Astroparticle Physics at Colliders

Transcription

1 Astroparticle Physics at Colliders Manuel Drees Bonn University Astroparticle Physics p. 1/29

2 Contents 1) Introduction: A brief history of the universe Astroparticle Physics p. 2/29

3 Contents 1) Introduction: A brief history of the universe 2) Inflation Astroparticle Physics p. 2/29

4 Contents 1) Introduction: A brief history of the universe 2) Inflation 3) Dark Energy Astroparticle Physics p. 2/29

5 Contents 1) Introduction: A brief history of the universe 2) Inflation 3) Dark Energy 4) Baryogenesis Astroparticle Physics p. 2/29

6 Contents 1) Introduction: A brief history of the universe 2) Inflation 3) Dark Energy 4) Baryogenesis 5) Dark Matter Astroparticle Physics p. 2/29

7 Contents 1) Introduction: A brief history of the universe 2) Inflation 3) Dark Energy 4) Baryogenesis 5) Dark Matter 6) Summary Astroparticle Physics p. 2/29

8 1 Introduction: History of the Universe Before the Big Bang: Speculations about pre BB universe, e.g. in superstring theory. Few predictions, no known connections with collider physics. Astroparticle Physics p. 3/29

9 1 Introduction: History of the Universe Before the Big Bang: Speculations about pre BB universe, e.g. in superstring theory. Few predictions, no known connections with collider physics. Inflation: Scale factor ( radius ) R e N R, N 60 Astroparticle Physics p. 3/29

10 1 Introduction: History of the Universe Before the Big Bang: Speculations about pre BB universe, e.g. in superstring theory. Few predictions, no known connections with collider physics. Inflation: Scale factor ( radius ) R e N R, N 60 Universe was dominated by vacuum energy; empty at end of inflation Astroparticle Physics p. 3/29

11 1 Introduction: History of the Universe Before the Big Bang: Speculations about pre BB universe, e.g. in superstring theory. Few predictions, no known connections with collider physics. Inflation: Scale factor ( radius ) R e N R, N 60 Universe was dominated by vacuum energy; empty at end of inflation Quantum fluctuations can cause density perturbations: confirmed by CMB observations (WMAP,... ) Astroparticle Physics p. 3/29

12 1 Introduction: History of the Universe Before the Big Bang: Speculations about pre BB universe, e.g. in superstring theory. Few predictions, no known connections with collider physics. Inflation: Scale factor ( radius ) R e N R, N 60 Universe was dominated by vacuum energy; empty at end of inflation Quantum fluctuations can cause density perturbations: confirmed by CMB observations (WMAP,... ) Scalar fields can get large vevs due to these fluctuations Astroparticle Physics p. 3/29

13 1 Introduction: History of the Universe Before the Big Bang: Speculations about pre BB universe, e.g. in superstring theory. Few predictions, no known connections with collider physics. Inflation: Scale factor ( radius ) R e N R, N 60 Universe was dominated by vacuum energy; empty at end of inflation Quantum fluctuations can cause density perturbations: confirmed by CMB observations (WMAP,... ) Scalar fields can get large vevs due to these fluctuations At least one model maybe testable at the LHC! Astroparticle Physics p. 3/29

14 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R > 3 MeV (BBN) Astroparticle Physics p. 4/29

15 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R > 3 MeV (BBN) Thought to begin with coherent oscillation of inflaton field Astroparticle Physics p. 4/29

16 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R > 3 MeV (BBN) Thought to begin with coherent oscillation of inflaton field Dynamics of thermalization has some connection to dynamics of heavy ion collisions ( RHIC, LHC) Astroparticle Physics p. 4/29

17 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R > 3 MeV (BBN) Thought to begin with coherent oscillation of inflaton field Dynamics of thermalization has some connection to dynamics of heavy ion collisions ( RHIC, LHC) Baryogenesis: Happened sometime after end of inflation Astroparticle Physics p. 4/29

18 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R > 3 MeV (BBN) Thought to begin with coherent oscillation of inflaton field Dynamics of thermalization has some connection to dynamics of heavy ion collisions ( RHIC, LHC) Baryogenesis: Happened sometime after end of inflation Many models exist Astroparticle Physics p. 4/29

19 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R > 3 MeV (BBN) Thought to begin with coherent oscillation of inflaton field Dynamics of thermalization has some connection to dynamics of heavy ion collisions ( RHIC, LHC) Baryogenesis: Happened sometime after end of inflation Many models exist Work at different temperatures Astroparticle Physics p. 4/29

20 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R > 3 MeV (BBN) Thought to begin with coherent oscillation of inflaton field Dynamics of thermalization has some connection to dynamics of heavy ion collisions ( RHIC, LHC) Baryogenesis: Happened sometime after end of inflation Many models exist Work at different temperatures Some models make predictions for colliders! Astroparticle Physics p. 4/29

21 History (cont.d) Creation of Dark Matter: Happened sometime after end of inflation Astroparticle Physics p. 5/29

22 History (cont.d) Creation of Dark Matter: Happened sometime after end of inflation Many models exist Astroparticle Physics p. 5/29

