1. The Cosmic Web & the CMB high resolution frontier Dick Bond Primary CMB anisotropies are strongly damped by photon-baryon shear viscosity at high L > 1000. this is where secondary anisotropies from the weakly and strongly nonlinear cosmic web dominate. In order of dominance of effect: thermal Sunyaev-Zeldovich effect (Compton scattering of CMB off hot gas, unique frequency signature), CMB weak lensing (smooths out peaks and troughs, no frequency signature), kinetic Sunyaev-Zeldovich effect (Thomson scattering of CMB off moving ionized gas, at high and low redshift), & more. Extragalactic radio (synchrotron) and infrared sources (dust emission) are important (frequency signatures, complex). Galactic foregrounds strongest at low L. To get the most out of CMB parameter estimation from primary anisoptropies, in particular n_s, m_neutrino, we need to take these fully into account. Planck to L~ 2000, ACT/SPT to 10000. Secondary signals are also cosmic-info-loaded: power spectrum of density fluctuations, in gas and dark matter. Dark energy equation of state from large SZ cluster samples (measures their thermal energy, related by virial to DM+gas gravitational energy) (& CMB weak lensing).

2. CMBology Foregrounds CBI, Planck Foregrounds CBI, Planck Secondary Anisotropies (CBI,ACT) (tSZ, kSZ, reion) Secondary Anisotropies (CBI,ACT) (tSZ, kSZ, reion) Non-Gaussianity (Boom, CBI, WMAP) Non-Gaussianity (Boom, CBI, WMAP) Polarization of the CMB, Gravity Waves (CBI, Boom, Planck, Spider) Polarization of the CMB, Gravity Waves (CBI, Boom, Planck, Spider) Dark Energy Histories (& CFHTLS-SN+WL) Dark Energy Histories (& CFHTLS-SN+WL) subdominant phenomena (isocurvature, BSI) subdominant phenomena (isocurvature, BSI) Inflation Histories (CMBall+LSS) Inflation Histories (CMBall+LSS) Probing the linear & nonlinear cosmic web wide open braking approach to preheating Kahler modulus potential T=  +i 

3. Primary Anisotropies Tightly coupled Photon-Baryon fluid oscillations viscously damped Linear regime of perturbations Gravitational redshifting Decoupling LSS Secondary Anisotropies Non-Linear Evolution Weak Lensing Thermal and Kinetic SZ effect Etc. 19 Mpc reionization 13.7Gyrs 10Gyrs today the nonlinear COSMIC WEB INFLATIONINFLATION 13.7-10 -50 Gyrs

4. [http://www.mpa-garching.mpg.de/Virgo/]

5. : : : : Momentum Space PROBES

6. : : : : Cosmic Momentum Space PROBES CMB expts & their phenomenology as high precision tests of Fundamental Physics ( “weakly or radically broken scale invariance”? dark energy “equation of state”? gravity waves? gravity beyond Einstein) : Boomerang 98/03, CBI 00-07, Acbar 01-06, WMAP 1/3, Planck (ESA/NASA + CdnSA 07), … ACT/SPT…Spider…CMBPol nonlinear Gas & Dark Matter Structure in the Cosmic Web the cluster/gp web “now”, the galaxy/dwarf system “then”

7. : : nonlinear Cosmic Web CMB ~2010+ Planck1+WMAP8+SPT/ACT/Quiet+Bicep/QuAD/Quiet +Spider+Clover resolution P(ln k) dynamics H(ln a) are related in inflation (HJ) ~10+ e-folds dynamics w(ln a) ~1+ e-folds

8. : : : : nonlinear Cosmic Web SZ/WL

9. : : ULSS+VLSS+LSS: CMB, primary & secondary (nonlinear) LSS (some VLSS): z-surveys (spectrum shape, clustering evolution, weak nonlinearity, nonG measures) - bias weak lensing – systematics at required precision level? Seems possible as of april07 cfhtls abundances (& distribution) of “rare events” – cluster system (high-z, radio galaxies, quasars, etal.) - SZ+Lens+optical+X + hope (gas) streaming & pair velocities: rehabilitated? SSS: Lyman alpha forest, high-z (1 st stars) but gas+NL+feedback : : calibrated candles: SN1a + PROBES

