Table 4
Comparison between the observed intensities ∫Idυ or fluxes !IdυdΩ of the rotational lines of CH+ and those predicted by MADEX for the selected astronomical sources.
| Parameter | Cold diffuse medium | Orion Bar | NGC 7027 | |||||||||
|
|
||||||||||||
| nH (cm-3) | 50 | 5 × 104 | 2 × 105 | |||||||||
| χ opt | 1–50 | 3 × 104 | 4 × 104 | |||||||||
| χ nir | 1–50 | 3 × 104 | 2 × 105 | |||||||||
| χ fir | 1–10 | 1 | 1 | |||||||||
| T fir | 18 | 55 | 150 | |||||||||
| τ fir | 1.7 × 10-5 | 5 × 10-2 | 1 × 10-2 | |||||||||
| β fir | 2.0 | 1.75 | 0.5 | |||||||||
| υexp (km s-1) | 5 | 10 | 20 | |||||||||
| Ω (sr) | 2.7 × 10-8 | 1.2 × 10-9 | ||||||||||
|
|
||||||||||||
| Transition | Intensity | Flux | Flux | |||||||||
| (in 10-10 erg s-1 cm-2 sr-1) | (in 10-14 erg s-1 cm-2) | (in 10-19 W cm-2) | ||||||||||
| ❶ | ❷ | ❸ | obsa | ❶ | ❷ | ❸ | obsb | ❶ | ❷ | ❸ | obsc | |
| J = 1−0 | 2.7 | 4.5 | 5.9 | <79 | 9.3 | 11.8 | 11.8 | 11.1 ± 1.8 | 0.4 | 0.5 | 0.5 | 0.47 ± 0.01 |
| J = 2−1 | 3.7 | 7.1 | 9.5 | <480 | 13.2 | 18.1 | 18.3 | 1.6 | 2.0 | 2.0 | 1.51 ± 0.05 | |
| J = 3−2 | 2.4 | 7.0 | 9.7 | 6.7 | 13.8 | 13.9 | 2.1 | 2.5 | 2.5 | 2.18 ± 0.17 | ||
| J = 4−3 | 2.3 | 7.7 | 1.1 | 6.1 | 13.4 | 13.5 | 1.6 | 2.1 | 2.1 | 2.00 ± 0.22 | ||
| J = 5−4 | 1.1 | 6.6 | 9.6 | 3.0 | 8.3 | 8.4 | 1.1 | 1.7 | 1.7 | 2.50 ± 0.41 | ||
| J = 6−5 | 1.1 | 6.3 | 9.2 | 2.9 | 7.5 | 7.6 | 0.7 | 1.3 | 1.3 | 2.41 ± 0.33 | ||
Notes. In all cases, MADEX was run in the three configurations ❶, ❷, and ❸ (see main text), and the far-infrared continuum emission was removed in the computation of the line intensities.
Detection limits computed with the rms noise level of the CH+ (1−0) and (2−1) spectra with the Herschel/HIFI instrument (Godard et al. 2012; M. Gerin, priv. comm.);
from Naylor et al. (2010) and Habart et al. (2010);
from Cernicharo et al. (1997) and Wesson et al. (2010).
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