1 / 28

CMB but also Dark Energy

This work explores the theory and phenomenology of extended Quintessence models of Dark Energy, including the funny effects of gravity and Dark Energy coupling. It investigates the CMB spectrum and bispectrum, B modes, acceleration, and structure formation. The fine-tuning and "coincidence" problems are analyzed, and search for attractor solutions is conducted. The paper also examines the effects of Dark Energy on weak lensing, as well as the backreaction of perturbations on the background metric.

Download Presentation

CMB but also Dark Energy

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. CMB but also Dark Energy Carlo Baccigalupi, Francesca Perrotta

  2. Work Fun • Theory, Extended Quintessence, funny effects of Gravity and Dark Energy Coupling • Phenomenology, CMB spectrum and bispectrum, B modes, acceleration and structure formation

  3. “Quintessence’’ models of DE A classical, minimally-coupled scalar field evolves in a potential V(f), while its energy density and pressure combine to produce a negative equation of state w=p/r • Fine-tuning problem: in analogy with L, the need to tune initial values of f to get the observed energy density and equation of state; • “Coincidence’’ problem: why rm ~ rfjust today ?  Search for ATTRACTOR SOLUTIONS (“tracking fields”)

  4. Extended Quintessence Perrotta F., Matarrese S., Baccigalupi C., Phys. Rev. D 61 (2000) 023507

  5. R-boost Klein-Gordon equation in EQ: • Since R diverges as a-3 as a 0 (if non-relativistic species are • present) , an “effective” potential is generated in the KG equation, • boosting the dynamics of f at early times. • EQ admits tracking trajectories AND they are good trackers (large basin of attraction)

  6. rr rm R-boost rf(TEQ) r*f(TEQ) r*f(mc) rf(mc)

  7. Approaching L without fine-tuning Matarrese S., Baccigalupi C., Perrotta F., to appear on Phys. Rev. D W0= -0.999, TEQ for different initial K,V

  8. W0= -0.999 for minimally coupled Q and different initial values of f

  9. Linear and non-linear perturbations • Clustering properties: scalar field perturbations may interact with matter perturbations in EQ models. • Weak lensing : variations of G induce corrections in distance calculations; perturbations gain a new d.o.f., the anisotropic stress • CMB effects (ISW, projection, lensing, bispectrum) • Effects on LSS and structure formation • Backreaction of EQ perturbations on the background metric? (difference between Einstein tensor formed from the averaged metric and the averaged value of the Einstein tensor) • Search for purely gravitational explanation of cosmic acceleration (EQ without potential) Perrotta F., Baccigalupi 2002; Perrotta et al. 2003 Acquaviva V., Baccigalupi C., Perrotta F., 2004

  10. Dark Energy and CMB

  11. DEfast • A cmbfast 4.0 based code for dark energy cosmologies • Scalar field dark energy models in ordinary or scalar-tensor cosmologies • Effective dark energy models (Linder 2003): w=w0+(1-a)(w1-w0) • Used for ~ 10 papers

  12. ISW and Projection

  13. CMB Cls and Dark Energy • ISW killed by Cosmic Variance • Projection degenerated with Ws, H0, K, … but still the basic effect on which CMB constraints on dark energy are based so far • Projection unable to probe w(z), two redshift integrals wash that out

  14. CMB Cls and Dark Energy Phys.Rev.D65, 063520, 2002

  15. CMB Cls and Dark Energy Efstathiou Tensor Degeneracy, 2003 Phys.Rev.D65, 063520, 2002

  16. Beyond Cls: CMB bispectrum Q (W ) ´dT(W )/T alm=sQ (W )Ylm(W )dW Blm l`m`l``m``=alm al`m` al``m`` Bl l`l``=åm m` m`` (mlm`l`m``l``) alm al`m` al``m`` l l`` l`

  17. Weak lensing and CMB bispectrum < Blm l`m`l``m`` >=0 < Blm l`m`l``m`` >0

  18. CMB bispectrum and w1 w1=-0.3 w0=w1=-0.9

  19. Beyond Cls: B modes in CMB Polarisation

  20. Dark Energy and Structure Formation

  21. DE theory & models, Francesca Perrotta DE, lin. Pert., Carlo Baccigalupi Trieste

  22. Lensing, Str.Form., Matthias Bartelmann Lensing, Massimo Meneghetti Heidelberg DE theory & models, Francesca Perrotta DE, lin. Pert., Carlo Baccigalupi

  23. Lensing, Str.Form., Matthias Bartelmann Lensing, Massimo Meneghetti Garching DE theory & models, Francesca Perrotta N-body, Klaus Dolag DE, lin. Pert., Carlo Baccigalupi Padua Str. Form., Giuseppe Tormen Bologna Str. Form., Lauro Moscardini

  24. Cluster Concentration Astron.Astrophys. 416, 853, 2004

  25. Simulating Arcs astro-ph/0405070

  26. More… • CMB bispectrum, how much does it helps? • Weak lensing and B modes on large scales in dark energy cosmologies • Non-linear structures and CMB lensing… • Bring the news on CMB and SNIa together, a Beyond Einstein proposal in preparation (Linder & Baccigalupi)

More Related