Table A.1.
Summary of the criteria applied for classification and segmentation of the pixels in I − σ diagrams.
| Classification | Observed σ(Hα) range | Clipped σ(Hα) for ASTRODENDRO | Physical interpretation |
|---|---|---|---|
| Low Σ(Hα) | Any; I(Hα) < Σ(Hα)DIG | σref − Δ(σm) | Diffuse ionised gas |
| Class 1 | σ(Hα) < σ(Hα)norm | σref − Δ(σm) | Unperturbed H II regions |
| Class 2 | [σ(Hα)norm,σ(Hα)1.5×norm) | σref | May be illusive, but likely periphery |
| of superbubbles; low-velocity shocks | |||
| Class 3 | [σ(Hα)1.5×norm,σ(Hα)3×norm) | max[σref + 2Δ(σm),σ(Hα)] | Expanding superbubbles; shocks; |
| other supersonic gas motions | |||
| Top σ | σ(Hα) ≥ min[σ(Hα)3×norm,100 km s−1] | max[σref + 3Δ(σm),σ(Hα)] | SNR/WR or other extreme source candidates |
Notes. – σ(Hα)norm, σ(Hα)1.5×norm and σ(Hα)3×norm are the upper boundaries of velocity dispersion defined by Gaussians in σ(Hα) vs log I(Hα) space with mean = σ(Hα)m and std = Δ(σm), 1.5Δ(σm) and 3Δ(σm), respectively. – σ(Hα)m and Δ(σm) are flux-weighted mean velocity dispersion and its standard deviation (see measured values for each galaxy in Table 1). – σref is the median σ(Hα) derived from all pixels classified as Class 2, 3 or Top σ.
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