Resolved photometry of four high-redshift quiescent galaxies reveals negative color gradients that lower estimated stellar masses by 0.1 dex relative to slit measurements, reducing model tensions under an age-driven interpretation.
Indicators of star formation: 4000 Angstrom break and Balmer lines
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
abstract
The behaviour of the 4000 Angstrom break index and of the equivalent width of the main Balmer lines is investigated a) for a single star as a function of effective temperature, gravity and metallicity and b) for a single stellar population as a function of age and metallicity. Consequences for the interpretation of integrated spectra are presented.
fields
astro-ph.GA 3years
2026 3verdicts
UNVERDICTED 3representative citing papers
Different quenching tracers applied to MaNGA galaxies produce varying inside-out versus outside-in fractions, with inside-out rising at higher stellar mass while halo-mass trends are weaker.
Simulations of high-redshift galaxies show the 1719 Å UV index reliably traces stellar metallicity while others are more sensitive to star formation history.
citing papers explorer
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Unbreaking the Universe: MINERVA Measurements of Color Gradients in Massive Quiescent Galaxies Can Help Ease Too-Early Star Formation Tensions
Resolved photometry of four high-redshift quiescent galaxies reveals negative color gradients that lower estimated stellar masses by 0.1 dex relative to slit measurements, reducing model tensions under an age-driven interpretation.
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Inside-Out vs. Outside-In Quenching of MaNGA Galaxies: Dependence on Stellar Mass and Environment
Different quenching tracers applied to MaNGA galaxies produce varying inside-out versus outside-in fractions, with inside-out rising at higher stellar mass while halo-mass trends are weaker.
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First Light And Reionization Epoch Simulations (FLARES) XXI: The UV Indices of Galaxies in the Early Universe
Simulations of high-redshift galaxies show the 1719 Å UV index reliably traces stellar metallicity while others are more sensitive to star formation history.