  The Sunyaev-Zeldovich thermal (tSZ) and kinetic (kSZ) effects can be used to
constrain the thermodynamic properties of pressure and density, respectively,
of galaxies and their surrounding regions. As SZ observations continue to
improve, it is important to understand any modeling systematics when inferring
properties from the data. Thus, a pipeline to forward model observed SZ
profiles was developed called Mop-c-GT. Previous studies have used this
repository to create modeled SZ profiles by selecting halos from the
IllustrisTNG simulation and found significant differences between the simulated
profiles and those recently measured by the Atacama Cosmology Telescope. There
are many uncertainties involved in modeling observed samples and in the forward
modeling process, so in this study, we explore methods implemented in Mop-c-GT
and in the selection of the simulated halos to test the effects on the
resulting modeled profiles. After testing several methods within the forward
modeling process and varying the halo selection from the simulation, we find
minimal differences between the simulated tSZ profiles of the original
calculation and the updated methods, indicating that the observations still
pose a challenge for the numerical methods used to describe the astrophysics of
these systems.
