Mixed axion/lsp dark matter: a new paradigm

Transcription

1 Mixed axion/lsp dark matter: a new paradigm Howard Baer University of Oklahoma OUTLINE SUSY WIMPs: miracle or not? strong CP problem and PQWW solution the PQMSSM mixed axion/axino CDM mixed axion/neutralino CDM can f a M GUT? Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

2 WIMPs: is there a WIMP miracle for SUSY? Weakly Interacting Massive Particles assume in thermal equil n in early universe Boltzman eq n: dn/dt = 3Hn σv rel (n 2 n 2 0) Ωh 2 = s pb σv ( ) 1/2 45 xf 1 ρ c /h 2 πg M P l σv ) ( m wimp 0 GeV thermal relic new physics at M weak! does this work for SUSY neutralinos? Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

3 χ 2 fit of msugra to Ω ez1 h 2, b sγ and (g 2) µ not LSP msugra with tanβ =, A 0 = 0, µ > not LSP msugra with tanβ = 54, A 0 = 0, µ > Ζ ~ Ζ ~ 1 m 1/2 (GeV) No REWSB m 0 (GeV) m h =114.1GeV LEP2 excluded SuperCDMS CDMSII CDMS ln(χ/dof) m 1/2 (GeV) No REWSB m 0 (GeV) m h =114.1GeV LEP2 excluded SuperCDMS CDMSII CDMS ln(χ 2 /DOF) HB, C. Balazs: JCAP 0305, 006 (2003) (numerous other recent χ 2, MCMC fits to find preferred regions) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

4 Ω ez1 h 2 as surface in m 0 vs. m 1/2 space tanβ =, A 0 = 0, µ > 0 (HB, A. Box) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

5 General scan over 19 param. MSSM dimensionful param s defined at M GUT m Q1, m U1, m D1, m L1, m E1 : GeV m Q3, m U3, m D3, m L3, m E3 : GeV M 1, M 2, M 3 : GeV A t, A b, A τ : GeV m Hu, m Hd : GeV tanβ : 2 60 m fw1 > 3.5 GeV m fw1 > 91.9 GeV (wino-like) m h > 111 GeV HB, Box, Summy, JHEP :023,20 Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

6 Why WIMP miracle really is a miracle for SUSY histogram of models vs. Ω ez1 h 2 with m ez1 < 500 GeV Total Number of Models Bino Wino Higgsino Mixed Ωh 2 Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

7 Gravitinos: spin- 3 2 partner of graviton gravitino problem in generic SUGRA models: overproduction of G followed by late G decay can destroy successful BBN predictions unless T R < 5 GeV (see Kawasaki, Kohri, Moroi, Yotsuyanagi; Cybert, Ellis, Fields, Olive; Jedamzik) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

8 Gravitinos as dark matter: again the gravitino problem neutralino production in generic SUGRA models: followed by late time Z 1 G + Xdecays can destroy successful BBN predictions: (see Kawasaki, Kohri, Moroi, Yotsuyanagi) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

9 Origin of strong CP problem QCD U(2) V U(2) A global symmetry (2 light quarks) U(2) V = SU(2) I U(1) B realized; U(2) A broken spontaneously expect 4 Goldstone bosons: πs and η, but instead m η m π : QCD does not respect somehow U(1) A (Weinberg) t Hooft resolution: QCD θ vacuum and instantons theory not U(1) A symmetric, and m η m π explained Generate additional term to QCD Lagrangian: L θ g2 s 32π F µν A violates P and T; conserves C In addition, weak interactions L Arg detm g2 s 32π F µν A θ = θ + Arg detm experiment: neutron EDM θ < How can this be? The strong CP problem F Aµν F Aµν Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

10 PQWW/KSVZ/DFSZ solution to the strong CP problem propose new chiral (Peccei-Quinn) symmetry U PQ (1); U PQ (1) spontaneously broken at scale f a ( 9 12 GeV) requires Goldstone boson field a(x), the axion ( L 1 2 µ a a µ a + f a + θ ) α s 8π F µν F A Aµν V eff (1 cos( θ + a f a )) axion field settles to minimum of potential: a = f a θ offending F F term 0; strong CP problem solved! m 2 a = 2 V eff a 2 with m a 6 µev 12 GeV f a Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15, 2011

