TOI-132 b: A short-period planet in the Neptune desert transiting a v = 11.3 G-type star

The Neptune desert is a feature seen in the radius-period plane, whereby a notable dearth of short period, Neptune-like planets is found. Here, we report the Transiting Exoplanet Survey Satellite (TESS) discovery of a new short-period planet in the Neptune desert, orbiting the G-type dwarf TYC8003-1117-1 (TOI-132). TESS photometry shows transit-like dips at the level of ∼1400 ppm occurring every ∼2.11 d. High-precision radial velocity follow-up with High Accuracy Radial Velocity Planet Searcher confirmed the planetary nature of the transit signal and provided a semi-amplitude radial velocity variation of 11.38+0.84-0.85 ms-1, which, when combined with the stellar mass of 0.97 ± 0.06 M⊙, provides a planetary mass of 22.40+1.90-1.92 M⊕. Modelling the TESS light curve returns a planet radius of 3.42+0.13-0.14 R⊕, and therefore the planet bulk density is found to be 3.08+0.44-0.46 g cm-3. Planet structure models suggest that the bulk of the planet mass is in the form of a rocky core, with an atmospheric mass fraction of 4.3+1.2-2.3 per cent. TOI-132 b is a TESS Level 1 Science Requirement candidate, and therefore priority follow-up will allow the search for additional planets in the system, whilst helping to constrain low-mass planet formation and evolution models, particularly valuable for better understanding of the Neptune desert

It takes two planets in resonance to tango around K2-146

Stars and planetary system

Hot planets around cool stars - two short-period mini-Neptunes transiting the late K-dwarf TOI-1260

Stars and planetary system

K2-280 b - a low density warm sub-Saturn around a mildly evolved star

Stars and planetary system

GJ 367b: a dense, ultrashort-period sub-Earth planet transiting a nearby red dwarf star

Stars and planetary system

Mass determinations of the three mini-Neptunes transiting TOI-125

Stars and planetary system

Discovery of TOI-1260d and the characterization of the multiplanet system

We report the discovery of a third planet transiting the star TOI-1260, previously known to host two transiting sub-Neptune planets with orbital periods of 3.127 and 7.493 d, respectively. The nature of the third transiting planet with a 16.6-d orbit is supported by ground-based follow-up observations, including time-series photometry, high-angular resolution images, spectroscopy, and archival imagery. Precise photometric monitoring with CHEOPS allows to improve the constraints on the parameters of the system, improving our knowledge on their composition. The improved radii of TOI-1260b and TOI-1260c are 2.36 ± 0.06 R⊕, 2.82 ± 0.08 R⊕ , respectively while the newly discovered third planet has a radius of 3.09 ± 0.09 R⊕. The radius uncertainties are in the range of 3 per cent, allowing a precise interpretation of the interior structure of the three planets. Our planet interior composition model suggests that all three planets in the TOI-1260 system contains some fraction of gas. The innermost planet TOI-1260b has most likely lost all of its primordial hydrogen-dominated envelope. Planets c and d were also likely to have experienced significant loss of atmospheric through escape, but to a lesser extent compared to planet b. © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society

A radial velocity study of the planetary system of pi mensae: improved planet parameters for pi Mensae c and a third planet on a 125 day orbit

Stars and planetary system

TOI-1670 b and c: an inner sub-Neptune with an outer warm Jupiter unlikely to have originated from high-eccentricity migration

Stars and planetary system