1 / 56

Dick Bond

Dick Bond. Inflation & its Cosmic Probes, now & then. Cosmic Probes CMB, CMBpol (E,B modes of polarization) B from tensor: Bicep, Planck, Spider, Spud, Ebex, Quiet, Pappa, Clover, …, Bpol CFHTLS SN(192) , WL(Apr07) , JDEM/DUNE BAO, LSS,Ly a.

bryony
Download Presentation

Dick Bond

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. Dick Bond Inflation & its Cosmic Probes, now&then Cosmic Probes CMB, CMBpol (E,B modes of polarization) B from tensor: Bicep, Planck, Spider, Spud, Ebex, Quiet, Pappa, Clover, …, Bpol CFHTLS SN(192),WL(Apr07), JDEM/DUNE BAO,LSS,Lya Inflation Thenk=(1+q)(a) ~r/160< = multi-parameter expansion in (lnHa ~ lnk) Dynamics ~ Resolution~ 10 good e-folds (~10-4Mpc-1 to ~ 1 Mpc-1 LSS) ~10+ parameters? Bond, Contaldi, Kofman, Vaudrevange 07 r(kp) i.e. k is prior dependent now, not then. Large (uniform ), Small (uniform ln). Tiny (roulette inflation of moduli; almost all string-inspired models) KKLMMT etc, Quevedo etal,Bond, Kofman, Prokushkin, Vaudrevange 07, Kallosh and Linde 07 General argument: if the inflaton < the Planck mass, then r < .007 (Lyth96 bound)

  2. Dick Bond Inflation & its Cosmic Probes, now&then Inflation Now1+w(a)= esf(a/aeq;as/aeq;zs)goes to(a)x3/2 = 3(1+q)/2 ~1 good e-fold. only ~2params Zhiqi Huang, Bond & Kofman 07es=0.0+-0.25 now, late-inflaton (potential gradient)2 to +-0.07 then Planck1+JDEM SN+DUNE WL, weak as < 0.3 now <0.21 then (late-inflaton mass is < Planck mass, but not by a lot) Cosmic Probes NowCFHTLS SN(192),WL(Apr07),CMB,BAO,LSS,Lya Cosmic Probes Then JDEM-SN + DUNE-WL + Planck1

  3. NOW

  4. Dick Bond Inflation & its Cosmic Probes, now&then Inflation now Dynamical background late-inflaton-field trajectories imprint luminosity distance, angular diameter distance, volume growth, growth rate of density fluctuations Prior late-inflaton primordial fluctuation information is largely lost because tiny mass (field sound speed=c?) late-inflaton may have an imprint on other fields? New late-inflaton fluctuating field power is tiny

  5. w-trajectories for V(f):pNGB example e.g.sorbo et07 For a given quintessence potential V(f), we set the “initial conditions” at z=0 and evolve backward in time. w-trajectories for Ωm(z=0) = 0.27 and (V’/V)2/(16πG)(z=0) = 0.25, the 1-sigma limit, varying the initial kinetic energy w0 = w(z=0) Dashed lines are our first 2-param approximation using an a-averaged es= (V’/V)2/(16πG) and c2 -fitted as. Wild rise solutions Slow-to-medium-roll solutions Complicated scenarios: roll-up then roll-down

  6. Approximating Quintessence for Phenomenology 1+w=2sin2 Zhiqi Huang, Bond & Kofman 07 + Friedmann Equations + DM+B Include a w<-1 phantom field, via a negative kinetic energy term 1+w=-2sinh2

  7. slow-to-moderate roll conditions 1+w< 0.3 (for 0<z<10) gives a 2-parameter model (as and es): Early-Exit Scenario: scaling regime info is lost by Hubble damping, i.e.small as CMB+SN+LSS+WL+Lya 1+w< 0.2 (for 0<z<10) and gives a 1-parameter model (as<<1):

  8. Some Models • Cosmological Constant (w=-1) • Quintessence (-1≤w≤1) • Phantom field (w≤-1) • Tachyon fields (-1 ≤ w ≤ 0) • K-essence (no prior on w) w(a)=w0+wa(1-a) Uses latest April’07 SNe, BAO, WL, LSS, CMB, Lya data effective constraint eq.

