3.55 keV X-ray line signal from excited dark matter in radiative neutrino model

Hiroshi Okada,Takashi Toma

doi:10.1016/j.physletb.2014.08.046

Hiroshi Okada, Takashi Toma

Open Access

https://doi.org/10.1016/j.physletb.2014.08.046

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Abstract

We study an exciting dark matter scenario in a radiative neutrino model to explain the X-ray line signal at 3.55 keV recently reported by XMN-Newton X-ray observatory using data of various galaxy clusters and Andromeda galaxy. We show that the required large cross section for the up-scattering process to explain the X-ray line can be obtained via the resonance of the pseudo-scalar. Moreover, this model can be compatible with the thermal production of dark matter and the constraint from the direct detection experiment.

Highlights

In the light of anomalous X-ray line signal at 3.55 keV from the analysis of XMN-Newton X-ray observatory data of various galaxy clusters and Andromeda galaxy [1, 2], dark matter (DM) whose mass is in the range from keV to GeV comes into one of the promising candidates
We account for the X-ray anomaly in terms of an excited DM scenario in a simple extended model with radiative neutrino masses [27], in which three right-handed neutrinos, a SU(2)L doublet scalar and a singlet scalar are added to the Standard Model (SM) and the first two lightest right-handed neutrinos are assumed to be a pair of ground state and excited state DM
We identify that N1 and N2 are a pair of ground and excited state DM for explaining the X-ray anomaly

Summary

INTRODUCTION

In the light of anomalous X-ray line signal at 3.55 keV from the analysis of XMN-Newton X-ray observatory data of various galaxy clusters and Andromeda galaxy [1, 2], dark matter (DM) whose mass is in the range from keV to GeV comes into one of the promising candidates. As for the GeV scale DM, on the other hand, the exciting DM scenario which requests a pair of ground state and excited DM is known to explain the X-ray [7]. We account for the X-ray anomaly in terms of an excited DM scenario in a simple extended model with radiative neutrino masses [27], in which three right-handed neutrinos, a SU(2)L doublet scalar and a singlet scalar are added to the Standard Model (SM) and the first two lightest right-handed neutrinos are assumed to be a pair of ground state and excited state DM. The pseudo scalar ρ does not mix after the symmetry breaking and the mass is just given √. The mass difference between the charged and neutral inert scalars is constrained as roughly less than O(100) GeV by the T parameter [30]

Neutrino sector

DARK MATTER

SUMMARY AND CONCLUSION