2019MNRAS.483.5355M

We present a comparative study of physical properties derived from gas and dust emission in a sample of 1068 dense Galactic clumps. The sources are selected from the cross-match of the Herschel Infrared Galactic Plane Survey with 16 catalogues of NH₃ line emission in its lowest inversion (1,1) and (2,2) transitions. The sample covers a large range in masses and bolometric luminosities, with surface densities above Σ = 0.1 g cm^–2 and with low virial parameters α < 1. The comparison between dust and gas properties shows an overall agreement between T_kin and T_dust at volumetric densities n >= 1.2 x 10⁴ cm^–3, and a median fractional abundance χ(NH₃) = 1.46 x 10^–8. While the protostellar clumps in the sample have small differences between T_kin and T_dust, prestellar clumps have a median ratio T_kin/T_dust = 1.24, suggesting that these sources are thermally decoupled. A correlation is found between the evolutionary tracer L/M and the parameters T_kin/T_dust and χ(NH₃) in prestellar sources and protostellar clumps with L/M < 1 L_☉ M_☉^–1. In addition, a weak correlation is found between non-thermal velocity dispersion and the L/M parameter, possibly indicating an increase of turbulence with protostellar evolution in the interior of clumps. Finally, different processes are discussed to explain the differences between gas and dust temperatures in prestellar candidates, and the origin of non-thermal motions observed in the clumps.