We report the discovery of TOI-3493 b, a sub-Neptune-sized planet on an 8.15-d orbit transiting the bright (V=9.3) G0 star HD 119355 (aka TIC 203377303) initially identified by NASA's TESS space mission. With the aim of confirming the planetary nature of the transit signal detected by TESS and determining the mass of the planet, we performed an

We present a unique discovery of three new detected systems showing two different phenomena together. These are 2+2 quadruple stellar systems showing two eclipsing binaries as the inner pairs. And besides that, these systems were also found to exhibit the precession of the inner orbits causing the inclination changes manifesting themselves through

The third science flight of the balloon-borne solar observatory SUNRISE carries three entirely new post-focus science instruments with spectropolarimetric capabilities, concurrently covering an extended spectral range from the near ultraviolet to the near infrared. Sampling a larger height range, from the low photosphere to the chromosphere, with

We present an analysis of the structure, kinematics, and chemo-dynamical properties of the Milky Way bulge using RR Lyrae stars from Optical Gravitational Lensing Experiment (OGLE), and giant stars from APOGEE and Gaia that have distances placing them in the inner Galaxy. First, using a sample of 1879 ab-type RR Lyrae stars (RRabs) from OGLE-IV, we

AM CVn systems are a subclass of cataclysmic variables where two DB WDs exchange H-depleted material under short period orbits -in the range approx. 5 - 65 minutes. The prototype, AM CVn (=HZ9) itself, was first discovered in 1957 as a "peculiar" DB WD by Greenstein & Matthews and in 1967 Smak found its characteristic 17-18 min photometric

In this work we made use of the lists of candidate members obtained by Gutiérrez Albarrán et al. (2024) for a target sample of 42 open clusters, ranging from 1 Myr to 5 Gyr and observed within the Gaia-ESO survey (GES), with the aim of studying Li as an age indicator and deriving an empirical Li-age relation for FGK late-type stars. We conducted a