Lumen modeling of IllustrisTNG50 shows that high ionization parameters from massive star clusters plus enhanced nitrogen abundances are needed to reproduce the extreme [OIII]/Hβ, [OIII]/[OII], and [NII]/Hα ratios seen in z>3 galaxies.
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New high-redshift empirical T_e-based metallicity calibrations for strong-line ratios derived from direct oxygen abundances in 46 galaxies spanning z=1.4-8.7.
Simulations of SPHEREx line intensity maps show cross-correlations (e.g., Hα × [OIII] at z=5) can reach S/N up to 99, probing galaxies with M < 4×10^10 M⊙, though most signal comes from brighter directly detectable galaxies.
Super-Eddington accretion boosts predicted LISA detections of high-redshift black hole binaries to ~64 per year while dropping ET detections to ~4 per year, compared to ~32 and ~64 under Eddington-limited growth.
citing papers explorer
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Origins of Extreme Emission-Line Ratios in z > 3 Galaxies: Insights from the Lumen Model
Lumen modeling of IllustrisTNG50 shows that high ionization parameters from massive star clusters plus enhanced nitrogen abundances are needed to reproduce the extreme [OIII]/Hβ, [OIII]/[OII], and [NII]/Hα ratios seen in z>3 galaxies.
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Direct T_e-based Metallicities of z=2-9 Galaxies with JWST/NIRSpec: Empirical Metallicity Calibrations Applicable from Reionization to Cosmic Noon
New high-redshift empirical T_e-based metallicity calibrations for strong-line ratios derived from direct oxygen abundances in 46 galaxies spanning z=1.4-8.7.
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On Cross-Correlating Line Intensity Maps from SPHEREx during Reionization
Simulations of SPHEREx line intensity maps show cross-correlations (e.g., Hα × [OIII] at z=5) can reach S/N up to 99, probing galaxies with M < 4×10^10 M⊙, though most signal comes from brighter directly detectable galaxies.
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Gravitational Waves from the Cosmic Dawn: Tracing Cosmic Black Hole Binaries with ET, LGWA and LISA
Super-Eddington accretion boosts predicted LISA detections of high-redshift black hole binaries to ~64 per year while dropping ET detections to ~4 per year, compared to ~32 and ~64 under Eddington-limited growth.