Astroparticle Physics and the LC
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1 Astroparticle Physics and the LC Manuel Drees Bonn University Astroparticle Physics p. 1/32
2 Contents 1) Introduction: A brief history of the universe Astroparticle Physics p. 2/32
3 Contents 1) Introduction: A brief history of the universe 2) Dark Energy Astroparticle Physics p. 2/32
4 Contents 1) Introduction: A brief history of the universe 2) Dark Energy 3) Baryogenesis Astroparticle Physics p. 2/32
5 Contents 1) Introduction: A brief history of the universe 2) Dark Energy 3) Baryogenesis 4) Dark Matter Astroparticle Physics p. 2/32
6 Contents 1) Introduction: A brief history of the universe 2) Dark Energy 3) Baryogenesis 4) Dark Matter 5) Summary Astroparticle Physics p. 2/32
7 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. 3/32
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. Inflation: Scale factor ( radius ) R e N R, N 60 Astroparticle Physics p. 3/32
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 Universe was dominated by vacuum energy; empty at end of inflation Astroparticle Physics p. 3/32
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 Quantum fluctuations can cause density perturbations: confirmed by CMB observations (WMAP,... ) Astroparticle Physics p. 3/32
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,... ) Scalar fields can get large vevs due to these fluctuations Astroparticle Physics p. 3/32
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 No known connections to collider physics Astroparticle Physics p. 3/32
13 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R 1 MeV (BBN) Astroparticle Physics p. 4/32
14 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R 1 MeV (BBN) Thought to begin with coherent oscillation of inflaton field Astroparticle Physics p. 4/32
15 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R 1 MeV (BBN) Thought to begin with coherent oscillation of inflaton field No direct connections to collider physics Astroparticle Physics p. 4/32
16 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R 1 MeV (BBN) Thought to begin with coherent oscillation of inflaton field No direct connections to collider physics Dynamics of thermalization has some connection to dynamics of heavy ion collisions ( RHIC, LHC) Astroparticle Physics p. 4/32
17 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R 1 MeV (BBN) Thought to begin with coherent oscillation of inflaton field No direct connections to collider physics Dynamics of thermalization has some connection to dynamics of heavy ion collisions ( RHIC, LHC) Baryogenesis: Happened sometime after end of inflation Astroparticle Physics p. 4/32
18 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R 1 MeV (BBN) Thought to begin with coherent oscillation of inflaton field No direct connections to collider physics 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. 4/32
19 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R 1 MeV (BBN) Thought to begin with coherent oscillation of inflaton field No direct connections to collider physics 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. 4/32
20 History (cont.d) Reheating: (Re-)populates Universe with particles. Re-heat temperature T R not known: T R 1 MeV (BBN) Thought to begin with coherent oscillation of inflaton field No direct connections to collider physics 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. 4/32
21 History (cont.d) Creation of Dark Matter: Happened sometime after end of inflation Astroparticle Physics p. 5/32
22 History (cont.d) Creation of Dark Matter: Happened sometime after end of inflation Many models exist Astroparticle Physics p. 5/32
23 History (cont.d) Creation of Dark Matter: Happened sometime after end of inflation Many models exist Work at different temperatures Astroparticle Physics p. 5/32
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. 5/32
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. 5/32
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. 5/32
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 come connection to collider physics (sphalerons) Astroparticle Physics p. 5/32
28 History (cont.d) QCD phase transition: Happened at T = T QCD 170 MeV, if T R > T QCD Astroparticle Physics p. 6/32
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 Astroparticle Physics p. 6/32
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 Big Bang Nucleosynthesis (BBN): Started at T 1 MeV Astroparticle Physics p. 6/32
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 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. 6/32
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 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. 6/32
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 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. 6/32
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 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. 6/32
35 History (cont.d) Decoupling of Matter and Radiation: Happened at T 0.3 ev Astroparticle Physics p. 7/32
36 History (cont.d) Decoupling of Matter and Radiation: Happened at T 0.3 ev Last scattering of CMB photons Astroparticle Physics p. 7/32
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. 7/32
