Abstract
From an assumed signal in a Dark Matter (DM) direct detection experiment a lower bound on the product of the DM-nucleon scattering cross section and the local DM density is derived, which is independent of the local DM velocity distribution. This can be combined with astrophysical determinations of the local DM density. Within a given particle physics model the bound also allows a robust comparison of a direct detection signal with limits from the LHC. Furthermore, the bound can be used to formulate a condition which has to be fulfilled if the particle responsible for the direct detection signal is a thermal relic, regardless of whether it constitutes all DM or only part of it. We illustrate the arguments by adopting a simplified DM model with a Z′ mediator and assuming a signal in a future xenon direct detection experiment.
Highlights
In fig. 3, we show for illustration the 90% confidence level (CL) lower bound on the Dark Matter (DM) density from CDMS-Si data as a function of σSI for mχ = 10 GeV and compare it with the 90% CL interval obtained from assuming the SHM
We have derived lower bounds on the product of the DM–nucleus scattering cross section and the local DM density from a positive signal in a direct detection experiment, which is independent of the DM velocity distribution
If an upper bound on the local DM density from kinematical Milky Way observations is applied, our bounds provide a robust lower bound on the scattering cross section
Summary
We review the relevant expressions for DD of dark matter. We focus on elastic scattering of DM particles χ with mass mχ off a nucleus with mass number A and mass mA, depositing the nuclear recoil energy ER. In the following we will concentrate on spin-independent (SI) and spin-dependent (SD) scattering from a contact interaction This implies that the differential scattering cross section dσA(v)/dER scales as 1/v2. Where GA[E1,E2](ER) is the detector response function describing the probability that a DM event with true recoil energy ER is reconstructed in the energy interval [E1, E2], including energy resolution, energy dependent efficiencies, and possibly quenching factors.. Where GA[E1,E2](ER) is the detector response function describing the probability that a DM event with true recoil energy ER is reconstructed in the energy interval [E1, E2], including energy resolution, energy dependent efficiencies, and possibly quenching factors.2 We use this notation to indicate energy integration and sum over targets
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