(Neutrino indirect) detection of neutralino dark matter in (non) universals SUSY GUT models

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1 (Neutrino indirect) detection of neutralino dark matter in (non) universals SUSY GUT models E. Nezri To cite this version: E. Nezri. (Neutrino indirect) detection of neutralino dark matter in (non) universals SUSY GUT models. COSMO-0 International Workshop on Particle Physics and the Early Universe, Sep 00, Chicago, United States. pp.1-15, 00. <inp > HAL Id: inp Submitted on 0 Feb 003 HAL is a multi-disciplinary open access archive for the deposit and dissemination of scientific research documents, whether they are published or not. The documents may come from teaching and research institutions in France or abroad, or from public or private research centers. L archive ouverte pluridisciplinaire HAL, est destinée au dépôt et à la diffusion de documents scientifiques de niveau recherche, publiés ou non, émanant des établissements d enseignement et de recherche français ou étrangers, des laboratoires publics ou privés.

2 (Neutrino Indirect) Detection of Neutralino Dark Matter in (non-)universals SUSY GUT Models. Emmanuel Nezri Laboratoire de Physique Corpusculaire de Clermont-Ferrand : Theory Centre de Physique des Particules de Marseille : Antares V.Bertin, E.N., J.Orloff, non-universal models, hep-ph/ V.Bertin, E.N., J.Orloff, hep-ph/ accepted in EPJ C (msugra) see also: and: J.L.Feng, K.T. Matchev, F. Wilczek, PRD63(01)04054 V. Barger, F. Halzen, D. Hooper, C. Kao, PRD65(0)0750 L. Bergström, J. Edsjö, P. Gondolo; PRD58(98) G. Jungman, M. Kamionkowski, K.Griest, Phys. Rep. 67 (96) 1

3 Contents Detecting cold dark matter (WIMPS) in neutrino telescopes msugra summary non-universality : Scalar sector Gaugino sector Conclusion

4 DM indirect detection with a neutrino telescope: ingredients A cold dark matter canditate: choose χ, lightest neutralino in Constrained MSSM A relic density: depends on (co-)annihilation processes σ A A cosmic storage ring: to re-start annihilation, need to concentrate n χ ; halo, clumps? too small for ν s! Need big, nearby, heavy body with large capture rate (C) depends on σ el χp. Sun: OK! Earth: small. χ = Majorana fermion: can self-annihilate, limiting the total population N χ : N χ = C C A N χ Annihilation rate: Γ A = 1 C AN χ = C tanh CC A t eq C can be insensitive to σ A among decay products χχ b b, t t, W W, ZZ,... ν +, only ν s can escape the sun and reach a detector. Φ(E ν ) depends on dominant annihilation channel Cerenkov detector watches for ν s converted into µ 3

5 DM indirect detection with a neutrino telescope: picture 4

6 Neutralino SM SUSY MSSM - group SU(3) SU() U(1) - Higgs doublets : tan β = v u vd, 5 scalars : h, A, H, H ± - R-parity conservation stable LSP - m p m p Soft breaking terms L soft In the basis ( i B, i W 3, H0 1, H0 ) : M χ = M 1 0 m Z cβsw m Z sβsw 0 M m Z cβcw m Z sβcw m Z cβsw m Z cβcw 0 µ m Z sβsw m Z sβcw µ 0 χ = z 11 b + z1 W 3 + z 13H0 1 + z 14 gaugino fraction : f G = z 11 + z 1 higgsino fraction : f H = z 13 + z 14 H0 5

7 Parameters at GUT scale GeV: a common gaugino mass m 1/ a common scalar mass m 0 a common trilinear coupling A 0 a common bilinear coupling B 0 Higgs parameter µ 0 + Renormalization group equations and radiative ElectroWeak Symmetry Breaking: 1 m Z = Input parameters : m H m d QEW tan β Hu SB QEW SB µ QEW SB tan β 1 achieved at Q EW SB m t 1 m t m 0, m 1/, A 0, tan β, sgn(µ) Advantages: REWSB, less free parameters, contact with acc. analyses, but also addressing CCB, Landau poles, high energy extrapoll. Thanks to Suspect authors kneur/suspect.html (study of the CMSSM with Suspect : hep-ph/ , A. Djouadi, M. Drees,J.L. Kneur) msugra/cmssm models Composition of the lightest neutralino : bino χ : for low m 0, RGE drive M 1 QEW SB = M QEW SB = 0.41m 1/ << µ QEW SB mixed bino-higgsino χ : EWSB m Hu Q EW SB µ QEW SB if tan β 5 for m 0 large (> ), increasing m 0 m less negative µ Hu decreases µ M 1 Focus point region hep-ph/ Feng, Matchev, Moroi 6

8 Experiment sensitivities in the (m 0, m 1/ ) plane A0=0 ; tan( β)=45 ; µ >0 m1/ (GeV) χ not LSP 0.3 Ω χ h =1 Exp. Excluded ICECUBE ANTARES km m1/ (GeV) χ not LSP 0.3 Ωh =1 Exp. Excluded ZEPLIN Max EDELWEISS II no EWSB no EWSB m0 (GeV) m0 (GeV) A 0 = 0 ; tan β = 45 ; µ > 0 Calculation with Suspect + Darksusy package : kneur/suspect.html edsjo/darksusy/ 7

9 msugra : Direct Detection Experiments vs Neutrino Telescopes scal σχ p : mχ µ flux : mχ msugra with 5 GeV threshold vs neutrino Indirect Dection -4 Bertin, Nezri, Orloff 0 Bertin, Nezri, Orloff 0 MACRO BAKSAN SUPER K 3-5 ANTARES 3 years - ICECUBE log10 σ χscal -p (pb) log10 µ flux from sun (km.yr -1) 4 msugra models vs Direct Detection 0.03 < Ω χ h < < Ωχ h < < Ω χ h < CDMS EDELWEISS 0.03 < Ωχ h < < Ω χ h < < Ω χ h < EDELWEISS II -8 ZEPLIN MAX mχ (GeV) mχ (GeV) 8

