Asymmetric dark matter from. and New Strong Dynamics. Mads Toudal Frandsen Rudolf Peierls Centre for Theoretical Physics

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1 Asymmetric dark matter from and New Strong Dynamics Rudolf Peierls Centre for Theoretical Physics November 5 th 2010

2 What is the world made of?

3 What is the world made of? Baryons but no antibaryons Baryon mass (mainly) from strong dynamics Ω DM /Ω B ~ O(1)

4 What should the world be made of? Mass scale Particle Symmetry/ Quantum # Λ QCD Baryons U(1) baryon number Stability Production Abundance > yr (dim-6 OK) freeze-out from thermal equilibrium asymmetry Chemical equilibrium maintained when annihilaton rate exceeds the Hubble expansion rate Ω B ~10-10 Ω B ~ 0.05 Freeze-out at T ~ m N /45, with: Have to invoke an asymmetry: Observed ratio is 10 9 times bigger: A 'baryon disaster'?!

6 Sakharov conditions for baryogenesis: 1. Baryon number violation 2. C and CP violation 3. Departure from thermal equilibrium Any pre-existing fermion asymmetry would be redistributed by the B+L violating processes (which conserve B-L) : The fermion number N i terms of the statistical function c i and the Chemical potential μ is: The fermion number violating processes (sphalerons) create equal number of fermion doublets: (Bahr, Chivukula & Farhi 90; Harvey and Turner 90)

8 What should the world be made of? Mass scale Particle Symmetry/ Quantum # Stability Production Abundance Λ QCD Nucleons U(1) baryon number > yr (dim-6 OK) freeze-out from thermal equilibrium asymmetry Ω B ~10-10 Ω B ~ 0.05 Λ Fermi ~ G F -1/2 Neutralino? R-parity? violated? freeze-out from thermal equilibrium Ω LSP ~ 0.3 In (softly broken) susy we could have a WIMP miracle : But why then is the abundance of thermal relics comparable to that of baryons born non-thermally, with Ω DM /Ω B ~ 5?

9 A TeV scale particle sharing the asymmetry (e.g. a technibaryon) could explain the ratio of dark to baryonic matter... (Nussinov 1985) Even more naturally is a ~ 5 GeV particle (e.g. a 'dark baryon' from a hidden strong sector) (Gelmini et al 87, Raby and West 87, DB Kaplan 92, Hooper et al 05, Kitano and Low 05, DE Kaplan et al 09, Kribs et al 09, Sannino and Zwicky 09, An et al 10, M.T.F & Sarkar 10,...) Mass scale Particle Symmetry/ Quantum # Λ QCD Nucleons U(1) baryon number Λ TC ~ Λ Fermi Λ DB ~5 Λ QCD Technibaryon? Dark Baryon? (Bahr, Chivukula and Farhi 90) U(1) techibaryon U(1) dark baryon number? Stability Production Abundance > yr (dim-6 OK) freeze-out from thermal equilibrium Asymmetry Ω B ~10-10 Ω B ~ 0.05 Asymmetry Ω TC ~ 0.3 Ω DB ~ 0.3 Is it natural to have similar initial asymmetry in the visible and dark sector?

10 Sakharov conditions for baryogenesis: 1. Baryon number violation 2. C and CP violation 3. Departure from thermal equilibrium Any pre-existing fermion asymmetry would be redistributed by the B+L violating processes (which conserve B-L) : The fermion number N i terms of the statistical function c i and the Chemical potential μ is: The fermion number violating processes (sphalerons) create equal number of fermion doublets: (Bahr, Chivukula & Farhi 90; Harvey and Turner 90)

If composite ADM is electrically neutral but has constituents with EW charges, sphalerons may distribute the asymmetry among baryons and dark matter Can we construct natural explicit models?

11 If composite ADM is electrically neutral but has constituents with EW charges, sphalerons may distribute the asymmetry among baryons and dark matter Can we construct natural explicit models? EW scale ADM from Technicolor models Minimal (Walking) Technicolour GeV scale ADM e.g. from a Dark mirror sector/world Technicolour breaks the electroweak symmetry and the technifermions can form composite ADM A dark mirror sector (e.g. a complete copy of the SM) is coupled via Higgs-Mirror Higgs and heavy right handed neutrinos which generate neutrino masses in the SM and provide leptogenesis of matter in the SM as well as ADM from the mirror sector

12 and LHC Phenomenology LAPTh Annecy-le-Vieux, November 5 th 2010 m.frandsen1@physics.ox.ac.uk

13 Outline 1 Technicolor and Technibaryon Dark Matter 2 3

14 Technicolor Technicolor: (Weinberg 78, Susskind 78) 1 In the SM without a Higgs, QCD breaks the EW symmetry: ū L u R + d L d R 0 M W = gf π 2. 2 Consider a new strongly interacting gauge theory with F TC Π = v EW = 246GeV. 3 Let the electroweak gauge group be a subgroup of the chiral symmetry group.

