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

We introduce the data analysis pipeline (DAP) for the Sloan Digital Sky Survey V Local Volume Mapper (LVM) project, referred to as the LVM-DAP. We outline our methods for recovering both stellar and emission-line components from optical integral field spectroscopy, highlighting the developments and changes implemented to address specific challenges

We report, for the first time, the detection of a sample of quenched and isolated dwarf galaxies (with 8.9 < log(M ⋆/M ⊙) < 9.5) in the least dense regions of the cosmic web, including voids, filaments, and walls. These dwarfs have no neighboring galaxy within 1.0 Mpc in projected distance. Based on the full spectral fitting of their central

We present photometric redshifts for 1 341 559 galaxies from the Physics of the Accelerating Universe Survey (PAUS) over 50.38 deg 2 of sky to i AB = 23. Redshift estimation was performed using DEEPz, a deep learning photometric redshift code. We analysed the photometric redshift precision when varying the photometric and spectroscopic samples