SUSY Dark Matter Models

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1 SUSY Dark Matter Models msugra model Normal scalar mass hierarchy NUHM NUHM2 MWDM BWCA LM3DM (compressed SUSY) mixed moduli-amsb (KKLT) Howard Baer Florida State University Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5, 2007

2 Some successes of SUSY GUT theories SUSY divergence cancellation maintains hierarchy between GUT scale Q = 0 6 GeV and weak scale Q = 00 GeV gauge coupling unification! Lightest Higgs mass m h < 30 GeV as indicated by radiative corrections! radiative breaking of EW symmetry if m t GeV! dark matter candidate: lightest neutralino Z stable see-saw mechanism for neutrino mass SO(0) SUSY GUT: baryogenesis via leptogenesis Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

3 Our strategy: Assume MSSM is valid effective theory between M weak and M GUT LSP is stable: good candidate for CDM Stipulate SSB terms at Q = M GUT and evaluate SSB at M weak via RG evolution EW symmetry broken radiatively by large m t Invoke minimal flavor violation ignore CP-viol. phases Spectra generated with Isajet/Isasugra We will use the measured value Ω CDM h 2 = 0.05 ± 0.0 as a guide to allowed phenomenology! Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

4 msugra model; allowed parameter space Case : paradigm msugra model (thanks to Arnowitt, Nanopoulos, Weinberg, other pioneers ) m0, m/2, A0, tan β, sign(µ) msugra,tanβ=0,a0=0,µ>0,mtop=75gev δaposx00:30,0,5, Ωh2< < Ωh < < Ωh < stau LSP 400 BF(b sγ)x04:2,3 Ωh2< < Ωh < < Ωh < 0.5 m/2 (GeV) 600 δaposx00:30,0,5, 2000 stau LSP msugra,tanβ=55,a0=0,µ>0,mtop=75gev BF(b sγ)x04:2,3 m/2 (GeV) NO REWSB LEP m0 (GeV) NO REWSB LEP m0 (GeV) Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

5 Main msugra regions consistent with WMAP most of parameter space excluded: Ω CDM h 2 too big! Exceptions: bulk region (low m 0, low m /2 ) stau co-annihilation region (m τ m ez ) HB/FP region (large m 0 where µ small) A-funnel (2m ez m A, m H ) h corridor (2m e Z m h ) stop co-annihilation region (particular A 0 values m t m ez ) Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

6 Constraints as χ2 on msugra model NO REWSB sqrt(χ2) NO REWSB m0 (TeV) sqrt(χ2) m/2 (GeV) stau LSP msugra, tgβ=55, µ>0, A0=0, mtop=75 GeV e+e- input for δaµ LEP2 excluded m/2 (GeV) 800 stau LSP 2000 msugra, tgβ=0, µ>0, A0=0, mtop=75 GeV e+e- input for δaµ LEP2 excluded m0 (TeV) Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

7 Sparticle reach of all colliders and relic density 600 msugra with tanβ = 0, A 0 = 0, µ > 0 Ωh 2 < 0.29 LEP2 excluded 600 msugra with tanβ = 45, A 0 = 0, µ < 0 Ωh 2 < 0.29 LEP2 excluded m /2 (GeV) LHC m /2 (GeV) LHC 600 LC LC LC LC Tevatron 200 Tevatron m 0 (GeV) m 0 (GeV) HB, Belyaev, Krupovnickas, Tata Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

8 HB/FP region: absolute measure of m g at LHC! LHC events characterized by high jet, b-jet, isol. lepton multiplicity No. of Jets Cuts C FP(3050,400,0,30,,75) QCD Jets tt W+jets Z+jets WW, WZ, ZZ Sum of Backgrounds No. of b-jets (60% eff.) Cuts C FP(3050,400,0,30,,75) QCD Jets tt W+jets Z+jets WW, WZ, ZZ Sum of Backgrounds σ (fb) 0 σ (fb) # of Jets # of b-jets Barger, Shaughnessy, Summy, Wang HB, Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

9 Measure m g in HB/FP region via total rate to 8% require cuts C plus n ( j) 7, n(b j) 2, M eff 400 GeV Augmented Effective Mass Cuts C, n b-jets >=2 (60% eff.) dσ/da T (fb/gev) 0.0 FP(3050,400,0,30,,75) QCD jets tt W+jets Z+jets WW, WZ, ZZ Sum of Backgrounds σ (fb) LEP2 excluded TH 00 fb - error TH ±5% TH ±5% ±00%BG BG A T (GeV) Barger, Shaugnessy, Summy, Wang m g ~ HB, Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