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. 7/32
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. 7/32
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. 7/32
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. 7/32
42 2 Dark Energy Origin and nature of DE are completely unclear: Biggest mystery in current cosmology! Astroparticle Physics p. 8/32
43 2 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. 8/32
44 2 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 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. 8/32
45 3 Baryogenesis Reminder: Sakharov conditions: Need Astroparticle Physics p. 9/32
46 3 Baryogenesis Reminder: Sakharov conditions: Need Violation of C and CP symmetries Astroparticle Physics p. 9/32
47 3 Baryogenesis Reminder: Sakharov conditions: Need Violation of C and CP symmetries Violation of baryon or lepton number Astroparticle Physics p. 9/32
48 3 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. 9/32
49 3 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): Have no connection to collider physics Astroparticle Physics p. 9/32
50 3 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): Have no connection to collider physics Some models work at rather low temperature: can be tested at colliders! Will discuss two such models. Astroparticle Physics p. 9/32
51 Leptogenesis with degenerate neutrinos Basic idea of leptogenesis: Astroparticle Physics p. 10/32
52 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. 10/32
53 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. 10/32
54 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. 10/32
55 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 and Underwood 2004 Astroparticle Physics p. 10/32
56 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. 11/32
57 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. 11/32
58 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! Constrain via precision measurements of Higgs properties? Astroparticle Physics p. 11/32
59 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! Constrain via precision measurements of Higgs properties? Other scenarios with low-scale leptogenesis: Grossman, Kashti, Nir, Roulet 2004; Hambye et al. 2003; Raidal, Strumia, Turzynski 2004 Astroparticle Physics p. 11/32
60 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. 12/32
61 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. 12/32
62 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. 12/32
63 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. 12/32
64 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. 12/32
65 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Astroparticle Physics p. 13/32
66 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Light Higgs: m h < 120 GeV Astroparticle Physics p. 13/32
67 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Light Higgs: m h < 120 GeV Light stop: m t 1 < m t Astroparticle Physics p. 13/32
68 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Light Higgs: m h < 120 GeV Light stop: m t 1 < m t Little t L t R mixing: θ t π/2 Astroparticle Physics p. 13/32
69 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Light Higgs: m h < 120 GeV Light stop: m t 1 < m t 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. 13/32
70 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Light Higgs: m h < 120 GeV Light stop: m t 1 < m t 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. 13/32
71 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Light Higgs: m h < 120 GeV Light stop: m t 1 < m t 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. 13/32
72 Baryogenesis (cont.d) Mechanism can work in MSSM! Requirements: Light Higgs: m h < 120 GeV Light stop: m t 1 < m t 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. 13/32
73 4 Dark Matter Several observations indicate existence of non-luminous Dark Matter (DM) (more exactly: missing force) Astroparticle Physics p. 14/32
74 4 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. 14/32
75 4 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. 14/32
76 4 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 = ± Bennet et al., astro ph/ Astroparticle Physics p. 14/32
77 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. 15/32
78 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. 15/32
79 Assumptions χ is effectively stable, τ χ τ U : partly testable at colliders Astroparticle Physics p. 16/32
80 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. 16/32
81 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. 16/32
82 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. 17/32
83 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. 17/32
84 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. 17/32
85 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. 17/32
86 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. 18/32
87 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. 18/32
88 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. 18/32
89 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. Well studied in the MSSM, but not much is known about extensions (e.g. NMSSM) Astroparticle Physics p. 18/32
90 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. 19/32
