Kinetic temperature of massive star-forming molecular clumps measured with formaldehyde V. The massive filament DR21

The kinetic temperature structure of the massive filament DR21 has been mapped using the IRAM 30 m telescope.

This mapping employed the para-H$_2$CO triplet ($J_{\rm K_aK_c}$ = 3$_{03}$--2$_{02}$, 3$_{22}$--2$_{21}$, and 3$_{21}$--2$_{20}$) on a scale of $\sim$0.1 pc.

By modeling the averaged line ratios of para-H$_{2}$CO with RADEX under non-LTE assumptions, the kinetic temperature of the dense gas was derived at a density of $n$(H$_{2}$) = 10$^{5}$ cm$^{-3}$.

The para-H$_2$CO lines reveal significantly higher temperatures than NH$_3$ (1,1)/(2,2) and FIR wavelengths.

The dense clumps appear to correlate with the notable kinetic temperature.

Among the four dense cores (N44, N46, N48, and N54), temperature gradients are observed on a scale of $\sim$0.1-0.3 pc.

This suggests that the warm dense gas is influenced by internal star formation activity.

With the exception of N54, the temperature profiles of these cores were fitted with power-law indices ranging from $-$0.3 to $-$0.5.

This indicates that the warm dense gas is heated by radiation emitted from internally embedded protostar(s) and/or clusters.

While there is no direct evidence supporting the idea that the dense gas is heated by shocks resulting from a past explosive event in the DR21 region, our measurements toward the DR21W1 region provide compelling evidence that the dense gas is indeed heated by shocks originating from the western DR21 flow.

Higher temperatures appear to be associated with turbulence.

The physical parameters of the dense gas in the DR21 filament exhibit a remarkable similarity to the results obtained in OMC-1 and N113.

This may imply that the physical mechanisms governing the dynamics and thermodynamics of dense gas traced by H$_{2}$CO in diverse star formation regions may be dominated by common underlying principles despite variations in specific environmental conditions.

(abbreviated) ;Comment: 16 pages, 8 figures, 3 tabels.

Accepted for publication by Astronomy & Astrophysics