Abstract
If dark matter (DM) originates from physics near the Planck scale it could be directly detected via its multiple scattering signals, yet this requires a large cross section for DM interactions with atoms. Hence, detection of such DM could imply mediation by new low mass messengers. We propose that a dark $U(1)_d$ remnant of the underlying spacetime geometry or a unified theory may survive down to small mass scales $\sim 1$ GeV, connecting low energy Standard Model (SM) and Planck scale phenomena. Typical required cross sections for direct detection of Planck scale DM can be achieved through the $U(1)_d$ interactions of DM with SM quarks. Low energy intense sources may uncover the GeV scale messengers of Planckian physics, allowing for testable predictions. We assume that $U(1)_d$ is gauged baryon number, which implies several new electroweak charged particles are expected to arise near the weak scale to cancel gauge anomalies. The model generically gives rise to kinetic mixing between the $U(1)_d$ gauge boson and the photon, which may be measurable. In this scenario, direct detection of DM and measurements of a low energy messenger, including its kinetic mixing with the photon, can potentially shed light on the high energy character of the scenario. Astrophysical considerations related to white dwarf stability against runaway nuclear fusion potentially disfavor DM heavier than $\sim 10^{17}$ GeV within our assumed messenger model.
Highlights
While the presence of dark matter (DM) as a major component—about 25%—of the cosmic energy budget has robust observational support, its basic properties remain largely unknown
Given that we have adopted a specific model here, we should ensure that choices of parameters that could lead to potential direct detection of Planck scale DM (PSDM) are consistent with astrophysical observations
In this work we considered the possibility that the mass of dark matter may be close to the Planck scale MP and lie in the range ∼1015–19 GeV
Summary
While the presence of dark matter (DM) as a major component—about 25%—of the cosmic energy budget has robust observational support, its basic properties remain largely unknown. As DM mass gets larger and its inferred number density drops, the constraints get less strong Even though it is not clear where new physics emerges above the weak scale, the implied scale of quantum gravity, given by the Planck mass MP ≈ 1.2 × 1019 GeV, offers an obvious target. Assuming the usual local Galactic energy density for DM, ρ ≈ 0.3 GeV=cm, it follows that the PSDM number density is very low within the Solar System This implies that the bounds on the interactions of PSDM with ordinary matter are not strong and this type of DM could potentially have a significant cross section for scattering off the target material. In the remainder of this work, we will introduce our model and its properties, discuss the current constraints on the model parameter space as well as provide possible implications for future experiments
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