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We use TESS, Spitzer, ground-based light curves and HARPS spectrograph radialvelocity measurements to establish the physical properties of the transitingexoplanet candidate TOI-674b. We perform a joint fit of the light curves andradial velocity time series to measure the mass, radius, and orbital parametersof the candidate. We confirm and characterize TOI-674b, a low-densitysuper-Neptune transiting a nearby M dwarf. The host star (TIC 158588995, $V =14.2$ mag, $J = 10.3$ mag) is characterized by its M2V spectral type with$\mathrm{M}_\star=0.420\pm 0.010$ M$_\odot$, $\mathrm{R}_\star = 0.420\pm0.013$ R$_\odot$, and $\mathrm{T}_{\mathrm{eff}} = 3514\pm 57$ K, and islocated at a distance $d=46.16 \pm 0.03$ pc. Combining the available transitlight curves plus radial velocity measurements and jointly fitting a circularorbit model, we find an orbital period of $1.977143 \pm 3\times 10^{-6}$ days,a planetary radius of $5.25 \pm 0.17$ $\mathrm{R}_\oplus$, and a mass of $23.6\pm 3.3$ $\mathrm{M}_\oplus$ implying a mean density of $\rho_\mathrm{p} = 0.91\pm 0.15$ [g cm$^{-3}$]. A non-circular orbit model fit delivers similarplanetary mass and radius values within the uncertainties. Given the measuredplanetary radius and mass, TOI-674b is one of the largest and most massivesuper-Neptune class planets discovered around an M type star to date. It isalso a resident of the so-called Neptunian desert and a promising candidate foratmospheric characterisation using the James Webb Space Telescope.

TOI-674b: an oasis in the desert of exo-Neptunes transiting a nearby M dwarf