Superstrings Model Braneword Inflation DM SnIa Mass Power Spectrum

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

• Superstrings Model • Braneword • Inflation DM• SnIa• Mass Power Spectrum• Angular Power Spectrum• Galaxies Formation

The ModelT. Matos, H. Compean, 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.

The CosmologyT. 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

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 (310-27 Mpl )4 m 10-23 eV

Numerical SimulationsMiguel Alcubierre, F. Siddhartha Guzman, Tonatiuh Matos, Dario Nuñez,

Luis A. Ureña and Petra Wiederhold. Class. Quant. Grav 19(2002)5017.

Oscillatons

Scalar Field Fluctuation=HaloTonatiuh 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 MassTonatiuh 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 SectionTonatiuh Matos and Luis A. Ureña, Phys. Lett. B538 (2002)246.

• cosh is renormalizable

• SFDM 22/ m = 82exp(I2)/[64(m)3]

• Reparametrizations factor = exp[2o2/(322)]

• Internal Contraction I 1/(162)

• If 2 MPl

22/ m = 10-25 - 10-23 cm2/GeV

The Inflaton as SFDMJames Lidsey, Tonatiuh Matos and Luis A. Ureña, Phys.Rev.,D66(2002)023514.

• Braneworld scenario: H2 = 8/(3Mpl2) (1 + /b)

b 2.881051GeV4

• V V0exp((8)/ Mpl)

• i 1.94 Mpl Vi 1.631056GeV4

end 1.90 Mpl Vend 2.331054GeV4

• Mpbh 109 Mpl tevap 10-16 s 0 10-18

Einst < 1.80 Mpl Einst. << b

pbh > 1.06 Mpl

exp > 0.01 Mpl

Conclusion

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

Universe