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Understanding the temperature structure of protoplanetary disks is key tointerpreting observations, predicting the physical and chemical evolution ofthe disk, and modeling planet formation processes. In this study, we constrainthe two-dimensional thermal structure of the disk around Herbig Ae star HD163296. Using the thermo-chemical code RAC2D, we derive a thermal structurethat reproduces spatially resolved ALMA observations (~0.12 arcsec (13 au) -0.25 arcsec (26 au)) of CO J = 2-1, 13CO J = 1-0, 2-1, C18O J = 1-0, 2-1, andC17O J = 1-0, the HD J = 1-0 flux upper limit, the spectral energy distribution(SED), and continuum morphology. The final model incorporates both a radialdepletion of CO motivated by a time scale shorter than typical CO gas-phasechemistry (0.01 Myr) and an enhanced temperature near the surface layer of thethe inner disk (z/r <= 0.21). This model agrees with the majority of theempirically derived temperatures and observed emitting surfaces derived fromthe J = 2-1 CO observations. We find an upper limit for the disk mass of 0.35Msun, using the upper limit of the HD J = 1-0 and J = 2-1 flux. With our finalthermal structure, we explore the impact that gaps have on the temperaturestructure constrained by observations of the resolved gaps. Adding a large gapin the gas and small dust additionally increases gas temperature in the gap byonly 5-10%. This paper is part of the MAPS special issue of the AstrophysicalJournal Supplement.

Molecules with ALMA at Planet-forming Scales (MAPS) XVII: Determining the 2D Thermal Structure of the HD 163296 Disk