TOI-732 TESS and CHEOPS detrended light curves

TOI-732 b is an ultra short period planet (P=0.76837931_-0.00000042_^+0.00000039^d) with a radius R_b_=1.325_-0.058_^+0.057^R_{Earth}_, a mass M_b_=2.46+/-0.19M_{Earth}_, and thus a mean density rho_b_=5.8_-0.8_^+1.0^g/cm^3^, while the outer planet at P=12.252284+/-0.000013d has R_c_=2.39_-0.11_^+0.10^R_{Earth}_, M_c_=8.04_-0.48_^+0.50^M_{Earth}_, and thus rho_c_=3.24_-0.43_^+0.55^g/cm^3^. Even with respect to the most recently reported values, this work yields to smaller uncertainties on the transit depths and on the RV semi-amplitudes up to a factor of ~1.6 and ~2.4 for TOI-732 b and c, respectively.

Both our interior structure calculations and the location of the planets in the Mass-Radius diagram leads us to classify TOI-732 b as a super-Earth and TOI-732 c as a mini-Neptune. Following the SVM approach, we quantified Rslope=-0.065_-0.013_^+0.024^, which is flatter than for Sun-like stars. In line with former analyses, we noted a more filled radius valley for M-planets and we further quantified the density valley slope as Rhoslope=-0.02_-0.04_^+0.12^.

Compared to FGK stars, the weaker dependence of the position of the radius valley with orbital period might indicate a heavier influence of formation relative to evolution mechanisms in shaping the radius valley around M-dwarfs.