2014MNRAS.441.1964B

While recent studies of the solar-mass protostar IRAS 16293-2422 have focused on its inner arcsecond, the wealth of Herschel/Heterodyne Instrument for the Far-Infrared (HIFI) data has shown that the structure of the outer envelope and of the transition region to the more diffuse interstellar medium is not clearly constrained. We use rotational ground-state transitions of CH (methylidyne), as a tracer of the lower density envelope. Assuming local thermodynamic equilibrium, we perform a χ2 minimization of the high spectral resolution HIFI observations of the CH transitions at ∼ 532 and ∼ 536GHz in order to derive column densities in the envelope and in the foreground cloud. We obtain column densities of (7.7±0.2)x10¹³/cm2 and (1.5±0.3)x10¹³/cm2, respectively. The chemical modelling predicts column densities of (0.5 - 2)x10¹³/cm2 in the envelope (depending on the cosmic ray ionization rate), and 5x10¹¹ to 2.5x10¹⁴/cm2 in the foreground cloud (depending on time). Both observed abundances are reproduced by the model at a satisfactory level. The constraints set by these observations on the physical conditions in the foreground cloud are however weak. Furthermore, the CH abundance in the envelope is strongly affected by the rate coefficient of the reaction H+CH⟶C+H2; further investigation of its value at low temperature would be necessary to facilitate the comparison between the model and the observations.