An international team of astronomers has captured the most detailed views to date of the mysterious filaments surrounding the giant galaxy M87. These long, thread-like structures are observed to move, evolve, and interact with their galactic environment, significantly influenced by the activity of the supermassive black hole at M87's core. Located approximately 55 million light-years away, M87 is a supergiant elliptical galaxy renowned for its extremely active central black hole, which contains about 6.5 billion solar masses. This black hole, first imaged by the Event Horizon Telescope (EHT), plays a crucial role in shaping these surrounding filaments. New observations, utilizing ground-based telescopes, reveal that the filaments are not static but dynamic, constantly interacting with the black hole's outflows and jets. The research indicates that these filaments are 'living' evidence of how the black hole impacts its host galaxy, even at great distances from its center. A mix of processes, including the black hole's jets, stellar explosions, and the interaction between hot and cold gas, appear to collectively shape and move these structures. M87 is noted as the closest known galaxy to host such extensive filamentary structures, making it a unique laboratory for studying these phenomena. The study, published in Monthly Notices of the Royal Astronomical Society, provides a comprehensive view of the filaments' motions, composition, and their intricate connections to the surrounding galactic environment and the central black hole's activity. Further analysis of EHT data has also shown dynamic changes in the magnetic fields around M87's black hole between 2017 and 2021. Polarization patterns have been observed to flip direction, indicating a turbulent and evolving environment. These findings offer new insights into how matter and energy behave in the extreme conditions surrounding black holes and how they power enormous jets. The consistency of the black hole's shadow size across different observation periods reinforces theoretical predictions, while the changes in polarization patterns highlight the dynamic nature of the accretion disk.