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Revisiting the Higgs mass and dark matter in the CMSSM

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Abstract

Taking into account the available accelerator and astrophysical constraints, the mass of the lightest neutral Higgs boson h in the minimal supersymmetric extension of the Standard Model with universal soft supersymmetry-breaking masses (CMSSM) has been estimated to lie between 114 and ∼130 GeV. Recent data from ATLAS and CMS hint that m h ∼125 GeV, though m h ∼119 GeV may still be a possibility. Here we study the consequences for the parameters of the CMSSM and direct dark matter detection if the Higgs hint is confirmed, focusing on the strips in the (m 1/2,m 0) planes for different tanβ and A 0 where the relic density of the lightest neutralino χ falls within the range of the cosmological cold dark matter density allowed by WMAP and other experiments. We find that if m h ∼125 GeV focus-point strips would be disfavoured, as would the low-tanβ \({\tilde{\tau}}\)–χ and \({\tilde{t}}_{1} \)–χ coannihilation strips, whereas the \({\tilde{\tau}}\)–χ coannihilation strip at large tanβ and A 0>0 would be favoured, together with its extension to a funnel where rapid annihilation via direct-channel H/A poles dominates. On the other hand, if m h ∼119 GeV more options would be open. We give parameterisations of WMAP strips with large tanβ and fixed A 0/m 0>0 that include portions compatible with m h =125 GeV, and present predictions for spin-independent elastic dark matter scattering along these strips. These are generally low for models compatible with m h =125 GeV, whereas the XENON100 experiment already excludes some portions of strips where m h is smaller.

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Notes

  1. As already mentioned, we focus here on μ>0. This assumption was motivated in the past by indications from g μ −2 and the desire to avoid strong constraints from b→sγ [92–97], but should perhaps be reviewed now in light of the growing tension between LHC missing-energy constraints [90, 91] and g μ −2 [98, 99].

  2. The true WMAP strips corresponding to Ω χ h 2=0.112±0.012 [50] at the 2σ level are often invisibly narrow. Accordingly, in these and most subsequent figure panels, the WMAP strips have been made more visible by colouring regions where 0.05<Ω χ h 2<0.15.

  3. Also visible in these panels between m 1/2∼1000 GeV and ∼1500 GeV is another WMAP-compatible strip running roughly parallel to the \({\tilde{\tau}}_{1} \)–χ coannihilation strip, which is due to rapid \({\tilde{\tau}}_{1} \)–\({\bar{\tilde{\tau}}_{1}}\) annihilation through direct-channel H/A poles.

  4. These funnels have been coloured only in the range Ω χ h 2=0.112±0.012 allowed by WMAP at the 2σ level.

  5. The available results from LHC missing-energy searches [90, 91] are insufficient to indicate which portions of this line might be excluded.

  6. See [65] for a discussion of the uncertainty in this parameter.

  7. This connection is only qualitative, since the processes dominating t-channel exchange are not identical with the processes dominating s-channel annihilation, and the cosmological annihilations involve a mixture of P- and S-wave annihilations.

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Acknowledgements

This work has been supported in part by the London Centre for Terauniverse Studies (LCTS), using funding from the European Research Council via the Advanced Investigator Grant 267352. The work of K.A.O. is also supported in part by DOE grant DE-FG02-94ER-40823 at the University of Minnesota.

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  1. Theoretical Particle Physics and Cosmology Group, Department of Physics, King’s College London, London, WC2R 2LS, UK

    John Ellis

  2. Theory Division, CERN, 1211, Geneva 23, Switzerland

    John Ellis

  3. William I. Fine Theoretical Physics Institute, School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA

    Keith A. Olive

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Ellis, J., Olive, K.A. Revisiting the Higgs mass and dark matter in the CMSSM. Eur. Phys. J. C 72, 2005 (2012). https://doi.org/10.1140/epjc/s10052-012-2005-2

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