Table 3
Properties measured in SDSO in this work, along the typical ranges that different categories or nebulae show in these properties.
| Properties | SDSO | Galactic nebula | Extragalactic nebula | |||||
|---|---|---|---|---|---|---|---|---|
| HII | DIG | SNR | PN | Bow shock | EELR | CGM shock | ||
| Radial velocity (km s−1) | −6 to −30 | −300 to +300 | −100 to | −500 | ||||
| Line width (σ) (km s−1) | ≤20 ([O III]) | <30 | ≤25 | >40 | 20-30 | >25 | 10-20 | >50 |
| log10([O III]/Hβ) | 0.04-0.15 | −1 to 0.8 | −0.5 to 0.5 | −0.5 to 1 | 0.5 to 1.2 | −1 to 1 | >0.4 | −0.5 to 1 |
| log10([O III]/[O II]) | ~-0.5 | — 1 to 1 | −0.5 to 0.5 | −0.8 to 0 | 0.6 to 1.3 | − | 0.3 to 0.8 | − |
| Electron density (cm−3) | <300 | <600 | 0.02-20 | 200-10 000 | <1000 | 0.1-1000 | 3-300 | − |
| Emission line separation | 6 arcmin | 5.2 arcsec to 10 deg | 0.13-6.6 arcsec | |||||
Notes. In the first and last rows we only separate Galactic and extragalactic nebula, stating simply the radial velocity from the heliocentric system. In the last line, we assume a physical separation between regions emitting in different emission lines ranging from 0.5 to 25 pc, based on the literature (see Sect. 4.2). The stated values show the apparent size when considering distances from 10 pc to 10 kpc (galactic nebula) and 770 kpc (M31 nebula). HII regions: Nakajima & Ouchi (2014), DIG: González-Díaz et al. (2024); den Brok et al. (2020), SNR: Li et al. (2024); How et al. (2018); Long et al. (2019), PNs: Mari et al. (2023); Wang et al. (2004), Galactic shocks: Green et al. (2022); Ocker et al. (2021); Schultz et al. (2005), EELRs: Keel et al. (2012a), Extragalactic shocks: Rodríguez-Baras et al. (2014); Arnaudova et al. (2024); Rich et al. (2011).
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