ140.206 | ⋯ | ⋯ |
| C IV λ154.906 | 154.469 ± 0.061 | 0.485(3) |
| C III λ190.873 | 189.922 ± 0.102 | 0.327(3) |
| Fe III λ205.271 (a) | 205.600 ± 0.555 | 0.230(3) |
| C II] λ232.644 | 232.390 ± 0.350 | 0.202(3) |
| [Ne IV] λ242.383 | 242.617 ± 0.324 | 0.198(3) |
| Mg II λ279.875 | 279.888 ± 0.039 | 0.212(3) |
| He I λ318.867 | 318.612 ± 0.295 | 0.136(3) |
| Hγ λ434.168 | 434.052 ± 0.067 | 0.081(3) |
| Fe II λ453.780 (a) | 454.281 ± 0.569 | 0.070(4) |
| Hβ λ 486.268 | 486.701 ± 0.118 | 0.085(4) |
| [O III] λ496.030 | ⋯ | ⋯ |
| [O III] λ500.824 | ⋯ | ⋯ |
| [N I] λ520.053 | 522.270 ± 0.615 | 0.054(4) |
| He I λ587.729 | 588.441 ± 0.411 | 0.044(4) |
| Hα λ656.461 | 656.283 ± 0.014 | 0.123(4) |
| He I λ706.720 | 706.666 ± 0.945 | 0.034(4) |
| O I λ844.868 | 850.091 ± 0.413 | 0.033(4) |
| Ca II λ850.036 | ⋯ | ⋯ |
Notes. Each emission line is visually inspected before a quadratic polynomial is fit in the vicinity of its apparent peak using five samples of flux density. The maximum of the quadratic curve provides the observed rest-frame wavelength position, λobs, of the line and its maximum flux density compared to Lyα, F/FLyα (where the number of significant digits is provided in parenthesis). Because of the intricacies inherent in the fit of a local continuum to faint, broad, and/or blended emission lines, such a continuum was not subtracted from the flux densities reported here. This explains the differences between this table and the values found in Table 9.
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