Dust grain size distributions evolve from large-grain dominated at high redshift to MRN-like at low redshift, driven primarily by shattering and ISM accretion after stars supply initial large grains, reproducing z=0 dust masses and Milky Way extinction properties.
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@doi [ApJ] 10.3847/1538-4357/aabf3c
17 Pith papers cite this work. Polarity classification is still indexing.
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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.
High-resolution mapping reveals nitrogen enrichment around super star clusters in NGC 5253, attributed to Wolf-Rayet stars with material expelled to surrounding gas.
JWST data show the clumpy galaxy fraction increasing from ~10% at z~7.75 to ~70% at z~2.75 for log(M*/Msun) >=9, with mass dependence and suggested formation mechanisms differing by epoch.
Measures a new nebular attenuation curve from 1400-9550 Å for galaxy GOODSN-17940 at z=4.41 that is steeper than Milky Way/SMC/Calzetti at long wavelengths, similar in blue-optical, and shallower in UV with no 2175 Å bump.
75% of massive compact quiescent galaxies at z~0 require three-component photometric models (bulge + disk + envelope), versus only 7% of mass-matched control quiescent galaxies.
Corrected empirical limits show the most massive galaxies never exceed the theoretical baryonic maximum of 0.16 times halo virial mass, keeping observations consistent with LambdaCDM at all redshifts.
JWST spectra of galaxies reveal a ~110 cMpc ionized bubble at z~6 with IGM transmission 0.17, an order of magnitude above average, linked to a galaxy overdensity.
Large sample of SN Ia hosts shows young mean progenitor age of 3.5 Gyr and only 1.5 Gyr evolution, leading to negligible cosmological bias of 0.007 mag.
Pantheon+ delivers tighter SN Ia constraints on Ω_M, w0, wa, and H0 from 1550 events, consistent with a cosmological constant, with SN systematics contributing less than one third to H0 uncertainty.
Dust attenuation follows a universal mass-dependent relation from z=0 to 7 with a transition at 10^9 solar masses where nebular attenuation steepens relative to stellar.
MaNGA data shows dwarf galaxies (log M* <= 9.5) remain mostly star-forming with weak environmental dependence while intermediate-mass galaxies (9.5 < log M* < 10) display stronger quenching trends, and dwarf early-types host younger stellar populations than their intermediate-mass counterparts.
A z=2.96 protocluster in COSMOS shows +0.2 dex higher stellar masses, mild SFR enhancement in low-mass galaxies, and no rise in quiescent fraction compared to the field.
BayeSN analysis of ZTF Type Ia supernovae confirms a ~0.1 mag intrinsic environmental step in standardized brightness that is not explained by differences in dust extinction properties.
Close major galaxy pairs exhibit 8.8% lower HI gas fractions and 15% higher HI star formation efficiency in S+S systems than mass- and redshift-matched isolated controls.
A z=4.0148 galaxy shows clumpy ring morphology consistent with either a collisional ring or strong lensing by a foreground galaxy at z~1.7.
Strong bars correlate with massive red galaxies, boost central star formation in low-mass systems while quenching it in high-mass ones, and increase AGN incidence, supporting bar-driven gas inflow.
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Dust and Grain Size Evolution in Galaxy Simulations: What Matters and What Does Not
Dust grain size distributions evolve from large-grain dominated at high redshift to MRN-like at low redshift, driven primarily by shattering and ISM accretion after stars supply initial large grains, reproducing z=0 dust masses and Milky Way extinction properties.
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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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The heart of NGC 5253 as seen with MUSE-NFM: nitrogen enrichment through stellar chemical feedback at parsec scales
High-resolution mapping reveals nitrogen enrichment around super star clusters in NGC 5253, attributed to Wolf-Rayet stars with material expelled to surrounding gas.
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The Fraction of Clumpy Galaxies in JADES over $2<z<9$
JWST data show the clumpy galaxy fraction increasing from ~10% at z~7.75 to ~70% at z~2.75 for log(M*/Msun) >=9, with mass dependence and suggested formation mechanisms differing by epoch.
