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We confirm the planetary nature of TOI-532b, using a combination of precisenear-infrared radial velocities with the Habitable-zone Planet Finder, TESSlight curves, ground based photometric follow-up, and high-contrast imaging.TOI-532 is a faint (J$\sim 11.5$) metal-rich M dwarf with Teff = $3957\pm69$ Kand [Fe/H] = $0.38\pm0.04$; it hosts a transiting gaseous planet with a periodof $\sim 2.3$ days. Joint fitting of the radial velocities with the TESS andground-based transits reveal a planet with radius of $5.82\pm0.19$R$_{\oplus}$, and a mass of $61.5_{-9.3}^{+9.7}$ M$_{\oplus}$. TOI-532b is thelargest and most massive super Neptune detected around an M dwarf with bothmass and radius measurements, and it bridges the gap between the Neptune-sizedplanets and the heavier Jovian planets known to orbit M dwarfs. It also followsthe previously noted trend between gas giants and host star metallicity for Mdwarf planets. In addition, it is situated at the edge of the Neptune desert inthe Radius--Insolation plane, helping place constraints on the mechanismsresponsible for sculpting this region of planetary parameter space.

TOI-532b: The Habitable-zone Planet Finder confirms a Large Super Neptune in the Neptune Desert orbiting a metal-rich M dwarf host