First interstellar detection of HNSO with column density (8 ± 1)×10^13 cm^{-2} and abundance ~6×10^{-10} relative to H2, proposed to form via NSO + H on icy grains.
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10 Pith papers cite this work. Polarity classification is still indexing.
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COLIBRE simulations find the galaxy gas-phase MZR already in place at z≈10 with little evolution until z≈5, then shallowens at low z, with high-mass turnover set by AGN feedback and low-mass end by core-collapse supernovae.
Hydrogen tunneling makes H-abstraction reactions by C2H, OH, and CN competitive in TMC-1 despite low individual rates, affecting aromatic abundance predictions.
The CH₃OH/CH₃CN ratio in the S68N outflow is constant at ~100-200 and matches gas-phase astrochemical models only when cosmic-ray ionization rates are raised to ~10^{-14} s^{-1}.
Abundance calculations for CaC_{2n+1}N (n=1-4) in IRC+10216 indicate observed CaNC originates from larger cyanopolyyne ions requiring molecular rearrangement during recombination.
Independent reanalysis of ALMA observations finds no evidence for t-HC(S)SH, derives column density upper limit of 4e14 cm^-2, and attributes prior detection claim to blending and modeling issues.
SKA will detect emission from heavy molecules and prebiotic species in obscured disk regions to constrain initial chemical conditions for planet formation.
UCLCHEM 4.0 is an updated open-source framework that solves time-dependent gas-grain chemical networks with built-in parametrizations for cloud collapse, cores, and shocks.
SKAO, especially SKA-Mid Band 5, is expected to overcome dust opacity and frequency limits to detect complex prebiotic molecules in high-mass and solar-type protostellar regions.
citing papers explorer
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Discovery of thionylimide, HNSO, in space: the first N-, S- and O-bearing interstellar molecule
First interstellar detection of HNSO with column density (8 ± 1)×10^13 cm^{-2} and abundance ~6×10^{-10} relative to H2, proposed to form via NSO + H on icy grains.
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The evolution of the galaxy gas-phase mass-metallicity relation from $z=15$ to $z=0$ in the COLIBRE cosmological simulations
COLIBRE simulations find the galaxy gas-phase MZR already in place at z≈10 with little evolution until z≈5, then shallowens at low z, with high-mass turnover set by AGN feedback and low-mass end by core-collapse supernovae.
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The impact of hydrogen atom tunneling on aromatic chemistry in TMC-1
Hydrogen tunneling makes H-abstraction reactions by C2H, OH, and CN competitive in TMC-1 despite low individual rates, affecting aromatic abundance predictions.
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Probing outflow physics through CH$_3$CN and CH$_3$OH chemistry
The CH₃OH/CH₃CN ratio in the S68N outflow is constant at ~100-200 and matches gas-phase astrochemical models only when cosmic-ray ionization rates are raised to ~10^{-14} s^{-1}.
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Ca-bearing cyanopolyynes in IRC+10216
Abundance calculations for CaC_{2n+1}N (n=1-4) in IRC+10216 indicate observed CaNC originates from larger cyanopolyyne ions requiring molecular rearrangement during recombination.
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Non-detection of HC(S)SH: Estimating Upper Limits and Constraining Chemistry
Independent reanalysis of ALMA observations finds no evidence for t-HC(S)SH, derives column density upper limit of 4e14 cm^-2, and attributes prior detection claim to blending and modeling issues.
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Unveiling Complex Chemistry in Planet-forming Disks with the SKAO
SKA will detect emission from heavy molecules and prebiotic species in obscured disk regions to constrain initial chemical conditions for planet formation.
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UCLCHEM 4.0: An open source gas-grain astrochemistry simulation framework
UCLCHEM 4.0 is an updated open-source framework that solves time-dependent gas-grain chemical networks with built-in parametrizations for cloud collapse, cores, and shocks.
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Chemical Complexity in the Early Stages of Star Formation in the SKAO Era
SKAO, especially SKA-Mid Band 5, is expected to overcome dust opacity and frequency limits to detect complex prebiotic molecules in high-mass and solar-type protostellar regions.
- Chemistry and IR emission of acetylene in planet-forming regions of T Tauri disks. Impact of elemental abundances and dust properties