Feebly Interacting $U(1)_{\rm B-L}$ Gauge Boson Warm Dark Matter and XENON1T Anomaly

Abstract

The recent observation of an excess in the electronic recoil data by the XENON1T detector has drawn many attentions as a potential hint for an extension of the Standard Model (SM). Absorption of a vector boson with the mass of m A ∈ (2 keV,3 keV) is one of the feasible explanations to the excess. In the case where the vector boson explains the dark matter (DM) population today, it is highly probable that the vector boson belongs to a class of the warm dark matter (WDM) due to its suspected mass regime. In such a scenario, providing a good fit for the excess, the kinetic mixing κ ∼ 10 −15 asks for a non-thermal origin of the vector DM. In this letter, we consider a scenario where the gauge boson is nothing but the U (1)B−L gauge boson and its non-thermal origin is attributed to the decay of the scalar talking to the SM sector via a portal with the SM Higgs boson. We discuss implications for the dark sector interactions that the vector DM offers when it serves as a resolution to both the small scale problems that ΛCDM model encounters and the XENON1T anomaly.

Pico-charged particles explaining 511 keV line and XENON1T signal

“…Recently the XENON1T detector has reported an excess of scattered electrons with recoil energies 1 − 7 keV over the background. Although one possible solution is the β decay of the residue Tritium nuclei in the sample [1] (see also [8]), this observation has instilled a considerable activity in the field [9][10][11][12][13]. In this paper, we show that our model can simultanously explain the 511 keV line and the XENON1T excess.…”

“…Some of the ideas proposed in the literature to explain the excess include axions [1,9], non-standard interaction for the solar pp neutrinos [10] and the absorption of the background vector dark matter of a mass of a few keV [11]. The shape of the electron recoil spectrum cannot be explained by the vanilla WIMP dark matter scattering as the recoil energy off the electrons will be smaller than 1 eV and below the detection threshold.…”

Freeze-in sterile neutrino dark matter in a class of U$(1)^\prime$ models with inverse seesaw

“…The non-observation of any signal in the direct detection DM experiments puts stringent bounds on the DM nucleon scattering cross section [23][24][25] which severely restrict the models with Weakly Interacting Massive Particles (WIMPs) whose masses are 1GeV. There are some scenarios where non-WIMP candidates such as Feebly Interacting Massive Particles (FIMPs) [26], Strongly Interacting Massive Particles (SIMPs) [27], light gauge bosons [28][29][30], the axions or Axion Like Particles (ALPs) [31][32][33][34][35][36], light sterile neutrinos [37], Primordial Black Holes (PBHs) [38,39] etc., can be potential DM candidates and at the same time evading the direct detection bounds.…”

Feebly coupled vector boson dark matter in effective theory

“…Vector boson DM (VDM) candidate can only appear in models with extended gauge group, the simplest being an Abelian U (1). Many possibilities of an Abelian VDM have been studied [19][20][21][22][23][24][25][26][27][28][29][30][31][32][33][34][35][36][37], while non-Abelian extensions to adopt VDM are fewer [38][39][40][41][42][43][44][45][46]. The VDM can become massive after spontaneous symmetry breaking of the additional gauge group and often requires additional stabilizing symmetry G DM [20,38].…”