We present high-speed photometry of the eclipsing cataclysmic variable CSS131106 J052412+004148. We determine the system parameters by modelling the eclipse light curve using the photometric eclipse method, in which the mass ratio is determined from the relative timings of the white dwarf and bright spot eclipses. Despite the blended white dwarf

The Hayabusa2 extended mission, nicknamed Hayabusa2# (# is pronounced SHARP, which stands for the Small Hazardous Asteroid Reconnaissance Probe), is JAXA's small body explorer to conduct science and engineering investigations in space. After the successful return to the Earth with the samples from the carbonaceous asteroid (162173) Ryugu on 2020

BL Lac objects (BLLs) are defined by the presence of very weak (typically < 5 Å) or even absent spectral lines. This makes determining their distance particularly challenging, especially at high redshift, where the sources are fainter and the host galaxy contribution in the optical band becomes negligible. Yet measuring their distance is crucial

Ultracompact binary systems, consisting of two compact objects in an orbit $\lesssim 0.5 {\rm R}_\odot$, should exhibit measurable rates of orbital period change ( $\dot{P} \ne 0$) due to the emission of gravitational waves (GWs). Measurements of $\dot{P}$ have so far been limited to the shortest-period ultracompact binaries ( $\lesssim 20$ min)

Context. Milky Way analogs (MWAs) are defined on the basis of structural, kinematic, and global physical parameters. Our advanced approach to searching for MWAs also includes principal features of the Milky Way (MW) such as its isolated position in the local cosmic web, absent or weak nuclear activity, and the low mass of the supermassive black

In a magnetically dominated model of star formation, we expect to see alignments between the magnetic field orientation of star-forming dense cores and the cloud-scale magnetic field. A. Pandhi et al. showed instead, however, that the orientation of cores and their angular momentum vectors appear random with respect to the larger-scale magnetic