15 Technicolor Technicolor: (Weinberg 78, Susskind 78) 1 In the SM without a Higgs, QCD breaks the EW symmetry: ū L u R + d L d R 0 M W = gf π 2. 2 Consider a new strongly interacting gauge theory with F TC Π = v EW = 246GeV. 3 Let the electroweak gauge group be a subgroup of the chiral symmetry group. Example: Scaled-up QCD!

16 Technicolor 1 The SM gauge group is augmented: G SM SU(3) c SU(2) W U(1) Y G TC.

17 Technicolor 1 The SM gauge group is augmented: G SM SU(3) c SU(2) W U(1) Y G TC. 2 The Higgs sector of the SM is replaced: L Higgs 1 4 F a µν F aµν + i Q L γ µ D µ Q L + i Q R γ µ D µ Q R +...

18 Technicolor 1 The SM gauge group is augmented: G SM SU(3) c SU(2) W U(1) Y G TC. 2 The Higgs sector of the SM is replaced: L Higgs 1 4 F a µν F aµν + i Q L γ µ D µ Q L + i Q R γ µ D µ Q R +... Minimal chiral symmetries: 3 GB s + Custodial + DM. SU L (2) SU R (2) U TB (1) SU V (2) U TB (1).

19 Technicolor dark matter Technocosmology (Nussinov 85) Lightest Technibaryon as Asymmetric Dark Matter

20 Technicolor dark matter Technocosmology (Nussinov 85) Lightest Technibaryon as Asymmetric Dark Matter The LTB abundance: Ω TB /Ω B = m TB /m B n TB /n B

21 Technicolor dark matter Technocosmology (Nussinov 85) Lightest Technibaryon as Asymmetric Dark Matter The LTB abundance: From initial n B n TB : Ω TB /Ω B = m TB /m B n TB /n B Ω TB /Ω B m TB /m B (m TB /T sphaleron ) 3/2 e m TB/T sphaleron T sphaleron v EW, (Chivukula and Walker 90; Bahr, Chivukula and Farhi 90; Harvey and Turner 90; Ellis et al 95; Sarkar 95; Gudnason, Kouvaris and Sannino 05)

22 Technicolor dark matter Technocosmology (Nussinov 85) Lightest Technibaryon as Asymmetric Dark Matter The LTB abundance: From initial n B n TB : Ω TB /Ω B = m TB /m B n TB /n B Ω TB /Ω B m TB /m B (m TB /T sphaleron ) 3/2 e m TB/T sphaleron T sphaleron v EW, M TB TeV (Chivukula and Walker 90; Bahr, Chivukula and Farhi 90; Harvey and Turner 90; Ellis et al 95; Sarkar 95; Gudnason, Kouvaris and Sannino 05)

23 Technicolor dark matter Technocosmology (Nussinov 85) Lightest Technibaryon as Asymmetric Dark Matter The LTB abundance: From initial n B n TB : Ω TB /Ω B = m TB /m B n TB /n B Ω TB /Ω B m TB /m B (m TB /T sphaleron ) 3/2 e m TB/T sphaleron T sphaleron v EW, M TB TeV (Chivukula and Walker 90; Bahr, Chivukula and Farhi 90; Harvey and Turner 90; Ellis et al 95; Sarkar 95; Gudnason, Kouvaris and Sannino 05) Scaled up technineutron now ruled out by recoil experiments σ TN,p cm 2

24 Extended Technicolor and fermion masses ETC ETC: (Eichten and Lane 80) New gauge theory with SM and TC fermions in the same multiplet. ψ L, QL Q L Q R ψ R,Q R

25 Extended Technicolor and fermion masses ETC ψ L, QL Q L Q R ψ R,Q R

26 Extended Technicolor and fermion masses ETC ψ L, QL Q L Q R ψ R,Q R 1 Four fermion operators: QQ QQ α Λ 2 ETC QQ ψψ + β + γ Λ 2 ETC ψψ ψψ Λ 2 ETC (Too!) Generically Λ ETC > 10 3 TeV to suppress FCNC s: (King 89; Evans and Ross 94; Appelquist and Shrock 02; Evans and Sannino 05; Christensen, Piai and Shrock 06)

27 Extended Technicolor and fermion masses ETC ψ L, QL Q L Q R ψ R,Q R 1 Four fermion operators: QQ QQ α Λ 2 ETC QQ ψψ + β + γ Λ 2 ETC ψψ ψψ Λ 2 ETC (Too!) Generically Λ ETC > 10 3 TeV to suppress FCNC s: (King 89; Evans and Ross 94; Appelquist and Shrock 02; Evans and Sannino 05; Christensen, Piai and Shrock 06) 3 Focus on Technicolor sector