91 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, tan β: Needed for χ 0 1 χ0 1 f f, V V, V φ, φφ (V : Massive gauge boson; φ: Higgs boson). Astroparticle Physics p. 19/32
92 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, tan β: 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. 19/32
93 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, tan β: 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. 19/32
94 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, tan β: 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. 19/32
95 Impact on particle physics (msugra) Parameter space is constrained by: w./ A. Djouadi, J.-L. Kneur, P. Slavich Sparticle searches, in particular χ ± 1, τ 1 searches at LEP: σ < 20 fb Astroparticle Physics p. 20/32
96 Impact on particle physics (msugra) Parameter space is constrained by: w./ A. Djouadi, J.-L. Kneur, P. Slavich 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. 20/32
97 Impact on particle physics (msugra) Parameter space is constrained by: w./ A. Djouadi, J.-L. Kneur, P. Slavich 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. 20/32
98 Impact on particle physics (msugra) Parameter space is constrained by: w./ A. Djouadi, J.-L. Kneur, P. Slavich 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. 20/32
99 Impact on particle physics (msugra) Parameter space is constrained by: w./ A. Djouadi, J.-L. Kneur, P. Slavich 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. 20/32
100 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. 21/32
101 msugra, m t = 178 GeV, tanβ = 10, µ>0, A 0 = All constraints included m 1/2 [GeV] m 0 [GeV] Astroparticle Physics p. 22/32
102 Is the apparently small size of the allowed parameter parameter space a problem? Not necessarily... Astroparticle Physics p. 23/32
103 Is the apparently small size of the allowed parameter parameter space a problem? Not necessarily... QED parameter space α e-05 1e-06 1e m e [GeV] Astroparticle Physics p. 23/32
104 msugra, m t = 178 GeV, tanβ = 10, µ>0, A 0 scanned 1000 All constraints included m 1/2 [GeV] m 0 [GeV] Astroparticle Physics p. 24/32
105 Beyond msugra The predicted Dark Matter density can be altered by modifying the SUSY model and/or by modifying the cosmological model. Reducing Ω χ 0 1 by changing the SUSY model: Dial up co-annihilation Astroparticle Physics p. 25/32
106 Beyond msugra The predicted Dark Matter density can be altered by modifying the SUSY model and/or by modifying the cosmological model. Reducing Ω χ 0 1 by changing the SUSY model: Dial up co-annihilation Increase h component of χ 0 1 Astroparticle Physics p. 25/32
107 Beyond msugra The predicted Dark Matter density can be altered by modifying the SUSY model and/or by modifying the cosmological model. Reducing Ω χ 0 1 by changing the SUSY model: Dial up co-annihilation Increase h component of χ 0 1 Increase W 3 component of χ 0 1 Astroparticle Physics p. 25/32
108 Beyond msugra The predicted Dark Matter density can be altered by modifying the SUSY model and/or by modifying the cosmological model. Reducing Ω χ 0 1 by changing the SUSY model: Dial up co-annihilation Increase h component of χ 0 1 Increase W 3 component of χ 0 1 These modifications lead to greatly altered collider phenomenology! Astroparticle Physics p. 25/32
109 10 1 m t = 178 GeV, m 0 =800 GeV, m 1/2 = 500 GeV, tanβ= 10, µ > 0, A 0 = 0 P=A 0 / (m 0 2 +m 2 1/2 ) 0.1 Ω χ 0 1 h χ ~0 1 t~ 1 coann P Astroparticle Physics p. 26/32
110 10 1 m t = 178 GeV, m 0 =800 GeV, m 1/2 = 500 GeV, tanβ= 10, µ > 0, A 0 = 0 P = (m 2 H /m2 f ~)-1 P=A 0 / (m 0 2 +m 2 1/2 ) 0.1 Ω χ 0 1 h χ ~0 1 h~ χ ~0 1 t~ 1 coann P Astroparticle Physics p. 27/32
111 10 1 m t = 178 GeV, m 0 =800 GeV, m 1/2 = 500 GeV, tanβ= 10, µ > 0, A 0 = 0 P = (m 2 H /m2 f ~)-1 P=A 0 / (m 0 2 +m 2 1/2 ) 0.1 Ω χ 0 1 h χ ~0 1 h~ P = (M 1 /M 2 )-1, M 1 fixed χ ~0 1 t~ 1 coann. χ 0 1 W~ P Astroparticle Physics p. 28/32
112 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. 29/32
113 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. 29/32
114 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. 29/32
115 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. 30/32
116 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. 30/32
117 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. 30/32
118 Nonstandard cosmology Can either reduce or increase density of stable χ 0 1 Astroparticle Physics p. 31/32
119 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. 31/32
120 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. 31/32
121 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. 31/32
122 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. 31/32
123 4 Summary Dark Energy: Difficult to probe at colliders; perhaps some possibilities if D > 4 Astroparticle Physics p. 32/32
124 4 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. 32/32
125 4 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. 32/32
126 4 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 Much work remains to be done Astroparticle Physics p. 32/32
127 4 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 Much work remains to be done Join the new Astro Particle Working Group! Convenors: A. Djouadi, M. Drees Astroparticle Physics p. 32/32
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