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Bose-Einstein Condesates as Galactic Dark Matter Halos Tonatiuh Matos, F. Siddhartha Guzman, Luis Ureña, Dario Nuñez, Argelia Bernal. Inflation + CDM Model = Cosmology Galaxies Formation

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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.

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The Model Examples: Braneword Scenario Superstrings V f 1 exp( ) + f 2 exp(- ) + … V = V 0 [cosh( ) – 1] H 2 = 8 /(3M pl 2 ) (1 + / b ) Inflation graceful exit BBN Cosmology Fix the free constants.

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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

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

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Natural Cut-off

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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 M pl ) 4 m eV

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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 M 2 Planck /m If m m eV M Mo

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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

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Density Profiles

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LSB Galaxies

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

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