Detection of a stellar bar in the extreme gas-rich galaxy GN20 at z=4.055 shows that gas-rich disks support rapid bar formation in the early universe.
P., Mayer, L., Carollo, C
7 Pith papers cite this work. Polarity classification is still indexing.
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Simulations of dwarf galaxies show V/σ rising with stellar mass, with HI gas and young stars more rotation-supported than old stars.
Simulations show Lindblad-resonance wrinkles from non-winding spirals are filled with zero-age stars on orbits normally occupied by much older populations, offering an age-based constraint on past transient spiral patterns.
A galaxy at z=3.16 has a bar with older stars making up 30% of its mass but only 8% of its recent star formation, supporting inside-out galaxy formation and possible early bar quenching.
Barred galaxies transition from actively star-forming at z~1-2 to quiescent at z~0, with the fraction of quiescent galaxies hosting bars increasing steeply over cosmic time.
ELMA automates projected bar-length estimation from galaxy images via iterative elliptical isophote fitting that locates the semi-major axis at peak ellipticity.
Star-forming galaxies show R_e,J ∝ (1+z)^(-0.92) and μ_J evolution with γ=3.07 while quiescent galaxies evolve faster (β=-1.34, γ=3.70) at fixed stellar mass, with evolution driven by luminosity and size changes.
citing papers explorer
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A stellar bar hidden in an extreme gas-rich disk galaxy at z=4.055
Detection of a stellar bar in the extreme gas-rich galaxy GN20 at z=4.055 shows that gas-rich disks support rapid bar formation in the early universe.
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$V/\sigma$ Trends with Mass for Dwarf Galaxies from the Marvelous Massive Dwarfs Suite
Simulations of dwarf galaxies show V/σ rising with stellar mass, with HI gas and young stars more rotation-supported than old stars.
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Wrinkles in Time. II. Stellar Age Trends in Kinematic Signatures from Transient Spiral Structure
Simulations show Lindblad-resonance wrinkles from non-winding spirals are filled with zero-age stars on orbits normally occupied by much older populations, offering an age-based constraint on past transient spiral patterns.
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Discovery of a Barred-Spiral Galaxy at $z_{spec}$ = 3.16 II. The Star Formation History
A galaxy at z=3.16 has a bar with older stars making up 30% of its mass but only 8% of its recent star formation, supporting inside-out galaxy formation and possible early bar quenching.
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Exploring the Relationship Between Bars, Star Formation Activity, and Host Galaxy Properties from $\mathbf{z \sim 0}$ to $\mathbf{z \sim 2}$
Barred galaxies transition from actively star-forming at z~1-2 to quiescent at z~0, with the fraction of quiescent galaxies hosting bars increasing steeply over cosmic time.
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ELMA: ELlipse-based bar MAjor axis estimator
ELMA automates projected bar-length estimation from galaxy images via iterative elliptical isophote fitting that locates the semi-major axis at peak ellipticity.
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COSMOS-Web: Galaxy Size and Surface Brightness Evolution at Rest-Frame 1.22 $\mu$m Since $z=3$
Star-forming galaxies show R_e,J ∝ (1+z)^(-0.92) and μ_J evolution with γ=3.07 while quiescent galaxies evolve faster (β=-1.34, γ=3.70) at fixed stellar mass, with evolution driven by luminosity and size changes.