Oscillatons as Galactic Dark Matter Halos Tonatiuh Matos

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Presentation transcript:

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

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

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.

The Cosmology T. 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

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

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.

Scalar Field Fluctuation = Oscillaton = Galaxy Halo Tonatiuh Matos and F. Siddhartha Guzman Class. 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

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.

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

Density Profiles

Density Profiles LSB Galaxies

Density Profiles LSB Galaxies

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