The classical globular clusters found in all galaxy types have half-light radii of r h ~ 2-4 pc, which have been tied to formation in the dense cores of giant molecular clouds. Some old star clusters have larger sizes, and it is unclear if these represent a fundamentally different mode of low-density star cluster formation. We report the discovery

We investigate the formation of infant globular cluster (GC) candidates in high-resolution cosmological simulations from the First Billion Years project. By analysing the evolution of the systems in the energy and angular momentum plane, we identify the redshift at which the infant GCs first became gravitationally bound, and we find evidence of

Rotations of asteroids have been set and altered by several processes since their formation. In the case of the near-Earth objects (NEOs), the rotational states are significantly affected by non-gravitational effects. In addition, an abundant population of binary systems has been found among NEOs with rotational periods very close to the spin

We compare the two largest galaxy morphology catalogues, which separate early- and late-type galaxies at intermediate redshift. The two catalogues were built by applying supervised deep learning (convolutional neural networks, CNNs) to the Dark Energy Survey data down to a magnitude limit of ~21 mag. The methodologies used for the construction of

We examine ultra-diffuse galaxies (UDGs) and their relation to non-UDGs in mass-radius-luminosity space. We begin by publishing Keck/KCWI spectroscopy for the Coma cluster UDG Y358, for which we measure both a recessional velocity and velocity dispersion. Our recessional velocity confirms association with the Coma cluster and Y358's status as a UDG

We present JWST/MIRI MRS spectroscopy of three Seyfert AGN in which we compare their nuclear Polycyclic Aromatic Hydrocarbons (PAHs) emission with that of star-forming regions. This study, for the first time, investigates local luminous Seyferts (L bol > 10 44.46 erg/s) over a wide wavelength range (4.9-28.1 μm) using sub-arcsecond angular