RECORD
The environments forming stellar and planetary systems
Instrumentation and Methods for Astrophysics · Submitted 15 Oct 2026
abstract compiled · 2026-10-20 · no language-model review
The authors' main claim It will thereby reveal the dust-obscured, embedded origins of planetary systems that optical and infrared facilities, including the ELT, see only once they emerge, and show how the birth environment shapes them.
The compiled record
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
Open the compiled record
The abstract, sentence by sentence
How does a star's birth environment set the mass, angular momentum and chemical complexity delivered to its planet-forming disk, and thereby whether it builds planets, brown dwarfs or stellar companions? This requires following material from the cloud to the sub-au to few-au scales where infalling gas, magnetized winds and the disk interact, across all star-forming environments. At frequencies where young disks are optically thin, current facilities, even ALMA after its Wideband Sensitivity Upgrade, fall short by a factor of a few in angular resolution and an order of magnitude in sensitivity. Likewise, resolving how disks around distant high-mass stars fragment into tight multiples requires a linear resolution of a few to a few tens of au, currently out of reach. Yet the disks characterized so far lie almost exclusively in nearby, isolated clouds at near-solar metallicity, although the environment (radiation field, ionization rate, gas and stellar density, pressure and metallicity) varies by orders of magnitude across the Galaxy. Most stars, probably including the Sun, form in clustered regions at kpc distances, and the widest metallicity range lies farther still, in the outer Galaxy, the Central Molecular Zone and the Magellanic Clouds. With three times finer angular resolution and ten times the sensitivity, ALMA2040 will follow the path of material from cloud to disk across the full stellar-mass spectrum and, for the first time, measure how this path changes with environment: resolving the sub-au infall-impact and wind-launching zones nearby, disk fragmentation and the onset of multiplicity in distant high-mass regions, and disk formation at a few tenths of solar metallicity. It will thereby reveal the dust-obscured, embedded origins of planetary systems that optical and infrared facilities, including the ELT, see only once they emerge, and show how the birth environment shapes them.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | How does a star's birth environment set the mass, angular momentum and chemical complexity delivered to its planet-forming disk, and thereby whether it builds planets, brown dwarfs or stellar companions? | background 0.83 | 0.04 | 0.04 | unclear 0.96 |
| s1 | This requires following material from the cloud to the sub-au to few-au scales where infalling gas, magnetized winds and the disk interact, across all star-forming environments. | background 0.72 | 0.05 | 0.03 | asserted 0.95 |
| s2 | At frequencies where young disks are optically thin, current facilities, even ALMA after its Wideband Sensitivity Upgrade, fall short by a factor of a few in angular resolution and an order of magnitude in sensitivity. | gap 0.62 | 0.14 | 0.03 | asserted 1.00 |
| s3 | Likewise, resolving how disks around distant high-mass stars fragment into tight multiples requires a linear resolution of a few to a few tens of au, currently out of reach. | gap 0.77 | 0.06 | 0.03 | asserted 0.99 |
| s4 | Yet the disks characterized so far lie almost exclusively in nearby, isolated clouds at near-solar metallicity, although the environment (radiation field, ionization rate, gas and stellar density, pressure and metallicity) varies by orders of magnitude across the Galaxy. | gap 0.75 | 0.15 | 0.04 | asserted 0.99 |
| s5 | Most stars, probably including the Sun, form in clustered regions at kpc distances, and the widest metallicity range lies farther still, in the outer Galaxy, the Central Molecular Zone and the Magellanic Clouds. | background 0.84 | 0.09 | 0.04 | hedged possibility 0.88 |
| s6 | With three times finer angular resolution and ten times the sensitivity, ALMA2040 will follow the path of material from cloud to disk across the full stellar-mass spectrum and, for the first time, measure how this path changes with environment: resolving the sub-au infall-impact and wind-launching zones nearby, disk fragmentation and the onset of multiplicity in distant high-mass regions, and disk formation at a few tenths of solar metallicity. | contribution 0.39 | 0.07 | 0.49 | asserted 1.00 |
| s7 | It will thereby reveal the dust-obscured, embedded origins of planetary systems that optical and infrared facilities, including the ELT, see only once they emerge, and show how the birth environment shapes them. | interpretation 0.53 | 0.10 | 0.44 | asserted 1.00 |
What was examined, and what was not
- arXiv listing abstract v1
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
The paper
Original abstract
How does a star's birth environment set the mass, angular momentum and chemical complexity delivered to its planet-forming disk, and thereby whether it builds planets, brown dwarfs or stellar companions? This requires following material from the cloud to the sub-au to few-au scales where infalling gas, magnetized winds and the disk interact, across all star-forming environments. At frequencies where young disks are optically thin, current facilities, even ALMA after its Wideband Sensitivity Upgrade, fall short by a factor of a few in angular resolution and an order of magnitude in sensitivity. Likewise, resolving how disks around distant high-mass stars fragment into tight multiples requires a linear resolution of a few to a few tens of au, currently out of reach. Yet the disks characterized so far lie almost exclusively in nearby, isolated clouds at near-solar metallicity, although the environment (radiation field, ionization rate, gas and stellar density, pressure and metallicity) varies by orders of magnitude across the Galaxy. Most stars, probably including the Sun, form in clustered regions at kpc distances, and the widest metallicity range lies farther still, in the outer Galaxy, the Central Molecular Zone and the Magellanic Clouds. With three times finer angular resolution and ten times the sensitivity, ALMA2040 will follow the path of material from cloud to disk across the full stellar-mass spectrum and, for the first time, measure how this path changes with environment: resolving the sub-au infall-impact and wind-launching zones nearby, disk fragmentation and the onset of multiplicity in distant high-mass regions, and disk formation at a few tenths of solar metallicity. It will thereby reveal the dust-obscured, embedded origins of planetary systems that optical and infrared facilities, including the ELT, see only once they emerge, and show how the birth environment shapes them.
Human review
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.