23 History (cont.d) Creation of Dark Matter: Happened sometime after end of inflation Many models exist Work at different temperatures Astroparticle Physics p. 5/29

24 History (cont.d) Creation of Dark Matter: Happened sometime after end of inflation Many models exist Work at different temperatures Most models have connections to collider physics! Astroparticle Physics p. 5/29

25 History (cont.d) Creation of Dark Matter: Happened sometime after end of inflation Many models exist Work at different temperatures Most models have connections to collider physics! Electroweak Phase Transition: Happened at T = T EW 100 GeV, if T R > T EW Astroparticle Physics p. 5/29

26 History (cont.d) Creation of Dark Matter: Happened sometime after end of inflation Many models exist Work at different temperatures Most models have connections to collider physics! Electroweak Phase Transition: Happened at T = T EW 100 GeV, if T R > T EW May be related to baryogenesis Astroparticle Physics p. 5/29

27 History (cont.d) Creation of Dark Matter: Happened sometime after end of inflation Many models exist Work at different temperatures Most models have connections to collider physics! Electroweak Phase Transition: Happened at T = T EW 100 GeV, if T R > T EW May be related to baryogenesis May have some connection to collider physics (sphalerons) Astroparticle Physics p. 5/29

28 History (cont.d) QCD phase transition: Happened at T = T QCD 170 MeV, if T R > T QCD Astroparticle Physics p. 6/29

29 History (cont.d) QCD phase transition: Happened at T = T QCD 170 MeV, if T R > T QCD Related to dynamics of heavy ion collisions, soft QCD (at negligible baryon density) Astroparticle Physics p. 6/29

30 History (cont.d) QCD phase transition: Happened at T = T QCD 170 MeV, if T R > T QCD Related to dynamics of heavy ion collisions, soft QCD (at negligible baryon density) Big Bang Nucleosynthesis (BBN): Started at T 1 MeV Astroparticle Physics p. 6/29

31 History (cont.d) QCD phase transition: Happened at T = T QCD 170 MeV, if T R > T QCD Related to dynamics of heavy ion collisions, soft QCD (at negligible baryon density) Big Bang Nucleosynthesis (BBN): Started at T 1 MeV Constrains many extensions of SM, if T R was sufficiently high to create new particles Astroparticle Physics p. 6/29

32 History (cont.d) QCD phase transition: Happened at T = T QCD 170 MeV, if T R > T QCD Related to dynamics of heavy ion collisions, soft QCD (at negligible baryon density) Big Bang Nucleosynthesis (BBN): Started at T 1 MeV Constrains many extensions of SM, if T R was sufficiently high to create new particles Sets lower bound on T R, if standard BBN is essentially correct Astroparticle Physics p. 6/29

33 History (cont.d) QCD phase transition: Happened at T = T QCD 170 MeV, if T R > T QCD Related to dynamics of heavy ion collisions, soft QCD (at negligible baryon density) Big Bang Nucleosynthesis (BBN): Started at T 1 MeV Constrains many extensions of SM, if T R was sufficiently high to create new particles Sets lower bound on T R, if standard BBN is essentially correct Matter Radiation Equilibrium: Happened at T 3 ev. Astroparticle Physics p. 6/29

34 History (cont.d) QCD phase transition: Happened at T = T QCD 170 MeV, if T R > T QCD Related to dynamics of heavy ion collisions, soft QCD (at negligible baryon density) Big Bang Nucleosynthesis (BBN): Started at T 1 MeV Constrains many extensions of SM, if T R was sufficiently high to create new particles Sets lower bound on T R, if standard BBN is essentially correct Matter Radiation Equilibrium: Happened at T 3 ev. Energy density of the Universe begins to be dominated by (dark) matter Astroparticle Physics p. 6/29

35 History (cont.d) Decoupling of Matter and Radiation: Happened at T 0.3 ev Astroparticle Physics p. 7/29

36 History (cont.d) Decoupling of Matter and Radiation: Happened at T 0.3 ev Last scattering of CMB photons Astroparticle Physics p. 7/29

37 History (cont.d) Decoupling of Matter and Radiation: Happened at T 0.3 ev Last scattering of CMB photons Visible structures (galaxies etc.) start to form Astroparticle Physics p. 7/29

38 History (cont.d) Decoupling of Matter and Radiation: Happened at T 0.3 ev Last scattering of CMB photons Visible structures (galaxies etc.) start to form Equilibrium of Matter and Dark Energy: Probably happened at redshift z 1 (T ev). Astroparticle Physics p. 7/29

39 History (cont.d) Decoupling of Matter and Radiation: Happened at T 0.3 ev Last scattering of CMB photons Visible structures (galaxies etc.) start to form Equilibrium of Matter and Dark Energy: Probably happened at redshift z 1 (T ev). Nobody knows when (or if) Dark Energy was created Astroparticle Physics p. 7/29