28 Constraints from LEP 1 A minimal matter content in the TC sector is favored: S 16πΠ W 3 B (0), T 4π s 2 W c2 W M2 Z (Π W 1 W 1(0) Π W 3 W 3(0)) Q, L W 3 B U 0 m t = ± 2.1 GeV m H = GeV m W prel. T 0 Γ ll d(r S naive = N TC ) -0.2 D 6π S = S naive (1 + δ) -0.4 sin 2 θ lept eff m H m t 68 % CL S (Kennedy and Lynn 89; Peskin and Takeuchi 90; Altarelli and Barbieri 91)

29 Minimal Technicolor Theory Space 2 EW charged Dirac Flavors. No QCD charges. ( ) Q L = U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ.

30 Minimal Technicolor Theory Space 2 EW charged Dirac Flavors. No QCD charges. ( ) Q L = U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. Orthogonal TC QCD TC Symplectic TC

31 Minimal Technicolor Theory Space 2 EW charged Dirac Flavors. No QCD charges. ( ) Q L = U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. Orthogonal TC R real QCD TC R complex Symplectic TC R pseudo-real

32 Minimal Technicolor Theory Space 2 EW charged Dirac Flavors. No QCD charges. ( ) Q L = U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. Orthogonal TC R real F of SO(N) QCD TC R complex F of SU(N) Symplectic TC R pseudo-real F of Sp(2N)

33 Minimal Technicolor Theory Space 2 EW charged Dirac Flavors. No QCD charges. ( ) Q L = U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. Orthogonal TC R real F of SO(N) SU(4)/SO(4) QCD TC R complex F of SU(N) G GB : SU(2) Symplectic TC R pseudo-real F of Sp(2N) SU(4)/Sp(4)

34 Minimal Technicolor Theory Space 2 EW charged Dirac Flavors. No QCD charges. ( ) Q L = U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. Orthogonal TC R real F of SO(N) SU(4)/SO(4) 3 Π 3 3 QCD TC R complex F of SU(N) G GB : SU(2) 3 Π Symplectic TC R pseudo-real F of Sp(2N) SU(4)/Sp(4) 3 Π 1 1

35 Minimal Technicolor Theory Space 2 EW charged Dirac Flavors. No QCD charges. ( ) Q L = U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. Orthogonal TC R real F of SO(N) SU(4)/SO(4) 3 Π 3 3 ( ) Π Ti T i Π T QCD TC R complex F of SU(N) G GB : SU(2) 3 Π ( Π 0 Π Π = + ) Π Π 0 Symplectic TC R pseudo-real F of Sp(2N) SU(4)/Sp(4) 3 Π 1 1 ( ) Π Ts Ts Π T

36 Minimal Technicolor Theory Space 2 EW charged Dirac Flavors. No QCD charges. ( ) Q L = U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. Orthogonal TC R real F of SO(N) SU(4)/SO(4) 3 Π 3 3 ( ) Π Ti T i Π T ( T 0 T T i = + ) T T 0 QCD TC R complex F of SU(N) G GB : SU(2) 3 Π ( Π 0 Π Π = + ) Π Π 0 Symplectic TC T s = R pseudo-real F of Sp(2N) SU(4)/Sp(4) 3 Π 1 1 ( ) Π Ts T s Π T ( ) T T 0

37 Dark Matter from Minimal Technicolor TIMP: Complex scalar, charged under the U(1) TB symmetry Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. (1)

38 Dark Matter from Minimal Technicolor TIMP: Complex scalar, charged under the U(1) TB symmetry Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. (1) itimp TIMP TIMP (M.T.F and F.Sannino 09) (Bahr, Chivukula and Farhi 90; Nussinov 92) (Ryttov and Sannino 08; Foadi, M.T.F and Sannino 09)

39 Dark Matter from Minimal Technicolor TIMP: Complex scalar, charged under the U(1) TB symmetry Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. (1) itimp TIMP 4 of SU(4) TIMP (M.T.F and F.Sannino 09) (Bahr, Chivukula and Farhi 90; Nussinov 92) (Ryttov and Sannino 08; Foadi, M.T.F and Sannino 09)

40 Dark Matter from Minimal Technicolor TIMP: Complex scalar, charged under the U(1) TB symmetry Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. (1) itimp TIMP 4 of SU(4) U L D L U L D L TIMP (M.T.F and F.Sannino 09) (Bahr, Chivukula and Farhi 90; Nussinov 92) (Ryttov and Sannino 08; Foadi, M.T.F and Sannino 09)

41 Dark Matter from Minimal Technicolor TIMP: Complex scalar, charged under the U(1) TB symmetry Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. (1) itimp TIMP 4 of SU(4) U L D L U L D L SM singlet TIMP (M.T.F and F.Sannino 09) (Bahr, Chivukula and Farhi 90; Nussinov 92) (Ryttov and Sannino 08; Foadi, M.T.F and Sannino 09)

