Why is it so difficult to fit a consistent atmosphere on Jupiter?

The distribution of trace gases and their variation with time in the giant planets' atmosphere is key to address fundamental questions about the formation environment of the planets and the dynamics that shape the current climate. On Jupiter water and ammonia vapor, key ingredients to answer these fundamental questions, are hidden below various layers of clouds, obstructing their exploration using remote-sensing observations. Only at the radio wavelengths the clouds become translucent to radiations, allowing us to explore the structure and dynamics below the cloud layers. We extend the high spectral resolution observation of the Very Large Array (VLA) in New Mexico with the long-wavelength observations of NASA's Juno Microwave Radiometer (MWR) data to study the distribution of the relevant trace gases on Jupiter. For this, we re-calibrate the Juno observations and derive nadir brightness temperature, its dependence on the emission angle, and the corresponding uncertainty. We combine VLA and MWR data to fit the atmosphere using a Markov-Chain Monte-Carlo method applied to a thermodynamic model and show how the atmosphere changes over the course of months and years. We focus especially on the robustness of the signal and the degeneracy in the inversion when deriving the atmospheric structure, and highlight the crucial ingredients missing for a robust understanding of Jupiter's atmosphere.