Table 3
Veil line properties.
| Line | vlsr | Tline | Δv(FWHM) |
|---|---|---|---|
| (km s−1) | (K) | (km s−1) | |
| 8.98 ± 0.01 | 17.58 ± 0.07 | 5.02 ± 0.01 | |
| [CII] | 3.2 ± 0.1 | 1.82 ± 0.05 | 6.6 ± 0.2 |
| − 0.1 ± 0.4 | 0.70 ± 0.04 | 17.9 ± 0.5 | |
| C280α | 0.7 ± 1.0 | − 0.023 ± 0.003(a) | 11 ± 1 |
| C351α | 2.3 ± 0.8 | − 0.0061 ± 0.0008(b) | 10 ± 1 |
Notes. The line properties correspond to the best fit parameters of Gaussian line profiles and the errors quoted are 1 σ. The fits were performed to the spectra presented in Fig. 6. (a) To convert to optical depth we adopted a continuumtemperature of 195 ± 6 K. (b) Optical depth. The flux density of Orion A and M 43 measured from the LOFAR continuum image at 149 MHz is 53 ± 3 Jy.
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