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Table D.1
Fits to the emission lines of the host galaxy.
| Spectral line | Flux (erg s-1 cm-2) | Corr. with E(B − V) | σ (km s-1) |
|
|
|||
| H-αλ6564 | (1.43 ± 0.10) × 10-16 | (3.08 ± 0.22) × 10-16 | 123 ± 11 |
| [O iii] λ5008 | (1.82 ± 0.07) × 10-16 | (5.09 ± 0.19) × 10-16 | 93 ± 4 |
| [O ii] λ3729 | (6.0 ± 0.3) × 10-17 | (2.31 ± 0.12) × 10-16 | 100 (Fixed) |
| [O ii] λ3727 | (3.9 ± 0.4) × 10-17 | (1.50 ± 0.15) × 10-16 | 100 (Fixed) |
Notes. The extinction correction is based on the photometric fit of the host galaxy, using a Calzetti extinction law with E(B − V) = 0.25 mag, as described in the main text.
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