Complex Scalar DM in a B-L Model

TL;DR

This paper introduces a complex scalar dark matter candidate within a $U(1)_{B-L}$ extended Standard Model, analyzing its relic abundance, detection prospects, and compatibility with experimental constraints, including neutrino masses and astrophysical bounds.

Contribution

It presents a novel implementation of a complex scalar dark matter candidate in a $U(1)_{B-L}$ model with detailed analysis of its phenomenology and experimental viability.

Findings

A 200 GeV dark matter candidate is compatible with current constraints.

The model naturally explains light neutrino masses and mixing.

Light CP-odd scalars are consistent with decay and astrophysical constraints.

Abstract

In this work, we implement a complex scalar Dark Matter (DM) candidate in a $U(1)_{B-L}$ gauge extension of the Standard Model. The model contains three right handed neutrinos with different quantum numbers and a rich scalar sector, with extra doublets and singlets. In principle, these extra scalars can have VEVs ($V_{\Phi}$ and $V_{\phi}$ for the extra doublets and singlets, respectively) belonging to different energy scales. In the context of $\zeta\equiv\frac{V_{\Phi}}{V_{\phi}}\ll1$, which allows to obtain naturally light active neutrino masses and mixing compatible with neutrino experiments, the DM candidate arises by imposing a $Z_{2}$ symmetry on a given complex singlet, $\phi_{2}$, in order to make it stable. After doing a study of the scalar potential and the gauge sector, we obtain all the DM dominant processes concerning the relic abundance and direct detection. Then, for a representative set of parameters, we found that a complex DM with mass around $200$ GeV, for example, is compatible with the current experimental constraints without resorting to resonances. However, additional compatible solutions with heavier masses can be found in vicinities of resonances. Finally, we address the issue of having a light CP-odd scalar in the model showing that it is safe concerning the Higgs and the $Z_{\mu}$ boson invisible decay widths, and also the energy loss in stars astrophysical constraints.