Dark Matter Direct Detection in the NMSSM

Transcription

1 Dark Matter Direct Detection in the NMSSM,DSU27. Dark Matter Direct Detection in the NMSSM Daniel E. López-Fogliani Universidad Autónoma de Madrid Departamento de Física Teórica & IFT DSU27 D. Cerdeño, C. Hugonie, D. L-F, C. Muñoz, A. Teixeira, JHEP 42 (24) 48. D. Cerdeño, E. Gabrielli, D. L-F, C. Muñoz, A. Teixeira, JCAP (27) (accepted).

2 Dark Matter Direct Detection in the NMSSM,DSU27. 2 Outline Direct Detection of Neutralino Dark Matter in the NMSSM The NMSSM The Neutralino-Nucleon Cross Section Experimental constraints Analysis of Neutralino DM in the NMSSM Conclusions

3 Dark Matter Direct Detection in the NMSSM,DSU27. 3 Why the NMSSM? The NMSSM Solves a problem of naturalness in the MSSM: why the µ parameter in µh H 2 is of order the electroweak scale. Superpotential ) W = ǫ ij (Y u H j 2 Qi u + Y d H i Q j d + Y e H i L j e ǫ ij λs H i H j κs3 Higgs soft terms of the NMSSM L Higgs soft = m 2 H i Hi H i + m 2 S S S + ( ǫ ij λaa λ SHH i j κa A κ S 3 + H.c.) A λ A κ

4 Dark Matter Direct Detection in the NMSSM,DSU27. 4 NMSSM potential After EW Symmetry breaking: < H >= v, < H 2 >= v 2, < S >= s µ eff = λs V Higgs neutral = g2 +g2 2 8 ( v 2 v 2 2) 2 + λ 2 ( s 2 v 2 + s 2 v v 2 v 2 2) + κ 2 s 4 + m 2 H v 2 + m 2 H 2 v m 2 S s 2 +( λκ v v 2 s 2 λa λ sv v κa κs 3 + H.c.)

5 Dark Matter Direct Detection in the NMSSM,DSU27. 5 Minimization of the scalar potential Finding a minimum of V is much harder than in the MSSM... From the minimization of the potential with respect to the phases of the VEV s we have four combinations of signs for A κ A λ, s and k : (i) sign(s) = sign(a λ ) = sign(a κ ), (ii) sign(s) = sign(a λ ) = sign(a κ ), with A κ > 3λv v 2 A λ /( sa λ + κ s 2 ). k > (iii) sign(s) = sign(a λ ) = sign(a κ ), with A κ < 3λv v 2 A λ /( sa λ + κ s 2 ). } (iv) sign(s) = sign(a λ ) = sign(a κ ), with A κ > 3λv v 2 A λ /( sa λ κ s 2 ). k < We must also satisfy the minimization Eqs. for v

6 Dark Matter Direct Detection in the NMSSM,DSU27. 6 NMSSM Particle content 8 < NMSSM Spectrum MSSM + : 2Higgs (CP even, CP odd) Neutralino M χ = M M Z sin θ W cos β M Z sin θ W sin β M 2 M Z cos θ W cos β M Z cos θ W sin β M Z sin θ W cos β M Z cos θ W cos β λs λv 2 M Z sin θ W sin β M Z cos θ W sin β λs λv λv 2 λv 2κs C A The lightest neutralino: χ = N B + N 2 W 3 + N 3 H + N 4 H 2 + N S 5 The lightest CP-even Higgs: h = S H + S 2 H2 + S 3SS 3S

7 ¼ ½ ¼ ½ ¼ ½ ¼ ½ ¼ Dark Matter Direct Detection in the NMSSM,DSU27. 7 Dark matter: Direct detection in the NMSSM º º º º Õ Õ Õ º º º º Õ Õ α h 3i = 3 a= m 2 h a C i Y Re[Ca HL ] α q 3i = 2 X= 4(m 2 Xi m2 χ L eff = α 3i χ χ q i q i [ (C ) Re Xi R )( ) ] C Xi L See also V. Barger et al., 7, for an analysis of MSSM singlet extensions.

8 Dark Matter Direct Detection in the NMSSM,DSU27. 8 Relic density Enough χ can survive annihilation (and coannihilation) in order to account for observed Ω For example: χ χ W ± W ±, Z Z h h, a a, h Z q q, l + l NMSSM similar to MSSM, but additional fingerprint -type processes like.. χ h q ( l + ) χ. q (l ). where χ singlino; h singlet BUT! Generating large σ may lead to excessive χ -annihilation (low Ω) See also Bélanger et al., 5

9 Dark Matter Direct Detection in the NMSSM,DSU27. 9 Constraints on the NMSSM parameter space and computation Relevant parameters at low scale λ, κ, tanβ, µ, A λ, A κ, M, M 2, M 3 (M, A ) Minimization of the potential Absence of Landau Pole for λ, κ, Y t, and Y b below M GUT Computation of the NMSSM spectrum NMHDECAY 2. Experimental constraints from LEP (Ellwanger, Hugonie) Neutralino Higgs Squark b s γ (g µ 2), rare B and K decays Our code Dark Matter Relic density Neutralino Nucleon Cross Section New MicrOMEGAs Our code

