The COLIBRE simulations reproduce the broad evolution of galaxy dust scaling relations from z=15 to 0, but overproduce the z<1 cosmic dust mass density and miss the most extreme sub-millimeter galaxies.
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At z=4-6, the dust-obscured star formation rate density is log rho = -1.52, implying that about 66% of cosmic star formation was obscured by dust, based on eight spectroscopically confirmed dusty galaxies.
In FirstLight EoR galaxies, star-forming clumps show grayer dust attenuation curves and ~10× higher dust column densities than the system-integrated average, while diffuse regions have steeper curves.
An archaeological reconstruction of galaxy growth from stellar ages systematically overestimates the mass of the most massive progenitor at early times, easing claimed tensions between early massive galaxies and LCDM.
ALMA spectral scans of four z>7.6 galaxies yield no [OIII] 88 micron detections, with REBELS-04's non-detection challenging expectations from its star formation rate.
IR SED broadening in high-z galaxies is driven primarily by luminosity density, requiring ~1.6–1.7 (up to ~2) corrections to modified-blackbody total infrared luminosities.
New JWST spectrum of a z=8.3 galaxy with prior ALMA dust detection shows AGN signatures, 0.15 Zsun metallicity, Mdust ~10^6 Msun, Tdust~91 K, and an [OIII] line ratio higher than nebular models allow.
A new ALMA-based measurement finds a mean dust emissivity index of 2.2 for 21 infrared-bright galaxies at z=1.5-4.2, with no evident redshift trend.
Using high-resolution galaxy simulations, the authors show that the scatter in the IRX-beta relation is dominated by variations in the intrinsic ultraviolet spectral slope, and that the high-redshift infrared excess deficit can be explained by a redshift-dependent dust temperature correction.
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DREAMS. JWST Spectroscopy of a $z=8.3$ Galaxy with an ALMA Dust Continuum Detection: Early Dust, Very High $T_{\rm dust}$, and a Multi-wavelength [OIII] Ratio Discrepancy
New JWST spectrum of a z=8.3 galaxy with prior ALMA dust detection shows AGN signatures, 0.15 Zsun metallicity, Mdust ~10^6 Msun, Tdust~91 K, and an [OIII] line ratio higher than nebular models allow.