Solar physics uses the CHIANTI atomic physics database to obtain properties about various elements and ionisation states. By using observed elemental abundances and these ionization states, one can use CHIANTI to obtain synthetic spectra of solar plasma from various features, which inform a response function used by the observational instruments themselves. This response function is vital to understanding observations. The Atmospheric Imaging Assembly (AIA) is a multi-wavelength imager on the Solar Dynamics Observatory that specifically looks at the solar corona to understand magnetic processes. This project aims to use SunPy to infer plasma properties like temperature and density by developing the routines necessary to calculate two response functions for the AIA using Python and ChiantiPy. They are wavelength response functions that calculate the amount of flux per wavelength as measured by AIA, and temperature response functions that calculate the sensitivity of light from the plasma per temperature as measured by AIA.