Planets form in disks of gas and dust around young stars. The disk molecular reservoirs and
their chemical evolution affect all aspects of planet formation, from the coagulation of dust …

Planets form and obtain their compositions in dust-and gas-rich disks around young stars,
and the outcome of this process is intimately linked to the disk chemical properties. The …

High dust density in the midplane of protoplanetary disks is favorable for efficient grain
growth and can allow fast formation of planetesimals and planets, before disks dissipate …

The Molecules with ALMA at Planet-forming Scales (MAPS) Large Program provides a
unique opportunity to study the vertical distribution of gas, chemistry, and temperature in the …

The gas-phase CO abundance (relative to hydrogen) in protoplanetary disks decreases by
up to two orders of magnitude from its interstellar medium value of∼ 10− 4, even after …

While dust disks around optically visible, Class II protostars are found to be vertically thin,
when and how dust settles to the midplane are unclear. As part of the Atacama Large …

Turbulence is a fundamental parameter in models of grain growth during the early stages of
planet formation. As such, observational constraints on its magnitude are crucial. Here we …

Accurate measurements of the physical structure of protoplanetary discs are critical inputs
for planet formation models. These constraints are traditionally established via complex …

High spatial resolution CO observations of midinclination (≈ 30–75) protoplanetary disks
offer an opportunity to study the vertical distribution of CO emission and temperature. The …

Constraining the physical and chemical structure of young embedded disks is crucial for
understanding the earliest stages of planet formation. As part of the Early Planet Formation …