A 6D kinematic census identifies 18 anomalous Cepheids with extreme orbits, including one possibly scattered by globular cluster E3, and finds consistency between dynamical and stellar ages.
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6 Pith papers cite this work, alongside 32 external citations. Polarity classification is still indexing.
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UNVERDICTED 6representative citing papers
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}.
A CNN trained on AREPO simulations and synthetic observations reverts edge-on 13CO spectral data to top-down views of the CMZ as a proof-of-concept for supervised reversion.
Bar-induced migration can move ω Cen from the GSE phase-space region, but requires Ω_b ≲ 26 km s^{-1} kpc^{-1}, challenging consensus on the bar speed.
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.
Spectra of the western eROSITA bubbles reveal two uniform components at 0.60 keV and 0.21 keV with sub-solar abundances, plus a geometrical model constraining horizontal size to ~6 kpc but leaving vertical extent uncertain.
citing papers explorer
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Rogue Ones: Orbital census of Galactic Cepheids and their Anomalies
A 6D kinematic census identifies 18 anomalous Cepheids with extreme orbits, including one possibly scattered by globular cluster E3, and finds consistency between dynamical and stellar ages.
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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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IRIS: Deciphering Spectral-Line Imagery of the Galactic Center by Machine-Learning on Simulations
A CNN trained on AREPO simulations and synthetic observations reverts edge-on 13CO spectral data to top-down views of the CMZ as a proof-of-concept for supervised reversion.
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Bar-induced migration of $\omega$ Centauri away from Gaia Sausage-Enceladus
Bar-induced migration can move ω Cen from the GSE phase-space region, but requires Ω_b ≲ 26 km s^{-1} kpc^{-1}, challenging consensus on the bar speed.
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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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The SRG/eROSITA diffuse soft X-ray background II. spectra and morphology of the eROSITA bubbles in the western Galactic hemisphere
Spectra of the western eROSITA bubbles reveal two uniform components at 0.60 keV and 0.21 keV with sub-solar abundances, plus a geometrical model constraining horizontal size to ~6 kpc but leaving vertical extent uncertain.