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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9 Pith papers cite this work. Polarity classification is still indexing.
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Massive stars in the Milky Way form over Myr timescales that increase with final mass, inferred from joint LF fitting of compact HII regions and OB stars under the inertial-inflow model.
Existing HeII emission-line diagnostics identify pure Pop III galaxies but fail for hybrid Pop III/Pop II systems, introducing spectral degeneracies that hide residual first stars.
Using JWST photometry of ~17,000 galaxies, the median Balmer break strength decreases from 1.5 to 1.1 (flux ratio) from z~3.5 to z~10, driven by stellar population age, with rare extremely strong breaks at both epochs tracing distinct populations.
An analytical model of galaxies evolving along the star-forming main sequence shows that episodic quiescence or late assembly is required to reproduce observed star formation histories and avoid over-massive galaxies today.
Realistic 1D neutrino-driven explosions produce lower Fe-peak yields and different lighter-element patterns than piston or bomb models, with explodability driving discrepancies across FRANEC, KEPLER, and MESA progenitors.
Hα survey of 357 ALFALFA LSBGs shows deviation from the Kennicutt-Schmidt law but adherence to the extended Schmidt law that includes stellar mass.
An evolving star formation efficiency f_*(z) = 10^{0.13z-3.5} plus SNII-driven dust processes explain the UV LF at z=5-13, with galaxies retaining ~0.15% dust-to-stellar mass at z>9 and ALMA z=5-7 observations not representing the average population.
FLAME pipeline derives stellar luminosities, radii, masses and ages for Gaia DR4 using analytical calculations followed by minimization and Bayesian model inference, with tests showing statistical agreement to literature values.
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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Compact HII Regions as Clocks of Massive-Star Formation: Evidence for Long Formation Timescales
Massive stars in the Milky Way form over Myr timescales that increase with final mass, inferred from joint LF fitting of compact HII regions and OB stars under the inertial-inflow model.
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On the detection of Population III galaxies: Emission Line Diagnostics for Hybrid Stellar Populations
Existing HeII emission-line diagnostics identify pure Pop III galaxies but fail for hybrid Pop III/Pop II systems, introducing spectral degeneracies that hide residual first stars.
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Tracing the Evolution of the Balmer Break from Cosmic Dawn to Cosmic Noon with JWST
Using JWST photometry of ~17,000 galaxies, the median Balmer break strength decreases from 1.5 to 1.1 (flux ratio) from z~3.5 to z~10, driven by stellar population age, with rare extremely strong breaks at both epochs tracing distinct populations.
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Built to Rest: The Evolving Star-Forming Main Sequence Requires Episodic Quiescence or Late Assembly
An analytical model of galaxies evolving along the star-forming main sequence shows that episodic quiescence or late assembly is required to reproduce observed star formation histories and avoid over-massive galaxies today.
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Explodability matters: how realistic neutrino-driven explosions change explosive nucleosynthesis yields
Realistic 1D neutrino-driven explosions produce lower Fe-peak yields and different lighter-element patterns than piston or bomb models, with explodability driving discrepancies across FRANEC, KEPLER, and MESA progenitors.
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An $\rm H\alpha$ Imaging Survey of the Low Surface Brightness Galaxies Selected from the Spring Sky Region of the 40% ALFALFA HI Survey
Hα survey of 357 ALFALFA LSBGs shows deviation from the Kennicutt-Schmidt law but adherence to the extended Schmidt law that includes stellar mass.
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Exploring the interplay between star formation efficiency and dust in regulating the UV luminosity of early systems in the JWST and ALMA era
An evolving star formation efficiency f_*(z) = 10^{0.13z-3.5} plus SNII-driven dust processes explain the UV LF at z=5-13, with galaxies retaining ~0.15% dust-to-stellar mass at z>9 and ALMA z=5-7 observations not representing the average population.
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Stellar masses and ages in Gaia Data Release 4 from the Final Luminosity Age Mass Estimator algorithm
FLAME pipeline derives stellar luminosities, radii, masses and ages for Gaia DR4 using analytical calculations followed by minimization and Bayesian model inference, with tests showing statistical agreement to literature values.