40 History (cont.d) Decoupling of Matter and Radiation: Happened at T 0.3 ev Last scattering of CMB photons Visible structures (galaxies etc.) start to form Equilibrium of Matter and Dark Energy: Probably happened at redshift z 1 (T ev). Nobody knows when (or if) Dark Energy was created If Dark Energy const: Plays no role for T > 0.1 ev Astroparticle Physics p. 7/29

41 History (cont.d) Decoupling of Matter and Radiation: Happened at T 0.3 ev Last scattering of CMB photons Visible structures (galaxies etc.) start to form Equilibrium of Matter and Dark Energy: Probably happened at redshift z 1 (T ev). Nobody knows when (or if) Dark Energy was created If Dark Energy const: Plays no role for T > 0.1 ev In models with dynamical Dark Energy ( quintessence ): Can affect dynamics of BBN, creation of Dark Matter,... Astroparticle Physics p. 7/29

42 2 Inflation Most models of inflation are not testable at colliders Astroparticle Physics p. 8/29

43 2 Inflation Most models of inflation are not testable at colliders Recent counter example: MSSM inflation, aka A term inflation Allahverdi et al., hep ph/ , , , , , Astroparticle Physics p. 8/29

44 2 Inflation Most models of inflation are not testable at colliders Recent counter example: MSSM inflation, aka A term inflation Allahverdi et al., hep ph/ , , , , , Basic idea: Use flat directions in space of scalar MSSM fields as inflationary potential: No quartic terms in potential; bi and trilinear terms from soft SUSY breaking Astroparticle Physics p. 8/29

45 2 Inflation Most models of inflation are not testable at colliders Recent counter example: MSSM inflation, aka A term inflation Allahverdi et al., hep ph/ , , , , , Basic idea: Use flat directions in space of scalar MSSM fields as inflationary potential: No quartic terms in potential; bi and trilinear terms from soft SUSY breaking Establishes link between inflationary potential and sparticle masses! Astroparticle Physics p. 8/29

46 2 Inflation Most models of inflation are not testable at colliders Recent counter example: MSSM inflation, aka A term inflation Allahverdi et al., hep ph/ , , , , , Basic idea: Use flat directions in space of scalar MSSM fields as inflationary potential: No quartic terms in potential; bi and trilinear terms from soft SUSY breaking Establishes link between inflationary potential and sparticle masses! SUSY can also play crucial role in re heating Allahverdi et al., hep ph/ , , Astroparticle Physics p. 8/29

47 3 Dark Energy Origin and nature of DE are completely unclear: Biggest mystery in current cosmology! Astroparticle Physics p. 9/29

48 3 Dark Energy Origin and nature of DE are completely unclear: Biggest mystery in current cosmology! In 4 dimensions: No connection to collider physics Astroparticle Physics p. 9/29

49 3 Dark Energy Origin and nature of DE are completely unclear: Biggest mystery in current cosmology! In 4 dimensions: No connection to collider physics In models with small extra dimensions: Connections to collider physics may exist (radion Higgs mixing; spectrum of KK states), but no example is known (to me) Astroparticle Physics p. 9/29

50 3 Dark Energy Origin and nature of DE are completely unclear: Biggest mystery in current cosmology! In 4 dimensions: No connection to collider physics In models with small extra dimensions: Connections to collider physics may exist (radion Higgs mixing; spectrum of KK states), but no example is known (to me) In models with large extra dimension: LHC may be black hole factory; cosmon should be produced in bh decay Astroparticle Physics p. 9/29

51 4 Baryogenesis Reminder: Sakharov conditions: Need Astroparticle Physics p. 10/29

52 4 Baryogenesis Reminder: Sakharov conditions: Need Violation of C and CP symmetries Astroparticle Physics p. 10/29

53 4 Baryogenesis Reminder: Sakharov conditions: Need Violation of C and CP symmetries Violation of baryon or lepton number Astroparticle Physics p. 10/29

54 4 Baryogenesis Reminder: Sakharov conditions: Need Violation of C and CP symmetries Violation of baryon or lepton number Deviation from thermal equilibrium (or CP T violation) Astroparticle Physics p. 10/29

55 4 Baryogenesis Reminder: Sakharov conditions: Need Violation of C and CP symmetries Violation of baryon or lepton number Deviation from thermal equilibrium (or CP T violation) Many models work at very high temperatures (GUT baryogenesis; most leptogenesis; most Affleck Dine): no direct connection to collider physics; indirect connections in some models possible Astroparticle Physics p. 10/29

56 4 Baryogenesis Reminder: Sakharov conditions: Need Violation of C and CP symmetries Violation of baryon or lepton number Deviation from thermal equilibrium (or CP T violation) Many models work at very high temperatures (GUT baryogenesis; most leptogenesis; most Affleck Dine): no direct connection to collider physics; indirect connections in some models possible Some models work at rather low temperature: can be tested at colliders! Will discuss two such models. Astroparticle Physics p. 10/29

