Gaia DR3 data shows the Milky Way bar pattern speed is biased high by 14.4 km s^{-1} kpc^{-1}, with a bias-corrected estimate of 29.3 ± 2.3 km s^{-1} kpc^{-1}.
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Bar-like galaxies in a massive simulated cluster form through diverse mechanisms including tidal interactions with BCG progenitors, with formation times spanning 3 to 11 Gyr and lengths of 2-6 kpc.
Hydrodynamical simulations demonstrate that classical bulges enable bar-driven formation of nuclear stellar disks that bifurcate into pressure-supported nuclear star clusters and rotationally-supported nuclear stellar rings after gas depletion.
Barred galaxies with residual central emission and NUV-r color transition at the bar end represent an intermediate evolutionary phase in bar-driven quenching before full central quenching.
citing papers explorer
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From Gaia to GaiaNIR: II. A new view of the Milky Way bar
Gaia DR3 data shows the Milky Way bar pattern speed is biased high by 14.4 km s^{-1} kpc^{-1}, with a bias-corrected estimate of 29.3 ± 2.3 km s^{-1} kpc^{-1}.
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Diverse lifestyles of bar-like galaxies and their coevolution with the brightest galaxy in the most massive cluster of TNG50
Bar-like galaxies in a massive simulated cluster form through diverse mechanisms including tidal interactions with BCG progenitors, with formation times spanning 3 to 11 Gyr and lengths of 2-6 kpc.
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The SMUGGLE-Ring project: Bar and bulge effects on nuclear disk and ring formation
Hydrodynamical simulations demonstrate that classical bulges enable bar-driven formation of nuclear stellar disks that bifurcate into pressure-supported nuclear star clusters and rotationally-supported nuclear stellar rings after gas depletion.
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Tracing evolutionary pathways of bar-driven quenching in local Universe disc galaxies
Barred galaxies with residual central emission and NUV-r color transition at the bar end represent an intermediate evolutionary phase in bar-driven quenching before full central quenching.