Transcript The Scalar Field Dark Matter Model Tonatiuh Matos, Dario

From Inflation to Galaxies Formation in the
Braneword Scenario
Tonatiuh Matos,
Miguel Alcubierre, Ruben Cordero, Ricardo Becerril, Hugo Compean,
F. Siddhartha Guzman, Dario Nuñez, Luis Ureña, Argelia Bernal,
Ahttp:/www.fis.cinvestav.mx/~tmatos
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Superstrings Model 
Braneword 
Inflation  DM
SnIa
Mass Power Spectrum
Angular Power Spectrum
Galaxies Formation
The Model
T. Matos, H. Compean, R. Cordero, in preparation.
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Braneword Scenario:
The radion must be stabilized
Superstrings 
V  f1exp() + f2exp(-) + …
• V = V0[cosh() – 1]  exp()
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H2 = 8/(3Mpl2)  (1 + /b)
 Inflation  graceful exit
 BBN  Cosmology 
Fix the free constants.
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T. Matos and L. Ureña, Class. Q. Grav. 17(2000)L75
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The Cosmology
Dark Matter:
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V0[cosh() –1]
Dark Energy:

• Baryons,
• Neutrinos, etc.
•    0.25
•    0.7
• b  0.05
Scalar Field
Fluctuations
T. Matos and L. Ureña,
Phys. Rev. D63(2001)063506
Results:
Natural Cut-off
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  10-23 eV
Numerical Simulations
Miguel Alcubierre, F. Siddhartha Guzman, Tonatiuh Matos, Dario Nuñez,
Luis A. Ureña and Petra Wiederhold.
Class. Quant. Grav 19(2002)5017.
Oscillatons
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);
The Newtonian Force
WIMPs
• Density profile in Galaxies
(r) r as r  0
• Numerical Simulations
•   -1.5
• NFW(r)1/r 1/(r+b)2
• Observations   - 0.5 - 0
• Number of Dwarf Galaxies >>
Dwarf Galaxies
The Critical Mass
Tonatiuh Matos and F. Siddhartha Guzman, Class.Q. Grav. 18(2001)5055
• M  0.1 M2Planck /m
• If m  10-23 eV
• M 1012 Mo
Perfil de
densidad
Galaxy Formation at z=7
Metalicity in z=2
Scalar Field DM Cross Section
Tonatiuh Matos and Luis A. Ureña, Phys. Lett. B538 (2002)246.
• cosh is renormalizable
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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 = 10-25 - 10-23 cm2/GeV
The Inflaton as SFDM
James Lidsey, Tonatiuh Matos and Luis A. Ureña, Phys.Rev.,D66(2002)023514.
• Braneworld scenario: H2 = 8/(3Mpl2)  (1 + /b)
• b  2.881051GeV4
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V  V0exp((8)/ Mpl)
• i  1.94 Mpl
Vi  1.631056GeV4
• end  1.90 Mpl
Vend  2.331054GeV4
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Mpbh  109 Mpl
Einst < 1.80 Mpl
pbh > 1.06 Mpl
exp > 0.01 Mpl
tevap  10-16 s
Einst. << b
0  10-18
Conclusion
• The scalar field is a good candidate
to be the Dark Matter of the
Universe