1. From Inflation to Galaxies Formation in the Braneword Scenario Tonatiuh Matos, Miguel Alcubierre, Ruben Cordero, Ricardo Becerril, Hugo Compean, F. Siddhartha Guzman, Dario Nuñez, Luis Ureña, Argelia Bernal, A http:/www.fis.cinvestav.mx/~tmatos Superstrings Model  Braneword  Inflation  DM SnIa Mass Power Spectrum Angular Power Spectrum Galaxies Formation

2. The Model T. Matos, H. Compean, R. Cordero, in preparation. Braneword Scenario: The radion must be stabilized Superstrings  V  f 1 exp(  ) + f 2 exp(-  ) + … V = V 0 [cosh(  ) – 1]  exp(  ) H 2 = 8  /(3M pl 2 )  (1 +  / b )  Inflation  graceful exit  BBN  Cosmology  Fix the free constants.

3. The Cosmology T. Matos and L. Ureña, Class. Q. Grav. 17(2000)L75 Dark Matter:  V 0 [cosh(  ) –1] Dark Energy:   Baryons, Neutrinos, etc.    0.25    0.7  b  0.05

4. Scalar Field Fluctuations T. Matos and L. Ureña, Phys. Rev. D63(2001)063506

5. Results:

6. Natural Cut-off

7. Summarizing SFDM model is insensitive to initial conditions Behaves as CDM 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 V 0  (3  10 -27 M pl ) 4  m   10 -23 eV

8. Numerical Simulations Miguel Alcubierre, F. Siddhartha Guzman, Tonatiuh Matos, Dario Nuñez, Luis A. Ureña and Petra Wiederhold. Class. Quant. Grav 19(2002)5017.

9. Oscillatons

10. 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);

11. The Newtonian Force

12. WIMPs Density profile in Galaxies  (r)  r  as r  0 Numerical Simulations   -1.5  NFW (r)  1/r 1/(r+b) 2 Observations   - 0.5 - 0 Number of Dwarf Galaxies >>

13. Dwarf Galaxies

14. The Critical Mass Tonatiuh Matos and F. Siddhartha Guzman, Class.Q. Grav. 18(2001)5055 M  0.1 M 2 Planck /m  If m m  10 -23 eV M  10 12 Mo

15. Perfil de densidad

16. Galaxy Formation at z=7

17. Metalicity in z=2

18. Scalar Field DM Cross Section Tonatiuh Matos and Luis A. Ureña, Phys. Lett. B538 (2002)246. cosh is renormalizable SFDM   2  2 / m  = 8  2 exp(I 2 )/[64  (m  ) 3 ] Reparametrizations factor  = exp[ 2  o  2 /(32  2 )] Internal Contraction I  1/(16  2 ) If   2 M Pl  2  2 / m  = 10 -25 - 10 -23 cm 2 /GeV

19. The Inflaton as SFDM James Lidsey, Tonatiuh Matos and Luis A. Ureña, Phys.Rev.,D66(2002)023514. Braneworld scenario: H 2 = 8  /(3M pl 2 )  (1 +  / b ) b  2.88  10 51 GeV 4 V  V 0 exp(  (8  )/ M pl )  i  1.94 M pl V i  1.63  10 56 GeV 4  end  1.90 M pl V end  2.33  10 54 GeV 4 M pbh  10 9 M pl t evap  10 -16 s  0  10 -18  Einst < 1.80 M pl  Einst. << b  pbh > 1.06 M pl  exp > 0.01 M pl

20. Conclusion The scalar field is a good candidate to be the Dark Matter of the Universe