1. Licia Verde University of Pennsylvania www.physics.upenn.edu/~lverde Connecting cosmology to fundamental physics

2. Cosmological data* can be used to test fundamental physics The interplay between astrophysics and fundamental physics has already produced spectacular findings (e.g. the solar neutrino problem) Cosmology has entered the precision era very recently Testing fundamental physics by looking up at the sky is not new *For now, CMB is the cleanest probe we have 4 Areas Dark matter (Spergel talk) Neutrinos (Spergel talk) Inflation Dark energy

3. Outline: Precision Cosmology: examples Inflation: what have we learned, prospects for the future Dark energy: what we have learned, prospects for the future Conclusions When things do not make sense… invoke a scalar field… Cosmology has a standard model: What have we learned? If you see the glass half empty: If you see the glass half full:

4. Bennett et al 2003 COBE 1992 WMAP 2003 Bennett et al. 1996

6. Today 2dFGRS

7. SDSS here SDSS

8. Hot and cold spots  Tiny ripples in density  seeds of galaxies Detailed statistical properties of these ripples tell us a lot about the Universe WMAP view of the primordial fireball Bond Efstathiou 1987

9. Hot and cold spots  Tiny ripples in density  seeds of galaxies Detailed statistical properties of these ripples tell us a lot about the Universe WMAP view of the primordial fireball

10. Matter overdensities compress cosmic fluids through gravity Photons (tightly coupled to the baryons) counteract this Sound speed is high (photon/baryon high) c s =c/3 1/2 Sound horizon c s t defines a maximum size Acoustic oscillations set in Damping: photons free streaming, finite thickness of LSS Phase correlation:structures of a given size start oscillating together What’s going on Work of Peebles & Yu, Sunyaev & Zeldovich ‘70

11. (From Hinshaw et al 2003) Status in early 2003

12. Approximation to the state of the art now WMAP1 + CBI + ACBAR+ CBI05+ Boomerang 05+VSA 210 100 1000

13. Approximation to the state of the art now WMAP1 + CBI + ACBAR+ CBI05+ Boomerang 05+VSA 210 100 1000

14. Primordial ripples Fundamental mode 1 deg compression rarefaction compression Acoustic peaks (extrema)

15. Primordial ripples Fundamental mode Geometry Potential wells compression baryons Rarefaction… etc Jungman, Kamionkowski, Kosowsky, Spergel, 1996 +primordial perturbations

16. Generation of CMB polarization Temperature quadrupole at the surface of last scatter generates polarization. Potential well Potential hill From Wayne Hu Rees 68, Coulson et al ‘94 ….. Hu& White 97(pedagogical) YES, there is also reionization

17. Polarization for density perturbation Radial (tangential) pattern around hot (cold) spots.

18. Image from J. Rhul.

20. E and B modes polarization E polarization from scalar, vector and tensor modes B polarization only from (vector) tensor modes Kamionkowski, Kosowsky, Stebbings 1997, Zaldarriga & Seljak 1997

21. ?

22. Inflation  V(  ) H ~ const Solves cosmological problems (Horizon, flatness). Cosmological perturbations arise from quantum fluctuations, evolve classically. Guth (1981), Linde (1982), Albrecht & Steinhardt (1982), Sato (1981), Mukhanov & Chibisov (1981), Hawking (1982), Guth & Pi (1982), Starobinsky (1982), J. Bardeen, P.J. Steinhardt, M. Turner (1983), Mukhanov et al. 1992), Parker (1969), Birrell and Davies (1982)

23. Flatness problem Horizon problem Structure Problem

24. WMAP Consistent with Simplest Inflationary Models Flat universe:  tot = 1.02 ± 0.02 Gaussianity: -58 < ƒ NL < 134 Power Spectrum spectral index nearly scale-invariant: n s = 0.99 ± 0.04 (WMAP only) Adiabatic initial conditions Superhorizon fluctuations (TE anticorrelations) WMAP TE data in bins of  l=10 Primordial Adiabatic i.c. Causal Seed model (Durrer et al. 2002) Primordial Isocurvature i.c. (Peiris et al. 2003) Hu & Sujiyama 1995 Zaldarriaga & Harari 1995 Spergel & Zaldarriaga 1997

