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

The dwarf spheroidal galaxies (dSphs) orbiting the Milky Way are widely regarded as systems supported by velocity dispersion against self-gravity, and as prime targets for the search for indirect dark matter (DM) signatures in the GeV-to-TeV $\gamma$-ray range owing to their lack of astrophysical $\gamma$-ray background. We present forecasts of the

High-resolution spectroscopic measurements of OB stars are important for understanding processes like stellar evolution but require labor-intensive observations. In contrast, photometric missions like the Transiting Exoplanet Survey Satellite (TESS) can monitor hundreds of thousands of stars with a range of temporal resolutions but do not provide

Aims. We investigate the pre-perihelion rotational parameters of the nucleus of 3I/ATLAS modeling jet structures observed in the inner coma. Methods. The comet was extensively monitored on 37 nights between 2025, July 2 and September 5, using the imaging capabilities of the Two-meter Twin Telescope (TTT) at the Teide Observatory (Tenerife, Canary

Context. Massive star evolution plays a crucial role in astrophysics; however, its study is subject to large uncertainties. This problem becomes more severe by the majority of massive stars being born in close binary systems, whose evolution is affected by interactions among their components. Aims. We want to constrain major uncertainties in

Context. The majority of massive stars are born with a close binary companion. How this affects their evolution and fate is still largely uncertain, especially at low metallicity. Aims. We derive synthetic populations of massive post-interaction binary products and compare them with corresponding observed populations in the Small Magellanic Cloud