The direct imaging of three planets orbiting the star HR 8799 reveals their projected separations of 24, 38, and 68 astronomical units. These planets exhibit counter-clockwise orbital motion and have masses between 5 and 13 times that of Jupiter. The system resembles a scaled-up version of the outer Solar System. Direct imaging allows the characterization of planetary atmospheres and is key to detecting Earth-like planets. High-contrast observations with the Keck and Gemini telescopes have confirmed these planets. The system's age is estimated to be between 30 and 160 million years, with a more conservative upper limit of ~5σ of the Pleiades age. The planets' low luminosity and the system's youth suggest they are not brown dwarfs but have planetary masses. The HR 8799 system has a debris disk with a mass of 0.1 Earth masses, indicating a massive protoplanetary disk. The planets' orbital radii and masses challenge the core accretion scenario, suggesting possible formation through gravitational instability. The planets' atmospheres are cool and dusty, with colors similar to brown dwarfs. The system's planets orbit in the same direction as our Solar System's planets, consistent with disk-based planet formation models. The HR 8799 system is a rare example of a young star with a massive debris disk, providing insights into planet formation and evolution. The study highlights the importance of direct imaging in detecting and characterizing exoplanets, especially those in wide orbits. The findings support the existence of planetary-mass companions and provide indirect evidence for their formation mechanisms. The system's planets are consistent with formation through instabilities in a massive protoplanetary disk, but the core accretion scenario cannot be ruled out. The presence of these massive planets leaves room for other Jovian-mass planets or even lower mass terrestrial planets in the inner part of the system. The study also indicates that Jovian-mass planetary companions to early-type stars are more common at separations beyond ~20 AU. The HR 8799 system is a significant discovery in exoplanet research, offering a unique opportunity to study planetary formation and evolution in a young, wide-orbit system.The direct imaging of three planets orbiting the star HR 8799 reveals their projected separations of 24, 38, and 68 astronomical units. These planets exhibit counter-clockwise orbital motion and have masses between 5 and 13 times that of Jupiter. The system resembles a scaled-up version of the outer Solar System. Direct imaging allows the characterization of planetary atmospheres and is key to detecting Earth-like planets. High-contrast observations with the Keck and Gemini telescopes have confirmed these planets. The system's age is estimated to be between 30 and 160 million years, with a more conservative upper limit of ~5σ of the Pleiades age. The planets' low luminosity and the system's youth suggest they are not brown dwarfs but have planetary masses. The HR 8799 system has a debris disk with a mass of 0.1 Earth masses, indicating a massive protoplanetary disk. The planets' orbital radii and masses challenge the core accretion scenario, suggesting possible formation through gravitational instability. The planets' atmospheres are cool and dusty, with colors similar to brown dwarfs. The system's planets orbit in the same direction as our Solar System's planets, consistent with disk-based planet formation models. The HR 8799 system is a rare example of a young star with a massive debris disk, providing insights into planet formation and evolution. The study highlights the importance of direct imaging in detecting and characterizing exoplanets, especially those in wide orbits. The findings support the existence of planetary-mass companions and provide indirect evidence for their formation mechanisms. The system's planets are consistent with formation through instabilities in a massive protoplanetary disk, but the core accretion scenario cannot be ruled out. The presence of these massive planets leaves room for other Jovian-mass planets or even lower mass terrestrial planets in the inner part of the system. The study also indicates that Jovian-mass planetary companions to early-type stars are more common at separations beyond ~20 AU. The HR 8799 system is a significant discovery in exoplanet research, offering a unique opportunity to study planetary formation and evolution in a young, wide-orbit system.