42 Dark Matter from Minimal Technicolor TIMP: Complex scalar, charged under the U(1) TB symmetry Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. (1) itimp (M.T.F and F.Sannino 09) TIMP 4 of SU(4) U L D L U L D L SM singlet M T N 3/2 TC F Π (Bahr, Chivukula and Farhi 90; Nussinov 92) TIMP (Ryttov and Sannino 08; Foadi, M.T.F and Sannino 09)

43 Dark Matter from Minimal Technicolor TIMP: Complex scalar, charged under the U(1) TB symmetry Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. (1) itimp (M.T.F and F.Sannino 09) TIMP 4 of SU(4) U L D L U L D L SM singlet M T N 3/2 TC F Π (Bahr, Chivukula and Farhi 90; Nussinov 92) TIMP (Ryttov and Sannino 08; Foadi, M.T.F and Sannino 09)

44 Dark Matter from Minimal Technicolor TIMP: Complex scalar, charged under the U(1) TB symmetry Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. (1) itimp R real (M.T.F and F.Sannino 09) TIMP 4 of SU(4) U L D L U L D L SM singlet M T N 3/2 TC F Π (Bahr, Chivukula and Farhi 90; Nussinov 92) TIMP R pseudo-real (Ryttov and Sannino 08; Foadi, M.T.F and Sannino 09)

45 Dark Matter from Minimal Technicolor TIMP: Complex scalar, charged under the U(1) TB symmetry Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. (1) itimp R real T 0 U L D L (M.T.F and F.Sannino 09) TIMP 4 of SU(4) U L D L U L D L SM singlet M T N 3/2 TC F Π (Bahr, Chivukula and Farhi 90; Nussinov 92) TIMP R pseudo-real T 0 U L D L (Ryttov and Sannino 08; Foadi, M.T.F and Sannino 09)

46 Dark Matter from Minimal Technicolor TIMP: Complex scalar, charged under the U(1) TB symmetry Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. (1) itimp R real T 0 U L D L Iso-spin 0 GB (M.T.F and F.Sannino 09) TIMP 4 of SU(4) U L D L U L D L SM singlet M T N 3/2 TC F Π (Bahr, Chivukula and Farhi 90; Nussinov 92) TIMP R pseudo-real T 0 U L D L SM singlet GB (Ryttov and Sannino 08; Foadi, M.T.F and Sannino 09)

47 Dark Matter from Minimal Technicolor TIMP: Complex scalar, charged under the U(1) TB symmetry Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. (1) itimp R real T 0 U L D L Iso-spin 0 GB M T 0 g F Π (M.T.F and F.Sannino 09) TIMP 4 of SU(4) U L D L U L D L SM singlet M T N 3/2 TC F Π (Bahr, Chivukula and Farhi 90; Nussinov 92) TIMP R pseudo-real T 0 U L D L SM singlet GB M 2 T 0 g 2 F 2 Π (Ryttov and Sannino 08; Foadi, M.T.F and Sannino 09)

48 Dark Matter from Minimal Technicolor TIMP: Complex scalar, charged under the U(1) TB symmetry Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ. (1) itimp R real T 0 U L D L Iso-spin 0 GB M T 0 g F Π TIMP 4 of SU(4) U L D L U L D L SM singlet M T N 3/2 TC F Π TIMP R pseudo-real T 0 U L D L SM singlet GB M 2 T 0 g 2 F 2 Π (M.T.F and F.Sannino 09) (Bahr, Chivukula and Farhi 90; Nussinov 92) (Ryttov and Sannino 08; Foadi, M.T.F and Sannino 09) (Other candidates in MT: Gudnason, Kouvaris and Sannino 05; Kainulainen, Virkajärvi and Tuominen 06, 09, 10; Kouvaris 07; Khlopov and Kouvaris 08)

49 Direct detection Charge radius L B = ie d B Λ 2 T µ T ν F µν. (Bagnasco, Dine and Thomas 93) T γ T T H T N N N N Composite Higgs L Yuk H = d Hv ev T TH or L GB H = d 13 Λ H µt µ T. (M.T.F and Sannino 09)

50 Direct detection Charge radius L B = ie d B Λ 2 T µ T ν F µν. (Bagnasco, Dine and Thomas 93) T γ T T H T N N N N Composite Higgs L Yuk H = d Hv ev T TH or L GB H = d 13 Λ H µt µ T. (M.T.F and Sannino 09) For colored baryons: Gluonic polarizabilities (Nussinov 92 ; Chivukula et al 92)

