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Relic abundance of dark matter in the Minimal Universal Extra Dimension model

in collaboration with Shigeki Matsumoto (KEK) Mitsuru Kakizaki (Bonn Univ.). Relic abundance of dark matter in the Minimal Universal Extra Dimension model. Masato Senami (ICRR, University of Tokyo) senami@icrr.u-tokyo.ac.jp. Phys. Rev. D 71, 123522 (2005)

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Relic abundance of dark matter in the Minimal Universal Extra Dimension model

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  1. in collaboration with Shigeki Matsumoto (KEK) Mitsuru Kakizaki (Bonn Univ.) Relic abundance of dark matterin the Minimal Universal Extra Dimension model Masato Senami (ICRR, University of Tokyo) senami@icrr.u-tokyo.ac.jp Phys. Rev. D 71, 123522 (2005) Nucl. Phys. B 735, 84 (2006) Phys. Lett. B 633, 671 (2006) Phys. Rev. D 74, 023504 (2006)

  2. Kaluza-Klein dark matter • Non-baryonic cold dark matter is established. • Weakly Interacting Massive Particle (WIMP) is excellent candidate • Relic abundance • Large scale structure • WIMP candidate • Lightest supersymmetric particle • Lightest Kaluza-Klein particle (LKP) in universal extra dimension (UED) models • …

  3. Universal Extra Dimension model Appelquist, Cheng, Dobrescu (2000) Universal means all SM particles propagate in spatial extra dimensions • KK tower appear (All particle has KK particles) • KK number n conservation KK number conservation Orbifold Compactification For deriving chiral fermion zero modes, an extra dimension is compactified on an orbifold KK parity conservation nevertheless stable LKP is a good candidate for dark matter c.f. R-parity and LSP

  4. The Minimal UED model • The Minimal Universal Extra Dimension model (MUED) • Five space-time dimension • The extra dimension is compactified on • MUED model brings only two new parameters. (extra dimension size ) (cut off scale ) in addition to the standard model parameter, mh

  5. Appelquist, Yee 2003;Gogoladze, Macesanu 2006 600 400 mh (GeV) allowed region 200 400 200 600 1/R (GeV) Constraint on 1 / R • Consistent with • muon g-2 • oscillation • B and K meson decays • Electroweak precision measurements • Allowed region • 1 / R > 300 GeV • 114 GeV < mh < 900 GeV This allowed region is limited by this work in cosmological reason.

  6. 1-loop corrected mass spectrum degenerate in mass Cheng, Matchev, Schmaltz (2002) Which particle is the LKP? • KK particle has degenerate mass in tree level • Radiative corrections remove the degeneracy LKP : • some KK particle are well degenerate with LKP (SM massless particles are exactly degenerate) 1/R=500 GeV, ΛR=20, mh=120 GeV 1～5％

  7. Relic abundance Decoupling Increasing Co-moving number density thermal equilibrium x = m / T (time) Coannihilation δ=O(1)% : MUED model • Some KK particles are degenerate with LKP in mass. • Coannihilation changes relic abundance of DM. < abundance is increased > abundance is decreased c.f. In SUSY models, coannihilation effects decrease the abundance

  8. Previous calculations • Coannihilation changes relic abundance of DM. • Kong, Matchev (2005), Burnell, Kribs(2005) • Effective annihilationcross section is decreased. • mh=120 GeV is assumed. • resonance processes are not included. • But,Relic abundance is dependent on • SM Higgs mass • second KK particle resonance processes Kong, Matchev (2005) 1/R (GeV)

  9. Excluded (Charged LKP) ,smaller larger KK Higgs particle • KK Higgs mass • larger KK particles for Goldstone boson enhance annihilation of KK Higgs

  10. Charged Higgs LKP • Too large • Charged KK Higgs is the LKP • Charged LKP • Charged LKP can not be a candidate for dark matter. • Charged LKP (1 / R < 1 TeV) • Excluded by the anomalous heavy water molecule search in sea water if TR> 1 MeV. • Inconsistent with the successful big bang nucleosynthesis.

  11. Constraint from electroweak precision measurements 1/R > 400 GeV mh < 300 GeV Electroweak precision measurements and charged LKP constraints 600 Excluded (Charged LKP region) 400 mh (GeV) 200 Allowed region 600 400 200 1/R (GeV)

  12. Result without resonance Excluded (Charged LKP region) KK Higgs coannihilation region Bulk region Allowed regionwithout resonance processes Dark shaded region is consistent with observed abundances.

  13. Two allowed region • Small mh (Bulk region) • Consistent with previous results • Largemh (KK Higgs coannihilation region) • Relic abundance is decreased drastically, allowed value of 1/R is increased. • This is due to the KK Higgs coannihilation.

  14. total LKP KK lepton KK Higgs total LKP KK lepton KK Higgs KK Higgs coannihilation region g : degree of freedom of KK particles • For large mh • large cross section of KK Higgs annihilation • and degenerated with LKP • free from a Boltzmann suppression after KK leptons decoupling • large contribution to Difference : KK Higgs

  15. KK Higgs coannihilation region sudden freeze-out Late time enhancement of the cross section reduces the abundance after the departure from equilibrium KK lepton decoupling • After sudden freeze-out, cross section may be increased. • Dark matter annihilation can decrease the relic abundance significantly after sudden freeze-out. • In UED models, the KK dark matter abundance should be calculated till late enough time.

  16. Resonance processes • Important processes • DM is non-relativistic • The energy of two first KK particles is almost degenerate with the mass of second KK modes • Resonance process mediated by second KK particles are important. SM KK(1) KK(2) KK(1) SM

  17. Result with resonance process Excluded (Charged LKP region) • Allowed region is shifted to larger 1/R by 150-300 GeV • For 1/R<800GeV, the KK graviton may be the LKP without resonance with resonance the KK graviton problem

  18. Resonance effects without resonance • origin of the shift All resonances KK Higgs Coannihilation region without resonance Bulk region

  19. Excluded (Charged LKP region) overabundance Summary • Relic abundance of the LKP is reduced by • KK Higgs coannihilation • second KK resonance processes • Allowed region • 600GeV<1/R<800GeV • mh < 230 GeV

  20. KK Graviton is LKP 1/R (GeV) KK Graviton • 1/R < 800GeV • KK graviton may be LKP i.e. DM is SuperWIMP • CMB and diffuse gamma exclude KK graviton DM • 1>R 800GeV • MUED is consistent with DM relic abundance only if mh > 180GeV. Feng, Rajaraman, Takayama, PRL91, PRD68 • KK graviton become heavy • Higher space-time dimension > MUED • KK particle in MUED in five dimension space-time • KK graviton in higher dimensional space-time K. R. Dienes, PRL88

  21. Relic abundance Decoupling Increasing Co-moving number density thermal equilibrium x = m / T (time) Dark matter relic abundance • General picture • At T ~ m (x~1), dark matter particle is in thermal equilibrium. • After annihilation rate dropped below the Hubble parameter, dark matter can not annihilate and the density per comoving volume is fixed. • Large cross section small relic abundance of dark matter

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