10 Non-universal scalar soft terms Sfermions : non-universality in sfermions matrices can lead to light third generation sfermions coannihilations χ τ, χ t can modify the relic density but happend in region out of reach of detectors. Detection imply real quarks mainly on u and d valence and due to their low Yukawa couplings RGE evolutions of the first and second generation squarks depend on gaugino soft masses their masses can not be lowered by changing scalar soft terms to enhance σ scal χ q and σspin χ q through the process χq q χq. Higgses : relax universality m Hi MGUT change life. = (1 + δ i )m 0 modify REWSB relation parameters, m A, µ can 9

11 non universal Higgs masses effects in the ( m 0, m 1/ ) plane m H =m0 ; m H1 =0.5*m0 ; A0=0 ; tan( β)=45 ; µ >0 m1/ (GeV) χ not LSP 0.05 Ω χ h = µ flux = 10 km yr - -1 µ flux = 10 km yr Exp. Excluded m1/ (GeV) χ not LSP Ω χ h = ZEPLIN Max EDELWEISS II Exp. Excluded 00 no EWSB 00 no EWSB m0 (GeV) m0 (GeV) m H = m 0 ; m H1 = 0.5m 0 ; A 0 = 0 ; tan β = 45 ; µ > 0 wider norewsb region m A(H) < m A(H) msugra good for relic density (χχ A b b) and direct detection at low m 0 (χq H χq) but lower indirect detection Barger et al PRD65 00, due to the low Isajet value of µ at high m 0 (Allanach, Kraml, Porod, SUSY 0, hep-ph/007314) which increases the higgsino fraction (?). 10

12 Free relations in gaugino mass parameters M GUT parameter essentially modify neutralino composition (and slightly low energy values of fields whitout SU(3) charge through RGE). Increasing the wino component of the χ + 1, χ0 neutralino favours χχ W + W, ZZ and enhance the annihilation cross section σ A χ χ. the strong χχ0 and χχ + 1 coannihilations become actives and Ω χ h strongly decreases. larger coupling entering in σ scal χ p increases the direct detection favours neutralino annihilations into the hard W + W spectrum increases the indirect detection muon fluxes However, the relevant value of M is very critical : = fine-tunning (except moduli decays giving wino in AMSB models. Moroi, Randall hep-ph/990657). M 3 GUT parameter 1-loop RGE analyse M 3 GUT is the main parameter for non-universality in the MSSM (Kazakov, Moultaka hep-ph/99171). (M scal soft low) = (M scal soft GUT ) + c 3 f 3 + c f + c 1 f 1 + corrections with f i = (MGUT i ) ( b i 1 1 (1+b i α 0 t) ) and c 3 strongly dominant. M 3 GUT < m 1/ decreases m A, m H, µ (and m q ) increase annihilation χχ A b b (χχ f f f) χχ Z t t, χχ χ+ i,χ i W + W, ZZ higgsino fraction very favourable for Ω χ h Gain for detection : direct detection : increase σ scal χ p via χq H χq (m H lower and z 11() z 13(4) ) indirect detection : increase capture σ spin via χ p χq Z χq (higgsino fraction ) and annihilation χχ W + W, ZZ, t t with energetic neutrinos 11

13 Effects of x = M 3() GUT m 1/ on relic density and detection rate Ω χ h µ flux σ scal msugra m0=1500 ; m1/=600 ; A0=0 ; tan( β)=45 ; µ >0 χ p log10 Ω h^ M3 m1/ M m1/ ) 1.yr log10 µ flux from sun (km M3 m1/ M m1/ log10 σ χ scal p (pb) M3 m1/ M m1/ x x x M m1/ M m1/ 1150 M m1/ µ QEWSB (GeV) M3 m1/ gaugino fraction M3 m1/ ma (GeV) M3 m1/ x x x µ f G m A 1

14 M 3 GUT effect on experiment sensitivities in the (m 0, m 1/ ) plane m1/ (GeV) ANTARES km ICECUBE χ not LSP Exp. Excluded 0.05 Ω χ h =1 0.3 A0=0 ; tan( β)=45 ; µ >0 ; M 3/m 1/ = no EWSB m1/ (GeV) EDELWEISS II ZEPLIN Max χ not LSP Exp. Excluded 0.05 Ω χ h = no EWSB m0 (GeV) m0 (GeV) M 3 GUT m 1/ = 0.63 ; tan β = 45 13

15 M 3 GUT effect on experiment sensitivities in the (m 0, m 1/ ) plane A0=0 ; tan( β)=10 ; µ >0 ; M 3/m 1/ = Exp. Excluded ANTARES km ICECUBE Exp. Excluded EDELWEISS II ZEPLIN Max 0.3 m1/ (GeV) χ not LSP Ω χ h = m1/ (GeV) χ not LSP Ω χ h = no EWSB 500 no EWSB m0 (GeV) m0 (GeV) M 3 GUT m 1/ = 0.55 ; tan β = 10 14

16 Conclusion RGE models OK with neutrino indirect detection : very heavy scalars (beyond reach of LHC) neutrino telescope signal in msugra m χ + < GeV Ωh 5 can be accomodated for all msugra points using x = M 3 GUT /m 1/ 0.6(±) + corrections(m 0, tan β, m b ) with a strong enhancement of detection rates improving the experiment possibilities. Earth out of reach neutrino telescopes in those framework. These models are compatible with the Standard Model value of (g ) µ : a SUSY µ 0. 15