51 Direct detection Charge radius L B = ie d B Λ 2 T µ T ν F µν. (Bagnasco, Dine and Thomas 93) T γ T T H T N N N N Composite Higgs L Yuk H = d Hv ev T TH or L GB H = d 13 Λ H µt µ T. (M.T.F and Sannino 09) For colored baryons: Gluonic polarizabilities (Nussinov 92 ; Chivukula et al 92) For spin-1/2 baryons: Dipole moments (Nussinov 92 ; Bagnasco, Dine and Thomas 93)

52 Direct Detection Limits on TIMPs Σnucleon cm TeV d12 3 mh db CDMS Ge XENON m T GeV (Foadi, M.T.F and Sannino 09; Belyaev, M.T.F, Sannino and Sarkar; Exclusion limits courtesy of C. Mccabe 10)

53 Direct Detection Limits on TIMPs Σnucleon cm TeV d12 3 mh db CDMS Ge XENON m T GeV (Foadi, M.T.F and Sannino 09; Belyaev, M.T.F, Sannino and Sarkar; Exclusion limits courtesy of C. Mccabe 10) Indirect detection of Decaying Dark Matter: (Nardi, Sannino and Strumia 09)

54 LHC signatures of (i)timps q Z,R 1,2 H T T (i)timp Invisible Higgs (Foadi, M.T.F and Sannino 08 ; Godbole, Guchait, Mazumdar, Moretti and Roy 03). q Z l + l

55 LHC signatures of (i)timps q Z,R 1,2 H T T (i)timp Invisible Higgs (Foadi, M.T.F and Sannino 08 ; Godbole, Guchait, Mazumdar, Moretti and Roy 03). q Z l + l itimp Antlers q W ± (M.T.F and Sannino 09 ; Han, Kim and Song 09) T Z,R ± 1,2 T 0 q T ± W T 0

56 LHC signatures of (i)timps q Z,R 1,2 H T T (i)timp Invisible Higgs (Foadi, M.T.F and Sannino 08 ; Godbole, Guchait, Mazumdar, Moretti and Roy 03). itimp Antlers (M.T.F and Sannino 09 ; Han, Kim and Song 09) q q q Z T Z,R ± 1,2 Note: The same signatures from a new stable heavy lepton! (M.T.F, Masina and Sannino 09 ; Antipin, Heikinheimo, Tuominen 09) T ± W ± W l + l T 0 T 0

57 (i)timp missing energy signals q Z,R 1,2 H Z q T T l + l Number of events/5 100 fb WW 10 1 ZZ M H =160 M H =200 M H =300 M A =500,gt=5,S= Missing p T (GeV) Number of events/5 100 fb WW 10 1 ZZ M H =160 M H =300 M H =450 M A =750,gt=5,S= Missing p T (GeV) (Foadi, M.T.F and Sannino 08; Godbole, Guchait, Mazumdar, Moretti and Roy 03).

58 Walking Technicolor 1 TC sector: Walking reduces the full S-parameter (Sundrum and Hsu 92; Appelquist and Sannino 98; Harada, Kurachi and Yamawaki 03; Kurachi and Shrock 06)

59 Walking Technicolor 1 TC sector: Walking reduces the full S-parameter (Sundrum and Hsu 92; Appelquist and Sannino 98; Harada, Kurachi and Yamawaki 03; Kurachi and Shrock 06) 2 ETC sector: Walking reduces tension between SM fermion masses and FCNC s (Holdom 81, 85; Yamawaki, Bando and Matumoto 86; Appelquist, Karabali and Wijewardhana 86)

60 Conformal window and Walking (Fig:Sannino, cp3-origins 09)

61 ETC fermion masses and Walking 1 Four fermion operators: α QQ QQ Λ 2 ETC QQ ψψ ψψ ψψ + β Λ 2 + γ ETC Λ ETC

62 ETC fermion masses and Walking 1 Four fermion operators: α QQ QQ Λ 2 ETC 2 Fermion masses: QQ ψψ ψψ ψψ + β Λ 2 + γ ETC Λ ETC M ψ QQ ETC Λ 2 ETC d(r TC ) Λ3 γ TC Λγ ETC Λ 2 ETC

63 ETC fermion masses and Walking 1 Four fermion operators: α QQ QQ Λ 2 ETC 2 Fermion masses: QQ ψψ ψψ ψψ + β Λ 2 + γ ETC Λ ETC M ψ QQ ETC Λ 2 ETC d(r TC ) Λ3 γ TC Λγ ETC Λ 2 ETC 3 Condensate enhancement from Walking: < QQ > ETC ( Λ ETC Λ TC ) γ(α ) < QQ > TC (Holdom 81, 85; Yamawaki, Bando and Matumoto 86; Appelquist, Karabali and Wijewardhana 86)

