Table 1
Characteristics of the various components present in the Orion-Eridanus region.
| Components | Reference | |||||||||
|---|---|---|---|---|---|---|---|---|---|---|
| Ionizing star | D | H II | Dense | PDR | ||||||
| log L* | log q | ne | R[CII] (a) | G0 (b) | G0 FIR(c) | nH | ||||
| (pc) | (L⊙) | (log (cm s−1) | (cm−3) | (pc) | (Habing field (d)) | (Habing field) | (cm−3) | |||
| M 42 | θ1 Ori C | 440 | 5.3 | 8.0 | 3.0 × 103 | 0.4 | 2.5 × 104 | 1.3 × 105 | 1.6 × 105 | 1 |
| M 43 | HD37061 | 440 | 4.8 | 7.2 | 5.0 × 102 | 0.6 | 3.0 × 103 | 5.0 × 103 | 2.3 × 104 | 2 |
| IC 434 | σ Ori | 385 | 4.8 | 7.6 | 1.0 × 102 | 4.0 × 0.3 | 103 | 2.1 × 102 | 4.6 × 103 | 3 |
| NGC 2024 | IRS2b | 415 | 5.2 | 7.0 | 1.5 × 103 | 0.1 | 3.5 × 104 | 5.6 × 103 | 7.0 × 104 | 4 |
| NGC 2023 | HD37903 | 350 | 4.1 | – | – | 0.4 | 9.0 × 103 | 6.0 × 102 | 5.0 × 102 | 5 |
| Mon R2 | NA | 880 | – | – | – | 0.04 | 3.7 × 104 | – | 4 × 104 | 6 |
| WIM | ne | Hα | ||||||||
| (cm−3) | (erg s−1 cm−2) | |||||||||
| Barnard’s Loop | 3.2 | 3.5 × 10−7 | 6 | |||||||
| λ Ori | 2.5 | 5.2 × 10−7 | 7 | |||||||
| ELDWIM | 1.0 | 1.8 × 10−6 | ||||||||
| SfMCs | nH | G0 (e) | ||||||||
| (cm−3) | (Habing Field) | |||||||||
| Orion Molecular Clouds A | 8 × 102-1 × 103 | 3–90 | 8 | |||||||
| Orion Molecular Clouds B | 9 × 102-1 × 103 | 3–80 | 9 | |||||||
| λ Ori Ring | 2 × 102-1 × 103 | 1–40 | 10 | |||||||
| Mon R2 | 4 × 104 | 2–16 | 11 | |||||||
Notes. (a) R[CII] is the radius where we multiply the modeled [C II] surface brightness by surface area to obtain [C II] flux (see Sect. 3.3). (b) G0 taken from references listed above. (c) G0 derived from FIR luminosity. (d)1 Habing field = 1.6 × 10−3. (e) G0 derived from dust temperature (see Sect. 3.4).
References. (1) Pogge et al. (1992); Simón-Díaz et al. (2006); Goicoechea et al. (2015); (2) Rodríguez (1999, 2002); O’Dell & Harris (2010); Simón-Díaz et al. (2011); (3) Ochsendorf & Tielens (2015); (4) Bik et al. (2003); Giannini et al. (2000); Graf et al. (2012); (5) Sandell et al. (2015); (6) Berné et al. (2009); (7) O’Dell et al. (2011); (8) Sahan & Haffner (2016); (9) Nishimura et al. (2015); (10) Nishimura et al. (2015); (11) Goldsmith et al. (2016).
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