Table 4
Characteristics of the molecular line emission over 5 deg2 of Orion B.
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) |
|---|---|---|---|---|---|---|---|---|
| Line | Intensity (Waverage) (K km s−1) |  [K] |
Luminosity (L′) (K km s1pc2) | Luminosity (L) (L⊙) | α (molecule) (M⊙/(K km s−1pc2)) | Acov [%] |  |
|
| (average spectrum) | 30” | 120” | ||||||
| 12CO J = 1−0 | 30.6 | 5.4 | 7300 | 1.7 × 100 | 0.43 | 78 | 92 | 1.2 |
| HCO+ J = 1−0 | 0.52 | 0.14 | 120 | 1.4 × 10−2 | 25 | 21 | 73 | 3.5 |
| HCN J = 1−0 | 0.46 | 0.06 | 110 | 1.2 × 10−2 | 29 | 16 | 60 | 3.8 |
| HNC J = 1−0 | 0.15 | 0.04 | 40 | 4.1 × 10−3 | 88 | 9 | 33 | 3.8 |
Notes. (2), (3): Line intensity and line peak temperature of the average spectrum in the mapped area. (4) and (5): Line luminosity in K km s−1 pc2 and L⊙ units. (6) Dense gas mass Mdg to line luminosity ratio, where Mdg = 3.1 × 103 M⊙ (mass at AV > 8 mag). (7) and (8): Percentage of the mapped area with 3σ line detections. (9): Ratio of cloud areas with 3σ line detection after spatial smoothing.
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