57 Leptogenesis with degenerate neutrinos Basic idea of leptogenesis: Astroparticle Physics p. 11/29

58 Leptogenesis with degenerate neutrinos Basic idea of leptogenesis: Out of equilibrium decay of heavy right handed neutrinos N i creates lepton asymmetry Astroparticle Physics p. 11/29

59 Leptogenesis with degenerate neutrinos Basic idea of leptogenesis: Out of equilibrium decay of heavy right handed neutrinos N i creates lepton asymmetry Is partially transformed to baryon asymmetry via elw sphaleron transitions Astroparticle Physics p. 11/29

60 Leptogenesis with degenerate neutrinos Basic idea of leptogenesis: Out of equilibrium decay of heavy right handed neutrinos N i creates lepton asymmetry Is partially transformed to baryon asymmetry via elw sphaleron transitions Standard thermal leptogensis with hierarchical heavy neutrinos reqires T R M GeV: Not testable at colliders Buchmüller, Di Bari, Plümacher 2002/3/4; Davidson 2003; Giudice et al Astroparticle Physics p. 11/29

61 Leptogenesis with degenerate neutrinos Basic idea of leptogenesis: Out of equilibrium decay of heavy right handed neutrinos N i creates lepton asymmetry Is partially transformed to baryon asymmetry via elw sphaleron transitions Standard thermal leptogensis with hierarchical heavy neutrinos reqires T R M GeV: Not testable at colliders Buchmüller, Di Bari, Plümacher 2002/3/4; Davidson 2003; Giudice et al If M 2 M 1 M 1 : effective CP violation enhanced: Can have M 1 TeV! Pilaftsis 1997/9; Pilaftsis & Underwood 2004 Astroparticle Physics p. 11/29

62 Leptogenesis (cont.d) N i l j H H ( H) N k l m ( l m ) Enhanced for i = 1, k = 2 Astroparticle Physics p. 12/29

63 Leptogenesis (cont.d) N i l j H H ( H) N k l m ( l m ) Enhanced for i = 1, k = 2 N i only couple to Higgs boson(s): productions at colliders not easy! Astroparticle Physics p. 12/29

64 Leptogenesis (cont.d) N i l j H H ( H) N k l m ( l m ) Enhanced for i = 1, k = 2 N i only couple to Higgs boson(s): productions at colliders not easy! If M N1,2 < 500 GeV: may see CPV at LHC! Bray et al., hep-ph/ Astroparticle Physics p. 12/29

65 Leptogenesis (cont.d) N i l j H H ( H) N k l m ( l m ) Enhanced for i = 1, k = 2 N i only couple to Higgs boson(s): productions at colliders not easy! If M N1,2 < 500 GeV: may see CPV at LHC! Bray et al., hep-ph/ Other scenarios with low-scale leptogenesis: Grossman, Kashti, Nir, Roulet 2004; Hambye et al. 2003; Raidal, Strumia, Turzynski 2004 Astroparticle Physics p. 12/29

66 Electroweak Baryogenesis Basic idea: Bubbles of true vacuum form in phase of exact SU(2). Baryon asymmetry generated during transport through bubble walls. Astroparticle Physics p. 13/29

67 Electroweak Baryogenesis Basic idea: Bubbles of true vacuum form in phase of exact SU(2). Baryon asymmetry generated during transport through bubble walls. B violation: elw sphalerons Astroparticle Physics p. 13/29

68 Electroweak Baryogenesis Basic idea: Bubbles of true vacuum form in phase of exact SU(2). Baryon asymmetry generated during transport through bubble walls. B violation: elw sphalerons Out of equlibrium: Elw. phase transition was strongly 1 st order Astroparticle Physics p. 13/29

69 Electroweak Baryogenesis Basic idea: Bubbles of true vacuum form in phase of exact SU(2). Baryon asymmetry generated during transport through bubble walls. B violation: elw sphalerons Out of equlibrium: Elw. phase transition was strongly 1 st order CP violation: in bubble wall Astroparticle Physics p. 13/29

70 Electroweak Baryogenesis Basic idea: Bubbles of true vacuum form in phase of exact SU(2). Baryon asymmetry generated during transport through bubble walls. B violation: elw sphalerons Out of equlibrium: Elw. phase transition was strongly 1 st order CP violation: in bubble wall Does not work in SM: cross over (no phase transition) for m H > 60 GeV! Astroparticle Physics p. 13/29

71 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Astroparticle Physics p. 14/29

72 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Light SM like Higgs: m h < 120 GeV: testable at LHC! Astroparticle Physics p. 14/29

73 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Light SM like Higgs: m h < 120 GeV: testable at LHC! Light stop: m t 1 < m t : testable at LHC? Astroparticle Physics p. 14/29

74 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Light SM like Higgs: m h < 120 GeV: testable at LHC! Light stop: m t 1 < m t : testable at LHC? Little t L t R mixing: θ t π/2 Astroparticle Physics p. 14/29