11 Axion cosmology Axion field eq n of motion: θ = a(x)/f a θ + 3H(T) θ + 1 V (θ) fa 2 θ = 0 V (θ) = m 2 a(t)fa(1 2 cos θ) Solution for T large, m a (T) 0: θ = const. m a (T) turn-on 1 GeV a(x) oscillates, creates axions with p 0: production via vacuum mis-alignment [ ] 7/6 Ω a h ev 2 m a θ 2 i h 2 astro bound: stellar cooling f a > 9 GeV Ω a h 2 (vacuum mis-alignment) f a /N (GeV) m a (ev) 9 WMAP 5: Ω CDM h 2 = 0.1 ± Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

12 Axion microwave cavity searches ongoing searches: ADMX experiment Livermore U Wash. Phase I: probe KSVZ for m a 6 5 ev Phase II: probe DFSZ for m a 6 5 ev beyond Phase II: probe higher values m a Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

13 We also know MSSM (plus gauge singlets) is compelling effective theory between M weak and M GUT Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

14 PQMSSM: Axions + SUSY mixed aã dark matter? axino is spin- 1 2 element of axion supermultiplet (R-odd; can be LSP) Raby, Nilles, Kim; Rajagopal, Wilczek, Turner â = s+ia 2 + i 2 θã L + i θθ L F a in 4-comp. notation mã model dependent: kev TeV Z 1 ãγ 1 f a /N = 12 GeV non-thermal ã production via Z 1 decay: axinos inherit neutralino number density Ω NTP ã h 2 = m ã m ez1 Ω ez1 h 2 : Covi, Kim, Kim, Roszkowski τ (s) m χ ~ 1 0 (GeV) f a /N = 11 GeV f a /N = GeV f a /N = 9 GeV Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

15 Thermally produced axinos If T R < f a, then axinos never in thermal equilibrium in early universe Can still produce ã thermally via radiation off particles in thermal equilibrium CKKR, BS, Strumia calculation: ( ) ( 3 Ω TP ã h gs 6 11 GeV ln f a /N g s ) 2 ( mã ) ( T R ) 1 GeV 4 GeV (1) TP 2 Ω~ a h = (solid), 0.01 (dashed), 0.1 (dashed-dotted) m~ a (GeV) = (purple), 0.01 (green), 1 (maroon) 9 T R (GeV) m a ~ = (GeV), Ω a ~ TP h 2 = 0.1 m a ~ = 0.01 (GeV), Ω a ~ TP h 2 = f a /N (GeV) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

16 Various leptogenesis scenarios WMAP observation: n b /s 0.9 : how to generate? SM EW baryogenesis ruled out; SUSY EWB nearly so Thermal leptogenesis very attractive but needs T R > mn1 > 2 9 GeV (Buchmuller, Plumacher); Naive conflict with upper bound on T R from BBN/gravitino problem Alternatively, one may have non-thermal leptogenesis where inflaton φ N i N i decay (Lazarides, Shafi; Kumekawa, Moroi, Yanagida) additional source of N i in early universe allows lower T R : ( ) ( ) n B s 8.2 TR 2mN1 ( mν3 ) 11 6 δ eff (2) GeV 0.05 ev Also, AD leptogenesis in φ = Hl D-flat direction: wide range of T R allowed (Dine, Randall, Thomas; Murayama, Yanagida) m φ Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

17 msugra model with mixed axion/axino CDM: mã fixed (m 0, m 1/2, A 0, tanβ, sgn(µ)) = (00 GeV, 300 GeV, 0,, +1) Ω a h 2 + Ωã TPh2 + Ω NTP ã h 2 = 0.11 model with mainly axion CDM seems favored! Ωh m a ~ = 0 kev (solid), 1 MeV (dashed) 7 WMAP Ω CDM h 2 TP 2 Ω~ a h NTP 2 Ω a ~ h Ω a h 2 (a) f a /N (GeV) T R (GeV) (b) f a /N (GeV) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

18 msugra p-space with mainly axion cold DM contours of log T R : msugra w/ tan β =, A 0 = 0 T R > 6 consistent with non-thermal leptogenesis most dis-favored msugra regions with neutralino DM are most favored by msugra with mainly axion DM! (HB, Box, Summy) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

