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Planet formation occurs around a wide range of stellar masses and stellarsystem architectures. An improved understanding of the formation process can beachieved by studying it across the full parameter space, particularly towardthe extremes. Earlier studies of planets in close-in orbits around high-massstars have revealed an increase in giant planet frequency with increasingstellar mass until a turnover point at 1.9 solar masses, above which thefrequency rapidly decreases. This could potentially imply that planet formationis impeded around more massive stars, and that giant planets around starsexceeding 3 solar masses may be rare or non-existent. However, the methods usedto detect planets in small orbits are insensitive to planets in wide orbits.Here we demonstrate the existence of a planet at 560 times the Sun-Earthdistance from the 6-10 solar mass binary b Centauri through direct imaging. Theplanet-to-star mass ratio of 0.10-0.17% is similar to the Jupiter-Sun ratio,but the separation of the detected planet is ~100 times wider than that ofJupiter. Our results show that planets can reside in much more massive stellarsystems than what would be expected from extrapolation of previous results. Theplanet is unlikely to have formed in-situ through the conventional coreaccretion mechanism, but might have formed elsewhere and arrived to its presentlocation through dynamical interactions, or might have formed via gravitationalinstability.

A wide-orbit giant planet in the high-mass b Centauri binary system