SOFIA observations provide the first experimental magnetic-dipole hyperfine constants for [13C II] and refined centroid frequency using astronomical data.
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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.
Time-dependent chemistry in 3D MHD simulations leads to H3+ abundances that, when analyzed under steady-state assumptions, imply CRIR values 2-5 times higher than the true input rate, with a median factor of ~3.
Stellar feedback regulates radial gas inflow in the Milky Way center, yielding time-averaged rates that fall from 5e-3 to 1e-6 solar masses per year with both smooth secular and episodic components.
RAYTHEIA is a new high-performance ray-tracing method that achieves near-ideal scaling and supports unprecedented-resolution 3D simulations of photodissociation regions in turbulent clouds.
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.
HINSA observations show CRIR decreasing with H2 column density in both clouds, with IC 348 values an order of magnitude above NGC 1333, modeled as an order-of-magnitude difference in low-energy CR populations from local acceleration sources.
citing papers explorer
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Space as a spectroscopic laboratory: High-resolution spectroscopy of the [$^{13}$C II] hyperfine structure with SOFIA/upGREAT
SOFIA observations provide the first experimental magnetic-dipole hyperfine constants for [13C II] and refined centroid frequency using astronomical data.
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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 cosmic ray ionization rate from H3+ observations can be overestimated due to neglect of time-dependent chemistry
Time-dependent chemistry in 3D MHD simulations leads to H3+ abundances that, when analyzed under steady-state assumptions, imply CRIR values 2-5 times higher than the true input rate, with a median factor of ~3.
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Simulations of gas inflow in the Milky Way I. Stellar-Feedback-Regulated Transport from the Central Molecular Zone to the Circumnuclear disk
Stellar feedback regulates radial gas inflow in the Milky Way center, yielding time-averaged rates that fall from 5e-3 to 1e-6 solar masses per year with both smooth secular and episodic components.
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RAYTHEIA: A high-performance ray-tracing algorithm for three-dimensional direction-dependent equations in astronomical simulations
RAYTHEIA is a new high-performance ray-tracing method that achieves near-ideal scaling and supports unprecedented-resolution 3D simulations of photodissociation regions in turbulent clouds.
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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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A HINSA view of cosmic-ray ionization in IC 348 and NGC 1333: evidence for a strong low-energy cosmic-ray disparity
HINSA observations show CRIR decreasing with H2 column density in both clouds, with IC 348 values an order of magnitude above NGC 1333, modeled as an order-of-magnitude difference in low-energy CR populations from local acceleration sources.