Bose-Einstein Condesates 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

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.

The Model• Examples:• Braneword Scenario• Superstrings • V f1exp() + f2exp(-) + …

• V = V0[cosh() – 1]

• 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 0.7b 0.05

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