10 Direct detection of SUSY DM scan over msugra space (Ω CDM h 2 0.) : Stage : CDMS, Edelweiss, Zeplin Stage 2: CDMS2, CRESST2, Edelweiss2 Zeplin2, Xenon-0 Stage 3: SuperCDMS, LUX, (mini)clean WARP, ArDM σ SI (pb) σ SI (pb) a) µ>0 msugra ~ (GeV) b) µ<0 m Z CDMS CDMS2 HB/FP region Super CDMS 25 kg WARP 400 kg stau co-annihilation region CDMS CDMS2 Super CDMS 25 kg WARP 400 kg m~ Z (GeV) tanβ=0 tanβ=30 tanβ=45 tanβ=50 tanβ=52 tanβ=55 : HB/FP region tanβ=55 : A-funnel region tanβ=55 : stau co-annihilation region Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

11 Indirect detection (ID) of SUSY DM: ν-telescopes Z Z b b, etc. in core of sun (or earth): ν µ µ in ν telescopes Amanda, Icecube, Antares Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5, 2007

12 ID of SUSY DM: γ and anti-matter searches Z Z q q, etc. γ in galactic core or halo Z Z q q, etc. e + in galactic halo Z Z q q, etc. p in galactic halo Z Z q q, etc. D in galactic halo Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

13 Direct and indirect detection of neutralino DM 600 msugra, A 0 =0 tanβ=0, µ>0 600 msugra, A 0 =0, tanβ=50, µ< not LSP Z ~ LHC DD µ 200 not LSP Z ~ DD m /2 (GeV) m /2 (GeV) LHC 600 LC LC LC LC500 µ 200 TEV LEP no REWSB 200 LEP no REWSB m 0 (GeV) Φ(p - )=3x0-7 GeV - cm -2 s - sr - Φ(γ)=0-0 cm -2 s - Φ sun (µ)=40 km -2 yr - (S/B) e+ =0.0 m h =4.4 GeV m 0 (GeV) Φ(p - ) 3e-7 GeV - cm -2 s - sr - (S/B) e+ =0.0 Φ(γ)=0-0 cm -2 s - Φ sun (µ)=40 km -2 yr - m h =4.4 GeV 0<Ωh 2 <0.29 σ(z ~ p)=0-9 pb Φ earth (µ)=40 km -2 yr - σ(z ~ p)=0-9 pb 0< Ωh 2 < 0.29 HB, Belyaev, Krupovnickas, O Farrill Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

14 SUGRA models with non-universal scalars Normal scalar mass hierarchy (NMH): BF(b sγ) prefers heavy 3rd gen. squarks (g 2) µ prefers light 2nd gen. sleptons m 0 (,2) = 00GeV, m 0 (3) = 400GeV, m /2 = 550GeV, b ~ R ~ tl τ ~ L τ ~ R A 0 = 0, tanβ = 30, µ > 0, m t = 75GeV m 0 () m 0 (2) m 0 (3) (preserve FCNC bounds) motivation: reconcile BF(b sγ) with (g 2) µ HB, Belyaev, Krupovnickas, Mustafayev JHEP 0406, 044 (2004) m (GeV) H d u ~ L u ~ R, d~ R e ~ L e ~ R ~ tr H u Q(GeV) Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

15 Normal scalar mass hierarchy: parameter space m0 () m0 (2) m0 (3) LHC: light sleptons, enhanced leptonic cascade decays ILC: first two gen. sleptons likely accessible; squarks/staus heavy msugra, tgβ=30, µ>0, A0=0, mtop=75 GeV,m0,2=00 GeV LEP2 excluded e+e- input for δaµ stau LSP sqrt(χ2) 3 m/2 (GeV) NO REWSB m03 (TeV) Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

16 SUGRA models with non-universal Higgs mass (NUHM) m 2 H u = m 2 H d m 2 φ m 0: Drees; HB, Belyaev, Mustafayev, Profumo, Tata motivation: SO(0) SUSYGUTs where Ĥ u,d φ(0) while matter ψ(6) m 2 φ m 0 higgsino DM for any m 0, m /2 m 2 φ < 0 can have A-funnel for any tan β m 0 =300GeV, m /2 =300GeV, tanβ=0, A 0 =0, µ>0, m t =78GeV Ωh WMAP m φ / m 0 m (TeV) µ m χ m A m φ / m 0 Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

