The Scalar Field Dark Matter Model Tonatiuh Matos, Miguel Alcubierre, Ruben Cordero, Ricardo Becerri

1
The Scalar Field Dark Matter ModelTonatiuh
Matos, Miguel Alcubierre, Ruben Cordero, Ricardo
Becerril, F. Siddhartha Guzman, Dario Nuñez,
Luis Ureña, Argelia Bernal,Ahttp/www.fis.cinvest
av.mx/tmatos

• Inflation
• Cosmology
• Galaxies Formation

2
Problems with the ?CDM Model

• Dark Energy
• Extrem Fine Tuning
• Coincidence
• Dark Matter
• WIMPs

3
WIMPs

• Density profile in Galaxies ?(r)? r? as r ? 0
• Numerical Simulations
• ? ? -1.5
• ?NFW(r)?1/r 1/(rb)2
• Observations ? ? - 0.5 - 0

• Number of Dwarf Galaxies gtgt

4
LSB Galaxies
5
Galaxy Formation at z7
6
Metalicity at z2
7
The ModelT. Matos, R. Cordero, in preparation.

• Braneword Scenario
• The radion must be stabilized
• Superstrings ?
• V ? f1exp(?) f2exp(-?)
• V V0cosh(??) 1 ? exp(??)

• H2 8?/(3Mpl2) ? (1 ?/?b)
• ? Inflation ? graceful exit
• ? BBN ? Cosmology ?
• Fix the free constants.

8
The CosmologyT. Matos and L. Ureña, Class. Q.
Grav. 17(2000)L75

• Dark Matter
• ?
• V0cosh(??) 1
• Dark Energy
• ? ?
• Baryons,
• Neutrinos, etc.
• ? ? ? 0.25
• ? ? ? 0.7
• ?b ? 0.05

9
Scalar Field FluctuationsT. 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? ? 10-23 eV

13
Numerical SimulationsMiguel 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 FluctuationHaloTonatiuh 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? ? 10-23 eV
• M ?1012 Mo

17
Scalar Field FluctuationHaloTonatiuh 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
Scalar Field DM Cross SectionTonatiuh 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? 10-25 - 10-23 cm2/GeV

20
The Inflaton as SFDMJames Lidsey, Tonatiuh Matos
and Luis A. Ureña, Phys.Rev.,D66(2002)023514.

• Braneworld scenario H2 8?/(3Mpl2) ? (1
  ?/?b)
• ?b ? 2.88?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 ? 10-16 s ?0 ?
  10-18
• ?Einst lt 1.80 Mpl ?Einst. ltlt ?b
• ?pbh gt 1.06 Mpl
• ?exp gt 0.01 Mpl

21
Conclusion

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