Dark Matter Theory Current status of WIMP DM Natsumi Nagata Univ. - PowerPoint PPT Presentation

Dark Matter Theory Current status of WIMP DM Natsumi Nagata Univ. of Tokyo Mar. 8th, 2019 Tohoku University Revealing the history of the universe with underground particle and nuclear research 2019

Target of the talk Tons of DM candidates have been proposed so far… e.g.) WIMPs Axion Talks by Andreas & Kawasaki-san Asymmetric DM Talk by Ibe-san SIMPs, FIMPs etc…

Target of the talk Tons of DM candidates have been proposed so far… e.g.) WIMPs Axion Asymmetric DM SIMPs, FIMPs etc… Let me focus on WIMP DM in this talk.

WIMP Weakly-Interacting Massive Particles (WIMPs) Electrically neutral and colorless particles. Stable. Masses of order Electroweak (EW) scale. Have interactions comparable to EW interactions. Observed Dark Matter (DM) density can be explained by their thermal relic.

<latexit sha1_base64="L92To7hEvMru86UljBW9Fy14jts=">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</latexit> TeV-scale physics and WIMP DM thermal relic abundance e.g.) WIMP DM predicted new physics at the TeV scale. WIMPs often appear in models motivated by naturalness. Expected to be tested in various experiments (such as LHC).

Goal of the talk DM candidates in TeV-scale new physics models have been severely constrained. Target has been narrowed down. On the other hand, the WIMP paradigm itself has not been fully tested yet. Further exploration is needed.

Outline Viable WIMP DM candidates in SUSY Current status of WIMP DM Summary

DM in SUSY models

Supersymmetry (SUSY) The LHC results, i.e. , • Bound on SUSY particles • 125 GeV Higgs mass SUSY particles are heavier than expected. Restrict WIMP DM candidates in (simple) SUSY models. Two simple setups • Constrained MSSM • High-scale SUSY

Constrained MSSM (CMSSM) Constrained MSSM (CMSSM) • Traditional benchmark model • Impose universality conditions at the GUT scale. Input parameters m 0 , m 1/2 , A 0 , tan β , sign( μ ) Soft parameters at low energies are obtained by using renormalization group equations.

DM in CMSSM tan β = 5, A 0 = 0, µ > 0 tan β = 6, A 0 = -4.2 m 0 , µ < 0 20 30 125 131 127 128 128 130 130 128 129 130 131 125 129 127 131 130 130 1 2 128 126 127 129 7 126 126 3 0 122 124 125 131 1 129 129 130 130 0.1 128 131 128 131 130 131 129 127 127 127 129 128 127 126 100 130 129 129 130 126 127 130 128 128 124 123 130 125 123 124 126 128 130 131 130 129 129 128 129 122 125 122 128 124 125 2 8 131 130 126 1 2 8 129 131 1 127 130 128 1 125 127 124 127 1 3 1 131 130 131 125 126 2 4 127 129 0 127 122 130 128 129 1 131 123 127 126 127 131 130 127 128 129 122 123 127 1 2 9 125 124 7 126 127 1 2 129 5 127 124 128 128 126 125 129 129 127 126 128 129 130 131 122 126 129 130 126 130 124 125 50 127 122 131 124 131 123 125 126 6 126 126 129 124 130 126 125 131 131 128 1 123 124 131 1 2 50 125 122 129 130 127 126 131 128 130 127 123 129 3 1 126 129 130 126 125 122 123 130 124 122 128 125 128 1 126 128 131 124 125 123 123 123 128 131 128 125 127 127 1 2 6 131 128 130 130 131 131 5 127 125 131 No EWSB 0.5 130 128 1 131 125 2 3 128 1 129 125 123 1 Stop LSP 127 1 125 124 3 130 126 126 125 126 126 9 0 129 m 0 (TeV) m 0 (TeV) 2 125 0.066 1 122 2 3 131 125 1 124 129 131 127 131 4 2 129 130 126 130 126 123 131 1 130 130 131 130 129 0.5 131 131 130 129 128 128 127 131 131 129 124 126 128 130 129 129 123 8 1 3 0 130 10 127 2 0.1 130 127 128 0.05 0.01 125 1 1 1 3 127 0.5 129 129 125 5 128 0 0.066 131 3 122 0.1 131 1 1 0.01 0.05 130 131 4 130 129 2 125 126 125 129 126 125 1 0.5 129 1 127 124 20 127 126 1.0 127 126 128 7 2 8 1 125 2 125 123 1 125 125 0.066 124 6 128 6 0 0.01 0.05 10 125 . 0 0.1 130 0.066 124 0.1 128 5 0.5 0.05 123 124 10 124 129 124 126 128 0.5 126 126 125 0.5 124 1 9 126 2 X 1 127 129 125 123 4 0.066 2 125 1 0.01 5 0.1 0 123 . 0 122 124 1 0.1 . 127 122 124 0 127 126 0.01 122 10 0.066 125 0.05 0.066 123 128 122 123 123 125 0.05 122 123 0.01 124 0.01 0.05 124 122 Stau LSP Stau LSP 124 0.05 122 0 0 1.0 1.0 3.0 3 5.0 5 7.0 7.0 9.0 9.0 5 10 15 m 1/2 (TeV) m 1/2 (TeV) Ω DM h 2 = 0.12 Proton lifetime [10 35 yrs] Higgs mass [GeV] Bino DM Higgsino-like DM (~1 TeV) (stop/stau coannihilation) J. Ellis, J. L. Evans, A. Mustafayev, N. Nagata, K. A. Olive, Eur. Phys. J. C76 , 592 (2016).

