1. Galaxy formation from the IIB Superstring with Fluxes Tonatiuh Matos

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 Scalar Field Dark Matter 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 Fluxes Phys.Rev.D67:046006,2003
Type IIB Superstrings With Fluxes

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

9. Bose-Einstein Condensates
Tc  TeV
m < eV
Mcrit  0.1 M2Planck /m

10. M  0.1 M2Planck /m If m  10-23 eV M 1012 Mo
Scalar Field Fluctuation = Halo Tonatiuh Matos and F. Siddhartha Guzman Class. 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  eV
M 1012 Mo

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

12. 

13. u

14. Omegas

15. Omegas
exp() zoom

16. Direct Proof of DM (Chandra)

17. Density Profiles

18. Density Profiles
LSB Galaxies

19. Density Profiles
LSB Galaxies

20. 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  eV

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

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