We present direct constraints on galaxy intrinsic alignments (IAs) using the Dark Energy Survey Year 3 (DES Y3), the Extended Baryon Oscillation Spectroscopic Survey (eBOSS), and its precursor, the Baryon Oscillation Spectroscopic Survey (BOSS). Our measurements incorporate photometric red sequence (redMaGiC) galaxies from DES with median redshift

The application of machine learning in solar physics has the potential to greatly enhance our understanding of the complex processes that take place in the atmosphere of the Sun. By using techniques such as deep learning, we are now in the position to analyze large amounts of data from solar observations and identify patterns and trends that may

We suggest a method to calculate the probability for the maximum amplitude of Solar Cycle 25 using Bayesian inference. We illustrate this approach with the predictions made by one particular phenomenological model that relates the time interval between termination events of preceding cycles with the amplitude of the next cycle. Our results show

Stellar multiplicity is a common consequence of the stellar formation process. Low-mass stars are the prime constituent of the nearby stellar population, with late-type accounting for the majority of the hydrogen-fusing objects in the Solar neighborhood. The CARMENES input catalogue of M dwarfs (Carmencita) is a comprehensive and homogeneous sample

Low-mass X-ray binaries (LMXB) are stellar systems where a neutron star or a black hole accretes mass from a low-mass ($\lesssim$ 1M$_\odot$) donor star. A subclass, so-called X-ray transients, spend most of their lives in a dim, quiescent state. However, these systems go into sporadic, powerful outbursts produced by one of the most energetic

In this contribution, we will show our results from a sample of 20 pairs of nearby seemingly isolated twin galaxies differing in nuclear activity. Firstly, we present a comparison of the parameter of the spin ($\lambda_{R}$), measured in a region dominated by the galaxy disc. This parameter allows us to assess the rotational support of a galaxy