Supersymmetry, nonthermal dark matter, and precision cosmology

Easther, Richard; Galvez, Richard; Özsoy, Ogan; Watson, Scott

doi:10.1103/physrevd.89.023522

Cited by 62 publications

(87 citation statements)

References 63 publications

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“…In addition, a long phase of soliton domination leads to a matter dominated expansion history before reheating takes place. This change in the expansion history affects the mapping of modes between horizon exit during inflation and re-entry at late times, thus affecting our interpretation of inflationary observables [71][72][73]. The long matter dominated phase also leads to additional gravitational structure formation in the early Universe before the inflaton decays away.…”

Section: A Additional Observational Consequencesmentioning

confidence: 99%

End of inflation, oscillons, and matter-antimatter asymmetry

Lozanov

Amin

2014

Phys. Rev. D

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The dynamics at the end of inflation can generate an asymmetry between particles and antiparticles of the inflaton field. This asymmetry can be transferred to baryons via decays, generating a baryon asymmetry in our Universe. We explore this idea in detail for a complex inflaton governed by an observationally consistent -"flatter than quadratic"-potential with a weakly broken global U (1) symmetry. We find that most of the inflaton asymmetry is locked in non-topological soliton like configurations (oscillons) produced copiously at the end of inflation. These solitons eventually decay into baryons and generate the observed matter-antimatter asymmetry for a range of model parameters. Through a combination of three dimensional lattice simulations and a detailed linearized analysis, we show how the inflaton asymmetry depends on the fragmentation, the magnitude of the symmetry breaking term and initial conditions at the end of inflation. We discuss the final decay into baryons, but leave a detailed analysis of the inhomogeneous annihilation, reheating and thermalization to future work.As part of our work, we pay particular attention to generating multifield initial conditions for the field fluctuations (including metric perturbations) at the end of inflation for lattice simulations. CONTENTS

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Section: A Additional Observational Consequencesmentioning

confidence: 99%

End of inflation, oscillons, and matter-antimatter asymmetry

Lozanov

Amin

2014

Phys. Rev. D

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“…Increasingly stringent direct detection bounds, most recently from XENON-100 [1] and LUX [2] are rapidly cutting into the parameter space of supersymmetry, particularly that of welltempered neutralinos [3], requiring fine-tuning to evade such constraints [4,5]. A pure Higgsino or Wino LSP with annihilation mainly to gauge boson final states can evade such constraints; however, these candidates are constrained by indirect detection [6][7][8][9]. Coannihilation (with slepton, sfermion, chargino, or heavier neutralino) can also result in the correct relic density, but involve a light state close to the LSP mass with stronger interactions that can be probed experimentally.…”

Section: Introductionmentioning

confidence: 99%

Dark matter at the pseudoscalar Higgs resonance in the phenomenological MSSM and SUSY GUTs

2015

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We study dark matter at the MSSM pseudoscalar Higgs resonance (A-funnel), which is one of the few remaining MSSM thermal dark matter candidates in the 100 − 1000 GeV range safe from direct detection constraints. To illustrate the various factors at play, this study is performed in two contrasting set-ups: a bottom-up phenomenological MSSM (pMSSM) approach that allows significant freedom, and the top-down, highly constrained Yukawa unified SO(10) GUT model. In the pMSSM, for µ > 0, the entire parameter space lies above the coherent neutrino background and mostly within reach of XENON1T and LZ, while blind spots exist at m A > 800 GeV for µ < 0; the strongest constraints come from A/H → τ τ searches at the LHC. For Yukawa unified models, the confluence of B s → µ + µ − constraints, fits to the bottom quark and Higgs masses, and gluino mass bounds from the LHC result in a prediction: realizing the pseudoscalar resonance requires gaugino mass non-universality, with a mass ratio that is determined to within a small range. * anandakrishnan.1@osu.edu †

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“…responsible for AMS-02 [65][66][67]. Alternatively, the positron ray flux might receive a boost from dark matter substructure, such as over dense clumps, clouds, or disks which would allow for a reduced annihilation rate [68][69][70][71][72][73][74][75][76][77].…”

Section: Jhep05(2016)033mentioning

confidence: 99%

AMS-02 fits dark matter

Balázs

2016

J. High Energ. Phys.

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In this work we perform a comprehensive statistical analysis of the AMS-02 electron, positron fluxes and the antiproton-to-proton ratio in the context of a simplified dark matter model. We include known, standard astrophysical sources and a dark matter component in the cosmic ray injection spectra. To predict the AMS-02 observables we use propagation parameters extracted from observed fluxes of heavier nuclei and the low energy part of the AMS-02 data. We assume that the dark matter particle is a Majorana fermion coupling to third generation fermions via a spin-0 mediator, and annihilating to multiple channels at once. The simultaneous presence of various annihilation channels provides the dark matter model with additional flexibility, and this enables us to simultaneously fit all cosmic ray spectra using a simple particle physics model and coherent astrophysical assumptions. Our results indicate that AMS-02 observations are not only consistent with the dark matter hypothesis within the uncertainties, but adding a dark matter contribution improves the fit to the data. Assuming, however, that dark matter is solely responsible for this improvement of the fit, it is difficult to evade the latest CMB limits in this model.

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Supersymmetry, nonthermal dark matter, and precision cosmology

Cited by 62 publications

References 63 publications

End of inflation, oscillons, and matter-antimatter asymmetry

End of inflation, oscillons, and matter-antimatter asymmetry

Dark matter at the pseudoscalar Higgs resonance in the phenomenological MSSM and SUSY GUTs

AMS-02 fits dark matter

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