Modeling Gas Emission from the Debris Disk around HD 110058

The discovery of gas in debris disks is a relatively recent accomplishment due to the high resolution and sensitivity of the Atacama Large Millimeter/submillimeter Array (ALMA). ALMA has allowed for the discovery of CO as the sole molecular gas detected in debris disks. By assuming Keplerian rotation of the detected gas, we can combine high-resolution 12CO(2-1) and (3-2) from ALMA with precise stellar parallaxes from Gaia to derive a dynamical mass for the host star. We measured velocity as a function of distance from the star by observing the redshift and blueshift of CO emission lines. As part of a larger project to measure the dynamical mass of all gas-bearing debris disk host stars, we found that our modeling code was producing results consistent with existing literature, except for disks observed close to edge-on. To understand what might be going wrong we sought to reproduce the results of Hales et al. (2022) who produced the parameters of the disk around HD 110058, one of the high inclination disks we had failed to produce consistent results for. Using the parameters from Hales et al. (2022), our code produced model spectra several orders of magnitude fainter than the corresponding ALMA data. Through extensive testing we were able to identify one actual bug in the code related to the geometry of observing disks at close to edge on. We also investigated differing assumptions made between the two different code repositories being used. Further inconsistencies appeared to be resolvable by investigating the numerical values for radius, height, and velocity used in the radiative transfer gridding for the model produced by the code and to what extent do they affect the predicted flux.