Abstract
We study the gravitational waves (GWs) spectrum produced during the electroweak phase transition in a scale-invariant extension of the Standard Model (SM), enlarged by a dark U(1)_{D} gauge symmetry. This symmetry incorporates a vector dark matter (DM) candidate and a scalar field (scalon). Because of scale invariance, the model has only two independent parameters and for the parameter space constrained by DM relic density, strongly first-order electroweak phase transition can take place. In this model, for a narrow part of the parameter space, DM-nucleon cross section is below the neutrino-floor limit, and therefore, it cannot be probed by the future direct detection experiments. However, for a benchmark point from this narrow region, we show the amplitude and frequency of phase transition GW spectrum fall within the observational window of space-based GW detectors such as eLISA.
Highlights
The detection of gravitational waves (GWs) [1] has opened up a new and independent avenue for probing of dark matter [2]
We use a benchmark point of the parameter space with below the neutrino-floor dark matter (DM)-nucleon cross section and show that the amplitude and frequency of phase transition GW spectrum fall within the observational window of eLISA
GW signal produced during first order electroweak phase transition as well as its discovery prospects are presented in Sect. 4, after which Sect. 5 comprises a summary and our conclusion
Summary
The detection of GWs [1] has opened up a new and independent avenue for probing of dark matter [2] These waves are ripples in the fabric of space-time generated by energetic and violent sources such as black hole and neutron star binaries, extreme mass ratio inspirals, and first order cosmological phase transitions. We use a benchmark point of the parameter space with below the neutrino-floor DM-nucleon cross section and show that the amplitude and frequency of phase transition GW spectrum fall within the observational window of eLISA Since, this particular choice of the parameter space is not constrained by colliders, and direct or indirect detection, GW signal plays an important role in probing the model for the chosen benchmark point. GW signal produced during first order electroweak phase transition as well as its discovery prospects are presented in Sect. 4, after which Sect. 5 comprises a summary and our conclusion
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