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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2 Pith papers cite this work. Polarity classification is still indexing.
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astro-ph.GA 2years
2026 2verdicts
UNVERDICTED 2representative citing papers
JWST auroral-line selected galaxies at high redshift show an MZR slope of 0.38 with selection biases favoring high-SFR low-metallicity systems, while stacked non-detections lie closer to the fundamental metallicity relation.
citing papers explorer
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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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Shape of Direct-Method Mass-Metallicity Relation with JWST: Fast-Track Nitrogen and Helium Enrichment
JWST auroral-line selected galaxies at high redshift show an MZR slope of 0.38 with selection biases favoring high-SFR low-metallicity systems, while stacked non-detections lie closer to the fundamental metallicity relation.