Table 6
Luminosities and masses of M42, M43 and NGC 1977 per subregion.
| Region | A | LFIR | L[C II] | L[C II] ∕LFIR | Mgas (a) | LCO(2–1) (b) | MCO (c) | L24μm (d) | LHα (e) | |
|---|---|---|---|---|---|---|---|---|---|---|
| [pc2] | [L⊙] | [L⊙] | [M⊙] | [L⊙] | [M⊙] | [L⊙] | [L⊙] | |||
| M42 | all | 45 | 1.8 × 105 | 510 | 2.8 × 10−3 | 10 900 | 1.1 | 8800 | 4700 | 3500 |
| OMC1(f) | 0.31 | 8.2 × 104 | 53 | 6.5 × 10−4 | 1500 | 8.9 × 10−2 | 720 | – | 1500 | |
| Bright Ridge(f) | 0.07 | 3.7 × 104 | 11 | 2.9 × 10−4 | 870 | 2.8 × 10−2 | 220 | – | 470 | |
| Eastern Rim | 1.3 | 1.7 × 104 | 59 | 3.5 × 10−3 | 510 | 9.2 × 10−2 | 740 | 810 | 260 | |
| OMC4 | 2.5 | 1.6 × 104 | 45 | 2.8 × 10−3 | 2100 | 1.5 × 10−1 | 1200 | 640 | 470 | |
| Veil Shell | 8.7 | 3.5 × 104 | 150 | 4.3 × 10−3 | 2500 | 2.3 × 10−1 | 1800 | 1200 | 590 | |
| M43 | all | 0.74 | 1.4 × 104 | 38 | 2.7 × 10−3 | 530 | 3.0 × 10−2 | 240 | 740 | 190 |
| background, H II | 0.13 | 3.1 × 103 | 8.9(g) | 2.8 × 10−3 | 53 | 4.6 × 10−3 | 37 | 100 | 99 | |
| faint CO, faint [C II] | 0.14 | 8.8 × 102 | 4.1 | 4.7 × 10−3 | 29 | 2.5 × 10−3 | 20 | 49 | 12 | |
| bright CO, faint [C II] | 0.16 | 2.0 × 103 | 6.0 | 3.0 × 10−3 | 200 | 9.2 × 10−3 | 74 | 87 | 18 | |
| shell | 0.31 | 8.2 × 103 | 19 | 2.3 × 10−3 | 250 | 1.4 × 10−2 | 110 | 410 | 63 | |
| NGC | all | 17 | 1.8 × 104 | 160 | 8.9 × 10−3 | 2600 | 1.2 × 10−1 | 950 | 1000 | 63 |
| 1977 | H II | 2.9 | 4.7 × 103 | 37(h) | 7.9 × 10−3 | 310 | 1.1 × 10−2 | 87 | 300 | 17 |
| OMC3 | 2.6 | 5.8 × 103 | 34 | 5.9 × 10−3 | 1200 | 8.9 × 10−2 | 720 | 190 | 8.6 | |
| faint Hα | 6.9 | 3.2 × 103 | 33 | 9.7 × 10−3 | 730 | 3.0 × 10−2 | 240 | 280 | 19 | |
| shell | 6.2 | 5.4 × 103 | 69 | 1.3 × 10−2 | 670 | 1.6 × 10−2 | 130 | 100 | 7.9 |
Notes. (a) Gas mass derived from dust mass, using NH ≃ 6 × 1024 cm−2 τ160 (Weingartner & Draine 2001). (b)The CO(2−1) map does not cover the entire NGC 1977 region (cf. Fig. 2 in Paper I). (c) Gas mass from CO(2−1) intensity, using
(Bolatto et al. 2013). (d) The MIPS 24 μm image is saturated toward the Huygens/OMC1 region. (e)The Hα surface brightness in the EON is largely due to scattered light from the bright Huygens Region (O’Dell & Harris 2010). Also Hα emission in M43 has to be corrected for a contribution of scattered light from the Huygens Region (Simón-Díaz et al. 2011). (f) The Bright Ridge contains the BN/KL region and Orion S and is part of OMC1. Values for OMC1 include the Bright Ridge, where we have estimated the FIR luminosity from an SED fit to the three PACS bands, that are only saturated at the core of BN/KL. (g) 2.4 L⊙ from background PDR, 6.0 L⊙ from ionized gas, 0.5 L⊙ from foreground neutral shell. (h) 6.2 L⊙ from ionized gas, 31 L⊙ from neutral shell.
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