Most long gamma-ray bursts (LGRBs) originate from a rare type of massive stellar explosion. Their afterglows, while rapidly fading, can initially be extremely luminous at optical and near-infrared wavelengths, making them detectable at large cosmological distances. Here we report the detection and observations of GRB 250314A by the SVOM satellite

Despite the wide range of planet─star (mis)alignments in the mature population of transiting exoplanets, the small number of known young transiting planets are nearly all aligned with the rotation axes of their host stars, as determined by the sky-projected obliquity angle. The small number of young systems with measured obliquities limits

Aims. In single-lens microlensing events, the event timescale (t E) is typically the only measurable parameter that constrains the lens mass. Since t E scales with the square root of the lens mass (t E ∝ M 1/2), a short duration may suggest a low-mass lens, such as a brown dwarf (BD). However, a short t E can also result from a high relative proper

We present combined James Webb Space Telescope (JWST) NIRSpec and MIRI/MRS integral field spectroscopy data of the nuclear and circumnuclear regions of the highly dust obscured Seyfert 2 galaxy NGC 7582, which is part of the sample of active galactic nucleaus (AGN) in the Galaxy Activity, Torus and Outflow Survey (GATOS). Spatially resolved

Thanks to new advances in astronomical imaging, we can now routinely explore disk galaxy profiles about two magnitudes deeper than the data available 20 years ago. In this regard, it is an opportune time to reevaluate the past classifications of different surface brightness types. In this paper we explore the stellar mass profiles of a sample of

We present a method of resolving the geometric structure in unresolved CCD images of the two-component stellar objects with relative separations below the full width at half maximum (FWHM). The practical applicability of this method has been demonstrated on example tests of the newly discovered binary, DENIS-P J1756296-451822, with a relative