L. J. Hall, Y. Nomura, S. Shirai (2012) High-scale SUSY M. Ibe, S. Matsumoto, T. T. Yanagida (2012) A. Arvanitaki, N. Craig, S. Dimopoulos, G. Villadoro (2012) N. Arkani-Hamed, A. Gupta, D. E. Kaplan, N. Weiner, and T. Zorawski (2012) Suppose that the SUSY-breaking field is not a singlet: Scalar Par � cles Higgsinos Gravi � no (2-5) O(10 ) TeV Higgsinos can be light if Gauginos there is an additional symmetry. Gluino O(1) TeV Bino Wino Gaugino masses are induced at loop level. e.g.) Anomaly mediation L. Randall and R. Sundrum (1998) G. F . Giudice, M. A. Luty, H. Murayama, and R. Rattazzi (1998)

L. J. Hall, Y. Nomura, S. Shirai (2012) High-scale SUSY M. Ibe, S. Matsumoto, T. T. Yanagida (2012) A. Arvanitaki, N. Craig, S. Dimopoulos, G. Villadoro (2012) N. Arkani-Hamed, A. Gupta, D. E. Kaplan, N. Weiner, and T. Zorawski (2012) Suppose that the SUSY-breaking field is not a singlet: Scalar Par � cles Higgsinos Gravi � no (2-5) O(10 ) TeV Gauginos Gluino m h > 127GeV O(1) TeV Bino 10 tan b Wino 135GeV m h = 125 GeV 130GeV 125GeV 120GeV High SUSY-breaking scale. m h < 115.5GeV 1 10 10 2 10 3 10 4 M. Ibe, S. Matsumoto, T. T. Yanagida (2012). M SUSY ê TeV

L. J. Hall, Y. Nomura, S. Shirai (2012) High-scale SUSY M. Ibe, S. Matsumoto, T. T. Yanagida (2012) A. Arvanitaki, N. Craig, S. Dimopoulos, G. Villadoro (2012) N. Arkani-Hamed, A. Gupta, D. E. Kaplan, N. Weiner, and T. Zorawski (2012) Suppose that the SUSY-breaking field is not a singlet: Scalar Par � cles Higgsinos Gravi � no (2-5) O(10 ) TeV Higgsinos can be light if Gauginos there is an additional symmetry. Gluino O(1) TeV Bino Wino Dark matter candidates in this setup.

DM candidates in High-scale SUSY WIMP DM candidates [3 TeV; anomaly mediation] Wino Higgsino [1 TeV] Bino [with coannihilation; bino-wino/bino-gluino] Which of them can actually be realized? Depends on UV physics.

<latexit sha1_base64="oDwIGboYJXZYPfv+4XdlkZT1/ME=">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</latexit> An example Parameter space in SU(5) SuperGUT PGM. M in = 10 18 GeV, tan β = 3.5, λ = 1, λ ‘ = 1, μ < 0 Gaugino mass contribution m 3/2 (TeV) Anomaly mediation + GUT threshold corrections. with κ Σ Bino-gluino coannihilation Bino-wino coannihilation Wino DM J. L. Evans, N. Nagata, K. A. Olive, 1902.09084.

Summary of DM in SUSY models CMSSM etc. Higgsino-like DM [~1 TeV] Bino-stop/stau coannihilation High-scale SUSY Wino [3 TeV] Higgsino [1 TeV] Bino-gluino/wino coannihilation How can we probe these scenarios??