Radial temperature profiles for IRAS 16293A derived in this work from H₂ CS transitions (blue lines) compared to dust (black lines and circles) and gas (orange lines) temperature profiles from the literature. The H₂CS temperature profile in the left panel is derived from the 7_2,6–6_2,5/7_4,3–6_4,2 line ratio and the profile in the right panel is based on fits to the peak flux rotation diagrams including only transitions with E_up < 200 K. The blue shaded area represents the 1σ uncertainty. The dashed black line shows the IRAS 16293 dust temperature assuming an envelope around a central source of 27 L_⊙ (Schöier et al. 2002), and the black dots represents dust temperature contours for IRAS 16293A from detailed modeling including both protostars and the bridge structure (Jacobsen et al. 2018). The gas temperatures are based on H₂ O observations with the ISO satellite using a model that computes the gas temperature through an envelope by solving a chemical network and equating the heating and cooling rates (Ceccarelli et al. 1996). The solid orange line shows the initial results assuming a single 27 L_⊙ protostar at 160 pc (Ceccarelli et al. 2000), the dashed orange line presents the revised results for a 22 L_⊙ protostar at 120 pc (Crimier et al. 2010). The dashed yellow line shows the midplane gas temperature for the Class 0/I disk L1527 based on optically thick ¹³CO and C¹⁸O emission (van ’t Hoff et al. 2018). The horizontal bar marks the beam size of the H₂ CS observations.