75 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Light SM like Higgs: m h < 120 GeV: testable at LHC! Light stop: m t 1 < m t : testable at LHC? Little t L t R mixing: θ t π/2 CP violation in χ sector: φ µ > 0.1, M 2, µ < 150 GeV Astroparticle Physics p. 14/29

76 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Light SM like Higgs: m h < 120 GeV: testable at LHC! Light stop: m t 1 < m t : testable at LHC? Little t L t R mixing: θ t π/2 CP violation in χ sector: φ µ > 0.1, M 2, µ < 150 GeV Remains to be checked: Astroparticle Physics p. 14/29

77 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Light SM like Higgs: m h < 120 GeV: testable at LHC! Light stop: m t 1 < m t : testable at LHC? Little t L t R mixing: θ t π/2 CP violation in χ sector: φ µ > 0.1, M 2, µ < 150 GeV Remains to be checked: Determination of θ t in presence of CP violation Astroparticle Physics p. 14/29

78 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Light SM like Higgs: m h < 120 GeV: testable at LHC! Light stop: m t 1 < m t : testable at LHC? Little t L t R mixing: θ t π/2 CP violation in χ sector: φ µ > 0.1, M 2, µ < 150 GeV Remains to be checked: Determination of θ t in presence of CP violation Determination of φ µ in relevant region of parameter space Astroparticle Physics p. 14/29

79 5 Dark Matter Several observations indicate existence of non-luminous Dark Matter (DM) (more exactly: missing force) Astroparticle Physics p. 15/29

80 5 Dark Matter Several observations indicate existence of non-luminous Dark Matter (DM) (more exactly: missing force) Galactic rotation curves imply Ω DM h Ω: Mass density in units of critical density; Ω = 1 means flat Universe. h: Scaled Hubble constant. Observation: h = 0.72 ± 0.07 Astroparticle Physics p. 15/29

81 5 Dark Matter Several observations indicate existence of non-luminous Dark Matter (DM) (more exactly: missing force) Galactic rotation curves imply Ω DM h Ω: Mass density in units of critical density; Ω = 1 means flat Universe. h: Scaled Hubble constant. Observation: h = 0.72 ± 0.07 Models of structure formation, X ray temperature of clusters of galaxies,... Astroparticle Physics p. 15/29

82 5 Dark Matter Several observations indicate existence of non-luminous Dark Matter (DM) (more exactly: missing force) Galactic rotation curves imply Ω DM h Ω: Mass density in units of critical density; Ω = 1 means flat Universe. h: Scaled Hubble constant. Observation: h = 0.72 ± 0.07 Models of structure formation, X ray temperature of clusters of galaxies,... Cosmic Microwave Background anisotropies (WMAP) imply Ω DM h 2 = Spergel et al., astro ph/ Astroparticle Physics p. 15/29

83 Density of thermal DM Decoupling of DM particle χ defined by: n χ (T f ) vσ(χχ any) = H(T f ) n χ : χ number density e m χ/t v: Relative velocity... : Thermal average H: Hubble parameter; in standard cosmology T 2 /M Planck Astroparticle Physics p. 16/29

84 Density of thermal DM Decoupling of DM particle χ defined by: n χ (T f ) vσ(χχ any) = H(T f ) n χ : χ number density e m χ/t v: Relative velocity... : Thermal average H: Hubble parameter; in standard cosmology T 2 /M Planck Gives average relic mass density Ω χ 1 vσ(χχ any) Gives roughly right result for weak cross section! Astroparticle Physics p. 16/29

85 Assumptions χ is effectively stable, τ χ τ U : partly testable at colliders Astroparticle Physics p. 17/29

86 Assumptions χ is effectively stable, τ χ τ U : partly testable at colliders No entropy production after χ decoupled: Not testable at colliders Astroparticle Physics p. 17/29

87 Assumptions χ is effectively stable, τ χ τ U : partly testable at colliders No entropy production after χ decoupled: Not testable at colliders H at time of χ decoupling is known: partly testable at colliders Astroparticle Physics p. 17/29

88 hermal WIMPs at colliders: Generalities Only vσ(χχ anything) is known Astroparticle Physics p. 18/29

89 hermal WIMPs at colliders: Generalities Only vσ(χχ anything) is known No guarantee that χ couples to light quarks or electrons (which we can collide) Astroparticle Physics p. 18/29

90 hermal WIMPs at colliders: Generalities Only vσ(χχ anything) is known No guarantee that χ couples to light quarks or electrons (which we can collide) At LHC: direct χ pair production is undetectable Astroparticle Physics p. 18/29

91 hermal WIMPs at colliders: Generalities Only vσ(χχ anything) is known No guarantee that χ couples to light quarks or electrons (which we can collide) At LHC: direct χ pair production is undetectable Hence can generally only test models with Überbau of heavier, strongly interacting new particles decaying into χ Astroparticle Physics p. 18/29

92 hermal WIMPs at colliders: Generalities Only vσ(χχ anything) is known No guarantee that χ couples to light quarks or electrons (which we can collide) At LHC: direct χ pair production is undetectable Hence can generally only test models with Überbau of heavier, strongly interacting new particles decaying into χ Such particles exist for best motivated χ candidates: SUSY, Little Higgs, universal extra dimension Astroparticle Physics p. 18/29

