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Using high angular resolution ALMA observations($0.02^{\prime\prime}\approx0.34$ pc), we study the thermal structure andkinematics of the proto super star cluster $13$ in the central region of NGC253through their continuum and vibrationally excited HC$_3$N emission from$J=24-23$ and $J=26-25$ lines arising from vibrational states up to $v_4=1$. Wehave carried 2D-LTE and non-local radiative transfer modelling of the radialprofile of the HC$_3$N and continuum emission in concentric rings of $0.1$ pcwidth. From the 2D-LTE analysis, we found a Super Hot Core (SHC) of $1.5$ pcwith very high vibrational temperatures ($>500$ K), and a jump in the radialvelocity ($21$ km s$^{-1}$) in the SE-NW direction. From the non-local models,we derive the HC$_3$N column density, H$_2$ density and dust temperature($T_\text{dust}$) profiles. Our results show that the thermal structure of theSHC is dominated by the greenhouse effect due to the high dust opacity in theIR, leading to an overestimation of the LTE $T_\text{dust}$ and its derivedluminosity. The kinematics and $T_\text{dust}$ profile of the SHC suggest thatstar formation was likely triggered by a cloud-cloud collision. We compareproto-SSC $13$ to other deeply embedded star-forming regions, and discuss theorigin of the $L_\text{IR}/M_{\text{H}_2}$ excess above $\sim100$ L$_\odot$M$_\odot^{-1}$ observed in (U)LIRGs.

On the thermal structure of the proto-Super Star Cluster 13 in NGC 253