Context. Surveys for exoplanets indicate that the occurrence rate of gas giant planets orbiting late-type stars in orbits with periods shorter than 1000 days is lower than in the case of Sun-like stars. This is in agreement with planet formation models based on the core or pebble accretion paradigm. Aims. The CARMENES exoplanet survey has been

Gamma-ray bursts (GRBs) are the most powerful transient objects in the Universe, and they are a primary target for the MAGIC Collaboration. Recognizing the challenges of observing these elusive objects with Imaging Atmospheric Cherenkov Telescopes (IACTs), we implemented a dedicated observational strategy that included an automated procedure for

Context. Spatially resolved observations of the Sun and the astronomical sample size of stellar bodies are the respective key strengths of solar and stellar observations. However, the large difference in object brightness between the Sun and other stars has led to distinctly different instrumentation and methodologies between the two fields. Aims

Context. In the current panorama of large surveys, the vast amount of data that are obtained with different methods, data types, formats, and stellar samples prevents an efficient use of the available information. Aims. The Survey of Surveys is a project to critically compile survey results into a single catalog to facilitate the scientific use of

We investigated three fan-shaped jets observed above sunspot light bridges or nearby sunspot regions. The study aimed to explore the dynamics and physical properties of jets' features that appear as blob-like structures at the tips of the jets, which we call 'dark blobs'. A transparent region is observed beneath the dark blobs, creating a visible

Context. The inference of the magnetic field vector from spectropolarimetric observations is crucial for understanding the physical processes governing the solar corona. Aims. We investigated what information on the magnetic fields of coronal bright points (CBPs) can be gained from the intensity and polarization of the Fe XIII 10747 Å, Fe XIV 5303