17 NUHM2 (2-parameter case) m 2 H u m 2 H d m 0 : HB, Belyaev, Mustafayev, Profumo, Tata motivation: SU(5) SUSYGUTs where Ĥu φ(5), Ĥ d φ( 5) can re-parametrize m 2 H u, m 2 H d µ, m A (Ellis, Olive, Santoso) large S term in RGEs light ũ R, c R squarks, mẽl < mẽr NUHM2: m 0 =300GeV, m /2 =300GeV, tanβ=0, A 0 =0, m t =78GeV µ (GeV) 900 Ah GS HS τ ~ 2.5 sqrt(χ 2 ) 400 msugra NUHM LEP m A (GeV) Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

18 Non-universal gaugino masses SUGRA models where GKF transforms non-trivially (Snowmass 96) Heterotic superstring models with orbifold compactification: SUSY breaking dominated by the moduli field KKLT model of type IIB string compactification with fluxes Extra-dimensional SUSY GUT models where SUSY breaking is communicated from the SUSY breaking brane to the visible brane via gaugino mediation (e.g. Dermisek-Mafi model) Here we adopt a phenomenological approach of independent M, M 2, M 3 but require consistency with WMAP MWDM: HB, Mustafayev, Park, Profumo, JHEP0507, 046 (2005) BWCA DM: HB, Krupovnickas, Mustafayev, Park, Profumo, Tata, JHEP052 (2005) 0. Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

19 LM3DM: HB, Mustafayev, Park, Profumo, Tata, JHEP0604 (2006) 04. Related work: Corsetti and Nath; Birkedal-Hansen and Nelson; Bertin, Nezri and Orloff; Bottino, Donato, Fornengo, Scopel; Belanger, Boudjema, Cottrant, Pukhov, Semenov; Mambrini, Munoz and Cerdeno; Auto, HB, Belyaev, Krupovnickas; Masiero, Profumo, Ullio Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

20 Ω ez h 2 vs. M Ωh m 0 =300 GeV, m /2 =300 GeV, tanβ=0, A 0 =0, µ>0, m t =78 GeV BWCA msugra MWDM BWCA msugra MWDM a) b) WMAP M (GeV) R B ~,W ~ w ~ B~ M (GeV) Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

21 Sparticle mass spectra vs M m 0 =300GeV, m /2 =300GeV, tan β =0, A 0 =0, µ >0, m t =78GeV sparticle masses (GeV) d ~ R u ~ R g ~ d ~ L b ~ 2 ~ t b ~ u ~ L t ~ e ~ L µ τ ~ ν ~ e,ν~ τ e ~ R Z ~ 2 τ ~ W ~ BWCA Z ~ msugra MWDM M /m /2 Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

22 MWDM: plot r M /M 2 (at M GUT which gives Ω CDM h 2 0. NUGM: tanβ=0, A 0 =0, µ>0, m t =78 GeV, Ωh 2 =0.26± m /2 (TeV) LEP m 0 (TeV) r = 0.6 r =.0 r :.5,.65,.7,.75,.8 Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

23 MWDM: small Z2 Z mass gap msugra: tanβ=0, A 0 =0, µ >0, m t =78 GeV NUGM: M m /2, tanβ=0, A 0 =0, µ >0, m t =78 GeV m /2 (TeV) m /2 (TeV) m Z2 - m Z = 00 GeV 0.3 m Z2 - m Z = 30 GeV LEP LEP m 0 (TeV) m 0 (TeV) Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

24 m(l + l ): mass gap observable at LHC for MWDM x 0-2 /σ dσ/dm (GeV - ) /σ dσ/dm (GeV - ) m Z2 - m Z a) msugra 0.06 b) MWDM x 0-2 x m Z2 - m Z 0.8 m Z3 - m Z m - m Z2 Z c) MWDM2 0.2 d) MHDM m(l + l - ) (GeV) m(l + l - ) (GeV) Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

