https://doi.org/10.1140/epjc/s10052-012-2005-2
Regular Article - Theoretical Physics
Revisiting the Higgs mass and dark matter in the CMSSM
1
Theoretical Particle Physics and Cosmology Group, Department of Physics, King’s College London, London, WC2R 2LS, UK
2
Theory Division, CERN, 1211, Geneva 23, Switzerland
3
William I. Fine Theoretical Physics Institute, School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
* e-mail: olive@physics.umn.edu
Received:
24
February
2012
Revised:
16
April
2012
Published online:
22
May
2012
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
–χ and 
–χ coannihilation strips, whereas the –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.
© Springer-Verlag / Società Italiana di Fisica, 2012
