Gravitino LSP as Dark Matter in the Constrained MSSM

Transcription

1 Gravitino LSP as Dark Matter in the Constrained MSSM Ki Young Choi The Dark Side of the Universe, Madrid, June 2006 Astro-Particle Theory and Cosmology Group The University of Sheffield, UK In collaboration with Cerdeño, Jedamzik, L.Roszkowski, R.Ruiz de Austri

2 1 Contents Dark matter Supersymmetry and Gravitino Problem Gravitino as Dark Matter Cosmic Lithium Problems with Gravitino Implications on vacuum structure of Universe Summary

3 2 Evidence for Dark Matter Rotation curves of galaxies in 21cm line from hyperfine splitting Flat behavior beyond the visible disks M(r) r, ρ 1/r 2 Mass of a cluster of galaxies Distribution of hot gas from X-ray emission Shape of the potential well using weak gravitational lensing

4 3 Cosmic Microwave Background WMAP satellitet 3-year results (2006) Ω m h 2 = ± Ω b h 2 = ± Ω DM = ± h =

5 3 Cosmic Microwave Background WMAP satellitet 3-year results (2006) Ω m h 2 = ± Ω b h 2 = ± Ω DM = ± h = What is Dark Matter

6 4 Particle Dark Matter Y/Y 0, Y = n X /s Hot Relic Increasing σv = = Cold Relic Standard Model neutrinos Ω ν h 2 = m i 93 ev < (WMAP) WIMP(Weak Interacting Massive Particle) is strongly favored Freeze-out of a massive particles Ω X = m X n X 109 GeV 1 x f g 1/2 M P σ A v Beyond Standard Model Y EQ x = m X /T

7 5 Supersymmetry Standard Model particles are doubled by superpartners LSP(Lightest Supersymmetric Particle) is stable with R-parity and a good candidate for Dark Matter Which is LSP?

8 5 Supersymmetry Standard Model particles are doubled by superpartners LSP(Lightest Supersymmetric Particle) is stable with R-parity and a good candidate for Dark Matter Which is LSP? Neutralino?

9 5 Supersymmetry Standard Model particles are doubled by superpartners LSP(Lightest Supersymmetric Particle) is stable with R-parity and a good candidate for Dark Matter Which is LSP? Neutralino? or Gravitino?

10 5 Supersymmetry Standard Model particles are doubled by superpartners LSP(Lightest Supersymmetric Particle) is stable with R-parity and a good candidate for Dark Matter Which is LSP? Neutralino? or Gravitino? χ 0 G

11 6 Gravitino Problem T R > T f Primordial Gravitino Freeze-out from thermal eq. Ω Gh m 1.17 G g 1 kev unstable : m G 10 TeV stable : m G 1 kev or Gravitino dilution T R < T f Diluted out by inflation Reproduced by thermal scatterings Ω Gh 2 TR GeV GeV m G m g (T ) 1T ev unstable : T R 10 8 GeV from BBN 2 stable : T R GeV from Ω tot < 1

12 7 Gravitino LSP in the CMSSM Constrained MSSM At M GUT gauginos M 1 = M 2 = M 3 = m 1/2 scalars m 2 q = m2 l = m 2 H b = m 2 H t = m 2 0 trilinear soft terms A b = A t = A 0 radiative EWSB five independent parameters: tan β, m 1/2, m 0, A 0, sgn(µ) Free parameter: m G M SUSY Experimental constraints m χ ± > 104 GeV(LEP) light higgs: m h > GeV(LEP) BR(B X s γ)= (3.34 ± 0.68) 10 4 e.g., tan β = 10, µ > 0, m G = m 0 G not LSP χ NLSP τ NLSP

13 8 Gravitino Relic abundance Thermal production: from thermal scattering, ( Ω T G P h2 0.2 TR GeV ) ( 100GeV m G ) ( ) m g (T ) 2 1T ev [Bolz,Brandenburg,Buchmüller., (2001)] Non-thermal production: from the decay of NLSP (τ sec) Ω NT P G h 2 = m G m NLSP Ω NLSP h 2 Total Gravitino relic abundance Ω Gh 2 Ω T P G h2 + Ω NT P G h 2

