1. Interacting Dark Energy and Dark Matter : a window to quintessence. Elcio Abdalla

2. Acknowledgements Bin Wang (Fudan -- Shanghai) Ru Keng Su, Jian Yong Shen, Zuo Yi Huang, Yun Gui Gong, Chi Yong Lin, Jia Dong Zang, Shao Yu Yin (China) Diego Pavon (Barcelona) Raul Abramo, Laerte Sodré, Sandro Micheletti (USPaulo)

3. Dark Matter and Dark Energy Already in the thirties (1933) Zwicky observed the velocities in the Coma cluster and verified that they are much bigger than what would be expected from the Newton law with a mass M=M lum as given by the luminous (optically observed) mass: V 2 = 2GM/R

4. P.J.E. Peebles Theory withour Dark Matter Observation Besides luminous matter there is circa 10 times more matter in an unknown clumping form Measuring Dark Matter

5. There are also very strong (indeed undeniable) indications that the Universe is undergoing na accelerated expansion phase: Observing IA Supernovae The Spectrum of Cosmic Radiation Background Dark Energy

6. 3.5 energia escura SN1997ff  m =1,   =0 IA Supernovas

7. RCF

9. Supernovae plus CRMB

10. All observations are consistent with Dark Energy and Dark Matter, where: 1.The total Energy Density equals the critical density 2.Clumping matter (baryons plus DM) represent 1/3 of the total energy content 3.Some strange (very strange) object is responsable for acceleration, representing 2/3 of the energy content of the Universe..

11. Moreover... 5-year WMAP has extremely tight constraints in that picture, errors are smaller than a few percent...

12. The essence of Dark Energy What is Dark Energy? Could it be simple? A new field? A Cosmological Constant? Is it interacting?

13. Friedmann equations lead to Thus we need a matter which fulfills How to get acceleration?

14. The first solution is the cosmological constant. It is a simple solution to the problem with w=-1. There are however some problems connected with the cosmological constant: 1. The energy density required to adjust to observations is of the order of 1 (MeV) 4, 120 of magnitude smaller than what would be obtained from a field theoretic computation. 2. It is a mistery the reason why the cosmological constant is important NOW.

15. Dark Matter and Dark Energy It has become cristal clear that circa 97% of the Universe is formed by two up to now unknown forms of matter. Baryonic Matter interacts with eletromagnetism leading to our (very wonderful) world. What if Dark Matter (30% of the Universe) interacts with Dark Energy (67% of the Universe)? What are the consequences?

16. w  = -1 1+z = a 0 /a radiation  matter : z~10 4 today The coincidence problem

17. The Coincidence Problem and DE/DM Interaction Why DE and DM are of the same order of magnitude today?

18. The Coincidence Problem and DE/DM Interaction We thus say that a decay of DE into DM aleviates the coincidence problem Question: can we test such ideas with observations?

19. Dark Matter and Dark Energy Interaction: preliminary view. We investigated the question of the suppression of the CMB power spectrum for lowest multipoles. We used the idea of holographic cosmic duality to understand the problem Examining the power spectrum, we have shown a suppression behavior which describes the low l features extremely well. The holographic idea (DE density proportional to the square of the scale factor) suits very well non trivial (e.g. no cosmological constant) models.

20. Holographic Model Idea motivated by strings/quantum gravity: the energy/entropy content cannot be larger than that of a Black Hole of the size of the Universe. Thus,

21. Interacting Holographic Model The simplest interaction Model for DE and DM is obtained from a two-fluid model:

22. Interacting Holographic Model The simplest models for Q is na interaction proportional to the energy density:

23. Interacting Holographic Model The proportionality constant b is a small number. The density appearing in the r.h.s. is either DE, DM or the total (depending on the model). They presumably follow one another at large, possibly being equivalent which to use.

24. Interacting Holographic Model Comparison with supernova data and measurements of w show that:

25. Interacting Holographic Model Comparing b and c with data arising also from the allowed values of w and amount of DE and DM today we find

26. Further on Phenomenology Age Constraint: age of Universe

27. Further on Phenomenology Age of Quasar APM 08279+5255.

28. Further on Phenomenology Low l CMB again

29. Further on Phenomenology

30. Order of magnitude estimate for b 2 (with some dependence on the DE equation of state): 1  : 0.10 < b 2 < 0.2 2  : -- 0.10 < b 2 < 0.24 Probability of b 2 positive: 95%.

31. Signature in Galaxy Clusters: na apparent correction of the Virial Theorem We only observe Baryonic Matter. Suppose Dark Matter pattern follows Baryonic Matter pattern Interaction with Dark Energy works as na external potential Thus, Virial Theorem acquires a correction.

32. Signature in Galaxy Clusters: na apparent correction of the Virial Theorem Usual Virial Theorem: 2K+U=0. In General Relativity: Layser Irvine Equation.

35. Signature in Galaxy Clusters: an apparent correction of the Virial Theorem Results

36. Signature in Galaxy Clusters: an apparent correction of the Virial Theorem Results

37. Modelling the Interaction Suppose there are DE/DM particles in interaction. Suppose there is a “Thompson scattering amplitude”. Existence of galaxies with M DM of the order of 10 M baryons we get b 2  3  QED In agreement with previous computations.

38. Further on Perturbations The interaction lr dm has strong non perturbative effects. Such non perturbative effects arise from classical solutions of the equations of motion of the order of 1/ l. Therefore, perturbative methods fails. The interaction lr de does not show the same behaviour. Thus, we need urgently further methods and alternatives.

39. Hubble “drag” Potencial  V()V() Slow- roll,  works as a cosmological  decaying in time V  Equation of motion small Scalar Fields

40. A Field Theoretic Model for DE/DM We consider the Lagrangian density L= -√(g)V(  ) √(1-  m  m ) -  i d  -(m-  )  The energy (non)conservation equations have a (nonvanishing) intertwining term proportional to , to the time derivative of  and to the density .

41. Likelihood --- 

42. Do we have any coupling? The present field theoretic model is compatible with zero coupling, though overwhelming majority of the integrated likelihood function points to a negative coupling, in conformity with previous results. The results are thus because of a severe degeneracy of b and f.

43. Thermodynamics and DE/DM An interaction between the Dark sectors leads also to similar conclusions. However, the thermodynamic functions are not known for the DE sector What is the temperature of DE? What is the temperature of DM?

44. Thermodynamics and DE/DM For the holographic model T DE it is naturally of the order of the Hawking Temperature of the horizon. In case this is true the DE temperature is several orders of magnitude smaller than unit. In case we use a gas to describe DE, it is natural to assume that T DE is of the order R -3w. For w= -1 this is very, very hot. Thus, what is T DE ? Do we have a non equilibrium mixture?

45. Conclusions At 1  level there are very good reasons to believe that DE and DM are interacting fields What happens to String Theory claims about anthropic principle and all that? Are there models in Quantum Field Theory which could properly describe interacting DE/DM (work in progress)?