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Table 2

Summary of integrated line intensities from the observations and derived parameters.

Source Integration range [C ii] [13C ii] F = 2−1 F = 1−0 F = 1−1 IR a  ⟨ τ [CII]  ⟩  N C +  b
[  km s-1] [K  km s-1] [K  km s-1] [K  km s-1] [K  km s-1] [1018 cm-2]
Orion Bar, peak 7−13 857 ± 5 17.2 ± 1.0 7.8 ± 0.5 − 30 ± 2 1.9 ± 0.2 10.1
Orion Bar, ridgec 7−13 772 ± 5 12.6 ± 1.0 5.1 ± 0.5 − 38 ± 3 1.3 ± 0.2 7.2
Orion Bar, frontd 7−13 506 ± 7 4.3 ± 0.7 2.1 ± 0.6 − 69 ± 12 0.0 ± 0.4 2.3
Orion Bar, backe 7−13 529 ± 6 6.3 ± 0.6 2.9 ± 0.6 − 50 ± 6 0.7 ± 0.3 3.9
Mon R2, total 5−25 362 ± 5 − 2.9 ± 0.7 0.7 ± 0.5 38 ± 10 1.3 ± 0.6 5.7
Mon R2, blue 5−12.5 173 ± 3 − 2.4 ± 0.7 0.8 ± 0.3 20 ± 5 3.2 ± 0.8 4.8
Mon R2, red 12.5−25 188 ± 4 − 0.7 ± 0.5 −0.3 ± 0.4 170 ± 120 0.0 ± 0.5 0.9
NGC 3603 10−−19 130 ± 2 − 1.4 ± 0.2 0.55 ± 0.15 25 ± 5 2.4 ± 0.4 3.6
Carina N −20−−5 143 ± 4 − 1.3 ± 0.3 0.7 ± 0.3 27 ± 7 2.2 ± 0.6 5.0
Carina S −38−−25 38 ± 2 2.7 ± 0.3f −0.1 ± 0.3 0.0 ± 0.3  >22  <2.9 0.2g
NGC 7023 −1−7 91 ± 2 1.07 ± 0.05 0.53 ± 0.07 0.19 ± 0.04 51 ± 6 0.6 ± 0.3 1.0

Notes. 

(a)

[C ii]/[13C ii] intensity ratio. From the sum over all [13C ii] hyperfine components assuming the ratios from Table 1 to correct for non-detected components.

(b)

Assuming a uniform Gaussian velocity profile for C+ and 13C+.

(c)

Average over the  ≈ 1000 square-arcsec with I([C ii]) ≥ 700 K km s-1 representing the main Bar emission (see contours in Fig. 4).

(d)

Average over the  ≈ 750 square-arcsec with 450 K km s-1  ≤ I([C ii]) ≤ 650 K km s-1 north-west of the Bar.

(e)

Average over the  ≈ 900 square-arcssec with 450 K km s-1  ≤    I([C ii]) ≤ 650 K km s-1 south-east of the Bar.

(f)

The identification of this emission as [13C ii] F = 2−1 is questionable because of the small separation from the [C ii] line. It may rather represent a different velocity component.

(g)

Assuming τ = 0.0 to compute the column density.

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