14 9 m G = m 0 Gravitino Relic abundance Ω Gh 2 = Ω T P G h2 + Ω NT P G h 2 ===== < Ω Gh 2 < (WMAP) ==== T R = GeV ==== small T R T R = 10 9 GeV D.Cerdeño, K.Jedamzik, K-Y C, L.Roszkowski, R.Ruiz de Austri, JCAP(2006)

15 10 NLSP decay (1 τ sec) NLSP decay produces photons and hadrons with high energy χ NLSP χ Gγ τ NLSP EM showers τ Gτ EM showers χ GZ, GHiggs, Gγ /Z τ GτZ, Gν τ W, Gτγ /Z had showers had showers Late time decay due to gravitational interaction: sec The high energy injection(em,had) at late times during or after BBN changes the light element abundances Strong constraints on NLSP

16 11 BBN constraints BBN constraints conservative observational limit m G = m 0, T R = 10 9 GeV < D/H < < Y p < < 7 Li/H < He/D < Li/ 7 Li < CMB constraints dimensionless chemical potential µ µ < D/H+Y p + 7 Li/H+ 3 He/D+ 6 Li/ 7 Li

17 12 BBN constraints χ NLSP is inconsistent with BBN : still possibility for sub-gev Gravitino (τ χ < 1 sec) m G = m 0, T R = 10 9 GeV τ NLSP region is allowed CMB constraint is weaker than BBN: potentially important for more precise CMB measurements How high T R is possible? D/H+Y p + 7 Li/H+ 3 He/D+ 6 Li/ 7 Li D.Cerdeño, K.Jedamzik, K-Y C, L.Roszkowski, R.Ruiz de Austri, JCAP(2006)

18 13 BBN constraints m G = 0.2m 0, T R = 10 9 GeV m G = 100 GeV, T R = 10 9 GeV D.Cerdeño, K.Jedamzik, K-Y C, L.Roszkowski, R.Ruiz de Austri, JCAP(2006)

19 14 Cosmic Lithium Problems Standard BBN predicts factor 2-3 more 7 Li than observed at low [Z] Standard BBN synthesize 6 Li around 6 Li/H orders below than observed Mathews et al., PRD (2005) η 10 = n B /n γ 10 10

20 15 Cosmic Lithium Problems and Gravitino Relic particle decay destruct 7 Li and produce 6 Li 7 Li overproduced, 6 Li solved 7 Li solved, 6 Li underproduced 7 Li solved, 6 Li solved K.Jedamzik, K-Y Choi, L.Roszkowski, R.Ruiz de Austri, (2005)

21 16 Ω Gh 2 τ NLSP m G m NLSP v 0 Ω Gh 2 Ω Gh , τ NLSP 10 3 sec m NLSP 1 TeV, m G 100 GeV v km/sec free streaming velocity at present 0.1 from matter power spectrum Jedamzik et al., (2005) K.Jedamzik, K-Y Choi, L.Roszkowski, R.Ruiz de Austri, (2005)

22 17 Vacuum structure of the Universe charge and/or color breaking (CCB) minima unbounded from below (UFB) directions (UFB-1,2,3) Among them, UFB-3= {H u, ν Li, e Lj, e Rj }, i j direction leads to electric charge breaking also (the strongest constraints) [Casas, Lleyda, Muñoz( 96)] tan β = 10, A 0 = 0 Condition V UFB-3 (Q = ˆQ) > V real min We live in a meta-stable state! D.Cerdeño, K.Jedamzik, K-Y Choi, L.Roszkowski, R.Ruiz de Austri, (2005)

23 17 Vacuum structure of the Universe charge and/or color breaking (CCB) minima unbounded from below (UFB) directions (UFB-1,2,3) Among them, UFB-3= {H u, ν Li, e Lj, e Rj }, i j direction leads to electric charge breaking also (the strongest constraints) [Casas, Lleyda, Muñoz( 96)] tan β = 50, 10, A 0 = 0 Condition V UFB-3 (Q = ˆQ) > V real min We live in a meta-stable state! D.Cerdeño, K.Jedamzik, K-Y Choi, L.Roszkowski, R.Ruiz de Austri, (2005)

