First pixel-by-pixel JWST absorption maps of multiple ice species toward six Class 0 protostars reveal abundance variations from heating and outflows, with total composition matching prestellar formation models covering ~90% of inventory.
Nature Astronomy , year = 2024, month = mar, volume =
8 Pith papers cite this work, alongside 51 external citations. Polarity classification is still indexing.
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representative citing papers
High-resolution mapping reveals nitrogen enrichment around super star clusters in NGC 5253, attributed to Wolf-Rayet stars with material expelled to surrounding gas.
MD simulations yield silicate grain shattering thresholds of ~6 km/s and post-collision size distributions inconsistent with power-law predictions from Jones et al. (1996) and Hirashita & Kobayashi (2013).
Radiative transfer modeling of protostellar ices shows absorption originates mainly from 1000-2000 au at the cavity-envelope transition, with apparent CO2/H2O and CO/H2O ratios potentially underestimated due to line-of-sight effects.
No change detected in ice absorption bands of EC 53 between phases, with ice abundances higher than typical for embedded protostars.
The pyRate model requires nondiffusive chemistry to form observed S-bearing species in irradiated CO2:CS2 ice but overpredicts OCS, CS and SO while underpredicting SO2 and sulfur allotropes.
Radiative-transfer simulations with common dust models generate a range of spectral indices but cannot reach the lowest observed emissivity indices in protostars without invoking unexpectedly large millimeter-sized grains.
SKAO will enable the first large-scale high-resolution surveys of cm-wavelength disk emission to constrain dust growth, pebble demographics, and planet formation processes.
citing papers explorer
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Mapping Interstellar Ice Inventory toward Class 0 Protostars in Star-forming Region Orion A with JWST Data
First pixel-by-pixel JWST absorption maps of multiple ice species toward six Class 0 protostars reveal abundance variations from heating and outflows, with total composition matching prestellar formation models covering ~90% of inventory.
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The heart of NGC 5253 as seen with MUSE-NFM: nitrogen enrichment through stellar chemical feedback at parsec scales
High-resolution mapping reveals nitrogen enrichment around super star clusters in NGC 5253, attributed to Wolf-Rayet stars with material expelled to surrounding gas.
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Silicate cosmic dust grain collisions in the interstellar medium: A molecular dynamics study
MD simulations yield silicate grain shattering thresholds of ~6 km/s and post-collision size distributions inconsistent with power-law predictions from Jones et al. (1996) and Hirashita & Kobayashi (2013).
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CORINOS V: Radiative transfer effects in protostellar ice observations
Radiative transfer modeling of protostellar ices shows absorption originates mainly from 1000-2000 au at the cavity-envelope transition, with apparent CO2/H2O and CO/H2O ratios potentially underestimated due to line-of-sight effects.
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EPISODE IV: Ice Inventory in the Envelope of EC 53
No change detected in ice absorption bands of EC 53 between phases, with ice abundances higher than typical for embedded protostars.
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Modeling the UV-photon irradiation of CS$_2$-bearing ices in the laboratory with the pyRate gas-grain astrochemical code. New insights into the missing sulfur problem
The pyRate model requires nondiffusive chemistry to form observed S-bearing species in irradiated CO2:CS2 ice but overpredicts OCS, CS and SO while underpredicting SO2 and sulfur allotropes.
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Pristine composition or size evolution: Can current dust models reproduce emissivities observed in nearby protostars?
Radiative-transfer simulations with common dust models generate a range of spectral indices but cannot reach the lowest observed emissivity indices in protostars without invoking unexpectedly large millimeter-sized grains.
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Demographics of planet-forming disks with the SKAO
SKAO will enable the first large-scale high-resolution surveys of cm-wavelength disk emission to constrain dust growth, pebble demographics, and planet formation processes.