We explore the interplay between Jeans analyses of velocity dispersions and millisecond-pulsar (MSP) timing measurements that trace line-of-sight accelerations to analyze the kinematics of Omega Centauri, performing the first combined analysis of its kind. By using HST proper motion data and recent MSP kinematic measurements, we are able to tightly

Active galactic nuclei (AGN) winds and jets are potential drivers of multi-phase outflows and can significantly modify the interstellar medium (ISM) properties of their host galaxies. The Quasar Feedback (QSOFEED) project aims to investigate the impact of multi-phase quasar-driven outflows and jets on the nuclear regions of quasar host galaxies

For the first time, the LIGHTS survey is routinely imaging galaxies at a depth and spatial resolution comparable to what LSST will produce in 10 years (i.e. ~31 mag/arcsec^2). This opens up the possibility of probing the edge of galaxies with a precision that we have not been able to achieve in the past. While we have been limited to one

In recent decades, observations of the X-ray and radio continuum have been instrumental in studying the coupling between accretion and ejection processes in low-mass X-ray binaries (LMXBs), with emphasis on systems harbouring black hole accretors. However, we have only recently begun to systematically study the evolution of their X-ray, optical and

Symbiotic stars are strongly interacting binaries with long orbital periods, containing an evolved red giant and a white dwarf or a neutron star embedded in a circumbinary nebula. They constitute unique astrophysical laboratories important for understanding the binary evolution and diverse processes occurring also in many other types of

Extremely faint galaxies (mu_V>27 mag/arcsec^2), have only been discovered in the Local Group. These galaxies are very low in mass (tens of 10^5 Msun) and compact (effective radius <1 kpc). These objects populate the least massive dark matter haloes capable of producing stars, providing us with valuable insights into the nature of star formation at