The infrared excess shown by white dwarfs can be an indicator of a low-mass substellar companion, like a brown dwarf or even an exoplanet. In this work, we describe the methodology followed to identify white dwarfs with infrared excess within 100 pc and we show the preliminary results. Our initial sample is an almost complete volume-limited white

Identifying new white dwarfs (WDs) heavy elements is crucial, as they serve as valuable tools for deducing the chemical characteristics of potential planetary systems accreting material onto their surfaces. To detect metallic WDs, we propose a methodology based on an unsupervised learning technique known as Self-Organizing Maps (SOM). This approach

The WEAVE-Apertif survey combines spatially resolved optical and HI spectroscopic observations to investigate galaxy evolution using a representative sample of 400 gas-rich galaxies. Utilizing the WEAVE large integral-field unit (LIFU) at the William Herschel Telescope (WHT) and the upgraded Apertif system at the Westerbork Synthesis Radio

The MONOS project has obtained WEAVE LIFU observations to study the cores of nine stellar clusters containing O and B stars. Most O stars form in multiple systems, which allows for the determination of stellar masses through their orbits. However, this process is complicated by the wide range of orbital periods and the presence of complex systems

WEAVE, the powerful multi-object spectrograph recently installed on the William Herschel Telescope (WHT), started science observations in October 2023. Over 500 hours of science observations have been taken with the Large Integral Field Unit (LIFU) mode in the first ∼10 months of observations, sharing nights with further technical and commissioning

Vortex flows are structures associated with the rotation of the plasma and/or the magnetic field that are present throughout the solar atmosphere. In recent years, their study has become increasingly important, as they are present on a wide variety of temporal and spatial scales and can connect several layers of the solar atmosphere. In this work