Table 1.
Best-fit parameters from modelling Mrk 1044’s central highest signal-to-noise spectrum with multiple Gaussian components.
| Hβ window |
Hα window |
|||||
|---|---|---|---|---|---|---|
| Component | Line | vr [km s−1] | σ [km s−1] | Line | vr [km s−1] | σ [km s−1] |
| Broad | Hβ+Fe II | −272 ± 11 | 1349 ± 14 | Hα | −232 ± 13 | 1232 ± 13 |
| Medium | Hβ+Fe II | −48 ± 4 | 281 ± 2 | Hα | 206 ± 87 | 212 ± 48 |
| Core | Hβ+[O III] | −144 ± 5 | 165 ± 17 | Hα+[N II] | −140 ± 7 | 180 ± 12 |
| Wing | Hβ+[O III] | −560 ± 20 | 251 ± 31 | Hα | −560 ± 20 | 251 ± 31 |
Notes. The left columns list the emission lines in the Hβ–[O III] region, the right columns the Hα+[N II] region. Velocities and dispersion are computed in the galaxy rest-frame. Lines that are listed together are kinematically coupled. Furthermore, we have kinematically tied the wing component between Hβ+[O III] and Hα. In each of the strong lines, the core component has a velocity that is significantly different from zero.
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