19 Axion/axino relic density in msugra: low fine-tune! Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

20 Reconcile thermal leptogenesis with G problem? need m G > TeV to avoid BBN constraints Yukawa-unified SUSY, Effective SUSY, AMSB, mirage unification invoke aã DM with ã = LSP to avoid overproduction of Z 1 s suppress thermal axino overproduction with large f a /N > 12 GeV suppress axion overproduction via misalignment angle θ i < 1 avoid BBN constraints on late decaying Z 1 ã + hadrons low rate Z 1 production Ω e Z 1 < 0.1 bino-like Z 1 γã with τ( Z 1 ) < 200 sec. Does it work? Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

21 BBN constraints on late decaying neutrals (Jedamzik) results for m X = 0 GeV 3 2 B h = 0 1 Ω X h τ (sec) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

22 Scan over PQMSSM parameters for Eff. SUSY model HB, Kraml, Lessa, Sekmen JCAP11 (20) 040 (also works well for Mirage Mediation) BM1, m ~ = 20 TeV BBN safe BBN excluded G T R = 2 GeV min 9 T R (GeV) p = 5 T dc TR f 11 (GeV) a Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

23 What about cosmology of saxion field s(x)? HB, Kraml, Lessa, Sekmen [JCAP14 (2011)039] saxion production in early universe Thermal production: coherent oscillations: -2 tot Y s TP Y s coh Y s -3 T R > T dec m s = 0 GeV -4 T R <T dec m s = 1 TeV Y s = T R GeV f /N (GeV) a Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

24 Saxion decay s gg, g g; s aa more model dependent, but may dominate T s = temp at which saxion entropy injection nearly complete T s 0.78g 1/4 Γs M Pl = 1 TeV, f a /N = m s GeV 8 Γ(s g ~ g ~ ) Γ (GeV) 6 4 Γ(s gg) m g ~ (GeV) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

25 Saxion domination and entropy T e = temp at which saxion density equals radiation If T s < T e, then saxions may dominate universe Entropy from saxion decay: r = S f /S i T e /T s (Scherrer, Turner) m s = 1 TeV r = 1-3 T (GeV) r = 1 T s T e T s T e (f 12 /N = GeV) a 12 (f /N = GeV) a 14 (f /N = GeV) a 14 (f /N = GeV) a T R 8 (GeV) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

26 Dilution of relics due to saxion decay If r > 1, saxions can dominate universe Entropy injection may dilute relics (including baryon asymmetry!) Beware BBN constraints on late decaying particles (Jedamzik) Must calculate relic abundances in RD, MD or DPD universe s i = f a m s = 0 GeV m s = 1 TeV m s = TeV BBN excluded r = 0 (GeV) T R 11 r = T R > T dec r = f /N (GeV) a Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

27 Aside: can we allow f a M GUT? Yes, but need m s 50 TeV (HB, A. Lessa, JHEP16 (2011) 027) 1 m = 150 GeV, Ω 2 h Z ~ Z ~ 1 1 =, m G ~ = 1 TeV, m s 2 h Ω a = 50 TeV, m~ a = 0 kev BBN excluded -2 2 Ω h -4 Ω TP 2 h Z ~ -6 TP 2 Ωa~ h Ω TP 2 h G ~ f a 15 (GeV) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

28 What if mã > m ez1 so Z 1 = LSP? Expect mixed axion/neutralino CDM: which will dominate? Neutralinos produced thermally as usual (RD, MD or DD universe) Axino production and decay (e.g. ã Z 1 γ) will augment neutralino production. Decay produced Z 1 s at temp T D = ΓãM P /(π 2 g (T D )/90) 1/4 can re-annihilate if σv n e Z 1 (T D ) > H(T D ) Axions produced as usual via vacuum misalignment (but evaluate in RD, MD or DD universe); can be diluted by entropy from axino decay Neglecting saxions, expect to work best for models with too low of usual thermal abundance (wino-like or higgsino-like neutralinos) HB, Lessa, Rajagopalan, Sreethawong, JCAP16 (2011) 031 Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

