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... 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
Emig, K.L.; Salas Munoz, P.A.; Gasperin, F. de; Oonk, J.B.R.; Toribio Perez, M.C.; Mechev, A.P.; ... ; Tielens, A.G.G.M. 2020
The Low Frequency Array enables studies of low-frequency carbon radio recombination lines with unprecedented sensitivity, spectral and spatial resolution. In this thesis we benefit from the... Show moreThe Low Frequency Array enables studies of low-frequency carbon radio recombination lines with unprecedented sensitivity, spectral and spatial resolution. In this thesis we benefit from the capabilities of LOFAR to study the cold interstellar medium through carbon radio recombination lines. We find that at low-frequencies these lines trace cold gas, associated with the C+/CI/CO interface of photo-dissociation regions. This opens up the possibility to study these interfaces over large regions of the Milky Way. Show less
Quantitative understanding of the interstellar medium requires knowledge of its physical conditions. Low-frequency carbon radio recombination lines (CRRLs) trace cold interstellar gas and can be... Show moreQuantitative understanding of the interstellar medium requires knowledge of its physical conditions. Low-frequency carbon radio recombination lines (CRRLs) trace cold interstellar gas and can be used to determine its physical conditions (e.g. electron temperature and density). In this work, we present spatially resolved observations of the low-frequency (≤390 MHz) CRRLs centred around C268α, C357α, C494α, and C539α towards Cassiopeia A on scales of ≤1.2 pc. We compare the spatial distribution of CRRLs with other interstellar medium tracers. This comparison reveals a spatial offset between the peak of the CRRLs and other tracers, which is very characteristic for photodissociation regions and that we take as evidence for CRRLs being preferentially detected from the surfaces of molecular clouds. Using the CRRLs, we constrain the gas electron temperature and density. These constraints on the gas conditions suggest variations of less than a factor of 2 in pressure over ˜1 pc scales, and an average hydrogen density of 200-470 cm-3. From the electron temperature and density maps, we also constrain the ionized carbon emission measure, column density, and path length. Based on these, the hydrogen column density is larger than 1022 cm-2, with a peak of ˜4 × 1022 cm-2 towards the south of Cassiopeia A. Towards the southern peak, the line-of-sight length is ˜40 pc over a ˜2 pc wide structure, which implies that the gas is a thin surface layer on a large (molecular) cloud that is only partially intersected by Cassiopeia A. These observations highlight the utility of CRRLs as tracers of low-density extended H I and CO-dark gas halo's around molecular clouds. Show less
We present a study of carbon radio recombination lines towards Cassiopeia A using low frequency array (LOFAR) observations in the frequency range 10-33 MHz. Individual carbon α lines are detected... Show moreWe present a study of carbon radio recombination lines towards Cassiopeia A using low frequency array (LOFAR) observations in the frequency range 10-33 MHz. Individual carbon α lines are detected in absorption against the continuum at frequencies as low as 16 MHz. Stacking several Cα lines we obtain detections in the 11-16 MHz range. These are the highest signal-to-noise measurements at these frequencies. The peak optical depth of the Cα lines changes considerably over the 11-33 MHz range with the peak optical depth decreasing from 4 × 10-3 at 33 MHz to 2 × 10-3 at 11 MHz, while the linewidth increases from 20 km s-1 to ˜150 km s-1. The combined change in peak optical depth and linewidth results in a roughly constant integrated optical depth. We interpret this as carbon atoms close to local thermodynamic equilibrium. In this work, we focus on how the 11-33 MHz carbon radio recombination lines can be used to determine the gas physical conditions. We find that the ratio of the carbon radio recombination lines to that of the 158 μm [C II] fine-structure line is a good thermometer, while the ratio between low-frequency carbon radio recombination lines provides a good barometer. By combining the temperature and pressure constraints with those derived from the linewidth, we are able to constrain the gas properties (electron temperature and density) and radiation field intensity. Given the 1σ uncertainties in our measurements these are: Te ≈ 68-98 K, ne ≈ 0.02-0.035 cm-3 and Tr,100 ≈ 1500-1650 K. Despite challenging radio frequency interference and ionospheric conditions, our work demonstrates that observations of carbon radio recombination lines in the 10-33 MHz range can provide insight into the gas conditions. Show less
