Radiative Transfer and Starless Cores

We develop a method of analyzing radio frequency spectral line observations to derive data on the temperature, density, velocity, and molecular abundance of the emitting gas. The method incorporates a radiative transfer code with a new technique for handling overlapping hyperfine emission lines within the accelerated lambda iteration algorithm and a heuristic search algorithm based on simulated annnealing. We apply this method to new observations of N2H + in three Lynds clouds thought to be starless cores in the first stages of star formation and determine their density structure. A comparison of the gas densities derived from the molecular line emission and the millimeter dust emission suggests that the required dust mass opacity is about κ1.3mm = 0.04 cm 2 g−1, consistent with models of dust grains that have opacities enhanced by ice mantles and fluffy aggregrates. Subject headings: ISM: individual (L1544, L1489-NH3, L1517B) — ISM: molecules — Stars: formation — radiative transfer