64 ETC fermion masses and Walking 1 Four fermion operators: α QQ QQ Λ 2 ETC 2 Fermion masses: QQ ψψ ψψ ψψ + β Λ 2 + γ ETC Λ ETC M ψ QQ ETC Λ 2 ETC d(r TC ) Λ3 γ TC Λγ ETC Λ 2 ETC 3 Condensate enhancement from Walking: < QQ > ETC ( Λ ETC Λ TC ) γ(α ) < QQ > TC (Holdom 81, 85; Yamawaki, Bando and Matumoto 86; Appelquist, Karabali and Wijewardhana 86) 4 (Too) Naively Λ ETC > 10 3 TeV to suppress FCNC s: (King 89; Evans and Ross 94; Appelquist and Shrock 02; Evans and Sannino 05; Christensen, Piai and Shrock 06)

65 Analytical approaches to the conformal window 3C 2 (R), α 4π = β 0 β 1. (Appelquist, Lane and Muhanta 88; Cohen and Georgi 89; Sannino and 1 Ladder approximation: α c = π Tuominen 04; Dietrich and Sannino 06; Ryttov and Sannino 07) 2 All-orders beta function conjecture(s) (Ryttov and Sannino 08; Antipin and Tuominen 09; Dietrich 09) 3 Dualities (Sannino 09) 4 Compactification approach (Unsal and Poppitz 09; Ogilvie and Myers 09;) 5 Worldline formalism (Armoni 09) 6 Holography (Hong and Yee 06; Alvares, Evans, Gebauer and Weatherill 09) 7 Metric Confinenement MC and Causal Analytic couplings (Oehme and Zimmerman 80; Nishijima 86; Oehme 1990; Gardi and Grunberg 98; M.T.F, Pickup and Teper 10)

66 Conformal window lower bounds: MC and AO N f N f Fundamental rep I N f II,SD N f II,MC N f CA N f II,AO N f N C 2 index symmetric rep N f N f Adjoint rep N C AS N C (M.T.F, T. Pickup and M. Teper 10) N C

67 Some Minimal Models of Walking Technicolor Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ.. (2)

68 Some Minimal Models of Walking Technicolor Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ.. (2) MWT model: (Sannino and Tuominen 04) G TC = SU(2). R = Adj. Leptons. (Dietrich, Sannino and Tuominen 05)

69 Some Minimal Models of Walking Technicolor Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ.. (2) MWT model: (Sannino and Tuominen 04) G TC = SU(2). R = Adj. Leptons. (Dietrich, Sannino and Tuominen 05) OMT model G TC = SO(4) NMWT model G TC = SU(3) UMT model G TC = SU(2) (M.T.F and F.Sannino 09) (Sannino and Tuominen 04) (Ryttov and Sannino 08)

70 Some Minimal Models of Walking Technicolor Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ.. (2) MWT model: (Sannino and Tuominen 04) G TC = SU(2). R = Adj. Leptons. (Dietrich, Sannino and Tuominen 05) OMT model G TC = SO(4) R = F (M.T.F and F.Sannino 09) NMWT model G TC = SU(3) R = 2S (Sannino and Tuominen 04) UMT model G TC = SU(2) R = F,Adj (Ryttov and Sannino 08)

71 Some Minimal Models of Walking Technicolor Q L = ( ) U +1/2 L,D 1/2 T +1/2 L, U R, D 1/2 R ; λ.. (2) MWT model: (Sannino and Tuominen 04) G TC = SU(2). R = Adj. Leptons. (Dietrich, Sannino and Tuominen 05) OMT model G TC = SO(4) R = F itimp (M.T.F and F.Sannino 09) NMWT model G TC = SU(3) R = 2S (Sannino and Tuominen 04) UMT model G TC = SU(2) R = F,Adj TIMP (Ryttov and Sannino 08)

72 Conformal window lower bounds: MC and AO N f N f Fundamental rep I N f II,SD N f II,MC N f CA N f II,AO N f N C 2 index symmetric rep N f N f Adjoint rep N C AS N C (M.T.F, T. Pickup and M. Teper 10) N C

73 Lattice simulations (Dedicated collaborations: Lattice Strong Dynamics (US) ; Strong BSM (EU) )

74 EFT for strong LHC common sector: SU L (2) SU R (2) U TB (1) SU V (2) U TB (1). New states: Lightest (axial)-vector triplets and scalar R ±,0 1, R ±,0 2, H. TIMPs Input parameters and constraints: Main free parameters: e, G F, M Z ; S, Sum Rules. M A, g, M H. (Appelquist, Da Silva and Sannino 99; Foadi, M.T.F, Ryttov and Sannino

75 EFT for strong LHC common sector: SU L (2) SU R (2) U TB (1) SU V (2) U TB (1). New states: Lightest (axial)-vector triplets and scalar R ±,0 1, R ±,0 2, H. TIMPs Input parameters and constraints: Main free parameters: e, G F, M Z ; S, Sum Rules. M A, g, M H. (Appelquist, Da Silva and Sannino 99; Foadi, M.T.F, Ryttov and Sannino EFTs for BESS models, 3-site/4-site models and LSTC (Casalbuoni, Deandrea, De Curtis, Dominici, Gatto, Grazzini 95; He et al 08; Lane and Martin 09)

