Table 3
Summary of the criteria adopted to classify the spectra based on spectral lines criteria.
| SP.TY. | Cat ID | [Oii] | Hβ | [Oiii] | Hδ | N (%) | |||
|
|
|||||||||
| e(a) | 1 | <0 | or | <0 | or | <0 | and | ≥4 | 6.9% |
| e(b) | 2 | <−40 | or | <−12.5 | ... | and | <4 | 2.5% | |
| e(c) | 3 | −40 to 0 | or | −12.5 to 0 | or | <0 | and | <4 | 29.9% |
| k | 4 | >0 | ... | ... | ... | ... | and | <3 | 49.6% |
| k+a | 5 | >0 | ... | ... | ... | ... | and | 3 to 8 | 10.4% |
| a+k | 6 | >0 | ... | ... | ... | ... | and | ≥8 | 0.7% |
Notes. Other lines (namely Hβ and [Oiii]) were introduced with respect to previous works to be able to classify a spectra in these cases when the [Oii] line was out of the observed spectral range or overwhelmed by noise. The last column presents the spectral type fractions, which are corrected for incompleteness, among galaxies to which a spectral classification could be assigned.
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