We present the first X-ray polarization measurements of GX 339–4. IXPE observed this source twice during its 2023–2024 outburst, once in the soft-intermediate state and again during a soft state. The observation taken during the intermediate state shows a significant (4σ) polarization degree P X = 1.3% ± 0.3% and polarization angle θ X = ‑74° ± 7°

Some ultra diffuse galaxies (UDGs) reveal many more globular clusters (GCs) than classical dwarf galaxies of the same stellar mass. These UDGs, with a mass in their GC system ( $M_{\rm GC}$) approaching 10 per cent of their host galaxy stellar mass ( $M_{\ast }$), are also inferred to have high halo mass to stellar mass ratios ( $M_{\rm halo}/M_{

We analysed the Atacama Large Millimetre/submillimetre Array (ALMA) far-infrared (FIR), 1.3 mm, dust continuum and CO emission of 12 starburst galaxies at z ∼ 2.1 ‑ 3.6 selected for their extreme brightness in the rest-frame UV, with absolute magnitudes of ‑23.4 to ‑24.7. We also analysed their Very Large Telescope (VLT) High Acuity Wide field K

Context. The flat-spectrum radio quasar (FSRQ) OP 313 entered an enhanced activity phase in November 2023 and has undergone multiple flares since then. This activity has motivated the organization of several large multi-wavelength campaigns, including two deep observations from the hard X-ray telescope NuSTAR. We investigate the broadband emission

Recent discoveries of copious amounts of dust in quiescent galaxies (QGs) at high redshifts (z ≳ 1 ‑ 2) challenge the conventional view that these objects have a negligible interstellar medium (ISM) in proportion to their stellar mass. We made use of the SIMBA hydrodynamic cosmological simulation to explore how dust and cold gas evolve in QGs and

We report on the discovery and spectroscopic confirmation of TOI-2458 b, a transiting mini-Neptune around an F-type star leaving the main-sequence with a mass of M ★ = 1.05 ± 0.03 M ⊙, a radius of R ★ = 1.31 ± 0.03 R ⊙, an effective temperature of T eff = 6005 ± 50 K, and a metallicity of ‑0.10 ± 0.05 dex. By combining TESS photometry with high