4U 1700─37 is a wind-fed high-mass X-ray binary comprising a compact object, most likely a neutron star, accreting from the O6.5 Iaf + supergiant HD 153919. Coherent pulsations have not been firmly detected and the magnetic field strength remains uncertain, with previous NuSTAR studies reporting only marginal candidate cyclotron resonant scattering

We report the discovery of three Milky Way satellite candidates: Carina IV, Phoenix III, and DELVE 7, in the third data release of the DECam Local Volume Exploration survey (DELVE). The candidate systems were identified by cross-matching results from two independent search algorithms. All three are extremely faint systems composed of old, metal

As the diversity of exoplanets continues to grow, it is important to revisit assumptions about habitability and classical habitable zone definitions. In this work, we introduce an expanded 'temperate' zone, defined by instellation fluxes in the range $0.1< S/\mathrm{S}_{\oplus }< 5$, thus encompassing a broader range of potentially habitable worlds

Context. Gas giant planets orbiting low-mass stars (T eff ≲ 4600 K) are uncommon outcomes of planet formation. Increasing the sample of well-characterised giants around early M dwarfs will enable population-level studies of their properties, offering valuable insights into their formation and evolutionary histories. Aims. We aim to confirm and

To investigate the formation and evolution of vertical structures in disk galaxies, we measure global sech 2 scale heights, averaging thin and thick components when present, for 2631 edge-on disk galaxies with M * > 10 10M ⊙ at 0 < z < 3.5 from the JWST COSMOS-Web survey. We show that dust extinction systematically overestimates scale heights at

Aims. In this work, we exploit the most robust, old, and cosmology-independent age estimates of individual stars from Gaia DR3 to place a lower bound on the age of the Universe, t U. These constraints can be used as an anchor point for any cosmological model, thus providing an upper limit to the Hubble constant H 0. Methods. Our primary stellar age