Resolved gas and dust maps in a z=2 quiescent galaxy reveal accreted material from tidal interactions and a past star-formation rejuvenation, indicating that gas content variations are not solely due to consumption timescales.
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The propagation of uncertainties in stellar population synthesis modeling III: model calibration, comparison, and evaluation
19 Pith papers cite this work, alongside 1,082 external citations. Polarity classification is still indexing.
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abstract
Stellar population synthesis (SPS) provides the link between the stellar and dust content of galaxies and their observed spectral energy distributions. In the present work we perform a comprehensive calibration of our own flexible SPS (FSPS) model against a suite of data. Several public SPS models are intercompared, including the models of Bruzual & Charlot (BC03), Maraston (M05) and FSPS. The relative strengths and weaknesses of these models are evaluated, with the following conclusions: 1) The FSPS and BC03 models compare favorably with MC data at all ages, whereas M05 colors are too red and the age-dependence is incorrect; 2) All models yield similar optical and near-IR colors for old metal-poor systems, and yet they all provide poor fits to the integrated J-K and V-K colors of both MW and M31 star clusters; 4) All models predict ugr colors too red, D4000 strengths too strong and Hdelta strengths too weak compared to massive red sequence galaxies, under the assumption that such galaxies are composed solely of old metal-rich stars; 5) FSPS and, to a lesser extent, BC03 can reproduce the optical and near-IR colors of post-starburst galaxies, while M05 cannot. Reasons for these discrepancies are explored. The failure at predicting the ugr colors, D4000, and Hdelta strengths can be explained by some combination of a minority population of metal-poor stars, young stars, blue straggler and/or blue horizontal branch stars, but not by appealing to inadequacies in either theoretical stellar atmospheres or canonical evolutionary phases (e.g., the main sequence turn-off). We emphasize that due to a lack of calibrating star cluster data in regions of the metallicity-age plane relevant for galaxies, all of these models continue to suffer from serious uncertainties that are difficult to quantify. (ABRIDGED)
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A JWST census detects neutral ISM absorption in 76 of 309 galaxies at 0.6<z<4 and outflows in 26, indicating AGN-driven neutral outflows dominate in quiescent systems at cosmic noon.
Progenitor age is the primary physical driver of the host-mass and host-sSFR magnitude steps in Type Ia supernovae, with the mass step eliminated by direct age correction.
Accreting X-ray sources cannot supply enough EUV photons to account for He III regions in metal-poor star-forming dwarf galaxies.
Milky Way abundance trends act as effective empirical proxies for nucleosynthetic yields, recovering alpha and Fe-peak abundances in quiescent galaxies with 0.05 dex median offset versus 0.23 dex for theory, indicating largely universal yields.
JWST data show massive quiescent galaxies in high-redshift proto-clusters formed and quenched simultaneously, with AGN signatures, indicating environmental triggering of quenching.
Discovery of a gravitationally lensed Type II supernova at z=1.37 with magnification ≳100×, confirmed via multi-telescope spectra and imaging.
Star formation histories inferred for z=2-5 massive quiescent galaxies imply past number densities that align with observed rapid evolution since z~7.
Spatially-resolved spectroscopy detects AGNs in 4-9% of low-mass galaxies, higher than single-fiber rates because it catches extended emission missed by central-point observations.
Abundant early heavy seeds plus frequent mergers produce the massive black holes seen by JWST at z>9 and yield about four LISA events per year at z>=8.
Massive quiescent galaxies at cosmic noon are compact and bulge-dominated with inside-out quenching, where inner regions formed stars ~0.5 Gyr earlier and quenched faster than outskirts.
COLIBRE simulations with SKIRT post-processing match observed galaxy luminosity functions from FUV to submm at z=0, except underpredicting bright mid-IR galaxies.
Massive quiescent galaxies at high redshifts show elevated fractions in small-scale overdensities, indicating environmental quenching via galaxy interactions plays a major role.
Simulations of high-redshift galaxies show the 1719 Å UV index reliably traces stellar metallicity while others are more sensitive to star formation history.
ASTRID simulation with dust model calibrated to SDSS at z=0 produces validated luminosity functions and LSST-ready mock catalogs of 378 million galaxies with predicted number counts in ugrizy bands from z=0 to 2.
Models with prominent TP-AGB phases best fit the near-IR spectra of high-redshift quiescent galaxies, yielding younger ages and lower stellar masses than models with weaker TP-AGB contributions.
Rest-frame 6-8um MIRI luminosity provides broken power-law SFR calibrations with 0.2-0.3 dex scatter and UV+IR composites at 0.15 dex, supporting robust use above log M* ~9 up to z~3.
AI techniques for photometric redshift estimation have converged and are now limited by the size, systematics, and selection effects in spectroscopic training samples rather than by methodology.
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Resolved Maps of Gas and Dust in a Massive Quiescent Galaxy at z=2 from INQUEST-JWST: Evidence of Accretion and Rejuvenation
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Low-mass Active Galaxies in the SAMI Galaxy Survey with Spatially-resolved Spectroscopy
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Morphological and Star Formation Properties of Cosmic Noon Massive Quiescent Galaxies
Massive quiescent galaxies at cosmic noon are compact and bulge-dominated with inside-out quenching, where inner regions formed stars ~0.5 Gyr earlier and quenched faster than outskirts.
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Galaxy luminosity functions from far-UV to submillimetre at $z=0$ in the COLIBRE simulations
COLIBRE simulations with SKIRT post-processing match observed galaxy luminosity functions from FUV to submm at z=0, except underpredicting bright mid-IR galaxies.
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The role of small-scale environments in the quenching of massive galaxies at $1<z<5$
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First Light And Reionization Epoch Simulations (FLARES) XXI: The UV Indices of Galaxies in the Early Universe
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The Galaxy Luminosity Functions in ASTRID: Predictions for LSST
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Prevailing thermally-pulsing-asymptotic-giant branch stars in the near-infrared rest-frame spectra of distant quiescent galaxies: towards robust galaxy ages and masses
Models with prominent TP-AGB phases best fit the near-IR spectra of high-redshift quiescent galaxies, yielding younger ages and lower stellar masses than models with weaker TP-AGB contributions.
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Calibrating Photometric Mid-Infrared Star Formation Rates for JWST
Rest-frame 6-8um MIRI luminosity provides broken power-law SFR calibrations with 0.2-0.3 dex scatter and UV+IR composites at 0.15 dex, supporting robust use above log M* ~9 up to z~3.
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Machine Learning Techniques for Astrophysics and Cosmology: Photometric Redshifts
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