1. An Experimentalist’s Perspective on Testing Field Theories with the CMB. L. Page, AlbaNova, June 2007

2. The current cosmological model agrees with virtually all cosmological measurements regardless of redshift or method. The model assumes a flat geometry (a couple %), a new form of matter (>15  ), something that mimics a cosmological constant (many  ), and a deviation from scale invariance ( =1, ~3  ).

3. WMAP3 only Models based on some kind of field theory of the early universe predict n s. WMAP3 + all

4. “Geometric Degeneracy” CMB alone tells us we are on the “geometric degeneracy” line Reduced closed open Assume flatness WMAP3 only best fit LCDM {

5. Testing Specific Field Theories Non-Gaussanity Anisotropies from Gravitational Waves. Spectrum of Fluctuations & Experimental handles (3) (1) (2)

6. Types of Cosmological Perturbations Tensors: h (GW strain) Temperature E polarization B polarization Temperature Scalars:, Or less! 0.3 n and r are predicted by models of the early universe

16. Power spectrum ~1 0 ~0.4 0 Physical size = plasma speed X age of universe at decoupling The overall tilt of this spectrum--- encoded in the “scalar spectral index” n s --- is the new handle on the early universe. Angular Power Spectrum. early in inflation later in inflation

17. Spectral Index, Experimental Challenges Three different spectra that differ only in spectral index. The black line is the best WMAP model.

18. Spectral Index Normalize the spectra to l=220 (mimics n s - amplitude degeneracy) The two window functions are for 0.1 deg FWHM beams with a 1% difference in solid angle. Only WMAP has achieved anything like this accuracy.

19. Spectral Index Divide by fractional window function. Conclusion: To probe the index the beams need to be understood to the 1% level. In addition, there are astrophysical challenges.

20. Spectral Index: Astrophysical Challenges The formation of the first stars produces free electrons that: (1) rescatter CMB photons thereby reducing the anisotropy and (2) polarize the CMB at large angular scales. These effects mimic a change in n s : “the n s - tau” degeneracy WMAP measures (2) to break the degeneracy

21. BB r=0.3 EE TE TT Approx EE/BB foreground BB Lensing (not primordial) BB inflation

22. Low-l EE/BB EE Polarization: from reionization by the first stars BB Polarization: null check and limit on gravitational waves. r<2.2 (95% CL) from just EE/BB EE BB Just Q and V bands.

23. Degeneracy Knowledge of optical depth breaks the degeneracy 1yr WMAP 3yr WMAP L WMAP1+ ACBAR+ CBI No SZ marg

24. Index and Tensors ( in 2d ) n s =1n s =0.95

25. What Does the Model Need to Describe the Data? Model needs, 8 Model needs not unity, 6 Model needs dark matter, 248 Model does not need: “running,” r, or massive neutrinos, < 3. changing one of the 6 parameters at a time…. The data are, of course, less restrictive when there are more parameters. (“2.8 sigma”) (“15 sigma”) ….but Eriksen & Huffenberger {

26. BB r=0.3 EE TE TT Approx EE/BB foreground Gravitational Waves B modes from lensing of E modes (not primordial). Reionization peak (z r =10) Horizon size at decoupling (z dec =1089) G-waves decay once inside the horizon. B modes from tensors only.

27. Expectations at l=100 Dust at 150 GHz from FDS 1000 close packed dets for 1 year at 350 uK-sec^{1/2} raw or 700 uK- sec^{1/2} on sky. Boxes inst sensitivity not sky rms sens. Lensing B modes From Jo Dunkley Lensing BB

28. Non-Gaussanity The quadrapole is not anomalously low. For the full sky, the 2-pt correlation function is not anomalous. All “detections” of non-Gaussanity are based on a posteriori statistics. That is, one seeks any oddity in the maps and quantifies it. The North-South asymmetry was visible in the COBE data. It would be fantastic to find a clear signature of cosmic non- Gaussanity. The WMAP team has not found one.

