Dark matter direct detection with non-Maxwellian velocity structure

Journal Article · Mon Feb 01 04:00:00 EST 2010 · Journal of Cosmology and Astroparticle Physics

DOI:https://doi.org/10.1088/1475-7516/2010/02/030· OSTI ID:22272996

Kuhlen, Michael ^[1]; Weiner, Neal ^[2]; Diemand, Jürg; Moore, Ben; Potter, Doug; Stadel, Joachim ^[3]; Madau, Piero ^[4]; Zemp, Marcel ^[5]

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1. School of Natural Science, Institute for Advanced Study, Einstein Lane, Princeton, NJ 08540 (United States)
2. Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003 (United States)
3. Institute for Theoretical Physics, University of Zurich, Winterthurerstrasse 190, 8057 Zurich (Switzerland)
4. Department of Astronomy and Astrophysics, University of California Santa Cruz, 1156 High Street, Santa Cruz, CA 95064 (United States)
5. Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, Michigan 48109 (United States)

The velocity distribution function of dark matter particles is expected to show significant departures from a Maxwell-Boltzmann distribution. This can have profound effects on the predicted dark matter - nucleon scattering rates in direct detection experiments, especially for dark matter models in which the scattering is sensitive to the high velocity tail of the distribution, such as inelastic dark matter (iDM) or light (few GeV) dark matter (LDM), and for experiments that require high energy recoil events, such as many directionally sensitive experiments. Here we determine the velocity distribution functions from two of the highest resolution numerical simulations of Galactic dark matter structure (Via Lactea II and GHALO), and study the effects for these scenarios. For directional detection, we find that the observed departures from Maxwell-Boltzmann increase the contrast of the signal and change the typical direction of incoming DM particles. For iDM, the expected signals at direct detection experiments are changed dramatically: the annual modulation can be enhanced by more than a factor two, and the relative rates of DAMA compared to CDMS can change by an order of magnitude, while those compared to CRESST can change by a factor of two. The spectrum of the signal can also change dramatically, with many features arising due to substructure. For LDM the spectral effects are smaller, but changes do arise that improve the compatibility with existing experiments. We find that the phase of the modulation can depend upon energy, which would help discriminate against background should it be found.

• OSTI ID: 22272996
• Journal Information: Journal of Cosmology and Astroparticle Physics, Journal Name: Journal of Cosmology and Astroparticle Physics Journal Issue: 02 Vol. 2010; ISSN 1475-7516
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
ASTROPHYSICS
BOLTZMANN STATISTICS
COMPARATIVE EVALUATIONS
COMPUTERIZED SIMULATION
COSMOLOGY
DISTRIBUTION FUNCTIONS
GEV RANGE
MILKY WAY
MODULATION
NONLUMINOUS MATTER
NUCLEONS
SCATTERING
VISIBLE RADIATION