76 Parameter space (Foadi, M.T.F and Sannino 07 ; Belyaev, Foadi, M.T.F, Järvinen, Pukhov, Sannino 08)

77 Mass spectrum, imposing S and WSR1 Mass Spectrum (TeV) R ± 2,0 0.6 R 1 ±,0 S=0.3 g = M A (TeV) Mass Spectrum (TeV) R ± 2,0 0.6 R 1 ±,0 S=0.3 g = M A (TeV) Figure: R 1,2 spectrum. (Foadi, M.T.F, Ryttov and Sannino 08)

78 LHC Phenomenology Basic phenomenology controlled by g, M A, M H. g/ g R 1,2 g R 1,2

79 LHC Phenomenology Basic phenomenology controlled by g, M A, M H. g/ g R 1,2 g R 1,2 Different decay channels probe R 1,R 2 and H.

80 LHC Phenomenology Basic phenomenology controlled by g, M A, M H. g/ g R 1,2 g R 1,2 Different decay channels probe R 1,R 2 and H. Di-lepton: R 0 1,2 l+ l. Single top: R ± 1,2 tb

81 LHC Phenomenology Basic phenomenology controlled by g, M A, M H. g/ g R 1,2 g R 1,2 Different decay channels probe R 1,R 2 and H. Di-lepton: R 0 1,2 l+ l. Single top: R ± 1,2 tb Di-boson: R 2 ZW/WW.

82 LHC Phenomenology Basic phenomenology controlled by g, M A, M H. g/ g R 1,2 g R 1,2 Different decay channels probe R 1,R 2 and H. Di-lepton: R 0 1,2 l+ l. Single top: R ± 1,2 tb Di-boson: R 2 ZW/WW. Higgs-Strahlung: R 1 HZ/HW.

83 LHC Phenomenology Basic phenomenology controlled by g, M A, M H. g/ g R 1,2 g R 1,2 Different decay channels probe R 1,R 2 and H. Di-lepton: R 0 1,2 l+ l. Single top: R ± 1,2 tb Di-boson: R 2 ZW/WW. Higgs-Strahlung: R 1 HZ/HW. Higgs-Decays: H ZZ/WW (b b?).

84 LHC Phenomenology Basic phenomenology controlled by g, M A, M H. g/ g R 1,2 g R 1,2 Different decay channels probe R 1,R 2 and H. Di-lepton: R 0 1,2 l+ l. Single top: R ± 1,2 tb Di-boson: R 2 ZW/WW. Higgs-Strahlung: R 1 HZ/HW. Higgs-Decays: H ZZ/WW (b b?). boosted tops, W, Z and H

85 LHC Phenomenology Basic phenomenology controlled by g, M A, M H. g/ g R 1,2 g R 1,2 Different decay channels probe R 1,R 2 and H. Di-lepton: R 0 1,2 l+ l. Single top: R ± 1,2 tb Di-boson: R 2 ZW/WW. Higgs-Strahlung: R 1 HZ/HW. Higgs-Decays: H ZZ/WW (b b?). boosted tops, W, Z and H Lattice can (in principle) narrow down parameter space for each model

86 LHC Phenomenology Basic phenomenology controlled by g, M A, M H. g/ g R 1,2 g R 1,2 Different decay channels probe R 1,R 2 and H. Di-lepton: R 0 1,2 l+ l. Single top: R ± 1,2 tb Di-boson: R 2 ZW/WW. Higgs-Strahlung: R 1 HZ/HW. Higgs-Decays: H ZZ/WW (b b?). boosted tops, W, Z and H Lattice can (in principle) narrow down parameter space for each model MWT/OMT, NMWT, UMT etc...

87 Vector Production σ(pb) 10 2 σ(pb) R ± R ± R ± 2 R ± S=0.3 g = S=0.3 g = Mass (TeV) Mass (TeV) Figure: DY production of R 1,2. (Belyaev, Foadi, M.T.F, Järvinen, Pukhov, Sannino 08)

88 Vector BRs BR(R ± 1) ff nl tb W ± Z BR(R ± 1) ff nl W ± H tb 10-3 W ± H 10-3 W ± Z S= S=0.3 g = Mass (TeV) g = Mass (TeV) Figure: BR s of R 1. (Belyaev, Foadi, M.T.F, Järvinen, Pukhov, Sannino 08)

