# Thermal balance and comparison of gas and dust properties of dense clumps in the Hi-GAL survey

## TL;DR

This study compares gas and dust properties in over a thousand dense Galactic clumps, revealing thermal decoupling in prestellar stages and correlations with evolutionary indicators, enhancing understanding of star formation processes.

## Contribution

It provides a comprehensive comparison of gas and dust temperatures and abundances in a large sample, highlighting thermal decoupling and evolutionary trends in dense clumps.

## Key findings

- Gas and dust temperatures agree at high densities
- Prestellar clumps show thermal decoupling with higher T_kin/T_dust ratios
- Turbulence increases with protostellar evolution

## Abstract

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 crossmatch of the Hi-GAL survey with 16 catalogues of NH$_3$ 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 $\Sigma=0.1$ g cm$^{-2}$ and with low virial parameters $\alpha<1$. The comparison between dust and gas properties shows an overall agreement between $T_{\textit{kin}}$ and $T_{\textit{dust}}$ at volumetric densities $n\gtrsim1.2\times10^{4}$ cm$^{-3}$, and a median fractional abundance $\chi$(NH$_3$)$=1.46\times10^{-8}$. While the protostellar clumps in the sample have small differences between $T_{\textit{kin}}$ and $T_{\textit{dust}}$, prestellar clumps have a median ratio $T_{\textit{kin}}/T_{\textit{dust}}=1.24$, suggesting that these sources are thermally decoupled. A correlation is found between the evolutionary tracer $L/M$ and the parameters $T_{\textit{kin}}/T_{\textit{dust}}$ and $\chi$(NH$_3$) in prestellar sources and protostellar clumps with $L/M<1$ L$_\odot$ M$_\odot^{-1}$. 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.