Of the over 150 different molecular species detected in the interstellar and circumstellar
media, approximately 50 contain 6 or more atoms. These molecules, labeled complex by …

Our Sun and planetary system were born about 4.5 billion years ago. How did this happen,
and what is the nature of our heritage from these early times? This review tries to address …

Planet-forming disks are not isolated systems. Their interaction with the surrounding medium
affects their mass budget and chemical content. In the context of the ALMA-DOT program …

Flattened, rotating disks of cool dust and gas extending for tens to hundreds of astronomical
units are found around almost all low-mass stars shortly after their birth. These disks …

Aims. Photodissociation by UV light is an important destruction mechanism for carbon
monoxide (CO) in many astrophysical environments, ranging from interstellar clouds to …

We present a census of molecular outflows across four active regions of star formation in the
Perseus molecular cloud (NGC 1333, IC348/HH211, L1448 and L1455), totalling an area of …

In their earliest stages, protostars accrete mass from their surrounding envelopes through
circumstellar disks. Until now, the smallest observed protostar-to-envelope mass ratio was …

The chemical composition of gas and ice in disks around young stars sets the bulk
composition of planets. In contrast to protoplanetary disks (Class II), young disks that are still …

Context. Theoretical studies of collapsing clouds have found that even a relatively weak
magnetic field may prevent the formation of disks and their fragmentation. However, most …

Context. Water is a key tracer of dynamics and chemistry in low-mass star-forming regions,
but spectrally resolved observations have so far been limited in sensitivity and angular …