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Observations and statistical studies have shown that giant planets are rarearound M dwarfs compared with Sun-like stars. The formation mechanism of theseextreme systems remains under debate for decades. With the help of the TESSmission and ground based follow-up observations, we report the discovery ofTOI-4201b, the most massive and densest hot Jupiter around an M dwarf known sofar with a radius of $1.22\pm 0.04\ R_J$ and a mass of $2.48\pm0.09\ M_J$,about 5 times heavier than most other giant planets around M dwarfs. It alsohas the highest planet-to-star mass ratio ($q\sim 4\times 10^{-3}$) among suchsystems. The host star is an early-M dwarf with a mass of $0.61\pm0.02\M_{\odot}$ and a radius of $0.63\pm0.02\ R_{\odot}$. It has significantsuper-solar iron abundance ([Fe/H]=$0.52\pm 0.08$ dex). However, interiorstructure modeling suggests that its planet TOI-4201b is metal-poor, whichchallenges the classical core-accretion correlation of stellar-planetmetallicity, unless the planet is inflated by additional energy sources.Building on the detection of this planet, we compare the stellar metallicitydistribution of four planetary groups: hot/warm Jupiters around G/M dwarfs. Wefind that hot/warm Jupiters show a similar metallicity dependence around G-typestars. For M dwarf host stars, the occurrence of hot Jupiters shows a muchstronger correlation with iron abundance, while warm Jupiters display a weakerpreference, indicating possible different formation histories.

A massive hot Jupiter orbiting a metal-rich early-M star discovered in the TESS full frame images