1. 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 =

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  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)

4. 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

5. 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

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 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  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