Inert Doublet Model and DAMA:

Transcription

1 Inert Doublet Model and DAMA: elastic and/or inelastic Dark Matter candidates C.A., FS. Ling, M.H.G. Tytgat arxiv: Chiara Arina TAUP July 1/5 Service de Physique Theorique 1 Universite Libre de Bruxelles (ULB)

2 Motivations DAMA signal Null experiments at 8.2 σ of C.L. Analysis of the compatibility in a specific model in two different limits Inert Doublet Model scalar particle as DM candidate (spin-independent interactions) A) Elastic scattering light WIMP O(10) GeV B) Inelastic scattering high mass range 500 GeV - 15 TeV 2 C. Arina (ULB PhysTh) - TAUP 2009

3 Direct searches - Event Rate Differential rate WIMP scattering off nucleus dr de R = ρ DM m DM dσ de R η(e R,t) Particle and nuclear physics Astrophysics: - SMH velocity distribution - local dark matter density (mean value of 0.3 GeV/cm^3) - source of uncertainties Total rate R(t) = E2 E 1 de R ɛ(e R ) dr G(E R, σ(e R )) de R Efficiency and energy resolution of the detector 3 C. Arina (ULB PhysTh) - TAUP 2009

4 dσ de R = m Nσ 0 n 2µ 2 n Particle physics Spin-independent cross-section on nucleon ( ) 2 fp 2 Z +(A Z)fn 2 f 2 n F 2 (E R ) Nuclear physics Uncertainties coupling to the nucleon (f) nuclear form factor (Helm) Scalar particle interaction: Z exchange h Z inelastic reaction DM 1 N DM 2 N m DM2 m DM1 = δ 100 kev Higgs exchange, elastic scattering DM N DM N 4 C. Arina (ULB PhysTh) - TAUP 2009

5 Inert Doublet Model Deshpande and Ma 78 Minimal assumption: extension of the SM Higgs sector: usual H 1 doublet and a additional inert doublet H 2 Z 2 symmetry: all SM particle are even except H 2 which is odd H 2 does not take a vev <H 2 >=0 asymmetric phase the neutral lightest component is stable and a DM candidate no FCNC because the does not couple to fermions H 2 no H 1 H 2 mixing 5 C. Arina (ULB PhysTh) - TAUP 2009

6 Scalar potential and particle content V (H 1,H 2 ) = µ 2 1 H µ 2 2 H λ 1 H λ 2 H 2 4 +λ 3 H 1 2 H λ 4 H 1 H λ 5 2 gauge interaction and real quartic couplings [ ] (H 1 H 2) 2 + h.c. after EWSB spectrum in the scalar sector: m 2 h = 2λ 1 v 2 MH 2 = µ λ v 2 H0 MA 2 = µ λ v 2 A0 MH 2 + = µ λ v 2 Hc usual Higgs + 3 inert scalar particles 2 neutral and one charged simple model 5 free parameters: 3 masses and two coupling λ Hc λ 3 /2 λ H0,A 0 (λ 3 + λ 4 ± λ 5 )/2 H0 and A0 symmetric for λ 5 < 0 H0 lightest and DM 6 C. Arina (ULB PhysTh) - TAUP 2009

7 Low mass regime M H0 M A0 = M H ± light around 10 GeV SU(2) custodial symmetry degenerate and heavy O(100) GeV same coupling governs the relic density and the scattering region at 10 GeV due to channeled scatter on Iodine (qi = 1 Iodine quenching factor) Main constraints for the O(10) GeV region: CDMS Ge Xenon10 DAMA total rate middle mass range excluded for elastic interactions 7 C. Arina (ULB PhysTh) - TAUP 2009

8 elastic scattering results for light H0 WMAP Best fit point m=12 GeV λ =0.12 chi2= 36 (34 d.o.f.) CDMS Ge Xenon10 DAMA total rate predictive model -> fixed by WMAP and direct detection uncertainties from nuclear physics: fn factor (coupling between Higgs and nucleon) 0.14 < fn < 0.66 here fn = C. Arina (ULB PhysTh) - TAUP 2009

9 Evolution of the DAMA region as a function of the mass splitting δ = 5 kev δ = 20 kev δ = 80 kev δ = 150 kev 9 C. Arina (ULB PhysTh) - TAUP 2009

10 High mass regime δ = M A0 M H0 λ 5 = ( m H0 100 GeV 100keV ) ( δ 100 kev The 2 neutral states are almost degenerates ) required small coupling = 0 Peccei-Quinn symmetry the doublet model is the only one in the framework of Scalar Multiplet DM that exhibit a small splitting relevant for inelastic DM Some annihilation and coannihilation diagrams contributing to the relic density +... Inelastic interaction through Z boson on the nucleon: H0 A0 10 C. Arina (ULB PhysTh) - TAUP 2009

11 high mass range: inelastic scattering Perturbative bound WMAP subdominant 3 best fit points but excluded by CRESST II and CDMSGe However 3 different zones: LEPII excluded - middle mass complatible with null detection experiments but subdominant CDMS Ge Cresst-II DAMA total rate - O(10) TeV with small splitting excluded by the DAMA total unmodulated rate -O(10) TeV with large splitting compatible at 99% C.L. and right relic density 11 C. Arina (ULB PhysTh) - TAUP 2009

12 Effect of the variation of the density at the sun position low mass regime with λ H0 =0.12 inelastic case for δ = 120 kev - step up of the compatibility between DAMA region and Xenon10 and CDMSGe for higher density clumpy nature of DM halo 0.3 GeV/cm^3 refers to the averaged local density of the smooth component at the location of the Earth 12 C. Arina (ULB PhysTh) - TAUP 2009

