Phase-space structure in the local dark matter distribution and its signature in direct detection experiments

Details Phase-space structure in the local dark matter distribution and its signature in direct detection experiments Phase-space structure in the local dark matter distribution and its signature in direct detection experiments

2008-12-02

arxiv.org/abs/0812.0362v1

Astronomy and Astrophysics

Astrophysics

15 pages, 15 figures, submitted to MNRAS. Pictures, movies, and further information on the Aquarius Project may be found at

Scientific paper

10.1111/j.1365-2966.2009.14630.x

We study predictions for dark matter phase-space structure near the Sun based on high-resolution simulations of six galaxy halos taken from the Aquarius Project. The local DM density distribution is predicted to be remarkably smooth; the density at the Sun differs from the mean over a best-fit ellipsoidal equidensity contour by less than 15% at the 99.9% confidence level. The local velocity distribution is also very smooth, but it differs systematically from a (multivariate) Gaussian distribution. This is not due to the presence of individual clumps or streams, but to broad features in the velocity modulus and energy distributions that are stable both in space and time and reflect the detailed assembly history of each halo. These features have a significant impact on the signals predicted for WIMP and axion searches. For example, WIMP recoil rates can deviate by ~10% from those expected from the best-fit multivariate Gaussian models. The axion spectra in our simulations typically peak at lower frequencies than in the case of multivariate Gaussian velocity distributions. Also in this case, the spectra show significant imprints of the formation of the halo. This implies that once direct DM detection has become routine, features in the detector signal will allow us to study the dark matter assembly history of the Milky Way. A new field, "dark matter astronomy", will then emerge.

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