89 l + l LHC using CalcHEP Number of events/ fb S=0.3 g = M ll (GeV) Number of events/ fb S=0.3 g = M T l (GeV) Figure: Left: Dilepton invariant mass distributions M ll for pp R 0 1,2 l+ l Right: Single lepton transverse mass distributions M T l pp R ± 1,2 l± (Belyaev, Foadi, M.T.F, Järvinen, Pukhov, Sannino 08)

90 Results for tb d N ev d M rec (tb) pp tb pp tt pp w+bb pp w+jj M(tb ), GeV rec d N ev d M(tb) M(tb), GeV Figure: Reconstructed (left plot) and partonic (right plot) invariant mass of top and b-quarks after final cuts. Distributions normalized to 30 fb 1. (A. Belyaev, M.T.F and A.Sherstnev in preparation)

91 Di-boson vs Higgs-strahlung q Z,R 2 W q Z,R 1 H q W/Z q W/Z Number of events/ fb S=0.3 g = M T 3l (GeV) Events/15 GeV S=0.3,s=0 M A = 700 GeV, M H =200 g ~ =5 pp WH WZZ pp ZH ZZZ pp WZZ background pp ZZZ background M WZZ(ZZZ) (GeV) (Belyaev, Foadi, M.T.F, Järvinen, Pukhov, Sannino 08)

92 Symmetric vs Asymmetric TIMPs Can pngb TIMPs have a symmetric relic density? Φ complex composite scalar with uncharged components ~ λs motivated by achieving Minimality & Walking (Dynamical realization of scalar singlet DM models) Specific model example: 'Ultra Minimal TC' Yield and relic density in the presence of asymmetry: (Griest & Seckel 85) α=0 (Ryttov & Sannino 09) (Belyaev, M.T.F, Sarkar & Sannino 10)

93 Symmetric vs Asymmetric TIMPs TIMPs with charged constituents Symmetric relic density of T0 (Belyaev, M.T.F, Sarkar & Sannino 10) Higgs interactions of T0 identical to those of φ α=0 T may also have charge radius interaction : In addition T0 has contact interactions with SM gauge bosons, due to EW charges of U, D: (Preskill 81; Chadha and Peskin 81)

Back to light ADM Most nuclear recoil experiments optimized to heavy WIMPs with little sensitivity to low mass particles O(keV) recoil energies Recently several experiments have reported events close

94 Back to light ADM Most nuclear recoil experiments optimized to heavy WIMPs with little sensitivity to low mass particles O(keV) recoil energies Recently several experiments have reported events close to threshold Region of interest for Solar neutrinos 10) ~ 5 GeV Dark Matter candidates with ~10-39 cm2 spin-independent cross-section remains viable. Spin-dependent cross-sections up to cm2

95 Signatures of light ADM Similar to TIMPs light ADM may be a composite scalar or fermion Higgs exchange can naturally provide cross-section up to ~10-41 cm2 Charge radius can provide ~10-39 cm2 SI cross-sections Large SI and SD cross-sections of fermionic ADM can be realized via magnetic moment interactions (Sigurdson et al 2006, Gardner 08, Heo 09, Masso et al 09, An et al 10, Banks et al 10, Barger et al 10...) MH=150 (Fit Courtesy of McCabe, McCabe 10) Interesting LHC signatures like for TIMPs incl 'monojets' (Goodman et al 10, Bai, Fox & Harnik 10)

96 Astrophysical aspects of light ADM Long range self-interactions are more tightly constrained by the 'Bullet cluster' (Feng, Kaplinghat and Yu 10)

100

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103 Recent study of effects of DM on white dwarves and neutron stars, see e.g. (Fairbairn and McCullough 10; Kouvaris 10)

104 Summary Asymmetric Dark Matter motivated by the asymmetry of baryonic matter and the wish to explain why ΩDM / ΩB ~ O(1) Technicolor is a natural and dynamical model of EWSB ~ TeV scale ADM (Technibaryon) and ~ 100 GeV scale ADM (pseudo Goldstone Boson TIMPs) arise in (Minimal Walking) Technicolor models of DEWSB. ~ GeV scale ADM (Dark Baryons) arise from strong dynamics in Hidden/Mirror/Unbaryon sectors, and is motivated in addition by problems in structure formation and potentially in helioseismology. Variety of signatures can test the scenarios

105 DM Production mechanisms Illustrative and simple model: A complex composite scalar Symmetric vs. asymmetric relics (Griest & Seckel 85) Freeze out vs. freeze-in (Asaka, Ishiwata & Moroi 05) (Belyaev, M.T.F, Sarkar & Sannino 10) (Hall, Jedamzik, March-Russel and West 10)

Walking in Monte-Carlo

Walking in Monte-Carlo University of Oxford MC4BSM, April 15 th 2010 m.frandsen1@physics.ox.ac.uk Outline 1 Bright and dark mass from Technicolor 2 3 Work in collaboration with: Alexander Belyaev (Southampton U.), Roshan Foadi