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Oscillatons as Galactic Dark Matter Halos Tonatiuh Matos http:/fis.cinvestav.mx/~tmatos

Oscillatons as Galactic Dark Matter Halos Tonatiuh Matos http:/www.fis.cinvestav.mx/~tmatos. Inflation + Scalar Field DM (SFDM) + Dark Energy. The model consists of. Cosmology + Galaxies Formation. =. THE SCALAR FIELD DARK MATTER MODEL.

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Oscillatons as Galactic Dark Matter Halos Tonatiuh Matos http:/fis.cinvestav.mx/~tmatos

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  1. Oscillatons as Galactic Dark Matter HalosTonatiuh Matoshttp:/www.fis.cinvestav.mx/~tmatos • Inflation • + • Scalar Field DM (SFDM) • + • Dark Energy • The model consists of Cosmology + Galaxies Formation =

  2. THE SCALAR FIELD DARK MATTER MODEL • It is an alternative model to CDM • SFDM model is insensitive to initial conditions • Behaves as CDM at cosmological scales • 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

  3. The Model comes from • Examples: • Braneword Scenario • Superstrings  • contain effective SF potentials: • V  f1exp() + f2exp(-) + … •  • V = V0[cosh() – 1] • If • H2 = 8/(3Mpl2)  (1 + /b) •  Inflation  graceful exit •  BBN  Cosmology  • Fix the free constants. • James Lidsey, Tonatiuh Matos and Luis A. Ureña. PhysRevD66(2002)023514.

  4. The CosmologyT. Matos and L. Ureña, Class. Q. Grav. 17(2000)L75 • SFDM with the SF potential: •  V = V0[cosh() –1] • Dark Energy:   • + • Baryons, Neutrinos, etc. •    0.23 •    0.73 • b  0.04

  5. Scalar Field FluctuationsT. Matos and L. Ureña,Phys. Rev. D63(2001)063506 The linear fluctuations of the SFDM model follow the CDM ones

  6. Natural Cut-off The linear fluctuations contain a natural cut-of in the mass power spectrum. Thus, this model has no problems with the production of substructure.

  7. Scalar Field Fluctuation = Oscillaton = Galaxy HaloTonatiuh Matos and F. Siddhartha GuzmanClass. Q. Grav. 17(2000)L9; T. Matos, F. S. Guzman and D. Nuñez, Phys. Rev. D62(2000)061301(R);Tonatiuh Matos and F. Siddhartha Guzman,Class.Q. Grav. 18(2001)5055 The critical mass of oscillatons collapse is • Mcrit 0.1 M2Planck /m • If m  10-23 eV   20 • Mcrit  1012 M¯~ Galaxy halo

  8. Galaxy virialization • The oscillatons virialize in a very short time. In this figure it is shown the rate of kinetic energy K and potential energy |W| of the scalar field fluctuation. It goes very fast to ½.

  9. Density Profiles Here we show the comparison between the NFW, Isothemal and the SFDM density profiles for galaxies.

  10. Density Profiles

  11. Density Profiles LSB Galaxies

  12. Density Profiles LSB Galaxies

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

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