The initial mass function (IMF) is a fundamental concept in astrophysics that describes the distribution of masses for newly formed stars. Despite significant progress in observational and theoretical studies, the shape of the IMF for the lowest masses remains uncertain. In this poster, we present the first results from our survey of the inner regions of the Orion Nebula Cluster (ONC) using the James Webb Space Telescope's Near-Infrared Camera (JWST NIRCam), aimed at determining the shape of the IMF in the planetary mass regime and establishing the opacity limit for star formation. Young star-forming regions such as the ONC provide an ideal laboratory for studying planetary mass objects as these faint sources are brightest when they are young. The ONC is particularly well-suited for this study, as it is the closest site of massive star formation, allowing for a statistically robust determination of the IMF while still being sensitive to the very lowest mass objects. Our work primarily focuses on the planetary mass regime, ranging from 1-13Mjup which is a key mass range for distinguishing between objects that form 'like stars' and 'like planets’. Determining the boundary between these two formation processes will provide crucial constraints on the competing theories of brown dwarf formation as well as empirically establish the opacity limit for star formation.