Varying the star formation history of galaxies while keeping total ionizing photons fixed changes the size and warmth of ionized regions, altering the topology of reionization and the 21-cm global signal and power spectrum.
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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.
citing papers explorer
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POLAR-II: modeling star formation history of galaxies on the 21-cm signal from Epoch of Reionization
Varying the star formation history of galaxies while keeping total ionizing photons fixed changes the size and warmth of ionized regions, altering the topology of reionization and the 21-cm global signal and power spectrum.
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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.