The Binary Fraction of Milky Way Field Stars in DESI: Dependence on Chemical Abundance

arXiv:2610.11102 · astro-ph.GA, astro-ph.SR · Submitted 2026-10-08 · Read on arXiv

astro-ph.GA, astro-ph.SR

Submitted: 2026-10-08

Updated: 2026-10-08

Code: https://github.com/segasai/rvspecfit

Terminology

• Abundance — 81× in this paper · explained in 1 episode
• Metallicity — 29× in this paper · explained in 3 episodes
• Calibration — 3× in this paper · explained in 7 episodes
• Milky Way Survey — 3× in this paper
• Core — 2× in this paper · explained in 2 episodes
• Department of Energy — 2× in this paper
• Trace — 2× in this paper · explained in 2 episodes
• Accuracy — 1× in this paper · explained in 1 episode
• Benchmark — 1× in this paper · explained in 2 episodes
• Consistency — 1× in this paper · explained in 3 episodes
• Dark Energy Spectroscopic Instrument — 1× in this paper
• European Space Agency — 1× in this paper
• Initial Mass Function (IMF) — 1× in this paper · explained in 2 episodes
• Modified Julian Date — 1× in this paper
• National Science Foundation — 1× in this paper
• Robustness — 1× in this paper · explained in 5 episodes
• Stellar Feedback — 1× in this paper · explained in 2 episodes
• Velocity Dispersion — 1× in this paper · explained in 2 episodes

Sources

• The DESI Experiment Part I: Science,Targeting, and Survey Design
• The DESI Experiment Part II: Instrument Design
• DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements
• The Backup Program of the Dark Energy Spectroscopic Instrument's Milky Way Survey
• The DESI Experiment, a whitepaper for Snowmass 2013
• The Origin and Evolution of Multiple Star Systems

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