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 Too early metalicity formation Etc.

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)

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

Cosmology from Superstrings Theory R. Kallosh R. Brandenberger

IIB Superstrings theory with Fluxes Phys.Rev.D67:046006,2003 Type IIB Superstrings With Fluxes

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

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

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  10-23 eV M 1012 Mo

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



u

Omegas

Omegas exp() zoom

Direct Proof of DM (Chandra)

Density Profiles

Density Profiles LSB Galaxies

Density Profiles LSB Galaxies

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

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

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