Kinetic temperature of massive star-forming molecular clumps measured with formaldehyde. IV. The ALMA view of N113 and N159W in the LMC

We mapped the kinetic temperature structure of two massive star-forming regions, N113 and N159W, in Large Magellanic Cloud (LMC). have used $\sim$1\hbox{$\,.\!\!^{\prime\prime}$}6\,($\sim$0.4\,pc) resolution measurements para-H$_2$CO\,$J_{\rm K_ aK_c}$\,=\,3$_{03}$--2$_{02}$, 3$_{22}$--2$_{21}$, 3$_{21}$--2$_{20}$ transitions near 218.5\,GHz to constrain RADEX non-LTE models physical conditions. The gas temperatures derived from para-H$_2$CO line ratios 3$_{22}$--2$_{21}$/3$_{03}$--2$_{02}$ 3$_{21}$--2$_{20}$/3$_{03}$--2$_{02}$ range 28 105\,K 29 68\,K N159W. Distributions dense traced by agree with those 1.3\,mm dust \emph{Spitzer}\,8.0\,$\mu$m emission, but do not significantly correlate H$\alpha$ emission. high ($T_{\rm kin}$\,$\gtrsim$\,50\,K) appear be correlated embedded infrared sources inside clouds and/or YSOs N159W regions. lower kin}$\,$<$\,50\,K) are measured at outskirts H$_2$CO-bearing distributions both It seems that weakly affected external non-thermal velocity dispersions well region, implying higher is related turbulence on a $\sim$0.4\,pc scale. heating appears dominated internal star formation activity, radiation, turbulence. mechanism regions LMC consistent Galactic located plane.