Transcript The Scalar Field Dark Matter Model Tonatiuh Matos, Dario

Bose-Einstein Condensates as Galactic Dark
Matter Halos
Tonatiuh Matos, F. Siddhartha Guzman, Luis Ureña, Dario Nuñez, Argelia Bernal.
http:/www.fis.cinvestav.mx/~tmatos
• Inflation
• +
• CDM Model
• =
• Cosmology
• Galaxies Formation
Mass
Power
Spectrum
Angular
Power
Spectrum
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
Problems with the CDM Model
• Dark Energy:
• Extreme fine tuning for 
• Coincidence
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Dark Matter:
Cuspy central density profiles
Too much substructure
Too late galaxy formation
Too early metalicity formation
Etc.
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 >>
LSB Galaxies
Galaxy Formation at z = 7 and z = 2
Metalicity at z=2
Some Alternatives
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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)
Bose-Einstein Condensates
 + dV/d = 0

• V = V0[cosh() – 1]
Bose-Einstein Condensates
Bose-Einstein Condensates
Bose-Einstein Condensates
Bose-Einstein Condensates
Scalar Field
Fluctuations
T. Matos and L. Ureña,
Phys. Rev. D63(2001)063506
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
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);
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
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);
Tonatiuh Matos and F. Siddhartha Guzman, Class.Q. Grav. 18(2001)5055
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);
Tonatiuh Matos and F. Siddhartha Guzman, Class.Q. Grav. 18(2001)5055
Density
Profiles
Density
Profiles
Density
Profiles
LSB
Galaxies
Conclusion
• The scalar field is a good candidate
to be the Dark Matter of the
Universe