2008A&A...482..535H

Cold cores in interstellar molecular clouds represent the very first phase in star formation. The physical conditions of these objects are studied in order to understand how molecular clouds evolve and how stellar masses are determined. The purpose of this study is to probe conditions in the dense, starless clump Ophichus D (Oph D). The ground-state (1₁₀->1₁₁) rotational transition of ortho-H₂D⁺ was observed with APEX towards the density peak of Oph D. The width of the H₂D⁺ line indicates that the kinetic temperature in the core is about 6K. So far, this is the most direct evidence of such cold gas in molecular clouds. The observed H₂D⁺ spectrum can be reproduced with a hydrostatic model with the temperature increasing from about 6K in the centre to almost 10K at the surface. The model is unstable against any increase in the external pressure, and the core is likely to form a low-mass star. The results suggest that an equilibrium configuration is a feasible intermediate stage of star formation even if the larger scale structure of the cloud is thought to be determined by turbulent fragmentation. In comparison with the isothermal case, the inward decrease in the temperature makes smaller, i.e. less massive, cores susceptible to externally triggered collapse.