Abstract
The pseudoscalar resonance or "A-funnel" in the Minimal Supersymmetric Standard Model~(MSSM) is a widely studied framework for explaining dark matter that can yield interesting indirect detection and collider signals. The well-known Galactic Center excess (GCE) at GeV energies in the gamma ray spectrum, consistent with annihilation of a $\lesssim 40$ GeV dark matter particle, has more recently been shown to be compatible with significantly heavier masses following reanalysis of the background. In this paper, we explore the LHC and direct detection implications of interpreting the GCE in this extended mass window within the MSSM A-funnel framework. We find that compatibility with relic density, signal strength, collider constraints, and Higgs data can be simultaneously achieved with appropriate parameter choices. The compatible regions give very sharp predictions of 200-600 GeV CP-odd/even Higgs bosons at low tan$\beta$ at the LHC and spin-independent cross sections $\approx 10^{-11}$ pb at direct detection experiments. Regardless of consistency with the GCE, this study serves as a useful template of the strong correlations between indirect, direct, and LHC signatures of the MSSM A-funnel region.
Highlights
It has been shown that this excess might be attributable to unresolved point sources [19,20,21], a conclusive verdict has not been reached
This relaxation of the allowed range of dark matter masses compatible with the GC excess (GCE) has interesting implications for Minimal Supersymmetric Standard Model (MSSM) dark matter, as it opens up the possibility of explaining the signal with the well-known pseudoscalar resonance or “A-funnel” mechanism, where the dark matter relic density is set by resonant s-channel annihilation through the pseudoscalar A, with mA ≈ 2mχ ( χ represents the lightest neutralino, which is the dark matter candidate)
Previous fits to the Galactic Center excess (GCE) with mχ
Summary
The lightest neutralino in the MSSM is a combination of the Bino, Wino, and neutral. Χ = N11B + N12W + N13Hd + N14Hu. As mentioned above, we are mainly interested in the region of parameters where the lightest neutralino is predominantly a Bino, N11 ∼ 1, N12 = 0, and N13, N14 1. We are mainly interested in the region of parameters where the lightest neutralino is predominantly a Bino, N11 ∼ 1, N12 = 0, and N13, N14 1 In this regime, the Bino mass parameter M1 and the neutralino components are approximately [25]. Sθ, cθ denote sin θ, cos θ respectively and mχ is the dark matter mass
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