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Rapid Dust Formation in the Early Universe
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abstract
Interstellar dust links the formation of the first stars to the rocky planet we inhabit by playing a pivotal role in the cooling and fragmentation of molecular clouds, and catalyzing the formation of water and organic molecules. Despite its central role, the origin of dust and its formation timescale remain unknown. Some models favor rapid production in supernova ejecta as the primary origin of dust, while others invoke slower production by evolved asymptotic giant branch stars or grain growth in the interstellar medium (ISM). The dust content of young early-universe galaxies is highly sensitive to the dust formation timescales. Here, we evaluate the dust content of 631 galaxies at $3 < z_{\rm spec} < 14$ based on rest-UV to optical spectroscopy obtained with JWST NIRSpec. We find that dust appears rapidly. Attenuation immediately follows star formation on timescales shorter than $\sim 30$ Myr, favoring dust production by supernovae. The degree of attenuation is $\sim 30$ times lower than expected if the entire supernova dust yield were preserved in the ISM, and had Milky Way-like grain properties. This can be reconciled if the early-universe dust is composed mostly of silicate or grains much larger than those in the Milky Way, and if significant dust destruction or ejection by outflows takes place.
Forward citations
Cited by 7 Pith papers
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Stardust Galaxies at z>9: A Dust-Origin Transition Behind the Excess of UV-Bright Galaxies
At z>9, the UV-bright galaxy excess can be explained by supernova-produced dust with low FUV opacity (κ≈10^3–10^4 cm^2/g) plus porous geometry and modest star-formation efficiency evolution.
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The Impact of Early Massive Galaxy Formation on the Cosmic Microwave Background
Massive early-type galaxies forming at z≈15-20 with a top-heavy stellar IMF could inject enough dust-reprocessed light to account for 1.4% to all of the present-day CMB energy density.
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CEERS: Forging the First Dust Grains in the Universe? A Population of Galaxies with spectroscopically-derived Extremely Low Dust Attenuation (GELDA) at 4.0<z<11.4
At z=4 to 11.4, 49 low-mass galaxies show essentially zero dust attenuation, dominate the highest-redshift bin (5 of 6), and their low dust-to-metal ratios are consistent with supernova-made stardust rather than ISM g...
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REBELS-IFU: Dust attenuation curves of 12 massive galaxies at $z\simeq7$
Dust attenuation curves of 12 massive z~7 galaxies from JWST NIRSpec spectra are mostly Calzetti-like, with three 2175 Angstrom bumps and slopes that correlate with A_V.
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Dust emission from the bulk of galaxies at the Epoch of Reionization
Stacked ALMA data reveal tentative infrared emission from typical z=6-7 galaxies, implying lower dust attenuation and star formation rates than UV-selected samples, and only upper limits at z>7.
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JWST Spectra Indicate a Large Mass of Postshock Dust Formed by SN 2010jl
SN 2010jl has produced at least 0.11 solar masses of dust by 13 years after explosion, likely about 0.2 solar masses, among the largest dust masses measured for a supernova from mid-infrared data alone.
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Dust removal timescale in galaxies across cosmic time
The dust removal timescale in galaxies decreases from about 1.8 Gyr at z~0.05 to about 0.4 Gyr at z>3, indicating more efficient dust clearing in the early universe.
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