Aims. We investigated the impact of photometric redshift errors in the ongoing Javalambre Physics of the Accelerating Universe Astrophysical Survey (J-PAS) on void identification and void properties using a watershed-based method. Our aim is to assess the recovery of individual voids and the overall void environment. Methods. We created galaxy mock

Context. Massive stars play a very important role in many astrophysical fields. Despite their scarcity with respect to less-massive counterparts, their influence on the chemo-dynamical evolution of the galaxies is substantial. Yet, some fundamental aspects of their evolution remain poorly constrained. In this regard, there is an open debate on the

Context. Hot Jupiters are among the most suitable targets for atmospheric studies. Expanding the number of hot gaseous giant planets with atmospheric characterisations can improve our understanding of the chemical-physical properties of their atmospheres, as well as the formation and evolution of these extreme planets. Aims. In this work, we use

We present two cases of Lyα changing-look (CL) quasars (J1306 and J1512) along with two additional candidates (J1511 and J1602), all discovered serendipitously at z > 2 through the Dark Energy Spectroscopic Instrument and the Sloan Digital Sky Survey. It is the first time to capture CL events in Lyα at high redshift, which is crucial for

The formation of low-mass stars is a complex and crucial process for understanding stellar evolution and planet formation. In the current scenario of low-mass star formation, after core collapse, the infalling material from the envelope is stored in the circumstellar disk. From this disk, the material reaches the forming star by following the star

The assembly of supermassive black hole (SMBH) mass (M •) and stellar mass (M *) in galaxies can be studied via the redshift evolution of the M •–M * relation, but the ways in which selection bias and physical assembly channels affect this evolution are uncertain. To address this, we compare the M •–M * relation for local massive (M * > 10 10.5 M ⊙