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Problems with the  CDM Model

Galaxy formation from the IIB Superstring with Fluxes Tonatiuh Matos http:/www.fis.cinvestav.mx/~tmatos. Problems with the  CDM Model. Dark Energy: Extreme fine tuning for  Coincidence Dark Matter: Cuspy central density profiles Too much substructure Too late galaxy formation

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Problems with the  CDM Model

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  1. Galaxy formation from the IIB Superstring with FluxesTonatiuh Matoshttp:/www.fis.cinvestav.mx/~tmatos

  2. Problems with the CDM Model • Dark Energy: • Extreme fine tuning for  • Coincidence • Dark Matter: • Cuspy central density profiles • Too much substructure • Too late galaxy formation • Too early metalicity formation • Etc.

  3. Some Alternatives • Self-Interacting DM • Warm DM • Super Heavy DM • Self-Annihilating DM • Repulsive DM • Fuzzy DM • Decaying DM • Scalar Field Dark Matter • V = V0 (cosh()-1)

  4. Cosmology from Superstrings Theory • R. Kallosh • R. Brandenberger • D. Wands, etc.

  5. Cosmology from Superstrings Theory • R. Kallosh • R. Brandenberger

  6. IIB Superstrings theory with FluxesPhys.Rev.D67:046006,2003 • Type IIB Superstrings With Fluxes

  7. Bose-Einstein Condensate  + dV/d = 0 • V = V0[cosh() – 1]

  8. Bose-Einstein Condensates • Tc TeV • m < 10-17 eV • Mcrit 0.1 M2Planck /m

  9. Scalar Field Fluctuation = HaloTonatiuh Matos and F. Siddhartha GuzmanClass. Q. Grav. 17(2000)L9; Tonatiuh Matos, F. Siddhartha Guzman and Dario Nuñez, Phys. Rev. D62(2000)061301(R);Tonatiuh Matos and F. Siddhartha Guzman,Class.Q. Grav. 18(2001)5055 • M  0.1 M2Planck /m • If m  10-23 eV • M 1012 Mo

  10. The ModelT. Matos, R. Luevano, H. H. Garcia Compean. • Inflation • hin • V = V0[cosh() – 1] +Axion •  exp() F2

  12. u

  13. Omegas

  14. Omegas exp()zoom

  15. Direct Proof of DM (Chandra)

  16. Density Profiles

  17. Density Profiles LSB Galaxies

  18. Density Profiles LSB Galaxies

  19. Summarizing • The IIB Superstring model: • Behaves as CDM after recombination. • Reproduces all the successes CDM above galactic scales. • Predicts a sharp cut-off in the mass power spectrum • The favored values for the two free parameters •  20 V0 (310-27 Mpl )4  m 10-23 eV

  20. Conclusions • The differences between IIB superstrings and CDM: • 1) Recombination • 2) Center of the Galaxies

  21. Conclusion • The Dilaton could be a good candidate to be the Dark Matter of the Universe

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