In this pilot study, we investigate the known PN population in M 33, a nearby spiral galaxy, at a distance of ≍ 840 kpc, using data from the DR3 of the Javalambre-Photometric Local Universe Survey (J-PLUS), a 12-band photometric dataset extensively used to identify H α line emitters. From the 143 known PNe of M 33, the photometry of only 13 is

Ultra-compact X-ray binaries (UCXBs) are a subclass of low-mass X-ray binaries (LMXBs) characterised by tight orbits and hydrogen-poor donor stars. We present a spectral and timing study in the hard X-ray band of 11 of the 20 confirmed UCXBs, based on 37 archival NuSTAR observations. Using both X-ray colours and fractional root mean square values

Context. Following the 2022 alert of a TESS object of interest transiting TOI-5624 (a G7 V star ∼ 100 pc away), a CHEOPS campaign in 2023 detected four planetary signals at P b ≍ 3.4, P c ≍ 7.9, P d ≍ 13.7, and P e ≍ 21.5 days. These signals were later confirmed by additional TESS and CHEOPS photometry in 2024-2025. Aims. By using TESS and CHEOPS

We identify two large-radius planets around the F-type star HD 114082 as the longest-period young transiting exoplanets known. From the first transit, detected by NASA's Transiting Exoplanet Survey Satellite (TESS), and a second dip, spotted by the Next-Generation Transit Survey (NGTS), we predicted midtransit times for HD 114082 b (planet b). We

Context. In this paper, we analyse a sample of low surface brightness dwarf galaxies with a mean effective surface brightness of μ̅ e,g > 24.2 μ ̄ e , g > 24.2 mag arcsec −2, detected using interpretable machine learning tools from the DES survey, and study their properties as a function of their position within the cosmic web to understand the

While the influence of supermassive black hole (SMBH) activity on habitability has garnered attention, the specific effects of active galactic nucleus (AGN) winds, particularly ultrafast outflows (UFOs), on planetary atmospheres remain largely unexplored. This study aims to fill this gap by investigating the relationship between SMBH mass at the