Table 5.
Performance of the best-fitting models for the secondary lines and bolometric luminosity.
| Line | ngal, det | Single models |
Mixed models |
||||
|---|---|---|---|---|---|---|---|
| Low | Ok | High | Low | Ok | High | ||
| [Si II]34.82 | 21 | 21 | 0 | 0 | 16 | 5 | 0 |
| [Fe II]17.94 | 1 | 0 | 1 | 0 | 0 | 1 | 0 |
| [Fe II]25.99 | 10 | 0 | 10 | 0 | 0 | 9 | 1 |
| [Fe III]22.93 | 11 | 0 | 7 | 4 | 0 | 8 | 3 |
| H2 S(0) 28.21 | 1 | 1 | 0 | 0 | 1 | 0 | 0 |
| H2 S(1) 17.03 | 8 | 5 | 1 | 2 | 5 | 0 | 3 |
| H2 S(2) 12.28 | 7 | 4 | 3 | 0 | 5 | 2 | 0 |
| H2 S(3) 9.66 | 0 | 0 | 0 | 0 | 0 | 0 | 0 |
| LBOL | 37 | 0 | 37 | 0 | 0 | 25 | 12 |
Notes. Columns 1–2: line label and number of galaxies in which the line is detected. Columns 3–4: number of galaxies in which the ratio of predicted over observed intensity is low, ok, and high, where the threshold is set to a factor of two. We report numbers for single and mixed models.
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