The ionization fraction in OMC-2 and OMC-3

Salas Munoz, P.A.; Rugel, M.R.; Emig, K.L.; Kauffmann, J.; Menten, K.M.; Wyrowski, F.; Tielens, A.G.G.M.

doi:doi:10.1051/0004-6361/202140670

Context. The electron density (n) plays an important role in setting the chemistry and physics of the interstellar medium. However, measurements of n in neutral clouds have been directly obtained only toward a few lines of sight or they rely on indirect determinations. Aims. We use carbon radio recombination lines and the far-infrared lines of C to directly measure neand the gas temperature in the envelope of the integral shaped filament (ISF) in the Orion A molecular cloud. Methods. We observed the C102 alpha (6109.901 MHz) and C109 alpha (5011.420 MHz) carbon radio recombination lines (CRRLs) using the Effelsberg 100 m telescope at approximate to 2 ' resolution toward five positions in OMC-2 and OMC-3. Since the CRRLs have similar line properties, we averaged them to increase the signal-to-noise ratio of the spectra. We compared the intensities of the averaged CRRLs, and the 158 mu m-[CII] and [(CII)-C-13] lines to the predictions of a homogeneous model for the C/C interface in...Show moreContext. The electron density (n) plays an important role in setting the chemistry and physics of the interstellar medium. However, measurements of n in neutral clouds have been directly obtained only toward a few lines of sight or they rely on indirect determinations. Aims. We use carbon radio recombination lines and the far-infrared lines of C to directly measure neand the gas temperature in the envelope of the integral shaped filament (ISF) in the Orion A molecular cloud. Methods. We observed the C102 alpha (6109.901 MHz) and C109 alpha (5011.420 MHz) carbon radio recombination lines (CRRLs) using the Effelsberg 100 m telescope at approximate to 2 ' resolution toward five positions in OMC-2 and OMC-3. Since the CRRLs have similar line properties, we averaged them to increase the signal-to-noise ratio of the spectra. We compared the intensities of the averaged CRRLs, and the 158 mu m-[CII] and [(CII)-C-13] lines to the predictions of a homogeneous model for the C/C interface in the envelope of a molecular cloud and from this comparison we determined the electron density, temperature and C column density of the gas. Results. We detect the CRRLs toward four positions, where their velocity (v approximate to 11 km s) and widths (sigma v approximate to 1 km s) confirms that they trace the envelope of the ISF. Toward two positions we detect the CRRLs, and the 158 mu m-[CII] and [13CII] lines with a signal-to-noise ratio >= 5, and we find ne= 0.65 +/- 0.12 cm-3 and 0.95 +/- 0.02 cm(-3), which corresponds to a gas density nH approximate to 5 x 10(3) cm(-3) and a thermal pressure of p approximate to 4 x 10. We also constrained the ionization fraction in the denser portions of the molecular cloud using the HCN(1-0) and CH(1-0) lines to x(e) <= 3 x 10. Conclusions. The derived electron densities and ionization fraction imply that x(e) drops by a factor >= 100 between the Clayer and the regions probed by HCN(1-0). This suggests that electron collisional excitation does not play a significant role in setting the excitation of HCN(1-0) toward the region studied, as it is responsible for only approximate to 10% of the observed emission.Show less

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The ionization fraction in OMC-2 and OMC-3