Nonthermal Two Component Dark Matter Model for Fermi-LAT $γ$-ray excess and 3.55 keV X-ray Line

Abstract

A two component model of nonthermal dark matter is formulated to simultaneously explain the Fermi-LAT results indicating a $γ$-ray excess observed from our Galactic Centre in the 1-3 GeV energy range and the detection of an X-ray line at 3.55 keV from extragalactic sources. Two additional Standard Model singlet scalar fields $S_2$ and $S_3$ are introduced. These fields couple among themselves and with the Standard Model Higgs doublet $H$. The interaction terms among the scalar fields, namely $H$, $S_2$ and $S_3$, are constrained by the application of a discrete $\mathbb{Z}_2\times \mathbb{Z}^\prime_2$ symmetry which breaks softly to a remnant $\mathbb{Z}^{\prime \prime}_2$ symmetry. This residual discrete symmetry is then spontaneously broken through an MeV order vacuum expectation value $u$ of the singlet scalar field $S_3$. The resultant physical scalar spectrum has the Standard Model like Higgs as $χ_{{}_{{}_1}}$ with $M_{χ_{{}_{{}_1}}}\sim 125$ GeV, a moderately heavy scalar $χ_{{}_{{}_2}}$ with $50 \,\,{\rm GeV} \leq M_{χ_{{}_{{}_2}}}\leq 80\,\,{\rm GeV}$ and a light $χ_{{}_{{}_3}}$ with $M_{χ_{{}_{{}_3}}} \sim 7$ keV. There is only tiny mixing between $χ_{{}_{{}_1}}$ and $χ_{{}_{{}_2}}$ as well as between $χ_{{}_{{}_1}}$ and $χ_{{}_{{}_3}}$. The lack of importance of domain wall formation in the present scenario from the spontaneous breaking of the discrete symmetry ${\mathbb{Z}_2^{\prime\prime}}$, provided $u\leq 10$ MeV, is pointed out. We find that our proposed two component dark matter model is able to explain successfully both the above mentioned phenomena $-$ the Fermi-LAT observed $γ$-ray excess (from the $χ_{{}_{{}_2}} \rightarrow {\rm b} \bar{\rm b}$ decay mode) and the observation of the X-ray line (from the decay channel $χ_{{}_{{}_3}}\rightarrowγγ$) by the XMM-Newton observatory.

11 eps Figures, 2 Tables, 32 Pages. Minor addition in Abstract. Inclusion in Section 1 of discussion of earlier attempts to explain the concerned phenomena by astrophysical processes. Extension of discussion in Section 6 to the case of a steeper dark matter density profile. Results unchanged. Version accepted for publication in JHEP