BoseEinstein Condensates as Galactic Dark Matter Halos Tonatiuh Matos, F' Siddhartha Guzman, Luis Ur

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Bose-Einstein Condensates as Galactic Dark Matter
HalosTonatiuh Matos, F. Siddhartha Guzman, Luis
Ureña, Dario Nuñez, Argelia Bernal.http/www.fis.
cinvestav.mx/tmatos

• Inflation
• ?CDM Model
• Cosmology
• Galaxies Formation

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Mass Power Spectrum
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Angular Power Spectrum
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Summarizing

• ?M 0.27 ? 0.1,
• ?? 0.73 ? 0.1
• ?0 1.

• Everything OK!!.

• The Matter Components
• ?M ?b ?? ?
• 0.04 ?DM,
• Where ?DM 0.23.
• But ?DM non ?? ??.
• ?DM ?? 0.96

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Problems with the ?CDM Model

• Dark Energy
• Extreme fine tuning for ?
• Coincidence
• Dark Matter
• Cuspy central density profiles
• Too much substructure
• Too late galaxy formation
• Too early metalicity formation
• Etc.

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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

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LSB Galaxies
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Galaxy Formation at z 7 and z 2
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Metalicity at z2
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Some Alternatives

• Self-Interacting DM
• Warm DM
• Super Heavy DM
• Self-Annihilating DM
• Repulsive DM
• Fuzzy DM
• Decaying DM

• Scalar Field Dark Matter
• V V0 (cosh(??)-1)

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Bose-Einstein Condensates

• ???? dV/d? 0
• V V0cosh(??) 1

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Bose-Einstein Condensates
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Bose-Einstein Condensates
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Bose-Einstein Condensates
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Bose-Einstein Condensates
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Scalar Field FluctuationsT. Matos and L. Ureña,
Phys. Rev. D63(2001)063506
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Natural Cut-off
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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

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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)T
onatiuh Matos and F. Siddhartha Guzman, Class.Q.
Grav. 18(2001)5055

• M ? 0.1 M2Planck ?/m?
• If m? ? 10-23 eV
• M ?1012 Mo

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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)T
onatiuh Matos and F. Siddhartha Guzman, Class.Q.
Grav. 18(2001)5055
22
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)T
onatiuh Matos and F. Siddhartha Guzman, Class.Q.
Grav. 18(2001)5055
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Density Profiles
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Density Profiles
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Density Profiles
LSB Galaxies
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Conclusion

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