25. 1.Primordial B-mode anisotropy –Inflation-generated gravity waves (tensor modes) polarize CMB –(Kamionkowski & Kosowski 1998) –A “smoking gun” of inflation => holy grail of CMB measurements –At least an order of magnitude smaller than E-mode polarization Gravity Waves in the CMB Inflation produces two types of perturbations: in the energy density ( as seen in TT) and in the gravitational field (gravity waves). Unlike temperature anisotropy, CMB polarization anisotropy can discriminate between scalar modes (density perturbations) and tensor modes (gravity waves). (r=tensor to scalar ratio)

26. Information about the shape of the inflaton potential is enclosed in the shape and amplitude of the primordial power spectrum of the perturbations. Information about the energy scale of inflation (the height of the potential) can be obtained by the addition of B modes polarization amplitude. In general the observational constraints of Nefold>50 requires the potential to be flat (not every scalar field can be the inflaton). But detailed measurements of the shape of the power spectrum can rule in or out different potentials. For example: Kahler inflation towards the KKLT minimum, or for multi-field other minima Seeing (indirectly) z>>1100

27. Primordial power spectrum=A k n Amplitude of the power law slope ln k ln P(k) A (convention dependent) !

28. Running of the spectral index generalize Taylor expand pivot d ln P/d ln k =0 >0 <0

29. “ Generic ” predictions of single field slow roll models Monte Carlo simulations following Kinney (2002) and Easther and Kinney (2002) Each point is a “viable” slow roll model, able to sustain inflation for sufficient e-foldings to make the universe flat. (hybrid) (Peiris et al. 2003)

30. WMAP Constraints on Inflationary Models Negative curvature (e.g.: new inflation) Small positive curvature (e.g.: chaotic inflation, extended inflation) Intermediate positive curvature Large positive curvature (e.g.: hybrid inflation) Recommended: For given model, sit on that point and run likelihood analysis (may need to integrate mode equation directly). lf 4 model: Not in such a good shape….. (From Peiris et al. 2003) See also Kinney et al. (2003)

31. Leach & Liddle 03 Barger et al 03 CMB only With LSS

32. The inflaton potential Kinney et al 2003

33. Prospects for the future: Better shape of the primordial power spectrum: WMAP II (more data, and breaking degeneracies) Planck ACT A: Probing smaller scales? Large-scale structure?

34. The CMB can also be used to measure large-scale structure ACT: The Atacama Cosmology Telescope www.hep.upenn.edu/act Toronto Princeton Penn CUNY Columbia Haverford U Mass P.I. Lyman Page

35. Region of the sky covered by ACT Strip of 2.5 degrees in width Courtesy of Carlos Hernandez-Monteagudo

36. B: Prospects for B Modes measurements

37. CMB CMB+ H prior (HST Key project) SN 1A LSS Dark Energy DARK ENERGY …. (Riess et al 04) (WMAP ext ‘03) (2dF Verde et al 02)

38. What have Supernovae observations shown? From Riess et al 04

39. W ?

40. With new SN data (Riess et al. 2004) WMAP

41. With new SN data (Riess et al. 2004) WMAP H prior from HST key project

42. With 2dF (LSS) But, why constant?

43. Assuming a flat Universe…. But, why w constant? Why flatness? + CFHTLS Sembloni et al 05 CTIO +CMB+SN Jarvis et al 05 (75 sq degrees, no redshifts) (3 sq degrees) Baryon oscill. SDSS Eisenstein et al. 05

