Few planetary systems have measured mutual inclinations, and even fewer are found to be non-coplanar. Observing the gravitational interactions between exoplanets is an effective tool to detect non-transiting companions to transiting planets. Evidence of these interactions can manifest in the light curve through transit timing variations (TTVs) and

At high metallicity, a majority of massive stars have at least one close stellar companion. The evolution of such binaries is subject to strong interaction processes, which heavily impact the characteristics of their life-ending supernova and compact remnants. For the low-metallicity environments of high-redshift galaxies, constraints on the

Trans-Neptunian objects (TNOs), icy remnants of planet formation orbiting beyond Neptune, comprise a dynamically and compositionally diverse population of >5000 known members. An extensive body of literature focuses on the dynamical structure of the trans-Neptunian region. Less information is available on TNO compositions due to the difficulty

Primitive asteroids in the Main Belt possess one of the most pristine inventories of materials in the Solar System. Main Belt primitive asteroids are particularly interesting due to clear evidence of phyllosilicates, i.e., silicates that have encountered liquid water and undergone chemical alteration. Since asteroids are thought to be likely

Aims. Pulsating variable stars are invaluable tracers for reconstructing the star formation history and chemical evolution of their host galaxies. In this work, we explore the variable star population of Leo II, a distant dwarf spheroidal satellite of the Milky Way. Methods. We analyse an extensive dataset of ground-based BVRI time-series

We present the discovery and validation of a super-Earth planet orbiting the M dwarf star TOI-1846 (TIC 198385543). The host star ( $K_{\rm mag} = 9.6$) is located 47 pc away and has a radius of $R_\star = 0.41 \pm 0.01$ $\rm \, R_\odot$, a mass of $M_\star = 0.40 \pm 0.02$ $\rm \, M_\odot$ and an effective temperature of $T_{\rm eff} = 3568 \pm 44