Null detection of 0.3-micron artificial grains in 1 m³ lunar regolith excludes Solar-type stars dispersing more than ~0.09 Earth masses of long-lived technomaterial over Galactic history.
Title resolution pending
12 Pith papers cite this work. Polarity classification is still indexing.
12
Pith papers citing it
citation-role summary
method 1
citation-polarity summary
roles
method 1polarities
use method 1representative citing papers
Dust grain size distributions evolve from large-grain dominated at high redshift to MRN-like at low redshift, driven primarily by shattering and ISM accretion after stars supply initial large grains, reproducing z=0 dust masses and Milky Way extinction properties.
Cosmological zoom-in simulations find that grain-grain shattering in diffuse ISM gas drives rising PAH mass fraction with time, naturally producing the observed PAH-metallicity relation and inverse qPAH-molecular gas trends.
JWST observations of z~1.1 galaxies produce PAH ratio maps showing larger and more neutral PAHs at larger radii, opposite local trends, linked to UV hardness via photo-destruction.
Four parameters suffice to describe dust attenuation curve diversity in TNG simulations, yielding a new symbolic-regression model that recovers curves and fluxes better than existing parameterizations while linking parameters to SFR surface density, metallicity, and geometry.
Six z~2-3 quasars with extreme LoBAL outflows and weak UV lines are interpreted as weak-emission-line quasars emerging from dust cocoons via disc winds that shatter grains and produce steeper extinction.
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).
A multiphase ISM grain-size model with low supernova dust yield reproduces observed dust-to-stellar mass ratios and UV luminosity functions at z=7-12 by letting small grains seed rapid metal accretion.
A z=4.556 QSO exhibits A_1500/A_V ≈8 with no 2175Å bump, taken as evidence for small-grain dominance from QSO-driven shattering or condensation.
New infrared spectra show reduced water ice and unusually strong aliphatic hydrocarbon absorption towards W44, attributed to shock and cosmic-ray processing in the associated molecular cloud.
Shiva is a new simulation tool that computes time-dependent dust size distributions and band gap energy evolution for HAC grains under photo-processing, sputtering, and shattering in specified interstellar conditions.
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.
citing papers explorer
-
Micron-Scale Technosignatures: How a Cubic Metre of Lunar Regolith May Begin to Constrain the Number of Past Technological Civilisations in the Galaxy
Null detection of 0.3-micron artificial grains in 1 m³ lunar regolith excludes Solar-type stars dispersing more than ~0.09 Earth masses of long-lived technomaterial over Galactic history.
-
Dust and Grain Size Evolution in Galaxy Simulations: What Matters and What Does Not
Dust grain size distributions evolve from large-grain dominated at high redshift to MRN-like at low redshift, driven primarily by shattering and ISM accretion after stars supply initial large grains, reproducing z=0 dust masses and Milky Way extinction properties.
-
The Lifecycle and Emission Properties of PAHs in Cosmological Hydrodynamic Galaxy Formation Simulations
Cosmological zoom-in simulations find that grain-grain shattering in diffuse ISM gas drives rising PAH mass fraction with time, naturally producing the observed PAH-metallicity relation and inverse qPAH-molecular gas trends.
-
PAHSPECS: Spatially Resolved PAH Spectroscopy at cosmic noon with JWST MIRI MRS
JWST observations of z~1.1 galaxies produce PAH ratio maps showing larger and more neutral PAHs at larger radii, opposite local trends, linked to UV hardness via photo-destruction.
-
Learning the Universe: The Structure of Dust Attenuation Curves in Galaxy Simulations
Four parameters suffice to describe dust attenuation curve diversity in TNG simulations, yielding a new symbolic-regression model that recovers curves and fluxes better than existing parameterizations while linking parameters to SFR surface density, metallicity, and geometry.
-
Extreme outflow velocities and weak UV emission lines indicate quasars shedding their dust cocoons
Six z~2-3 quasars with extreme LoBAL outflows and weak UV lines are interpreted as weak-emission-line quasars emerging from dust cocoons via disc winds that shatter grains and produce steeper extinction.
-
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).
-
Grain-size evolution and rapid dust growth in high-redshift galaxies
A multiphase ISM grain-size model with low supernova dust yield reproduces observed dust-to-stellar mass ratios and UV luminosity functions at z=7-12 by letting small grains seed rapid metal accretion.
-
A Steep-Extinction QSO at z=4.6: JWST Evidence for Abundant Small Dust Grains
A z=4.556 QSO exhibits A_1500/A_V ≈8 with no 2175Å bump, taken as evidence for small-grain dominance from QSO-driven shattering or condensation.
-
Dust Absorption towards Supernova Remnant W44
New infrared spectra show reduced water ice and unusually strong aliphatic hydrocarbon absorption towards W44, attributed to shock and cosmic-ray processing in the associated molecular cloud.
-
Shiva: the dust destruction model
Shiva is a new simulation tool that computes time-dependent dust size distributions and band gap energy evolution for HAC grains under photo-processing, sputtering, and shattering in specified interstellar conditions.
-
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.