10 Dark Matter Direct Detection in the NMSSM,DSU27. Muon anomalous magnetic moment (a µ ) Experimental data: Theoretical for SM: a µ = 65928(6) a µ = (5.) a µ = (27.6 ± 8) At to 2σ level the SUSY contribution must be:.6 a SUSY µ 43.6 SUSY contributions at loop-level: Dominant: Sneutrino and Chargino Charged Sleptons and Neutralino

11 Dark Matter Direct Detection in the NMSSM,DSU27. a SUSY µ as a function of M The horizontal solid line indicates the lower bound of the allowed 2σ interval. Choosing typical NMSSM values µ = 5 GeV, 8 A λ 8 GeV, 3 A κ 3 GeV, and low tan β, tan β = 5, in order to analyze departures from the MSSM. From bottom to top, m L,E = TeV with A E = TeV, m L,E = 5 GeV with A E = TeV, m L,E = 5 GeV with A E = 2.5 TeV.

12 Dark Matter Direct Detection in the NMSSM,DSU27. 2 b s γ Experimental data [HFAG 6]: BR(b sγ)= (3.55 ±.27) 4 Theoretical calculation for the SM [Gambino 5]: BR(b sγ)= (3.73 ±.3) 4 SUSY contributions at loop-level Charged Higgs H ± and up quarks u, c, t Chargino χ ± and up squarks ũ, c, t Neutralino χ and down squarks d, s, b gluino g and down squarks d, s, b In our analysis: dominant H ± -mediated contribution! [No flavour mixing other than the V CMK ] BR(b sγ) /m 4 H ± with m 2 H ± = 2µ2 sin(2β) κ λ v2 λ 2 + 2µA λ sin(2β) + m2 W

13 Dark Matter Direct Detection in the NMSSM,DSU27. 3 BR(b sγ) in the NMSSM: Results M = 6 GeV, M 2 = 32 GeV, A λ = 4 GeV, A κ = 2 GeV, µ = 3 GeV, tan β = 5 b sγ isocurves mimic m H ± isocurves b sγ typically maximal close to tachyon border Improve b sγ: larger (A λ, µ, tanβ) Worsens exclusion by LEP constraints

14 Dark Matter Direct Detection in the NMSSM,DSU27. 4 Relic density in the λ-κ plane For the same parameters as the previous study M = 6 GeV, M 2 = 32 GeV, A λ = 4 GeV, A κ = 2 GeV, µ = 3 GeV, tan β = 5 red dots m χ = m h ; black full m χ = m Z, m W ; red dashed 2m χ = m h 2 ; Very light neutral Higgs: m h 2 GeV; singlet component: S ; Higgsino-Bino LSP; (N5 2.35) moving to small κ with respect to λ small m χ and more singlino

15 Dark Matter Direct Detection in the NMSSM,DSU27. ' Dark Matter: 5 Ω and direct detection $ For the same parameters as the previous study M = 6 GeV, M2 = 32 GeV, Aλ = 4 GeV, Aκ = 2 GeV, µ = 3 GeV, tan β = 5 Gray Experimentally accepted (accelerators) Dark Gray In addition fulfil. Ωh2.3 Black Satisfies all experimental constraints including WMAP.94 Large σ &. Ωh2..29 exchange of light singlet-like Higgs %

16 Dark Matter Direct Detection in the NMSSM,DSU27. 6 NMSSM DM: further examples M = 33 GeV, M 2 = 66 GeV, A λ = 57 GeV, A κ = 6 GeV, µ = 6 GeV, tan β = 5 Green dash Z 2 5 =.5 a µ more than 2σ away a µ 7.2 Compatible with Ω and b sγ (2σ) Within CDMS-Soudan range: χ singlino-like and h singlet like.

17 Dark Matter Direct Detection in the NMSSM,DSU27. 7 NMSSM DM M 2 43 GeV, 8 A λ 8 GeV, 3 A κ 3 GeV, µ 3 GeV, tan β = 5

18 Dark Matter Direct Detection in the NMSSM,DSU27. 8 Conclusions ❶ Systematic analysis of the NMSSM parameter space Taken into account LEP constraints BR(b s γ) bounds (as well as others) WMAP data on Ω Investigated prospects for direct detection of DM ❷ In the NMSSM, large σ χ p can be obtained Associated to t-channel exchange of very light Higgs (m h 7 GeV), large singlet component (escapes detection) NMSSM nature is further evidenced in having a singlino-higgsino LSP ❸ Impact of Ω and BR(b s γ) Ω often relies on the same light-higgs exchange that gives large σ large σ χ p excessive annihilation BR(b s γ) typically larger in regions where DM is WMAP-compatible & within range of present detectors