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Superstrings Model  Braneword  Inflation  DM SnIa Mass Power Spectrum

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 

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Superstrings Model  Braneword  Inflation  DM SnIa Mass Power Spectrum

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

  2. The ModelT. Matos, H. Compean, R. Cordero, in preparation. • Braneword Scenario: • The radion must be stabilized • Superstrings  • V  f1exp() + f2exp(-) + … • V = V0[cosh() – 1]  exp() • H2 = 8/(3Mpl2)  (1 + /b) •  Inflation  graceful exit •  BBN  Cosmology  • Fix the free constants.

  3. The CosmologyT. Matos and L. Ureña, Class. Q. Grav. 17(2000)L75 • Dark Matter: •  • V0[cosh() –1] • Dark Energy: •   • Baryons, • Neutrinos, etc. •    0.25 •    0.7 • b  0.05

  4. Scalar Field FluctuationsT. 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 V0  (310-27 Mpl )4  m  10-23 eV

  8. Numerical SimulationsMiguel Alcubierre, F. Siddhartha Guzman, Tonatiuh Matos, Dario Nuñez, Luis A. Ureña and Petra Wiederhold. Class. Quant. Grav19(2002)5017.

  9. Oscillatons

  10. 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);

  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 MassTonatiuh Matos and F. Siddhartha Guzman,Class.Q. Grav. 18(2001)5055 • M  0.1 M2Planck /m • If m  10-23 eV • M 1012 Mo

  15. Perfil de densidad

  16. Galaxy Formation at z=7

  17. Metalicity in z=2

  18. Scalar Field DM Cross SectionTonatiuh Matos and Luis A. Ureña, Phys. Lett. B538 (2002)246. • cosh is renormalizable • SFDM  • 22/ m = 82exp(I2)/[64(m)3] • Reparametrizations factor •  = exp[2o2/(322)] • Internal Contraction I  1/(162) • If   2 MPl • 22/ m = 10-25 - 10-23 cm2/GeV

  19. The Inflaton as SFDMJames Lidsey, Tonatiuh Matos and Luis A. Ureña,Phys.Rev.,D66(2002)023514. • Braneworld scenario: H2 = 8/(3Mpl2)  (1 + /b) • b  2.881051GeV4 • V  V0exp((8)/ Mpl) • i  1.94 Mpl Vi  1.631056GeV4 • end  1.90 Mpl Vend  2.331054GeV4 • Mpbh  109 Mpl tevap  10-16 s 0  10-18 • Einst < 1.80 Mpl Einst. << b • pbh > 1.06 Mpl • exp > 0.01 Mpl

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

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