Recent observational studies suggest that feedback from active galactic nuclei (AGNs) may play an important role in the formation and evolution of low-mass dwarf galaxies, an issue that has received little attention from a theoretical perspective. We investigate this using two sets of 12 cosmological magneto-hydrodynamical simulations of the

We study the bar fraction in the MACS J0647.8+7015 cluster of galaxies at z=0.59 using the observations obtained with the NIRCam instrument mounted on the JWST telescope. We visually inspected the near infrared images obtained with the F200W filter of all the cluster members to identify the presence of bars. The cluster member selection was based

It has been 20 years since the classification of galaxy disk types observed in deep imaging was established. These classifications, which notably consist of pure exponential, truncated, and antitruncated, have significantly enriched our understanding of the structural diversity within galaxies. Using ultra-deep imaging, most spiral galaxy profiles

The number of globular clusters plays a fundamental role in understanding the early stages of galaxy formation. We know that the GC population of normal galaxies correlates with the amount of dark matter in these objects. Extending this analysis to the number of globulars in very low surface brightness galaxies is therefore key to understanding the

The QUIJOTE (Q-U-I JOint TEnerife) experiment combines the operation of two radio-telescopes and three instruments working in the microwave bands from 10 to 47 GHz at the Teide Observatory, Tenerife, which has already been presented in previous SPIE meetings. The new Multi Frequency Instrument (MFI2) led by the Instituto de Astrofísica de Canarias

We study the impact of black hole nuclear activity on both the global and radial star formation rate (SFR) profiles in X-ray-selected active galactic nuclei (AGN) in the field of miniJPAS, the precursor of the much wider J-PAS project. Our sample includes 32 AGN with z < 0.3 detected via the XMM-Newton and Chandra surveys. For comparison, we