Fire in the Heart: A Characterization of the High Kinetic Temperatures and Heating Sources in the Nucleus of NGC253

The nuclear starburst within the central similar to 15 \u27\u27 (similar to 250 pc; 1 \u27\u27 similar or equal to 17 pc) of NGC 253 has been extensively studied as a prototype for the starburst phase in galactic evolution. Atacama Large Millimeter/submillimeter Array (ALMA) imaging within receiver Bands 6 and 7 has been used to investigate the dense gas structure, kinetic temperature, and heating processes that drive the NGC 253 starburst. A total of 29 transitions from 15 molecular species/isotopologues have been identified and imaged at 1.\u27\u27 5-0.\u27\u27 4 resolution, allowing for the identification of five of the previously studied giant molecular clouds within the central molecular zone (CMZ) of NGC 253. Ten transitions from the formaldehyde (H2CO) molecule have been used to derive the kinetic temperature within the similar to 0.\u27\u27 5-5 \u27\u27 dense gas structures imaged. On similar to 5 \u27\u27 scales we measure T-K greater than or similar to 50 K, while on size scales less than or similar to 1 \u27\u27 we measure T-K greater than or similar to 300 K. These kinetic temperature measurements further delineate the association between potential sources of dense gas heating. We have investigated potential heating sources by comparing our measurements to models that predict the physical conditions associated with dense molecular clouds that possess a variety of heating mechanisms. This comparison has been supplemented with tracers of recently formed massive stars (Br gamma) and shocks ([Fe II]). Derived molecular column densities point to a radially decreasing abundance of molecules with sensitivity to cosmic-ray and mechanical heating within the NGC 253 CMZ. These measurements are consistent with radio spectral index calculations that suggest a higher concentration of cosmic-ray-producing supernova remnants within the central 10 pc of NGC 253