25 Bino-wino co-annihilation (BWCA) scenario If M /M 2 < 0, then no mixing between bino-wino Can only reduce relic density via bino-wino co-annihilation (m e Z m fw m e Z 2 ) when M M 2 at Q = M weak plot r = M /M 2 (at M GUT ) Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

26 2005/07/ BWCA: tanβ=0, A 0 =0, µ>0, m t =78 GeV, Ωh 2 =0.26± m /2 (TeV) LEP m 0 (TeV) r :.5,.65,.7,.75,.77 Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

27 In BWCA at m 0 < 500 GeV, BF( Z 2 Z γ) enhanced! MWDM: M 2 m /2, tanβ=0, A 0 =0, µ >0, m t =78 GeV BWCA: M 2 m /2, tanβ=0, A 0 =0, µ >0, m t =78 GeV m /2 (TeV) m /2 (TeV) LEP LEP m 0 (TeV) m 0 (TeV) Haber+Wyler; Ambrosanio+Mele; Baer+Krupovnickas: JHEP 0209, 038 (2002) Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

28 Mixed higgsino DM from a low M 3 (LM3DM) Ωh WMAP m 0 =300 GeV, m /2 =300 GeV, tanβ=0, A 0 =0, µ>0, m t =75 GeV MHDM2 LEP2 Excluded MHDM msugra M 3 (GeV) R H ~ a) b) MHDM2 LEP2 Excluded MHDM msugra M 3 (GeV) low M 3 low m g, m q, µ called compressd SUSY in related scenario by S. P. Martin Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

29 Sparticle mass spectra for LM3DM 2006/02/ MHDM: m 0 =300GeV, m /2 =300GeV, tan β =0, A 0 =0, µ >0, m t =75GeV sparticle masses (GeV) b ~ ~ t2 b ~ A d ~ L u ~ L u ~ R, d~ R 400 e ~ L, τ~ 2 ν ~ e, ν~ τ µ Z ~ 3 Z ~ 2 g ~ ~ t τ ~ e ~ R Z ~ W ~ 00 WMAP WMAP msugra M 3 /m /2 low m g, m q, µ huge DM detection rates! Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

30 Direct/indrct DM rates greatly enhanced for LM3DM m 0 =300 GeV, m /2 =300 GeV, tanβ=0, A 0 =0, µ>0, m t =75 GeV σ ~ Z p (pb) MHDM2 MHDM msugra 0 6 MHDM2 MHDM msugra 0 5 a) 0 4 b) CDMS2 0 3 LEP2 0 2 IceCube 0 LEP2 Excluded 0 0 Excluded XENON Φ µ sun (km -2 yr - ) R γ GLAST LEP2 Excluded R e c) d) Pamela LEP2 Excluded R p Pamela LEP2 Excluded M 3 (GeV) R D e) f) GAPS LEP2 Excluded M 3 (GeV) Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

31 In LM3DM, BF( g Z i ) loop decay enhanced! MHDM: -M 3 m /2, tanβ=0, A 0 =0, µ >0, m t =75 GeV 2006/02/ MHDM: M 3 m /2, tanβ=0, A 0 =0, µ >0, m t =75 GeV 2006/02/ m /2 (TeV) m /2 (TeV) BF(g ~ Z ~ g)= BF(g ~ Z ~ g)= m 0 (TeV) m 0 (TeV) Baer, Tata, Woodside: PRD42 (990) 568. Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

32 In LM3DM, ratio m g : m f W : m ez 2.5 :.5 : Can search for p p g g jets+ E T at Tevatron; Search is not pre-empted by LEP2 bouds on m fw Can see m g from GeV: HB, Mustafayev, Tata PRD75, (2007) σ (fb) σ (fb) /09/ LM3DM: m 0 =500GeV, tanβ=0, A 0 =0, µ >0, m t =75GeV 2-jet 4-jet 5σ at 5fb - 5σ at 5fb m /2 (GeV) σ (fb) σ (fb) jet 3l 5σ at 5fb - 5σ at 5fb m /2 (GeV) Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

33 Mixed modulus-amsb models KKLT model: type IIB superstring compactification with fluxes stabilize moduli/dilaton via fluxes and e.g. gaugino condensation on D7 brane introduce anti-d3 brane (uplifting potential; de Sitter universe with Λ > 0 small SUSY breaking due to D3 brane mass hierarchy: m moduli m 3/2 m SUSY MSSM soft terms calculated by Choi, Falkowski, Nilles, Olechowski, Pokorski phenomenology: Choi, Jeong, Okumura, Falkowski, Lebedev, Mambrini,Kitano, Nomura see also: HB, E. Park, X. Tata, T. Wang, JHEP0608, 04 (2006); PLB64, 447 (2006); hep-ph/ Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

