Abstract
In this work, we investigate the beyond standard model (BSM) impact of leptophilic U(1) models, namely $ U(1)_{L_\mu-L_e}$, $U(1)_{L_e-L_\tau}$ and $U(1)_{L_\mu-L_\tau}$ on coherent elastic neutrino-nucleus scattering (CE$\nu$NS) and hence its effect on dark matter (DM) direct detection experiments. Imposing the latest relevant experimental constraints on these models, we obtain $\mathcal{O}(50\%)$ enhancement for case of $U(1)_{L_\mu-L_\tau}$ in a region $m_Z' \approx 20~$MeV. Subsequently, we observe that the enhancement seen in CE$\nu$NS is roughly getting translated to enhancement by a factor of 2.7 (for Germanium based detectors) and 1.8 (for Xenon based detectors) in the neutrino scattering event rate which eventually enhances the neutrino floor by same amount. This enhancement is more prominent in the region with DM masses less than 10 GeV. The model parameter space that leads to this enhancement, can simultaneously explain both anomalous magnetic moment of muon ($(g-2)_{\mu}$) and observed DM relic density, in a modified scenario. Enhancement of neutrino floor requires increased number of DM-nucleon scattering events in the future DM direct detection experiments, to establish themselves to be DM signal events. In absence of any DM signal, those experiments can directly be used to measure the neutrino rate, quantifying the BSM effects.
Highlights
AND MOTIVATIONThe majority of the matter present in our Universe is in the form of a nonluminous matter called dark matter (DM)
We have studied the new physics contribution from leptophilic Uð1Þe−μ, Uð1Þe−τ and Uð1Þμ−τ models to the CEνNS, eventually leading to an enhancement to the neutrino floor, which is soon going to become sensitive to the future DM direct detection experiments
Due to tighter constraints from ν − e− scattering cross section measured by TEXONO for the Uð1Þe−μ and Uð1Þe−τ models in the same mZ0 − gi−j parameter space, we could not manage any sizable (≥5%) enhancement
Summary
The majority of the matter present in our Universe is in the form of a nonluminous matter called dark matter (DM). These Uð1Þ models are well motivated by results from DM indirect detection experiments (e.g., DAMPE [7] and AMS02 [8] etc), along with the possible explanation of eþ=e− excess observed in cosmic rays through DM annihilation to leptons via Z0 In this parameter region of Uð1ÞLμ−Lτ , there is an extra contribution through Z0 − γ in the CEνNS process, paving way to its significant enhancement compared to the SM value, aided by the lightness of the Z0 boson. Experiments measure the cross sections of the processes where neutrinos scatter off the electron i.e., the να − e process These processes will be significantly modified where the light Z0 couples to the electron along with different neutrinos, while for the Uð1Þμ−τ, these interaction only happen through a Z − Z0 mixing, and constraints are less stringent. The effective weak interaction vertex in the neutrino part for the BSM case of Uð1Þi−j model can be written as, QνNi−j g2i−j
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