Abstract
A network of synchronized detectors can increase the likelihood of discovering the QCD axion within the axion quark nugget (AQN) dark matter model. A similar network can also discriminate the x rays emitted by the AQNs from the background signal. These networks can provide information on the directionality of the dark matter flux (if any), as well as its velocity distribution, and can therefore test the Standard Halo Model. We show that the optimal configuration to detect AQN-induced axions is a triangular network of stations 100 km apart. For x rays, the optimal network is an array of tetrahedral units.
Highlights
The Standard Halo Model (SHM) is locally characterized by an average dark matter (DM) density ρDM ≈ 0.3 GeV cm−3 and a velocity distribution insensitive to the environment, for example, to the dynamics of the planets and the Sun
We propose a framework that can test some fundamental assumptions of the SHM, such as the magnitude of the DM density and the DM velocity distribution in the local environment
In a recent proposal [10,11], it was suggested to use a broadband detection strategy to search for axions within the context of the axion quark nugget (AQN) dark matter model
Summary
The Standard Halo Model (SHM) is locally characterized by an average dark matter (DM) density ρDM ≈ 0.3 GeV cm−3 and a velocity distribution insensitive to the environment, for example, to the dynamics of the planets and the Sun (see [1]). The main problem with broadband detection is the difficulty to distinguish between the AQN signal and large random noise and spurious events, but the dominant random background noise can be eliminated with the following observational strategy: (i) separate the DM signal from the larger noise by explicitly looking for annual and daily modulations, which are specific to the former and (ii) use synchronized detectors to discriminate between the DM signal and the larger noise, by looking at the time delays recorded by two or more nearby detectors, as these delays are unambiguously fixed by the distances between the detectors Developing such a detection strategy is relevant to the search of any DM particles that leave a detectable trace, being neutrinos [12], infrasonic or seismic events [13,14], or x rays.
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