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The Higgs mass beyond the CMSSM

  • Regular Article - Theoretical Physics
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Abstract

The apparent discovery of a Higgs boson with mass ∼125 GeV has had a significant impact on the constrained minimal supersymmetric extension of the Standard Model (the CMSSM). Much of the low-mass parameter space in the CMSSM has been excluded by supersymmetric particle searches at the LHC as well as by the Higgs mass measurement and the emergent signal for B s →μ + μ −. Here, we consider the impact of these recent LHC results on several variants of the CMSSM with a primary focus on obtaining a Higgs mass of ∼125 GeV. In particular, we consider the one- and two-parameter extensions of the CMSSM with one or both of the Higgs masses set independently of the common sfermion mass, m 0 (the NUHM1,2). We also consider the one-parameter extension of the CMSSM in which the input universality scale M in is below the GUT scale (the sub-GUT CMSSM). Finally, we reconsider mSUGRA models with sub-GUT universality, which have the same number of parameters as the CMSSM. We find that when M in<M GUT large regions of parameter space open up where the relic density of neutralinos can successfully account for dark matter with a Higgs boson mass ∼125 GeV. Interestingly, we find that the preferred range of the A-term in sub-GUT mSUGRA models straddles that predicted by the simplest Polonyi model.

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Notes

  1. Historically, this sign of μ has been favoured by the supersymmetric interpretation of g μ −2 (we display g μ −2-compatible regions in Fig. 2 but not in subsequent figures) and to facilitate compatibility with b→sγ. However, since the LHC constraints now disfavour regions of the CMSSM parameter space that ‘explain’ the g μ −2 discrepancy (as seen in Fig. 2), this assumption should be taken with a grain of salt.

  2. Because of the combination of recent experimental constraints, we are forced to consider substantially larger ranges in the displayed supersymmetric parameters such as m 0 and m 1/2. Therefore, here and in many other figures, for reasons of visibility we shade wider strips where 0.06<Ω χ h 2<0.2.

  3. As discussed in [38], this limit is generally stronger than other direct searches for supersymmetry at the LHC in the models studied, and is largely independent of tanβ and A 0. Based on the analysis in [130], in the upper left panel of Fig. 2 we have assumed that the constraint published in [128] is independent of m 1/2 when extrapolated to lower m 0.

  4. We recall that the focus-point strip is excluded by the XENON100 upper limit on spin-independent dark matter scattering.

  5. The width of the structure is enhanced for visibility by colouring the area where 0.06<Ω χ h 2<0.2.

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Acknowledgements

The work of J.E. and F.L. was supported in part by the London Centre for Terauniverse Studies (LCTS), using funding from the European Research Council via the Advanced Investigator Grant 267352: this also supported visits by K.A.O. to the CERN TH Division, which he thanks for its hospitality. The work of F.L. and K.A.O. was supported in part by DOE grant DE-FG02-94ER-40823 at the University of Minnesota, and the work of F.L. was also supported in part by a Doctoral Dissertation Fellowship at the University of Minnesota. P.S. gratefully acknowledges support and resources from the Center for High Performance Computing at the University of Utah.

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Authors and Affiliations

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

    John Ellis & Feng Luo

  2. TH Division, Physics Department, 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

  4. Department of Physics, University of Utah, Salt Lake City, UT, 84112, USA

    Pearl Sandick

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  1. John Ellis
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  2. Feng Luo
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  3. Keith A. Olive
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  4. Pearl Sandick
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Correspondence to Pearl Sandick.

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Ellis, J., Luo, F., Olive, K.A. et al. The Higgs mass beyond the CMSSM. Eur. Phys. J. C 73, 2403 (2013). https://doi.org/10.1140/epjc/s10052-013-2403-0

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  • DOI: https://doi.org/10.1140/epjc/s10052-013-2403-0

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