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