Table 1.
Wavelengths of our six emission lines of interest, together with the SDSS filter (in brackets) in which they fall for a selection of redshifts, for illustration.
| λz | Hα | Hβ | [O II] | [O III] | [N II] | [S II] |
|---|---|---|---|---|---|---|
| z = 0 | 6563 (r) | 4861 (g) | 3727–3729 (u) | 5007 (g) | 6584 (r) | 6717–6731 (r) |
| z = 0.02 | 6694 (r) | 4958 (g) | 3801–3803 (u) | 5107 (g) | 6716 (r) | 6851–6865 (i) |
| z = 0.12 | 7350 (i) | 5444 (g) | 4174–4176 (g) | 5608 (r) | 7374 (i) | 7523–7539 (i) |
| z = 0.22 | 8006 (i) | 5930 (r) | 4546–4549 (g) | 6108 (r) | 8032 (i) | 8195–8211(i) |
Notes. This information is used for the aperture corrections performed on emission-line luminosities, as described in Sect. 2.2. From top to bottom, we tabulate emission-line wavelenghts at: rest-frame (λ0, first row), z = 0.02 (second), z = 0.12 (third), z = 0.22 (fourth). The relation between them is: λz = λ0(1 + z).
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