Gaia Data Release 3
Open Access

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)
Lyϵλ93.780 94.356 ± 1.327 0.344(2)
Lyδλ94.974
C IIIλ97.702 98.632 ± 0.237 0.393(2)
N IIIλ99.069
Lyβλ102.572 103.423 ± 0.139 0.479(2)
O VIλ103.383
Fe IIλ111.208 (a) 112.098 ± 0.500 0.328(2)
Lyαλ121.567 122.250 ± 0.033 1.000(2)
O Iλ130.435 130.495 ± 0.545 0.402(2)
Si IIλ130.682
Si IVλ139.676 139.568 ± 0.098 0.427(2)
O IV] λ140.206
C IVλ154.906 154.469 ± 0.061 0.485(3)
C IIIλ190.873 189.922 ± 0.102 0.327(3)
Fe IIIλ205.271 (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 IIλ279.875 279.888 ± 0.039 0.212(3)
He Iλ318.867 318.612 ± 0.295 0.136(3)
Hγλ434.168 434.052 ± 0.067 0.081(3)
Fe IIλ453.780 (a) 454.281 ± 0.569 0.070(4)
Hβλ 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 Iλ587.729 588.441 ± 0.411 0.044(4)
Hαλ656.461 656.283 ± 0.014 0.123(4)
He Iλ706.720 706.666 ± 0.945 0.034(4)
O Iλ844.868 850.091 ± 0.413 0.033(4)
Ca IIλ850.036

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.

(a)

Broad feature composed of Fe multiplets.

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