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Inflation + CDM Model = Cosmology Galaxies Formation

Bose-Einstein Condensates as Galactic Dark Matter Halos Tonatiuh Matos, F. Siddhartha Guzman, Luis Ureña, Dario Nuñez, Argelia Bernal. http:/www.fis.cinvestav.mx/~tmatos. Inflation + CDM Model = Cosmology Galaxies Formation. Mass Power Spectrum. Angular Power Spectrum. Summarizing.

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Inflation + CDM Model = Cosmology Galaxies Formation

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  1. Bose-Einstein Condensates as Galactic Dark Matter HalosTonatiuh Matos, F. Siddhartha Guzman, Luis Ureña, Dario Nuñez, Argelia Bernal.http:/www.fis.cinvestav.mx/~tmatos • Inflation • + • CDM Model • = • Cosmology • Galaxies Formation

  2. Mass Power Spectrum

  3. Angular Power Spectrum

  4. Summarizing • M ~ 0.27  0.1, •  ~ 0.73  0.1 • 0 ~ 1. • Everything OK!!. • The Matter Components • M = b +  +  ~ • 0.04 + DM, • Where DM ~ 0.23. • But DM non  ??. DM + ~ 0.96

  5. 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.

  6. 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 >>

  7. LSB Galaxies

  8. Galaxy Formation at z = 7 and z = 2

  9. Metalicity at z=2

  10. Some Alternatives • 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)

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

  12. Bose-Einstein Condensates

  13. Bose-Einstein Condensates

  14. Bose-Einstein Condensates

  15. Bose-Einstein Condensates

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

  17. Natural Cut-off

  18. 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

  19. 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

  20. 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

  21. 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

  22. Density Profiles

  23. Density Profiles

  24. Density Profiles LSB Galaxies

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

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