We use TESS, Spitzer, ground-based light curves and HARPS spectrograph radial velocity measurements to establish the physical properties of the transiting exoplanet candidate TOI-674b. We perform a joint fit of the light curves and radial velocity time series to measure the mass, radius, and orbital parameters of the candidate. We confirm and characterize TOI-674b, a low-density super-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 $mathrm{M}_star=0.420pm 0.010$ M$_odot$, $mathrm{R}_star = 0.420pm 0.013$ R$_odot$, and $mathrm{T}_{mathrm{eff}} = 3514pm 57$ K, and is located at a distance $d=46.16 pm 0.03$ pc. Combining the available transit light curves plus radial velocity measurements and jointly fitting a circular orbit model, we find an orbital period of $1.977143 pm 3times 10^{-6}$ 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 similar planetary mass and radius values within the uncertainties. Given the measured planetary radius and mass, TOI-674b is one of the largest and most massive super-Neptune class planets discovered around an M type star to date. It is also a resident of the so-called Neptunian desert and a promising candidate for atmospheric characterisation using the James Webb Space Telescope.
تحميل البحث