11. massive clusters:  > 100, peak-patches Filaments  ~ 5-10 bridge clusters, groups bead the bridges Membranes:  ~ 2 Voids:  < 0 “Molecular” picture  CDM 400 Mpc treeSPH 512 3 gas+CDM particles

12. 1.2 billion light years across gas+dark matter simulation of cosmic structure evolution (LCDM concordance) ~~ biggest gasdynamical simulations ~ 0.3 billion particles Millenium dark matter simulation: ~ 10 billion particles

14. The most massive, collapsed structures in the universe. They contain galaxies, hot, ionized gas (10 7-8 K) and dark matter. They are good probes, because they are massive and “easy” to detect, but they have complex interiors. Galaxy Clusters X-ray emission Sunyaev-Zel’dovich effectLight from galaxies Gravitational lensing Virgo-ish cluster with and without cosmic ray pressure, as would be seen by CBI1 (includes CMB, heating, cooling – Pfrommer, Sievers, Springel +B) - =

15. pass the CMB thru the cosmic web; CBI extra power?? 512 3 LCDM sim tSZ maps: rotate & translate copies(z) of 400 Mpc box

16. pass the CMB thru the cosmic web; CBI extra power??

17. 2004 2005 2006 2007 2008 2009 Polarbear (300 bolometers) @Cal SZA (Interferometer) @Cal APEX (~400 bolometers) @Chile SPT (1000 bolometers) @South Pole ACT (3000 bolometers) @Chile Planck 08.8 (84 bolometers) HEMTs @L2 Bpol @L2 ALMA (Interferometer) @Chile (12000 bolometers) SCUBA2 Quiet1 Quiet2 Bicep @SP QUaD @SP CBI pol to Apr’05 @Chile Acbar to Jan’06, 07f @SP WMAP @L2 to 2009-2013? 2017 (1000 HEMTs) @Chile Spider Clover @Chile Boom03 @LDB DASI @SP CAPMAP AMI GBT 2312 bolometer @LDB JCMT @Hawaii CBI2 to early’08 EBEX @LDB LMT @Mexico LHC

18. WMAP3 sees 3 rd pk, B03 sees 4 th

19. CBI excess 02

20. Readhead et al. ApJ, 609, 498 (2004) CBI excess 04

21. state November 06 state November 06 CBI excess 06

22. Current high L state November 07 Current high L state November 07 CBI sees 4 th 5 th pk CBI excess 07

23. CBI@5040m

24. CBI Dataset CBIpol Sept 02 – Apr 05 CBIpol observed 4 patches of sky – 3 mosaics & 1 deep strip Pointings in each area separated by 45’. Mosaic 6x6 pointings, for 4.5 o2, deep strip 6x1. Lost 1 mode per strip to ground. Combined TT ~ 5yrs of data from Nov 99 – Aug 02 (3 mosaics + 3 deep fields) lead- trail + CBIpol (Sept 02 – Apr 05) total CBI2: upgrade 0.9m to 1.4m dishes; observing from Jun 06

25. What is the redshift range that contributes to the SZ effect? all from 0 to ~2

27. What sort of objects in the cosmic web dominate the SZ effect? clusters and groups, with only a little from the filament outskirts, unless there has been substantial energy injection along the filaments

29. 512 3 LCDM sim tSZ,kSZ,X,WL maps: rotate & translate copies(z) of 400 Mpc box redshift cut

30. 512 3 LCDM sim tSZ,kSZ,X,WL maps: rotate & translate copies(z) of 400 Mpc box Halo mass cut

31. TSZ KSZ 512 3 LCDM sim SZ power spectra for various realizations

32. 512 3 LCDM sim SZ power halo overdensity cut cf. virial density 512 3 LCDM sim SZ power halo mass cut

33. ACBAR (150 GHz cf. 30 GHz CBI) Kuo etal. Nov06, ApJ07 Direct analysis, no lead-main-trail strategy 30% more data in the 00-01 acbar observing campaigns Calibration improvement WMAP-Boomerang98-ACBAR 10% to 6% significant improvement over Kuo etal 2004 (std used in WMAP1/3) Kuo etal. Nov06, ApJ07 Direct analysis, no lead-main-trail strategy 30% more data in the 00-01 acbar observing campaigns Calibration improvement WMAP-Boomerang98-ACBAR 10% to 6% significant improvement over Kuo etal 2004 (std used in WMAP1/3) Jan08: Full ACBAR data includes 2005 observations 3.7 times more effective integration time 6.5 time more sky coverage a very significant improvement over Kuo etal 2006 Best parameter determinations (until Nov07 work) Weak lensing included: a small impact on parameters

