We show that the perturbation at the peak of the light curve of microlensing event KMT-2019-BLG-0371 is explained by a model with a mass ratio between the host star and planet of q ∼ 0.08. Due to the short event duration (t E ∼ 6.5 days), the secondary object in this system could potentially be a massive giant planet. A Bayesian analysis shows that

The evolution of high mass stars (>8M_sun) is strongly dictated by their interior structure, specifically the mixing processes near the core and in the surrounding envelope. Asteroseismology can open up these stellar interiors but unfortunately Kepler did not provide any high-mass stars with identified modes for this endeavour. The TESS space

Context. It is now well-established that small, rocky planets are common around low-mass stars. However, the detection of such planets is challenged by the short-term activity of host stars. Aims: The HARPS-N red Dwarf Exoplanet Survey programme is a long-term project at the Telescopio Nazionale Galileo aimed at monitoring nearby, early-type, M

CARMENES is a spectrograph built for the 3.5 m telescope at the Calar Alto Observatory. The main aim is to detect low mass planets around M dwarfs. In order to achieve this goal, it is critical to characterize the monitored stars, especially their activity and rotation. Using Quick-Look Pipeline TESS data from its first two cycles, we studied the

Evolution of surface magnetic features in the star, such as stellar spots or faculae, can leave a signature in the lightcurves. These features allow us to study the surface rotation period, Prot, of stars. However, the length of the observations is an important limiting factor to determine reliable Prot. Indeed, it is commonly accepted that it is

In order to understand the formation and evolution of small terrestrial planets not only their internal structure but also the architecture of their host system must be known. Systems harboring long-period cold gas and icy giants (a > 1 au) tend to host close-in small planets (a < 0.3 au, Rp < 4 R⊕) (Masuda et al. 2020). How does the presence of