Context. Recent observations suggest that planet formation starts early, in protostellar disks
of≤ 10 5 yr, which are characterized by strong interactions with the environment, such as …

Context. Pre-stellar cores represent the earliest stage of the formation process of stars and
planets. By characterizing the physical and chemical structure of these cores, we can …

Spectral lines of ammonia, NH 3, are useful probes of the physical conditions in dense
molecular cloud cores. In addition to advantages in spectroscopy, ammonia has also been …

We present 500 and 700 au resolution 1 and 3 mm Atacama Large Millimeter/submillimeter
Array observations, respectively, of protostellar cores in protoclusters Sagittarius B2 (Sgr B2) …

Much of what we know about molecular clouds, and by extension star formation, comes from
molecular line observations. Interpreting these correctly requires knowledge of the …

The internal structure of the prestellar core G208. 68-19.02-N2 (G208-N2) in the Orion
Molecular Cloud 3 (OMC-3) region has been studied with the Atacama Large Millimeter …

Context. HCN, HNC, and their isotopologues are ubiquitous molecules that can serve as
chemical thermometers and evolutionary tracers to characterize star-forming regions …

Context. In the centre of pre-stellar cores, deuterium fractionation is enhanced due to low
temperatures and high densities. Therefore, the chemistry of deuterated molecules can be …

ABSTRACT Cold (10 K) and dense (cm) cores of gas and dust within molecular clouds,
known as starless and dynamically evolved pre-stellar cores, are the birthplaces of low …

Recent observations of the pre-stellar core L1544 and the younger starless core L1498 have
revealed that complex organic molecules (COMs) are enhanced in the gas phase towards …