The average dust attenuation law at 2<z<7 is empirically measured from stacked SEDs and matches the local starburst curve with R_V=3.98, a flatter UV slope, and no 2175A bump.
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Spatially resolved JWST observations of lensed LAE HCM 6A at z=6.57 reveal Lyα escaping from a dust-cleared central clump in the youngest region, with age-dependent Calzetti-like attenuation curves.
Clumpy turbulent structures in HII regions leave the slope of the internal nebular attenuation curve unchanged because dust obscuration in dense clumps is offset by higher local emission-line production.
Switching between four common stellar population synthesis models produces systematic offsets of up to 0.6 dex in stellar mass and 0.4 dex in star formation rate for the same galaxies.
citing papers explorer
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A first empirical derivation of the average dust attenuation law at 2<z<7
The average dust attenuation law at 2<z<7 is empirically measured from stacked SEDs and matches the local starburst curve with R_V=3.98, a flatter UV slope, and no 2175A bump.
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Resolving dust and Ly{\alpha} emission in a lensed galaxy at the epoch of reionization with JWST/CANUCS
Spatially resolved JWST observations of lensed LAE HCM 6A at z=6.57 reveal Lyα escaping from a dust-cleared central clump in the youngest region, with age-dependent Calzetti-like attenuation curves.
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The Internal Nebular Attenuation Curve of Three-Dimensional Turbulent HII regions
Clumpy turbulent structures in HII regions leave the slope of the internal nebular attenuation curve unchanged because dust obscuration in dense clumps is offset by higher local emission-line production.
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Impact of stellar population models on the estimated physical properties of galaxies
Switching between four common stellar population synthesis models produces systematic offsets of up to 0.6 dex in stellar mass and 0.4 dex in star formation rate for the same galaxies.