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The AURORA Survey: The Nebular Attenuation Curve of a Galaxy at z=4.41 from Ultraviolet to Near-Infrared Wavelengths
Measures a new nebular attenuation curve from 1400-9550 Å for galaxy GOODSN-17940 at z=4.41 that is steeper than Milky Way/SMC/Calzetti at long wavelengths, similar in blue-optical, and shallower in UV with no 2175 Å bump.
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Small and Complex I: The Three Component Structure of $z \sim 0$ Massive Compact Quiescent Galaxies
75% of massive compact quiescent galaxies at z~0 require three-component photometric models (bulge + disk + envelope), versus only 7% of mass-matched control quiescent galaxies.
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Empirical estimates of how massive galaxies can be in {\Lambda}CDM
Corrected empirical limits show the most massive galaxies never exceed the theoretical baryonic maximum of 0.16 times halo virial mass, keeping observations consistent with LambdaCDM at all redshifts.
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Using Ly$\alpha$ Transmitted Spectrum to Probe IGM Transmission and Identify Ionized Structures in Cosmic Reionization
JWST spectra of galaxies reveal a ~110 cMpc ionized bubble at z~6 with IGM transmission 0.17, an order of magnitude above average, linked to a galaxy overdensity.
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Old Universe, Young SNe Ia: A Statistical Analysis of Type Ia Supernova Progenitor Age from 6,983 TITAN Host Galaxies, and Implications for Cosmology
Large sample of SN Ia hosts shows young mean progenitor age of 3.5 Gyr and only 1.5 Gyr evolution, leading to negligible cosmological bias of 0.007 mag.
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The Pantheon+ Analysis: Cosmological Constraints
Pantheon+ delivers tighter SN Ia constraints on Ω_M, w0, wa, and H0 from 1550 events, consistent with a cosmological constant, with SN systematics contributing less than one third to H0 uncertainty.
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SDSS+JWST Census of Stellar and Nebular Dust Attenuation at $z \sim 0$-7: Mass Dependence and Redshift Evolution
Dust attenuation follows a universal mass-dependent relation from z=0 to 7 with a transition at 10^9 solar masses where nebular attenuation steepens relative to stellar.
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Dwarf and Intermediate-Mass Galaxies in MaNGA: Evidence for Different Evolutionary Trends
MaNGA data shows dwarf galaxies (log M* <= 9.5) remain mostly star-forming with weak environmental dependence while intermediate-mass galaxies (9.5 < log M* < 10) display stronger quenching trends, and dwarf early-types host younger stellar populations than their intermediate-mass counterparts.
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Early Emergence of Environmental Effects: Accelerated Galaxy Assembly in a z=2.96 Protocluster in the COSMOS Field
A z=2.96 protocluster in COSMOS shows +0.2 dex higher stellar masses, mild SFR enhancement in low-mass galaxies, and no rise in quiescent fraction compared to the field.
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On the origin of the environmental step: A BayeSN view of the ZTF SN Ia DR2
BayeSN analysis of ZTF Type Ia supernovae confirms a ~0.1 mag intrinsic environmental step in standardized brightness that is not explained by differences in dust extinction properties.
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HI Gas and Star Formation in Major Galaxy Pairs from the FAST All-Sky HI Survey (FASHI)
Close major galaxy pairs exhibit 8.8% lower HI gas fractions and 15% higher HI star formation efficiency in S+S systems than mass- and redshift-matched isolated controls.
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JWST's PEARLS: A clumpy ring galaxy at $z = 4.0148$
A z=4.0148 galaxy shows clumpy ring morphology consistent with either a collisional ring or strong lensing by a foreground galaxy at z~1.7.
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Investigating the Effects of Bars on Star Formation and Nuclear Activity of Galaxies Using DESI Survey Data
Strong bars correlate with massive red galaxies, boost central star formation in low-mass systems while quenching it in high-mass ones, and increase AGN incidence, supporting bar-driven gas inflow.