93 SUSY Dark Matter Conditions for successful DM candidate: Must be stable χ = LSP and R parity is conserved (if LSP in visible sector) Astroparticle Physics p. 19/29

94 SUSY Dark Matter Conditions for successful DM candidate: Must be stable χ = LSP and R parity is conserved (if LSP in visible sector) Exotic isotope searches χ must be neutral Astroparticle Physics p. 19/29

95 SUSY Dark Matter Conditions for successful DM candidate: Must be stable χ = LSP and R parity is conserved (if LSP in visible sector) Exotic isotope searches χ must be neutral Must satisfy DM search limits χ ν And the winner is... Astroparticle Physics p. 19/29

96 SUSY Dark Matter Conditions for successful DM candidate: Must be stable χ = LSP and R parity is conserved (if LSP in visible sector) Exotic isotope searches χ must be neutral Must satisfy DM search limits χ ν And the winner is... (or in hidden sector) χ = χ 0 1 Astroparticle Physics p. 19/29

97 χ 0 1 relic density To predict thermal χ 0 1 relic density: have to know σ( χ 0 1 χ 0 1 SM particles) In general, this requires knowledge of almost all sparticle and Higgs masses and of all couplings of the LSP! Astroparticle Physics p. 20/29

98 χ 0 1 relic density To predict thermal χ 0 1 relic density: have to know σ( χ 0 1 χ 0 1 SM particles) In general, this requires knowledge of almost all sparticle and Higgs masses and of all couplings of the LSP! Neutralino mass matrix in the MSSM: 0 1 M 0 = M 1 0 M Z cosβ sinθ W M Z sinβ sinθ W 0 M 2 M Z cosβ cosθ W M Z sinβ cosθ W M Z cosβ sinθ W M Z cosβ cosθ W 0 µ M Z sinβ sinθ W M Z sinβ cosθ W µ 0 C A Astroparticle Physics p. 20/29

99 χ 0 1 relic density To predict thermal χ 0 1 relic density: have to know σ( χ 0 1 χ 0 1 SM particles) In general, this requires knowledge of almost all sparticle and Higgs masses and of all couplings of the LSP! Neutralino mass matrix in the MSSM: 0 1 M 0 = M 1 0 M Z cosβ sinθ W M Z sinβ sinθ W 0 M 2 M Z cosβ cosθ W M Z sinβ cosθ W M Z cosβ sinθ W M Z cosβ cosθ W 0 µ M Z sinβ sinθ W M Z sinβ cosθ W µ 0 C A = Can determine decomposition of χ 0 1 by studying χ± 1, χ0 2, χ0 3. Astroparticle Physics p. 20/29

100 χ 0 1 annihilation in the MSSM m fl, m fr, θ f: Needed for χ 0 1 χ0 1 f f Astroparticle Physics p. 21/29

101 χ 0 1 annihilation in the MSSM m fl, m fr, θ f: Needed for χ 0 1 χ0 1 f f m h, m H, m A, α, tanβ: Needed for χ 0 1 χ0 1 f f, V V, V φ,φφ (V : Massive gauge boson; φ: Higgs boson). Astroparticle Physics p. 21/29

102 χ 0 1 annihilation in the MSSM m fl, m fr, θ f: Needed for χ 0 1 χ0 1 f f m h, m H, m A, α, tanβ: Needed for χ 0 1 χ0 1 f f, V V, V φ,φφ (V : Massive gauge boson; φ: Higgs boson). For many masses: lower bounds may be sufficient Astroparticle Physics p. 21/29

103 χ 0 1 annihilation in the MSSM m fl, m fr, θ f: Needed for χ 0 1 χ0 1 f f m h, m H, m A, α, tanβ: Needed for χ 0 1 χ0 1 f f, V V, V φ,φφ (V : Massive gauge boson; φ: Higgs boson). For many masses: lower bounds may be sufficient If coannihilation is important: final answer depends exponentially on mass difference Astroparticle Physics p. 21/29

104 χ 0 1 annihilation in the MSSM m fl, m fr, θ f: Needed for χ 0 1 χ0 1 f f m h, m H, m A, α, tanβ: Needed for χ 0 1 χ0 1 f f, V V, V φ,φφ (V : Massive gauge boson; φ: Higgs boson). For many masses: lower bounds may be sufficient If coannihilation is important: final answer depends exponentially on mass difference Parameters in Higgs and squark sector are also needed to predict χ 0 1 detection rate, i.e. σ( χ0 1 N χ0 1 N) Astroparticle Physics p. 21/29

105 Impact on particle physics (msugra) w./ A. Djouadi, J.-L. Kneur, hep-ph/ Parameter space is constrained by: Sparticle searches, in particular χ ± 1, τ 1 searches at LEP: σ < 20 fb Astroparticle Physics p. 22/29