34 Parameter space of MM-AMSB (mirage unification) model MSSM sparticle mass scale m 3/2 6π 2 M s Ratio of modulus-mediated and anomaly-mediated contributions set by a phenomenological parameter α Modulus-mediated contributions depend on location of fields in extra dimensions. These contributions depend on modular weights of the fields, determined by where these fields are located. modular weights n i = 0 () (( 2 )) for D7 (D3) ((intersection)) Gauge kinetic function indices l a = (0) on D7 (D3) branes. Model completely specified by m 3/2, α, tanβ, sign(µ), n i, l a Radiative EWSB determines µ 2 as usual; model into Isajet 7.75 Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

35 Soft SUSY Breaking Terms The soft terms renormalized at Q M GUT are given by, ( M a = M s la α + b a ga) 2, A ijk = M s ( (3 n i n j n k )α + γ i + γ j + γ k ), m 2 i = Ms 2 ( ( ni )α 2 ) + 4αξ i γ i, with ξ i = j,k (3 n i n j n k ) y2 ijk 4 a l a g 2 ac a 2(f i ), and γ i = 8π 2 γ i log µ Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

36 Meauring modular weights at LHC and ILC A plot of the mirage unification scale versus modulus-amsb mixing parameter α, assuming l =. Mirage Unification Scale (GeV) α At Q = µ mir. = M GUT e 8π2 /(lα), can determine soft terms via RG running up, if weak scale parameters are known. Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

37 α=6, m 3/2 =2 TeV, tanβ=0, µ >0, m t =75 GeV α=6, m 3/2 =2 TeV, tanβ=0, µ >0, m t =75 GeV Mass (GeV) M 3 a) sign(m i 2) m i 2 (GeV) d R, b R t L t R e L, e R, u L b) τ L τ R H d u R 400 M M -400 H u Q (GeV) Q (GeV) At Q = µ mir., ratio of scalar to gaugino masses is given by m i ni =. µmir l a M a For l a =, this measures the matter modular weight! Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

38 Gaugino masses at weak scale in MM-AMSB: m 3/2 =.5 TeV, tanβ=0, µ >0, m t =75 GeV M i (M weak ) (GeV) Excl. ZMW Excl. ZMW M 3 M M Excl. NZMW Excl. NZMW α Low mirage unification scale If M (weak) = ±M 2 (weak), potential for agreement with relic density via MWDM or BWCA! Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

39 α vs. m 3/2 space for n m = n H = 0: Gravitino mass vs. α, tanβ=0, µ>0, ZMW Gravitino Mass (TeV) Ωh 2 < <Ωh 2 <0.5 Ωh 2 >0.5 τ LSP t LSP LHC reach LC 500 reach LC 000 reach Stop coannihilation region. Mixed higgsino region at low positive alpha. BWCA for α < 0. No MWDM region. α Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

40 α vs. m 3/2 space for n m = 2, n H = : Gravitino mass vs. α, tanβ=0, µ>0, NZMW Gravitino Mass (TeV) Ωh 2 < <Ωh 2 <0.5 Ωh 2 >0.5 τ LSP t LSP LHC reach LC 500 reach LC 000 reach Stau coannihilation, Higgs funnel, MWDM and BWCA regions clearly seen. Also, mixed bino-wino-higgsino region (via low M 3 ). Bulk region at low m 3/2. α Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

41 Conclusions: SUSY dark matter models We use the measured relic density of CDM as a guide to SUSY phenomenology in the MSSM msugra models: allowed regions HB/FP region: measure m g to 8% NMH NUHM NUHM2 MWDM BWCA DM LM3DM mixed moduli-amsb (KKLT, mirage unification) data coming soon from LHC will be final arbiter! Howie Baer, TAMU Particle Physics & Cosmology workshop, May 5,

Constraints on SUSY parameters from present data

Constraints on SUSY parameters from present data Howard Baer Florida State University ILC-Cosmology working group MSSM Models of SUSY breaking Constraints WMAP allowed regions Non-universality Beyond the