Table 3
Luminosities and masses of M 42, M 43, and NGC 1977.
| Region | A | LFIR | L[C II ] | L[C II ] ∕LFIR | Mgas (a) | LCO(2-1) (b) | MCO (c) | L24 μm (d) | LHα (e) | |
|---|---|---|---|---|---|---|---|---|---|---|
| [pc2] | [L⊙] | [L⊙] | [M⊙] | [L⊙] | [M⊙] | [L⊙] | [L⊙] | |||
| M 42 | All | 45 | 1.8 × 105 (f) | 510 | 2.8 × 10−3 | 10 000 | 1.1 | 8800 | 4700 | 3500 |
| OMC1 | 0.4 | 8.2 × 104 (f) | 53 | 6.5 × 10−4 | 640 | 8.9 × 10−2 | 720 | – | 1500 | |
| shell | 10.0 | 5.2 × 104 | 209 | 4.0 × 10−3 | 3000 | 3.2 × 10−1 | 2500 | 2000 | 850 | |
| M 43 | 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(f) | 2.8 × 10−3 | 53 | 4.6 × 10−3 | 37 | 100 | 99 | |
| shell | 0.31 | 8.2 × 103 | 19 | 2.3 × 10−3 | 250 | 1.4 × 10−2 | 110 | 410 | 63 | |
| NGC 1977 | All | 17 | 1.8 × 104 | 160 | 8.9 × 10−3 | 2600 | 1.2 × 10−1 | 950 | 1000 | 63 |
| OMC3 | 2.6 | 5.8 × 103 | 34 | 5.9 × 10−3 | 1200 | 8.9 × 10−2 | 720 | 190 | 8.6 | |
| 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).
(c) Molecular 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 M 43 has to be corrected for a contribution of scattered light from the Huygens Region (Simón-Díaz et al. 2011). (f) BN/KL and Orion S contributewith LFIR ≃ 3 × 104 L⊙.
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