106 Impact on particle physics (msugra) w./ A. Djouadi, J.-L. Kneur, hep-ph/ Parameter space is constrained by: Sparticle searches, in particular χ ± 1, τ 1 searches at LEP: σ < 20 fb Higgs searches, in particular light CP even Higgs search at LEP (parameterized) Astroparticle Physics p. 22/29

107 Impact on particle physics (msugra) w./ A. Djouadi, J.-L. Kneur, hep-ph/ Parameter space is constrained by: Sparticle searches, in particular χ ± 1, τ 1 searches at LEP: σ < 20 fb Higgs searches, in particular light CP even Higgs search at LEP (parameterized) Brookhaven g µ 2 measurement: Take envelope of constraints using τ and e + e data for SM prediction Astroparticle Physics p. 22/29

108 Impact on particle physics (msugra) w./ A. Djouadi, J.-L. Kneur, hep-ph/ Parameter space is constrained by: Sparticle searches, in particular χ ± 1, τ 1 searches at LEP: σ < 20 fb Higgs searches, in particular light CP even Higgs search at LEP (parameterized) Brookhaven g µ 2 measurement: Take envelope of constraints using τ and e + e data for SM prediction Radiative b decays (BELLE,... ): Take B(b sγ) Astroparticle Physics p. 22/29

109 Impact on particle physics (msugra) w./ A. Djouadi, J.-L. Kneur, hep-ph/ Parameter space is constrained by: Sparticle searches, in particular χ ± 1, τ 1 searches at LEP: σ < 20 fb Higgs searches, in particular light CP even Higgs search at LEP (parameterized) Brookhaven g µ 2 measurement: Take envelope of constraints using τ and e + e data for SM prediction Radiative b decays (BELLE,... ): Take B(b sγ) Simple CCB constraints (at weak scale only) Astroparticle Physics p. 22/29

110 1000 msugra, m t = 178 GeV, tanβ = 10, µ>0, A 0 = 0 All constraints except DM included τ 1 is LSP m 1/2 [GeV] h is too light 100 χ ~ m 0 [GeV] is too light Astroparticle Physics p. 23/29

111 msugra, m t = 178 GeV, tanβ = 10, µ>0, A 0 = All constraints included m 1/2 [GeV] m 0 [GeV] Astroparticle Physics p. 24/29

112 Predicting Ω χ 0 1 h 2 from LHC data The precision with which Ω χ 0 1 h 2 can be predicted strongly depends on SUSY parameters: black Battaglia et al., hep ph/ Astroparticle Physics p. 25/29

113 Predicting Ω χ 0 1 h 2 from LHC data The precision with which Ω χ 0 1 h 2 can be predicted strongly depends on SUSY parameters: black Battaglia et al., hep ph/ Bulk region : χ 0 1 χ 0 1 l + l via l exchange, needs rather light χ 0 1, l: Ω χ 0 1 h 2 to 7%! Astroparticle Physics p. 25/29

114 Predicting Ω χ 0 1 h 2 from LHC data The precision with which Ω χ 0 1 h 2 can be predicted strongly depends on SUSY parameters: black Battaglia et al., hep ph/ Bulk region : χ 0 1 χ 0 1 l + l via l exchange, needs rather light χ 0 1, l: Ω χ 0 1 h 2 to 7%! Focus point region: χ 0 1 χ0 1 V V,Zh (V = Z,W ± ) via h component of χ 0 1: Ω χ 0 1 h 2 to 82% Astroparticle Physics p. 25/29

115 Predicting Ω χ 0 1 h 2 from LHC data The precision with which Ω χ 0 1 h 2 can be predicted strongly depends on SUSY parameters: black Battaglia et al., hep ph/ Bulk region : χ 0 1 χ 0 1 l + l via l exchange, needs rather light χ 0 1, l: Ω χ 0 1 h 2 to 7%! Focus point region: χ 0 1 χ0 1 V V,Zh (V = Z,W ± ) via h component of χ 0 1: Ω χ 0 1 h 2 to 82% Co annihilation region : m χ 0 1 m τ1 : Ω χ 0 1 h 2 to 170% Astroparticle Physics p. 25/29

116 Predicting Ω χ 0 1 h 2 from LHC data The precision with which Ω χ 0 1 h 2 can be predicted strongly depends on SUSY parameters: black Battaglia et al., hep ph/ Bulk region : χ 0 1 χ 0 1 l + l via l exchange, needs rather light χ 0 1, l: Ω χ 0 1 h 2 to 7%! Focus point region: χ 0 1 χ0 1 V V,Zh (V = Z,W ± ) via h component of χ 0 1: Ω χ 0 1 h 2 to 82% Co annihilation region : m χ 0 1 m τ1 : Ω χ 0 1 h 2 to 170% Funnel region : m χ 0 1 m A /2: Ω χ 0 1 h 2 to 400% Astroparticle Physics p. 25/29

