OB associations are unbound groups of young stars made prominent by their bright OB
members, and have long been thought to be the expanded remnants of dense star clusters …

We present Ekster, a new method for simulating star clusters from birth in a live galaxy
simulation that combines the smoothed-particle hydrodynamics (SPH) method Phantom with …

It remains unclear how galactic environment affects star formation and stellar cluster
properties. This is difficult to address in Milky Way-mass galaxy simulations because of …

We quantify the spatial distribution of stars for two subclusters centred around the
massive/intermediate-mass stars S Mon and IRS 1/2 in the NGC 2264 star-forming region …

Observations of clusters suffer from issues such as completeness, projection effects,
resolving individual stars, and extinction. As such, how accurate measurements and …

Many theoretical studies have shown that external photoevaporation from massive stars can
severely truncate, or destroy altogether, the gaseous protoplanetary disks around young …

The abundance of the short-lived radioisotopes 26Al and 60Fe in the early Solar system is
usually explained by the Sun either forming from pre-enriched material, or the Sun's …

ABSTRACT Galactic Wolf–Rayet (WR) star membership of star-forming regions can be used
to constrain the formation environments of massive stars. Here, we utilize Gaia DR2 …

The-parameter is used extensively to quantify the spatial distributions of stars and gas in star-
forming regions as well as older clusters and associations. It quantifies the amount of …

The dominant formation mechanism of brown dwarfs and planetary-mass objects (PMOs) in
star-forming regions is presently uncertain. Do they form like stars, via the collapse and …