A data-driven decomposition of stellar abundance vectors into four latent patterns identifies distinct contributions from core-collapse supernovae, Type Ia supernovae, and AGB stars across the Milky Way disc.
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Observational identification of a low-α Splash population in APOGEE DR17 and GASTRO simulations showing that clumpy proto-disk scattering, but not a major merger alone, heats old thin-disk stars to form both high- and low-α Splash components.
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Spectroscopic measurements confirm a tight 6D phase-space clump of four RGB stars as part of the distant southern spur of the Sagittarius stream, likely stripped from Sagittarius's halo in the earliest interaction phases.
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.
The Milky Way stellar disk shows a broken radial density profile with four components, azimuthal dependence, inner and outer flaring, and a density-metallicity bump possibly from radial migration.
PhDLspec combines differential spectra from physical stellar models with a transformer to derive approximately 30 stellar parameters from low-resolution spectra hundreds of times faster than traditional calculations.
300S stellar stream exhibits three density peaks, smooth width variations, a possible 4.7 degree gap, and a kink modeled as resulting from Large Magellanic Cloud interaction across its full known footprint.
A public catalogue provides geometric and photogeometric distances plus uncertainties for 1.47 billion Gaia EDR3 stars derived via probabilistic inference with a three-dimensional Galactic prior.
New high-resolution spectra yield abundances for 7 neutron-capture elements in open cluster stars, revealing flat Milky Way gradients for second-peak s- and r-process species and shallower slopes for first-peak s-process.
DESI K-giant catalog identifies Aleph, Sagittarius, GSE, Cetus-Palca and Orphan-Chenab, then shows residual halo high-angular-momentum stars have bimodal MDFs unlike GSE or Sagittarius.
The MAGIC survey provides photometric metallicities for RGB stars over ~3000 deg² using CaHK narrow-band imaging plus DELVE g,r,i data, recovering 13/14 known ultra-faint dwarfs and confirming a distant Reticulum II member.
A blind 12D chemo-dynamical clustering analysis with UMAP and HDBSCAN on SDSS-V DR19 and Gaia DR3 data recovers seven known halo substructures and reports five new tightly bound candidates FO1-FO5.
TOI-4311 hosts a 0.99-day super-Earth (1.38 R_earth, 4.5 M_earth) and 15-day sub-Neptune (2.47 R_earth), plus a candidate 38-day planet, with the dense inner planet potentially challenging formation theories given the host's galactic population.
A uniform spectroscopic catalog of 625 exoplanet hosts shows subsolar-metallicity giant-planet hosts are alpha-enhanced relative to both iron-rich hosts and typical metal-poor field stars.
FIRE-2 simulations show that stellar radial redistribution scatter saturates at ~2 kpc for stars older than ~3 Gyr, with net orbital changes depending on age and current radius, broadly matching Milky Way observations.
Chemical tagging with seven elements recovers 63 kinematically rejected stars in 22 open clusters, 35% of which lie outside Jacobi radii as extra-tidal debris.
Optimized filters centered at 3920-3960 Angstrom yield metallicity estimates with 0.18-0.39 dex precision down to [Fe/H] ~ -4 for metal-poor stars from Gaia XP spectra, enabling a catalog of 14.5 million such stars.
A large sample of blue horizontal-branch stars reveals that the Milky Way halo anisotropy increases from the center, stays radially dominated after removing merger debris, and shows older stars on colder, less radial orbits in the inner regions.
The Sagittarius dwarf progenitor had a metallicity gradient of roughly -0.3 dex per kpc prior to infall.
Negative Ca II IRT residual indices in FGK stars arise mainly because synthetic photospheric templates miss chromospheric structure and NLTE effects that deepen the observed cores.
The Milky Way retrograde halo contains debris from multiple accreted dwarf galaxies, shown by distinct metallicity distribution peaks that remain separate even when combined with orbital dynamics.
New CCSN yield tables at varying metallicities are inserted into galactic chemical evolution models and tuned to reproduce the Si-group and Fe-group abundances measured by Hitomi in the Perseus Cluster.
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A data-driven decomposition of stellar abundance vectors into four latent patterns identifies distinct contributions from core-collapse supernovae, Type Ia supernovae, and AGB stars across the Milky Way disc.
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The Low-$\alpha$ Splash Population in the Milky Way
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