29. A significant fraction of the full-sky quadrupole comes from: Extra cold spot: ( Vielva et al. 2004, Cruz et al. gave 1.8% prob. 2005) (Hajian 2007) Note “fingers” present in the southern Galactic hemisphere. Detection of SH persists! Alignment? See Max! (de Oliveira-Costs et al. 2004)

30. Distribution by map temp. by frequency (accounting for uneven weighting) Distribution by resolution. Cold spot Data are an excellent representation of a Gaussian! Gaussian 4 0 pix 1 0 pix 0.25 0 pix

31. 2006 2007 2008 2009 Polarbear-I (300 bolometers) California SZA (Interferometer) Owens Valley APEX (~400 bolometers) Chile SPT (1000 bolometers) South Pole ACT (3000 bolometers) Chile Planck (50 bolometers) L2, data 2012 (12000 bolometers) SCUBA2 QUAD BiCEP BRAIN QUIET CLOVER EBEX SPIDER PAPPA What’s Next?

32. Cluster (SZ, KSZ X-rays, & optical) Diffuse SZ OV/KSZ CMB: l>1000 Lensing Observations: Science: Growth of structure Eqn. of state Neutrino mass Ionization history ACT Atacama Cosmology Telescope Optical X-ray Theory Inflation Power spectrum Columbia Haverford U. KwaZulu-Natal Rutgers U. Catolica Cardiff UMass CUNY UBC NIST INAOE NASA/GSFC UPenn U. Pittsburgh U. Toronto Princeton Collaboration:

33. New Type of Telescope M. Devlin is lead Telescope at AMEC in Vancouver. Ship to Chile in 2006.

34. 8x32 Array of 1mm x 1mm detectors. Now in Chile on the telescope. Arrays of bolometers Irwin et al. Warm electronics based on SCUBA2 Halpern et al. UBC (S. Staggs is lead) Moseley et al, NASA/GSFC

35. First Light from ACT June 8, 2007

36. Expanding CMB Photosphere Stuart Lange, Senior Thesis, 2007 (with Temperature decrease scaled out)

37. An Experiment for the Century Power spectrum of difference between two maps made 100 years apart. Error bars with a 3000x3000 array of detectors.

38. Thank You!

39. From Wayne Hu Polarization of the CMB is produced by Thompson scattering of a quadrupolar radiation pattern. Seljak & Zaldarriaga 2 deg CMB Polarization Whenever there are free electrons, the CMB is polarized. The polarization field is decomposed into “E” and “B” modes. E B

40. Gravitational wave Density wave Terminology: E/B Modes E-modes B-modes k k

41. Equation of State & Curvature WMAP+CMB+2dFGRS+SDSS+SN Interpret as amazing consistency between data sets.

42. Verde et al. 2003 2dFGRS Lyman alpha WMAP 3D z<3 (3) The spectrum of scalar fluctuations. 2D and now SDSS as well. z=1089

43. Low-l EE/BB EE (solid) BB (dash) EE/BB model at 60 GHz r=0.3 Since reionization is late we see it at large angular scales. This is our handle on the optical depth.

44. More simulations of mm-wave sky. Survey area High quality area 150 GHz SZ SimulationMBAC on ACT PLANCK WMAP PLANCK Target Sensitivity (i.e. ideal stat noise only) de Oliveira-Costa Burwell/Seljak 1.5’ beam ACT SPT & APEX as well. / Diffuse KSZ

45. (2) Gaussanity Simple models of inflation have f NL =0.05 Gaussanity means that the real and imaginary parts of each a lm are independent normal deviates. Komatsu et al. ‘03 Express sky as: We quantify the Gaussanity with: Babich & Zaldarriaga 04 Current WMAP limit: Planck limit : f NL =5 Ultimate CMB limit : f NL =3 More exotic models of inflation have f NL =10 to 100.

46. The scalar index, n s, with six parameters. WMAP +SDSS Tegmark et al. 2004 +SDSS Galaxies and Lya Seljak et al. 2004 Simple models of inflation predict: This is significant in that it is a clear departure from scale invariance. We expect n s to 1% by 2008 from the CMB.

47. Running of the scalar index. SDSS Galaxies Tegmark et al. 2004 Galaxies and Lya Seljak et al. 2004 In the two recent analyses of WMAP plus SDSS there is no evidence for running. An analysis of CBI+WMAP+LSS shows evidence of running at the 3- sigma level (-0.085+/-0.031) but the CBI team does not place a lot of weight on the result. Readhead et al. 2004

48. Stability of instrument is critical Physical temperature of B-side primary over three years. Jarosik et al. Three parameter fit to gain over three years leads to a clean separation of gain and offset drifts. 3yr Model Data based on dipole Model based on yr1 alone