Empirical Determination of Dark Matter Velocities Using Metal-Poor Stars

Jonah Herzog-Arbeitman, Mariangela Lisanti, Piero Madau, Lina Necib

Research output: Contribution to journalArticle

12 Citations (Scopus)

Abstract

The Milky Way dark matter halo is formed from the accretion of smaller subhalos. These sub-units also harbor stars - typically old and metal-poor - that are deposited in the Galactic inner regions by disruption events. In this Letter, we show that the dark matter and metal-poor stars in the Solar neighborhood share similar kinematics due to their common origin. Using the high-resolution eris simulation, which traces the evolution of both the dark matter and baryons in a realistic Milky Way analog galaxy, we demonstrate that metal-poor stars are indeed effective tracers for the local, virialized dark matter velocity distribution. The local dark matter velocities can therefore be inferred from observations of the stellar halo made by the Sloan Digital Sky Survey within 4 kpc of the Sun. This empirical distribution differs from the standard halo model in important ways and suggests that the bounds on the spin-independent scattering cross section may be weakened for dark matter masses below ∼10 GeV. Data from Gaia will allow us to further refine the expected distribution for the smooth dark matter component, and to test for the presence of local substructure.

Original languageEnglish (US)
Article number041102
JournalPhysical review letters
Volume120
Issue number4
DOIs
StatePublished - Jan 24 2018

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dark matter
stars
metals
halos
solar neighborhood
harbors
substructures
scattering cross sections
tracers
baryons
kinematics
velocity distribution
analogs
galaxies
high resolution
simulation

All Science Journal Classification (ASJC) codes

  • Physics and Astronomy(all)

Cite this

Herzog-Arbeitman, Jonah ; Lisanti, Mariangela ; Madau, Piero ; Necib, Lina. / Empirical Determination of Dark Matter Velocities Using Metal-Poor Stars. In: Physical review letters. 2018 ; Vol. 120, No. 4.
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Empirical Determination of Dark Matter Velocities Using Metal-Poor Stars. / Herzog-Arbeitman, Jonah; Lisanti, Mariangela; Madau, Piero; Necib, Lina.

In: Physical review letters, Vol. 120, No. 4, 041102, 24.01.2018.

Research output: Contribution to journalArticle

TY - JOUR

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AU - Herzog-Arbeitman, Jonah

AU - Lisanti, Mariangela

AU - Madau, Piero

AU - Necib, Lina

PY - 2018/1/24

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N2 - The Milky Way dark matter halo is formed from the accretion of smaller subhalos. These sub-units also harbor stars - typically old and metal-poor - that are deposited in the Galactic inner regions by disruption events. In this Letter, we show that the dark matter and metal-poor stars in the Solar neighborhood share similar kinematics due to their common origin. Using the high-resolution eris simulation, which traces the evolution of both the dark matter and baryons in a realistic Milky Way analog galaxy, we demonstrate that metal-poor stars are indeed effective tracers for the local, virialized dark matter velocity distribution. The local dark matter velocities can therefore be inferred from observations of the stellar halo made by the Sloan Digital Sky Survey within 4 kpc of the Sun. This empirical distribution differs from the standard halo model in important ways and suggests that the bounds on the spin-independent scattering cross section may be weakened for dark matter masses below ∼10 GeV. Data from Gaia will allow us to further refine the expected distribution for the smooth dark matter component, and to test for the presence of local substructure.

AB - The Milky Way dark matter halo is formed from the accretion of smaller subhalos. These sub-units also harbor stars - typically old and metal-poor - that are deposited in the Galactic inner regions by disruption events. In this Letter, we show that the dark matter and metal-poor stars in the Solar neighborhood share similar kinematics due to their common origin. Using the high-resolution eris simulation, which traces the evolution of both the dark matter and baryons in a realistic Milky Way analog galaxy, we demonstrate that metal-poor stars are indeed effective tracers for the local, virialized dark matter velocity distribution. The local dark matter velocities can therefore be inferred from observations of the stellar halo made by the Sloan Digital Sky Survey within 4 kpc of the Sun. This empirical distribution differs from the standard halo model in important ways and suggests that the bounds on the spin-independent scattering cross section may be weakened for dark matter masses below ∼10 GeV. Data from Gaia will allow us to further refine the expected distribution for the smooth dark matter component, and to test for the presence of local substructure.

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