Stellar feedback regulates radial gas inflow in the Milky Way center, yielding time-averaged rates that fall from 5e-3 to 1e-6 solar masses per year with both smooth secular and episodic components.
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M51 group shows more advanced dynamical evolution than M101, with flattened age and nebular metallicity gradients, enhanced dust, and environmental quenching signatures from interactions.
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Simulations of gas inflow in the Milky Way I. Stellar-Feedback-Regulated Transport from the Central Molecular Zone to the Circumnuclear disk
Stellar feedback regulates radial gas inflow in the Milky Way center, yielding time-averaged rates that fall from 5e-3 to 1e-6 solar masses per year with both smooth secular and episodic components.
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Analysis of spatially resolved stellar populations and emission line properties in nearby galaxies with J-PLUS data. II-Results for the M51 group and first comparison with the M101 group
M51 group shows more advanced dynamical evolution than M101, with flattened age and nebular metallicity gradients, enhanced dust, and environmental quenching signatures from interactions.