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Gravitons and Dark Matter in Universal Extra Dimensions

Gravitons and Dark Matter in Universal Extra Dimensions. Nausheen R. Shah Carlos E. M. Wagner PRD 74:104008, 2006 [ arXiv : hep-ph/0608140] Enrico Fermi Institute and Kavli Institute for Cosmological Physics, University of Chicago. HEP Division, Argonne National Labs .

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Gravitons and Dark Matter in Universal Extra Dimensions

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  1. Gravitons and Dark Matter in Universal Extra Dimensions Nausheen R. Shah Carlos E. M. Wagner PRD 74:104008, 2006 [arXiv: hep-ph/0608140] Enrico Fermi Institute and Kavli Institute for Cosmological Physics, University of Chicago. HEP Division, Argonne National Labs.

  2. Universal Extra Dimensions • Models beyond Standard Model (SM) frequently imply the existence of extra dimensions (ED). • Simplest incorporation of ED: Universal Extra Dimensions (UED). • All fields propagate in ED. • Only one free parameter: mKK~1/R. Nausheen R. Shah Cosmo 08

  3. Universal Extra Dimensions • D = 5: S1/Z2 (-1)KKKK Parity LKP Stable LKP DM Candidate w/ mKK ~ O(1) TeV Nausheen R. Shah Cosmo 08

  4. Gravitons? • G1 as the LKP very tightly constrained by Big Bang Nucleosynthesis (BBN) and diffuse gamma spectrum. • Usually effect of the G1considered not important, when it is not the LKP, since all interactions are Planck suppressed. • We will show that in fact the gravitons can have significant effects on the DM density. Nausheen R. Shah Cosmo 08

  5. Reheating Temperature Thermal Production of LKP Non-thermal Graviton Production Via Collisions LKP Freeze Out BBN BBN and Diffuse Gamma Ray Constraints on Graviton Decay. Gravitons decay to the LKP • WGn~ C [TR / mKK]7/2 • C~O(1) Present Day WDM = WLKP + WGn Nausheen R. Shah Cosmo 08

  6. Reheating Temperature • Demanding that WDM = WLKP + WGnbe consistent with observation constrains the reheating temperature, TR, as a function of the LKP mass: Nausheen R. Shah Cosmo 08

  7. Values of TR obtained by demanding a proper DM density, for different values of the graviton production parameter, C, for D=5. Also shown are lines of constant ratios of TR to the LKP mass. Nausheen R. Shah Cosmo 08

  8. Additional Contributions to the Annihilation Cross-Section • A precise calculation of LKP density must include co-annihilation and second KK resonances effects. This changes the numerical results obtained, but the qualitative picture presented remains unchanged. • These corrections can be quantified by noting that due to the weak logarithmic dependence of xF, we can approximately parameterize Y as being proportional to mKK: • The change in mWG necessary to reproduce the correct DM density for a given TR: Nausheen R. Shah Cosmo 08

  9. Ratio of the LKP mass consistent with DM density to the one obtained in the absence of gravitons, mWG, for TR = 20 mKK and D=5 Nausheen R. Shah Cosmo 08

  10. TR = 40 mKK, D = 5. Nausheen R. Shah Cosmo 08

  11. TR = 100 mKK, D=5. Nausheen R. Shah Cosmo 08

  12. Decay Lifetimes Gn, for n>1, primarily decays to a pair of gauge bosons with equal KK numbers, with lifetime given by: Only long lived graviton is G1: Nausheen R. Shah Cosmo 08

  13. Constraints on the G1-B1 mass difference. • If we assume that TR is such that W = 0.23, we find that to preserve BBN predicted light element abundances : • Requiring that late decays don’t destroy the diffuse photon flux: Nausheen R. Shah Cosmo 08

  14. Combined constraints due to both BBN and observed diffuse flux on the mass difference. Nausheen R. Shah Cosmo 08

  15. One Loop Corrections to the KK Masses. • The gauge boson mass matrix due to the Higgs vev in the B n, W 3n basis: • Since the mixing is very small, the first KK mode of the photon is very well approximated by the B1: Nausheen R. Shah Cosmo 08

  16. Absolute value of the one loop corrections to the B1 mass in the MUED as a function of mKK. The graviton would be the LKP below masses ~ 800 GeV. Nausheen R. Shah Cosmo 08

  17. Determining TR • Due to small couplings to matter, provided the G1 is not the LKP, it will not be produced in laboratory experiments. • If conclusive evidence for UED is found in collider experiments, and relevant properties of the first and second modes were measured, then assuming that no other exotic particle exists, we could estimate the contribution of the Gnto WDM, and therefore be able to infer TR. Nausheen R. Shah Cosmo 08

  18. If LKP observed at LHC, the reheating temperature required to make up the deficit DM density by KK gravitons. Nausheen R. Shah Cosmo 08

  19. Conclusion • We have studied the cosmological effects of the inclusion of the KK graviton tower in detail. • Conventionally, due to Planck suppression, the graviton has been ignored. We have shown that it can in fact have significant effects. • Requiring that the graviton decays don’t destroy BBN predicted light element abundances and the diffuse gamma ray flux, we have obtained a bound on the mass difference between the G1 and the LKP, which is consistent with the one obtained from one loop corrections in the MUED for a large range of values of mKK. • If UED is observed experimentally, we show that an upper limit on the reheating temperature can be deduced. Nausheen R. Shah Cosmo 08

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