1. The Scalar Field Dark Matter Model Tonatiuh Matos, Miguel Alcubierre, Ruben Cordero, Ricardo Becerril, F. Siddhartha Guzman, Dario Nuñez, Luis Ureña, Argelia Bernal, Ahttp:/
Inflation
Cosmology
Galaxies Formation

2. Problems with the CDM Model
Dark Energy:
Extrem Fine Tuning
Coincidence
Dark Matter:
WIMP’s

3. WIMPs Density profile in Galaxies (r) r as r  0
Numerical Simulations
  -1.5
NFW(r)1/r 1/(r+b)2
Observations  
Number of Dwarf Galaxies >>

4. LSB Galaxies

5. Galaxy Formation at z=7

6. Metalicity at z=2

7. The Model T. Matos, R. Cordero, in preparation.
Braneword Scenario:
The radion must be stabilized
Superstrings 
V  f1exp() + f2exp(-) + …
V = V0[cosh() – 1]  exp()
H2 = 8/(3Mpl2)  (1 + /b)
 Inflation  graceful exit
 BBN  Cosmology 
Fix the free constants.

8. The Cosmology T. Matos and L. Ureña, Class. Q. Grav. 17(2000)L75
Dark Matter: 
V0[cosh() –1]
Dark Energy:
 
Baryons,
Neutrinos, etc.
   0.25
   0.7
b  0.05

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

10. Results:

11. Natural Cut-off

12. 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  eV

13. Numerical Simulations Miguel Alcubierre, F
Numerical Simulations Miguel Alcubierre, F. Siddhartha Guzman, Tonatiuh Matos, Dario Nuñez, Luis A. Ureña and Petra Wiederhold. Class. Quant. Grav 19(2002)5017.

14. Oscillatons

15. Oscillatons

16. Scalar Field Fluctuation=Halo Tonatiuh Matos and F
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 M2Planck /m
If m  eV
M 1012 Mo

17. Scalar Field Fluctuation=Halo Tonatiuh Matos and F
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

18. Density Profiles for LSB

19. cosh is renormalizable
Scalar Field DM Cross Section Tonatiuh Matos and Luis A. Ureña, Phys. Lett. B538 (2002)246.
cosh is renormalizable
SFDM 
22/ m = 82exp(I2)/[64(m)3]
Reparametrizations factor
 = exp[2o2/(322)]
Internal Contraction I  1/(162)
If   2 MPl
22/ m = cm2/GeV

20. The Inflaton as SFDM James Lidsey, Tonatiuh Matos and Luis A
The Inflaton as SFDM James Lidsey, Tonatiuh Matos and Luis A. Ureña, Phys.Rev.,D66(2002)
Braneworld scenario: H2 = 8/(3Mpl2)  (1 + /b)
b  2.881051GeV4
V  V0exp((8)/ Mpl)
i  1.94 Mpl Vi  1.631056GeV4
end  1.90 Mpl Vend  2.331054GeV4
Mpbh  109 Mpl tevap  s 0  10-18
Einst < 1.80 Mpl Einst. << b
pbh > 1.06 Mpl
exp > 0.01 Mpl

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