117 Predicting Ω χ 0 1 h 2 from LHC data The precision with which Ω χ 0 1 h 2 can be predicted strongly depends on SUSY parameters: black Battaglia et al., hep ph/ Bulk region : χ 0 1 χ 0 1 l + l via l exchange, needs rather light χ 0 1, l: Ω χ 0 1 h 2 to 7%! Focus point region: χ 0 1 χ0 1 V V,Zh (V = Z,W ± ) via h component of χ 0 1: Ω χ 0 1 h 2 to 82% Co annihilation region : m χ 0 1 m τ1 : Ω χ 0 1 h 2 to 170% Funnel region : m χ 0 1 m A /2: Ω χ 0 1 h 2 to 400% Based on spectrum information only! Astroparticle Physics p. 25/29

118 Hidden Sector Dark Matter Any msugra parameter set can have the right DM density if LSP is in hidden or invisible sector. It could be: The axino Covi et al., hep-ph/ Astroparticle Physics p. 26/29

119 Hidden Sector Dark Matter Any msugra parameter set can have the right DM density if LSP is in hidden or invisible sector. It could be: The axino Covi et al., hep-ph/ The gravitino Buchmüller et al.; J.L. Feng et al.; J. Ellis et al.; Di Austri and Roszkowski;... Astroparticle Physics p. 26/29

120 Hidden Sector Dark Matter Any msugra parameter set can have the right DM density if LSP is in hidden or invisible sector. It could be: The axino Covi et al., hep-ph/ The gravitino Buchmüller et al.; J.L. Feng et al.; J. Ellis et al.; Di Austri and Roszkowski;... A modulino Astroparticle Physics p. 26/29

121 Hidden Sector DM (contd.) Unfortunately, Ω DM can no longer be predicted from particle physics alone; e.g. Ω Gh 2 T reheat Astroparticle Physics p. 27/29

122 Hidden Sector DM (contd.) Unfortunately, Ω DM can no longer be predicted from particle physics alone; e.g. Ω Gh 2 T reheat hidden sector LSP may leave no imprint at colliders, unless lightest visible sparticle (LVSP) is charged; LVSP is quite long-lived Astroparticle Physics p. 27/29

123 Hidden Sector DM (contd.) Unfortunately, Ω DM can no longer be predicted from particle physics alone; e.g. Ω Gh 2 T reheat hidden sector LSP may leave no imprint at colliders, unless lightest visible sparticle (LVSP) is charged; LVSP is quite long-lived Detection of hidden sector DM seems impossible: Cross sections are way too small! Astroparticle Physics p. 27/29

124 Nonstandard cosmology Can either reduce or increase density of stable χ 0 1 Astroparticle Physics p. 28/29

125 Nonstandard cosmology Can either reduce or increase density of stable χ 0 1 Increase: through incease of H(T f ); or through non-thermal χ 0 1 production mechanisms. Astroparticle Physics p. 28/29

126 Nonstandard cosmology Can either reduce or increase density of stable χ 0 1 Increase: through incease of H(T f ); or through non-thermal χ 0 1 production mechanisms. Reduce: through decrease of H(T f ); through late entropy production; or through low T reheat. Astroparticle Physics p. 28/29

127 Nonstandard cosmology Can either reduce or increase density of stable χ 0 1 Increase: through incease of H(T f ); or through non-thermal χ 0 1 production mechanisms. Reduce: through decrease of H(T f ); through late entropy production; or through low T reheat. None of these mechanisms in general has observable consequences (except DM density). Astroparticle Physics p. 28/29

128 Nonstandard cosmology Can either reduce or increase density of stable χ 0 1 Increase: through incease of H(T f ); or through non-thermal χ 0 1 production mechanisms. Reduce: through decrease of H(T f ); through late entropy production; or through low T reheat. None of these mechanisms in general has observable consequences (except DM density). If χ 0 1 makes DM: Can use measurements at colliders to constrain cosmology! Astroparticle Physics p. 28/29

129 6 Summary Dark Energy: Difficult to probe at colliders; perhaps some possibilities if D > 4 Astroparticle Physics p. 29/29

130 6 Summary Dark Energy: Difficult to probe at colliders; perhaps some possibilities if D > 4 Baryogenesis: Some models can be tested at colliders, others cannot Astroparticle Physics p. 29/29

131 6 Summary Dark Energy: Difficult to probe at colliders; perhaps some possibilities if D > 4 Baryogenesis: Some models can be tested at colliders, others cannot Dark Matter: Astroparticle Physics p. 29/29

132 6 Summary Dark Energy: Difficult to probe at colliders; perhaps some possibilities if D > 4 Baryogenesis: Some models can be tested at colliders, others cannot Dark Matter: Many models can be tested at colliders, some cannot Astroparticle Physics p. 29/29

133 6 Summary Dark Energy: Difficult to probe at colliders; perhaps some possibilities if D > 4 Baryogenesis: Some models can be tested at colliders, others cannot Dark Matter: Many models can be tested at colliders, some cannot SUSY WIMPs: Relic density often depends very sensitively on parameters: need very accurate measurements in collider experiments! Astroparticle Physics p. 29/29