We present our analysis of a large sample (over 150k) of candidate Galactic RR Lyrae (RRL) stars for which we derived high quality photometry at UV, optical and infrared wavelengths, using data from publicly available surveys. For a sub-sample of these stars (∼ 2,400 fundamental mode field RRLs) we have measured their individual metallicity using

We investigate the properties of pulsating variable stars in two galaxies at the edge or nearby the Local Group: VV 124 and KKr 25, located at ∼1.3 and ∼2 Mpc, respectively. We have identified well populated samples of RR Lyrae stars and Cepheids in both systems. We discuss how these can be used to trace the properties of different stellar

Kepler asteroseismology has played an important role in the characterization of host stars and their planetary systems. Target selection biases, however, meant that this synergy would remain mostly confined to main-sequence stars. The advent of TESS has since lifted this restriction, enabling the systematic search for transiting planets around

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

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

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