29 Z 1 = wino from gaugino AMSB model Expect mixed axion/neutralino CDM: which will dominate? 4 3 inoamsb, m 3/2 = 50 TeV, tanβ =, f a /N = 12 GeV, T R = GeV, θ i = Ω Z ~ 1 h2 Ω a h 2 Ω tot h 2 2 T D = T fr Ωh BBN -1-2 Ω DM h m a ~ [GeV] Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

30 Z 1 = wino from gaugino AMSB model f a /N [GeV] inoamsb, m 3/2 = 50 TeV, tanβ =, T R = GeV, θ i = Ω tot h 2 > 1 < Ω tot h 2 < < Ω tot h 2 < < Ω tot h 2 < < Ω tot h 2 < 0.88 Ω tot h 2 < 0.01 T D = T fr m a ~ [GeV] Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

31 In case Z 1 = wino from AMSB, see at Xe-0, 1-ton Assume CDM is wino dominated Distinct lower limit to σ SI ( Z 1 p) unlike SUGRA HB, Demisek, Rajagopalan, Summy, JCAP07 (20) 014 Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

32 σ SI [pb] HCAMSB tanβ = HCAMSB tanβ = 40 mamsb tanβ = mamsb tanβ = 40 inoamsb tanβ = inoamsb tanβ = 40 CDMS XENON 0 LUX 300 XENON 0 upgrade XENON 1 ton [GeV] m Z ~ 1 Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

33 Coupled Boltzmann calculation of mixed a/bino CDM Include σv (T) Include neutralino production/entropy injection from both axino/saxion decay HB, A. Lessa, W. Sreethawong, arxiv: (2011) ) 4 ρ (GeV T R = GeV 12 f = GeV a = m = 1 TeV G ~ m a ~ m s θ i = 5 TeV = 0.5, θ s = 1 T = 0.5 GeV T = MeV ρ ρ R Z ~ 1 ρ (TP) a ρ (CO) a ρ (TP) s ρ (CO) s ρ~ (TP) a ρ ~ (TP) G T (GeV) ρ (MSSM) Z ~ R/R 0 Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

34 Mixed a/bino CDM: coupled Boltzmann calculation saxion entropy versus gluino injection only BBN challenged points have low enough relic density (m, m, A 0 1/2 0, tanβ, µ) = (400 GeV, 400 GeV, 0,, > 0) BBN Allowed BBN Excluded 2 h Z ~ 1 Ω -1-3 Ω 2 h Z ~ 1 = f 12 a (GeV) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

35 can allow f a GeV! Mixed a/bino CDM: A-funnel DM tends to be neutralino rather than axion dominated at large f a (m, m, A 0 1/2 0, tanβ, µ) = (400 GeV, 400 GeV, 0, 55, > 0) BBN Allowed BBN Excluded 2 h Z ~ 1 Ω -1-3 Ω 2 h Z ~ 1 = f 12 a (GeV) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

36 can allow f a GeV! Mixed a/wino CDM: AMSB either neutralino or axion domination possible inoamsb (m, m, A 0 1/2 0, tanβ, µ) = (0 GeV, GeV, 0,, > 0) BBN Allowed BBN Excluded 2 h Z ~ 1 Ω -1-3 Ω 2 h Z ~ 1 = f 12 a (GeV) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

37 Mixed a/ b h CDM: focus point can allow f a GeV! DM tends to be neutralino rather than axion dominated at large f a (m, m, A, tanβ, µ) = (4525 GeV, 275 GeV, 0,, > 0) 0 1/2 0 9 BBN Allowed 7 BBN Excluded h Z ~ 1 Ω -1-3 Ω 2 h Z ~ 1 = f a 13 (GeV) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,

38 Conclusions SUSY WIMP-only CDM suffers 3 problems: too much or too little CDM; G problem; strong CP problem PQ strong CP solution + SUSY: need both mixed axion/axino CDM if ã is LSP then low fine-tuning of Ω aã h 2 T R 6 11 possible: solve gravitino problem if m G > 5 TeV allow for non-thermal (possibly thermal) leptogenesis The case f a M GUT allowed for mixed aã DM Mixed a Z 1 CDM: wino or higgsino DM enhanced by ã, s decay Mixed a Z 1 CDM: overabundant binos mainly enhanced by axino/saxion decays (unless BBN-challenged) Howard Baer, PittPAC dark matter meeting, University of Pittsburgh, November 15,