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 members of the M92 stream yield a Milky Way bar pattern speed of 29.1 +0.7/-0.4 km s^{-1} kpc^{-1}.
Boötes III has σ_v ≈ 1.7 km/s, a recent ~9.5 kpc pericenter on a polar eccentric orbit, and is actively tidally disrupting, with debris broadly consistent with the Styx stream.
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.
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.
Revised radial-velocity response model including V_R,sin and V_R,cos applied to Milky Way kinematic data constrains spiral pitch angle to ~10°, density contrast 5-18%, and pattern speed 10-20 km/s/kpc.
The Milky Way stellar halo is radially anisotropic inside ~35 kpc and becomes tangentially dominated farther out; after removing known accreted structures the profile stays radially biased at all radii.
An improved distribution-function modeling technique applied to thousands of stars yields a 4 million solar-mass central black hole and a total mass of 2.0-2.3 x 10^7 solar masses within 10 pc of the Milky Way nucleus.
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 Sagittarius dwarf progenitor had a metallicity gradient of roughly -0.3 dex per kpc prior to infall.
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.
Axisymmetric self-consistent models fitted to NSD kinematic data yield a mass of 1.05 x 10^9 solar masses, radial scale length ~89 pc, vertical scale ~28 pc, and declining velocity dispersion.
N-body simulations demonstrate that the inspiral of globular clusters in UGC 7346 results in the formation of a nuclear star cluster with mass (4.1-4.5)×10^5 solar masses within 1.5 Gyr.
An updated orbital frequency method shows multiple Milky Way bar lengths and pattern speeds are consistent with star data within 5 percent.
A two-wave radial corrugation model fitted to LAMOST and Gaia data reproduces the observed periodic radial velocity variations and explains the inner-outer disk transition in the Milky Way.
N-body simulations of a massive binary black hole in Leo I find orbital hardening to 1 pc followed by stalling due to the final parsec problem, with merger unlikely in a Hubble time owing to low stellar and dark matter densities.
An updated SynthPop Galactic model for Roman RGBTDS matches much of the bulge’s stellar content and kinematics but over-predicts optical microlensing rates by ~20% and fails near |b|≲0.5°.
citing papers explorer
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The Low-$\alpha$ Splash Population in the Milky Way
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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Constraining the Galactic bar using the M92 stellar stream
Spectroscopic members of the M92 stream yield a Milky Way bar pattern speed of 29.1 +0.7/-0.4 km s^{-1} kpc^{-1}.
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Bo\"otes III is a Tidally Disrupting Ultra-Faint Dwarf Galaxy on an Eccentric Polar Orbit
Boötes III has σ_v ≈ 1.7 km/s, a recent ~9.5 kpc pericenter on a polar eccentric orbit, and is actively tidally disrupting, with debris broadly consistent with the Styx stream.
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Tracing the very early disruption of the Sagittarius dwarf galaxy in the distant Milky Way halo
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.
-
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.
-
Tracing the kinematic perturbations of the Milky Way spiral arms with APOGEE DR17 and Gaia DR3
Revised radial-velocity response model including V_R,sin and V_R,cos applied to Milky Way kinematic data constrains spiral pitch angle to ~10°, density contrast 5-18%, and pattern speed 10-20 km/s/kpc.
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Characterizing the velocity anisotropy of the Milky Way's stellar halo
The Milky Way stellar halo is radially anisotropic inside ~35 kpc and becomes tangentially dominated farther out; after removing known accreted structures the profile stays radially biased at all radii.
-
Distribution function-based modelling of discrete kinematic datasets, in application to the Milky Way nuclear star cluster
An improved distribution-function modeling technique applied to thousands of stars yields a 4 million solar-mass central black hole and a total mass of 2.0-2.3 x 10^7 solar masses within 10 pc of the Milky Way nucleus.
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Disentangling the Distant Stellar Halo Using K-Giants in the DESI Year 3 Data
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.
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The Metallicity Gradient of Sagittarius Dwarf Spheroidal Galaxy Prior to Infall Constrained by S-PLUS Observations of its Tidal Stream
The Sagittarius dwarf progenitor had a metallicity gradient of roughly -0.3 dex per kpc prior to infall.
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Substructures of the Milky Way's Retrograde Halo: Evidence for Multiple Accretion Events
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.
-
Self-consistent modelling of the Milky Way's Nuclear Stellar Disc
Axisymmetric self-consistent models fitted to NSD kinematic data yield a mass of 1.05 x 10^9 solar masses, radial scale length ~89 pc, vertical scale ~28 pc, and declining velocity dispersion.
-
Formation of a nuclear star cluster through the inspiral of globular clusters: A case study of the dwarf elliptical galaxy UGC 7346
N-body simulations demonstrate that the inspiral of globular clusters in UGC 7346 results in the formation of a nuclear star cluster with mass (4.1-4.5)×10^5 solar masses within 1.5 Gyr.
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Self-consistent dynamical modelling of the Milky Way bar with orbital frequency analysis
An updated orbital frequency method shows multiple Milky Way bar lengths and pattern speeds are consistent with star data within 5 percent.
-
The multiple corrugations in the Galactic disk derived from the LAMOST and Gaia survey data
A two-wave radial corrugation model fitted to LAMOST and Gaia data reproduces the observed periodic radial velocity variations and explains the inner-outer disk transition in the Milky Way.
-
Dark Matter's influence on Evolution of MBHB in Dwarf Galaxies: A Case Study of Leo I dSph
N-body simulations of a massive binary black hole in Leo I find orbital hardening to 1 pc followed by stalling due to the final parsec problem, with merger unlikely in a Hubble time owing to low stellar and dark matter densities.
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An Updated SynthPop Model for Microlensing Simulations I: Model Description & Evaluation
An updated SynthPop Galactic model for Roman RGBTDS matches much of the bulge’s stellar content and kinematics but over-predicts optical microlensing rates by ~20% and fails near |b|≲0.5°.