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Inflation Cosmology Galaxies Formation

The Scalar Field Dark Matter Model Tonatiuh Matos, Miguel Alcubierre, Ruben Cordero, Ricardo Becerril, F. Siddhartha Guzman, Dario Nuñez, Luis Ureña, Argelia Bernal, A http:/www.fis.cinvestav.mx/~tmatos. Inflation Cosmology Galaxies Formation. Problems with the CDM Model. Dark Energy:

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Inflation Cosmology Galaxies Formation

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  1. The Scalar Field Dark Matter ModelTonatiuh Matos, Miguel Alcubierre, Ruben Cordero, Ricardo Becerril, F. Siddhartha Guzman, Dario Nuñez, Luis Ureña, Argelia Bernal,Ahttp:/www.fis.cinvestav.mx/~tmatos • Inflation • Cosmology • Galaxies Formation

  2. Problems with the CDM Model • Dark Energy: • Extrem Fine Tuning • Coincidence • Dark Matter: • WIMP’s

  3. 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 >>

  4. LSB Galaxies

  5. Galaxy Formation at z=7

  6. Metalicity at z=2

  7. The ModelT. Matos, 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.

  8. 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

  9. Scalar Field FluctuationsT. Matos and L. Ureña,Phys. Rev. D63(2001)063506

  10. Results:

  11. Natural Cut-off

  12. 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

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

  14. Oscillatons

  15. Oscillatons

  16. 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

  17. 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

  18. Density Profiles for LSB

  19. 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

  20. 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

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

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