We present an independent spectroscopic and radial velocity analysis for nine stars from the Pennsylvania-Toruń Planet Search. For BD+24 4697, we present an updated true companion's mass (0.16±0.02 M☉) as well as evidence of stellar activity. For BD+54 1640 and BD+65 1241 we present true masses of companions, m=0.15±0.04 M☉ and m=0.091± 0.005 M☉

Despite their importance, the dynamical properties of massive stars remain poorly understood. Rotation is a key driver of internal mixing and angular momentum transport, significantly influencing massive star evolution. However, constraining rotation from spectroscopy is challenging, as spectral lines often exhibit excess broadening beyond rotation

The discovery of a significant number of rapidly rotating low-mass stars showing no or few flares in TESS observations was a surprise, as rapid rotation has previously been linked to high stellar activity. Here we present TESS and HiPERCAM u sg sr si sz s observations of one of these stars, LP 89-187, which has a rotation period of 0.117 d. TESS

Gamma-ray bursts (GRBs) offer a powerful window to probe the progenitor systems responsible for the formation of heavy elements through the rapid neutron capture (r-) process, thanks to their exceptional luminosity, which allows them to be observed across vast cosmic distances. GRB 241105A, observed at a redshift of $z = 2.681$, features a short

Broad-band mid-infrared (MIR) imaging with high-spatial resolution is useful to study extended dust structures in the circumnuclear regions of nearby active galactic nuclei. However, broad-band imaging filters cannot distinguish dust continuum emission from emission lines, and so accounting for the emission line contamination becomes crucial in

Observations and high-resolution hydrodynamical simulations indicate that massive star clusters form through a complex hierarchical assembly. We use simulations including post-Newtonian dynamics (the BIFROST code) and stellar evolution (the SEVN module) to investigate this collisional assembly. With a full initial stellar mass function, we study