Abstract: The Boomerang Supernova Remnant (SNR G106-3+2.7) is a complex system discovered in 1990 with the Dominion Radio Astronomical Observatory, and has been the object of intense observational studies from radio up to gamma-rays since then. The source displays a comet-shaped morphology, with a "Head" and a "Tail" region associated to a powerful pulsar (PSR J2229+6114) and its Pulsar Wind Nebula, and to the interaction of the SNR with the surrounding gas, respectively. Recently, the system has also been detected at UHE gamma-rays with the HAWC and  LHAASO detectors, making it one of the most promising candidates for the acceleration of high-energy galactic cosmic-rays. However, the exact origin of this high-energy gamma-ray emission keeps being highly controversial.

In this work, I will discuss the results of a morphological study carried out on the Boomerang SNR with data obtained by the MAGIC telescopes and making use of next-generation open-source analysis tools like Gammapy and Pybkgmodel. These software tools allow a novel 3D-analysis technique appropriate for extended sources with energy-dependent morphologies. The possibility to use different background estimation methods for such extended-source analyses will become crucial in VHE astronomy in the coming years. In my presentation I will discuss some preliminary results of the project, the challenges implied with this novel approach, and I will provide an outlook on future developments along that line.