1. Program 1.The standard cosmological model 2.The observed universe 3.Inflation. Neutrinos in cosmology

2. Three questions How much ? ? ? Is there enough mass to close the universe ? Is there evidence for the acceleration of the universe ? Is the universe curved ? Dark matter SN1a CMB

3. Dark matter From BBN & CMB: Non-baryonic Dark Matter From counting: Two Dark Matter Problems Baryonic Dark Matter Many (independent evidences) of DM existence All based on gravitation (until now) How much ? From observation: The facts

4. Dark matter (i) Rotation curves of spiral galaxies Expect: (Kepler) DM halos Local density Planets

5. Dark matter (ii)Galaxy Cluster velocities Virial theorem relates v to M Defined as radius that contains M/2 (50’s) NGC 3198

6. DM Lensing (iii)Gravitational Lensing M Apparent True L S

7. DM Lensing (iv)Macro Lensing Also good to determine H_0 (if time delay measured)

8. DM Lensing (v)Microlensing Magnification Result:

9. SN1a as standard candles SN high redshift Others Cepheids (low z) … How much ?

10. Expansion and acceleration universe accelerates Notice precision (it used to be 200%) Observation

11. Expansion and acceleration

12. Coasting point: smaller in the past

13. Decoupling and CMB rates Compton Double Compton Bremsstrahlung Important for chemical equilibrium (Effective for z > 10^7) How much ? Effective for z > 10^3 (Limits on energy injection for ex. Particle decays, …)

14. Recombination Saha equation x 0 T(eV) time Full calculation Decoupling when e are bound to p forming Hidrogen Last scattering of photons; universe becomes transparent

15. Black Body radiation COBE COsmic Backgroung Explorer

16. Distribution before & after decoupling Keep same form of equilibrium Photon redshift and dilution New temperature

17. Anisotropies gravitation Sources of primary anisotropies 1. from spots where radiation is compressed are hotter 2. climbing potential wells are redshifted 3. from regions with velocity are Doppler-shifted Temperature anisotr. related to density anisotr.

18. Correlations anisotropy Two-point correlation

19. From COBE to WMAP dipole Maximum fluctuation 75 \mu K

20. Correlations observed

21. Correlations expected Acoustic oscillations

22. Acoustic horizon Last-scattering surface is at (in comoving coor.) Consider comoving scale of sound horizon at LS Projection on the LS surface: Sound velocity

23. The position of first peak Open: looks smaller flat open

24. Cosmological parameters from CMB Inertia of baryon-photon fluid depends on Affects relative heights of peaks Flat univ. Other cosmological parameters …

25. CMB polarization - Polarization at ~ 5% level - Acoustic peaks - E, B modes

26. The concordance model

27. Cosmic triangle

28. Nature of DM and DE is a challenge DM Probably particle physics plays a role DE Perhaps particle physics plays a role Particle physics Cosmology

29. The nature of DM

30. Weakly Interacting Massive Particles (Lightest Supersymmetric Particle) Axions Massive Astrophysical Compact Halo Object Axinos, Boson stars, Mirror stars, Quark nuggets, etc

31. Particles in thermal equilibrium For a species in equilibrium ER NR Define

32. Evolution equation (I) Decay law Species Universe expands

33. Evolution equation (II) 1) High T, int. rate is high and 2)Depends on energy have to thermalize with thermal distributions Boltzmann eq.

34. Evolution equation: freeze-out Interaction rate Expansion rate Freeze-out Particle is coupled Particle is not coupled

35. Hot and Cold

36. WIMPs as dark matter Heavy neutrino excluded (LEP + direct search) Lightest superparticle (LSP) good candidate Typical weak x-section

37. Direct WIMP search CDMS (as an example, there are several searches) Constraints wimp + nuclei -> wimp + nuclei + Energy depend on assumption on WIMP coupling

38. DAMA signal Claim WIMP observed m ~ 50 GeV DAMA/LIBRA project

39. The nature of DE

40. Quintessence Alternative to cosm. const.: quintessence Observed value of cosmological constant much smaller than would expect from vacuum energy in the Standard Model of particle physics Slow-rolling field with instead of Particle physics models giving quintessence fields. Concordance problem: why now ?

41. w from observation Also: variation of w with time (crucial por cc vs qu)