34. σ 8 Tension of WMAP3 SZ treatment does not include errors from non-Gaussianity of clusters, uncertainty in SZ CL WMAP3+cbicomb05 +acbar03+B03 Std 6 +  8SZ^7 σ 8 WMAP3 620 cut = 0.79±0. 053 = 0.96±0.10 SZ (  m = 0.26±0.038) (  = 0.0874±0.0030) CFHTLS survey’05: 0.86 +-.05 + Virmos-Descart & non-G errors s 8 = 0.80 +-.04 if  m = 0.3 +-.05 cf. weak lensing

35. Current state November 07 Current state November 07 CBI excess 04 cf. CBI excess 07

36. Current CBI+BIMA PS Fit CMB+Excess model to CBItot data Red curve SPH simulation- based template (Bond et al.), 1.03 +- 0.07 blue curve analytic (Komatsu&Seljak, Spergel et al.06). 0.92+-0.07 Magenta points CBI w/ finer binning. Black points latest BIMA. Models extrapolated to BIMA points – not a fit. If CBI excess were due to unexpected source population, BIMA would see them. They don’t.

37. CBI2@5040m why Atacama? driest desert in the world. thus: cbi, toco, apex, asti, act, alma, quiet, clover

38. CBI2 Forecast – 9 Months on CMB Forecast gives 12% error on current excess, assuming level doesn’t change. GBT follow-up observations. CBI2 fields all are in areas where multi- wavelength data is available (COSMOS, UKIDSS, VIRMOS). Weak-lensing definitely, also some X-Ray, IR, radio… Red/Blue=9-month spectrum with big dishes, different scan strategies. Caltech, NRAO, Oxford, CITA, Imperial by about Feb07 CMBPrimary +SZESecondary  8 7  8 2

39. Sample CBI2 clusters Clusters from early CBI2 observations. Many more now (Nov07): CBI2 very good at clusters at z~0.15, & close enough so other wavelength follow-ups are easier.

40. ACT@5170m

41. Cluster (SZ, KSZ X-rays, & optical) Diffuse SZ OV/KSZ CMB: l>1000 Lensing Observation s: 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:

42. Simulations of mm-wave data. Survey area High quality area 150 GHz SZ SimulationMBAC on ACT 2X noise PLANCK MAP PLANCK Statistical uncertainties based on 1 season with best measured noise. de Oliveira-Costa Burwell/Seljak 1.7’ beam ACT WMAP

44. Sample forecast for SZ cluster surveys 4000 sq deg with SPT, 22000 clusters Subha Majumdar & Graham Cox CITA04

45. The SZ & cluster frontier high/low  8 issue will be resolved (soon: CBI2, ACT/SPT, SZA, APEX?) but cluster complexity (non-equilibrium, non-thermal e.g. cosmic ray pressure, inhomogeneous, merging, entropy injection, cooling flow avoidance) must be fully addressed for high precision on other parameters to be realized. combine SZ at varying resolution + optical + gravitational lens + X-ray + embedded IR/radio source observations

46. 2004 2005 2006 2007 2008 2009 Polarbear (300 bolometers) @Cal SZA (Interferometer) @Cal APEX (~400 bolometers) @Chile SPT (1000 bolometers) @South Pole ACT (3000 bolometers) @Chile Planck 08.8 (84 bolometers) HEMTs @L2 Bpol @L2 ALMA (Interferometer) @Chile (12000 bolometers) SCUBA2 Quiet1 Quiet2 Bicep @SP QUaD @SP CBI pol to Apr’05 @Chile Acbar to Jan’06, 07f @SP WMAP @L2 to 2009-2013? 2017 (1000 HEMTs) @Chile Spider Clover @Chile Boom03 @LDB DASI @SP CAPMAP AMI GBT 2312 bolometer @LDB JCMT @Hawaii CBI2 to early’08 EBEX @LDB LMT @Mexico LHC

47. PRIMARY END @ 2012? CMB ~2009+ Planck1+WMAP8+SPT/ACT/Quiet+Bicep/QuAD/Quiet +Spider+Clover