44. Constraints on QUINTESSENCE Keeping flatness and power law P(k) Galaxy surveys

45. THE SYMPTOMS Or OBSERVATIONAL EFFECTS of DARK ENERGY Recession velocity vs brightness of standard candles: dL(z) CMB acoustic peaks: Da to last scattering LSS: perturbations amplitude today, to be compared with CMB (or Matter density today) Da to z survey

46. HOW TO MAKE A DIAGNOSIS? combination of approaches! Any modification of gravity of the form of f( R ) can be written as a quintessence model for a(t) This degeneracy is lifted when considering the growth of structure Effort in determining what the growth of structure is in a given Dark Energy model!

47. COMPLEMENTARITY IS THE KEY! The questions we want to ask: Is it a cosmological constant? A rolling scalar field? A fluid? Is it a w= -1? w(z)? Is it a breakdown of GR at horizon scales? Measurements of the growth of cosmological structures will help to disentangle the two cases. For not mentioning: control of systematics! Backreaction… Example: Things could be “going wrong” in other ways

48. We can “measure” dark energy because of its effects on the expansion history of the universe and the growth of structure SN: measure d L CMB: A and ISW  a(t) LSS or LENSING: g(z) or r(z)  a(t) AGES: H(z)  a(t)

49. Growth of structure: clusters surveys with optical follow up The shape of the red envelope: i.e. relative ages of galaxies, i.e. H(z) Highly volatile mutual funds Bonds CD’s MEASURING DARK ENERGY: future prospects CMB angular-size distance (improvement?) Combined with acoustic BAO in galaxy distribution At 0<z<2 (or so…) SZ +WL masses X-rays Supernovae KSZ Gamma-Ray bursts Not to scale ISW ……. See eg. Jimenez et al 03, Simon et al 05

50. Conclusions: Precision cosmology is here Cosmology and particle physics are now asking the same questions (but addressing them in complementary ways) We can test fundamental physics by looking up at the sky Inflationary models can be ruled in/out (watch this space) Dark energy: for now it is consistent with a cosmological constant Rolling scalar field/constant/modification of gravity? Cosmological observations have discriminative power. The next few years (days) will be exciting

51. Something funny?

52. SOMETHING FUNNY? Cornish et al. 2003 Phillips & Kogut 2004 Luminet et al. 2003 Roukema et al. 2004 l Cl de Olivera Costa et al. 2004 The football shaped Universe? Dore talk. etc.

53. r Tensor to scalar ratio Up to now scalar Primordial gravity waves would give tensor modes (perturbations on the metric of space-time alone) (metric perturbations can be scalar,vector, tensors) Would be the “smoking gun” of inflation Would affect CMB Temperature and Polarization We have not measured it (only weak constraints). n t exist also, but inflation gives consistency relation

54. Relation to inflation V Not only: But also “Jerk”

55. Low quadrupole…. ISW Cross-correlate CMB with LSS in the foreground ! Boughn & Crittenden (2003) Nolta et al. (2003) (X-ray, Radio galaxies) Scranton et al. (2003)(SDSS) } Afshordi et al. (2003) (2MASS) Gaztanaga et al. (2003) (APM) Hernandez-Monteagudo et al 2005 (point sources…)

56. The low multipole anomalies: planarity and alignment l=2 l=3 Slide from J.Magueijo Found by many groups in independent ways (de Oliveira-Costa et al, 2004; Schwarz et al 2004; Ralston et al 2004; Roukema et al 2005, Bielewicz et al 2005, etc) Bielewicz et al 2005, etc)

57. Isotropy? Jaffe et al 2005 Eriksen et al 03 also reported N/S asymmetry Bianchi VIIh

58. What have we learned? Glass is half full: Cosmic concordance Content, geometry, neutrinos, dark energy, P(k) shape, what seeded the primordial perturbations? Glass is half empty: the puzzles (more space in the discussion)

59. In 2000 Kinney Melchiorri Riotto 2000