24 17 Vacuum structure of the Universe charge and/or color breaking (CCB) minima unbounded from below (UFB) directions (UFB-1,2,3) Among them, UFB-3= {H u, ν Li, e Lj, e Rj }, i j direction leads to electric charge breaking also (the strongest constraints) [Casas, Lleyda, Muñoz( 96)] tan β = 50, 10, A 0 = 0 Condition V UFB-3 (Q = ˆQ) > V real min We live in a meta-stable state! D.Cerdeño, K.Jedamzik, K-Y Choi, L.Roszkowski, R.Ruiz de Austri, (2005)

25 18 Summary Gravitino can be a good candidate for Dark Matter Neutralino NLSP and O(100)GeV Gravitino LSP is disfavored by BBN Stau NLSP and Gravitino LSP is a possible combination in CMSSM Both Lithium problems can be solved simultaneously by the decay of a stau relic 1000 sec after the Big Bang Stau NLSP indicate a hint about the vacuum structure of our Universe

26 19 Constraint on Reheating Temperature tan β = 10, m 1/2 = 500GeV, m 0 = 50GeV( τnlsp) Ω Gh 2 = Ω T P G h2 + Ω NT P G h 2 T R GeV for m G 30 GeV D.Cerdeño, K.Jedamzik, K-Y Choi, L.Roszkowski, R.Ruiz de Austri, (2005)

27 20 Contents of present Unverse WMAP data with other CMB experiments (ACBAR and CBI), 2dFGRAS measurements, and Lyα forest data determines the best-fit cosmological parameters[spergel et.al, (2003)]: 8 Ω tot = Ω Λ + Ω m + = 1.02 ± 0.02 (Flat Universe) energy Ω Λ = 0.73 ± 0.04 (accelerating) Ω tot = >< >: matter Ω m = 0.27 ± 0.04 radiation 8 < : Ω b h 2 = ± (BBN, CMB) Ω DM h 2 = Ω ν h 2 < (h = ) Ω γ = (2.471 ± 0.004) 10 5 (T 0 = ± 0.002K 95% CL)

28 21 Supersymmetry Extends SM with superpartners Solves hierarchy problem Gauge coupling unification Radiative EW symmetry breaking Possible new source for CP and flavor Lightest Supersymmetric Particle: non-baryonic dark matter candidate Neutralino

29 22 Gravitino Problem If T R > T f, Gravitino freezes ( out ) from thermal equilibrium with the relic density Ω Gh ( m = 1.17 G ) g 1 kev Ω G ρ G ρ c Stable : m G 1 kev from Ω tot < 1 or Gravitino dilution Unstable : m G 10 TeV from BBN constraint If T R < T f, the freeze-out Gravitino is diluted away by Inflation and reproduced by thermal scattering in the reheating period with abundance ( ) ( ) Y G n G nγ = m2 g TR 12m 2 G GeV T R : Reheating temperature [Bolz,Brandenburg,Buchmüller, (2001)]

30 23 unstable : T R 10 8 GeV from BBN [Ellis,Kim,Nanopoulos( 84), Cyburt et al.( 02), Kawasaki et al.( 04)] stable : T R GeV from Ω tot < 1 Ωh 2 = m 100 GeV Y

31 24 Gravitino Relic abundance m G = m 0 Non-thermal production: NLSP decay Ω Gh 2 > χ NLSP χ Gγ χ GZ, GHiggs, G(γ /Z )q q = < Ω NT P G h 2 < τ NLSP τ Gτ τ GτZ, Gν τ W s, Gτ(γ /Z )q q Ω Gh 2 < Ω NT P G h 2 = m G m NLSP Ω NLSP h 2

32 25 Combining UFB and BBN For T R = 10 9 GeV, m G = m 0, tan β = 10 m G = 0.2m 0, tan β = 50 all excluded small regions left allowed

33 26 m G = 10 GeV, tan β = 10 m G = 100 GeV, tan β = 50