13 Asymmetric dark matter in the primordial Universe charge asymmetry in the dark sector PQ becomes exact for λ 5 0 small breaks the symmetry H n H n (h) f f H n H n hh annihilation through Higgs neglected EW phase transition delicate H n X H nx 4 point interaction term is dominant simplified boltzmann equation for the number density gives an upper bound on the interaction rate = (n H n n H n ) s(t ) λ 5 < 10 7 g 1/4 T 10 GeV masses O(1-100) TeV asymmetry wash out masses < 100 GeV out of equilibrium in the early universe masses O(100) GeV produced the actual number density 13 C. Arina (ULB PhysTh) - TAUP 2009

14 Conclusions Compatibility of the DAMA data with the others exclusion experiments in the Inert Doublet Model The Inert Doublet Model is based on very minimal assumption: an additional inert Higgs doublet to the SM stable by means of a Z2 symmetry 2 different limit in the parameter space: Light WIMP regime compatible at 3 sigma C.L. elastic scattering once High mass regime compatible at 3 sigma C.L. inelastic scattering O(1-100) TeV always compatible with WMAP O(100) GeV subdominant halo component: primordial asymmetry responsible of the actual number density small coupling fixed by WMAP and direct detection, no more free parameters interesting signatures for antimatter (Tytgat et al 08) muon flux from neutrino flux from the sun in the range of SuperKamiokande (Andreas et al 08) technically natural protected by the PQ symmetry Another inelastic Dark Matter candidate is the mixed sneutrino -> small splitting natural consequence of the small neutrino masses (CA, N. Fornengo 07 and CA, F.Bazzocchi, N. Fornengo, J.Valle, J. Romao 08) 14 Thanks! C. Arina (ULB PhysTh) - TAUP 2009

15 Back-up slides 15 C. Arina (ULB PhysTh) - TAUP 2009

16 Annual modulation For an isotropic WIMP velocity distribution the annual modulation can be approximated with a cosine motion v = v + v rot cos γ cos ω(t t 0 ) DAMA modulated amplitude Dama coll., Eur.Phys.J.C56: ,2008 (arxiv: ) S m = dr de R mod 1 2 { dr (June 2) dr } (December 2) de R de R goodness of fit over the 36 bins 16 C. Arina (ULB PhysTh) - TAUP 2009

17 Astrophysics Inverse Averaged velocity distribution η(e R,t)= d 3 v f( v(t)) v v min assumed isotropic truncated Maxwellian distribution v 0 = 220 km/s 450 km/s< < 650 km/s v min = 1 ( MN E R 2M N E R µ minimum velocity to = 0 elastic scattering ) + δ = 100 KeV inelastic scattering required an higher velocity to ER sensitive to tail WIMp distribution = 0.3 GeV/cm^3 local density at the sun position 17 C. Arina (ULB PhysTh) - TAUP 2009

18 Velocity distribution η(e R,t)= d 3 v f( v(t)) v v min Basic assumptions: different halo models and/or velocity values analyzed eg. Belli 02, March-Russell 08, Savage 09 and more... If the velocity distribution in the galactic frame is isotropic: η = 2π v E (v + v )F(v esc ) 2π v E v+ v F(v) dv with: v ± = min{v esc,v min ± v } F(v) = v f gal (v) dv = escape velocity = minimum WIMP velocity to scatter = Earth velocity in the galactic frame v (t) =v + v EO (t) 18 C. Arina (ULB PhysTh) - TAUP 2009

19 Mixed Sneutrino as Inelastic Dark Matter 19 C. Arina (ULB PhysTh) - TAUP 2009

20 Inert Doublet Model Constraints H 1 =(h + (v + h + ig 0 )/ 2) T H 2 =(H + (H 0 + ia 0 )/ H 1 = v = µ 2 1/λ 1 = 246GeV 2) T µ 2 2 > 0 potential bounded from below at tree level rho parameters: small splitting between MA0 and MHp Related to dark matter Deshpande and Ma 78, Ma 06, Barbieri et al. 06, L.Lopez Honorez et al. 07, Hambye and Tytgat C. Arina (ULB PhysTh) - TAUP 2009

21 More on phenomonology of light scalar WIMP gamma line (Edsjo et al. 07) colliders constraints (Edsjo et al. 08) Neutrino flux from the sun and superkamiokande (muon flux) S.Andreas, M.H.G.Tytgat, Q.Swillens JCAP0810 (2008) Antimatter flux E. Nezri, M.H.G.Tytgat, G. Vertongen JCAP0904 (2009) anti-deuteron flux can be reach by GAPS, below bess 21 C. Arina (ULB PhysTh) - TAUP 2009

22 Scattering on nucleon F (E R ) = 3e q2 s 2 /2 sin(qr) qr cos(qr) (qr) 3 Helm form factor Higgs-nucleon coupling fm N N q m q qq N = g hnn v Andreas, Hambye, Tytgat (2008) σ inel Z = 1 2δ µ 2 σel Z Nv2 22 C. Arina (ULB PhysTh) - TAUP 2009

23 More on the asymmetry Boltzmann equation 4 point cross-section d dx 2 x Hs(T ) (γ S σ A = σ S = λ2 5 32πs Y h Y n e qy h e q + γ A Y n (Y n e q) 2 ) γ thermal averaged cross-section References for Inert Doublet Model Light singlet and doublet scalar: T.Hambye and M.H.G.Tytgat, Phys.Lett.B659 (2008) S.Andreas, T.Hambye and M.H.G.Tytgat, JCAP0810 (2008) Scalar Multiplet Dark Matter T.Hambye, FS. Ling, L.Lopez-Honorez and J.Rocher, arxiv: C. Arina (ULB PhysTh) - TAUP 2009