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.

• The Matter Components

M = b + + ~ • 0.04 + DM,• Where DM ~ 0.23.• But DM non ??.

DM + ~ 0.96

• Everything OK!!.

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.

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• 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 (310-27 Mpl )4 m 10-23 eV

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);

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 = 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);

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

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);

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