  9. 45 low-z SN + ESSENCE SN + SNLS 1st year SN+ Riess high-z SN, 192 “gold”SN all fit with MLCS illustrates the near-degeneracies of the contour plot

  10. Higher Chebyshev expansion is not useful: data cannot determine >2 EOS parameters9 & 40 into Parameter eigenmodesDETF Albrecht etal06, Crittenden etal06, hbk07 piecewise parameterization 4,9,40 z-modes of w(z) 9 4 s1=0.12 s2=0.32 s3=0.63 40 Data used 07.04: CMB+SN+WL +LSS+Lya

  11. Measuring constant w (SNe+CMB+WL+LSS) 1+w = 0.02 +/- 0.05

  12. Measuring es(SNe+CMB+WL+LSS+Lya) Modified CosmoMC with Weak Lensing and time-varying w models

  13. 3-parameter parameterization next order corrections: Wm (a) (depends on es redefines aeq) ev = es (a) (adds newzs parameter) enforce asymptotic kinetic-dominance w=1(add as power suppression) perfect moderate-to-slow roll fits ... & even the baroque … correction on w only ~ 0.01

  14. fits the baroque wild-rising trajectories

  15. Measuring the 3 parameters with current data • Use 3-parameter formula over 0<z<4 & w(z>4)=wh(irrelevant parameter unless large). as<0.3

  16. Comparing 1-2-3-parameter results CMB + SN + WL + LSS +Lya estrajectoriesareslowly varying: why the fits are good Conclusion: for current data, the multi-parameter complications are largely irrelevant (as<0.3): we cannot reconstruct the quintessence potential we can only measure the slope es

  17. Thawing, freezing or non-monotonic? With freezing prior: With thawing prior: Thawing: 1+w monotonic up as z decreases Freezing: 1+w monotonic down to 0 as z decreases ~15% thaw, 8% freeze, most non-monotonic with flat priors

  18. the quintessence field is below the reduced Planck mass

  19. Forecast: JDEM-SN(2500 hi-z + 500 low-z)+ DUNE-WL(50% sky, gals @z = 0.1-1.1, 35/min2 ) + Planck1yr Beyond Einstein panel: LISA+JDEM es=0.02+0.07-0.06 ESA as<0.21 (95%CL)

  20. Inflation now summary • the data cannot determine more than 2 w-parameters (+ csound?). general higher order Chebyshev expansion in1+was for “inflation-then”=(1+q)is not that useful. Parameter eigenmodesshow what is probed • The w(a)=w0+wa(1-a) phenomenology requires baroque potentials • Philosophy of HBK07:backtrack from now (z=0) all w-trajectories arising from quintessence(es >0) and the phantom equivalent (es <0); use a 3-parameter model to well-approximate even rather baroque w-trajectories. • We ignore constraints on Q-density from photon-decoupling and BBN because further trajectory extrapolation is needed. Can include via a prior on WQ(a) at z_dec and z_bbn • For general slow-to-moderate rolling one needs 2 “dynamical parameters” (as, es) & WQ to describe w to a few % for the not-too-baroque w-trajectories. • asis < 0.3 current data (zs>2.3) to <0.21 (zs>3.7) in Planck1yr-CMB+JDEM-SN+DUNE-WL future In the early-exit scenario, the information stored inasis erased by Hubble friction over the observable range &w can be described by a single parameteres. • a 3rdparamzs, (~des /dlna) is ill-determined now & in aPlanck1yr-CMB+JDEM-SN+DUNE-WL future • To use: given V, compute trajectories, do a-averaged es& test (or simpler es-estimate) • for eachgiven Q-potential, velocity, amp, shape parameters are needed to define a w-trajectory • current observations are well-centered around the cosmological constantes=0.0+-0.25 • in Planck1yr-CMB+JDEM-SN+DUNE-WL futureesto +-0.07 • but cannot reconstruct the quintessence potential, just the slope es& hubble drag info • late-inflaton mass is < Planck mass, but not by a lot • Aside: detailed results depend upon the SN data set used. Best available used here (192 SN), soon CFHT SNLS ~300 SN + ~100 non-CFHTLS. will put all on the same analysis/calibration footing – very important. • Newest CFHTLS Lensing data is important to narrow the range over just CMB and SN

  21. THEN

  22. Dick Bond Inflation & its Cosmic Probes, now&then Inflation then Amplitude As, average slope <ns>, slope fluctuations dns = ns -< ns > (running, running of running, …) for scalar (low L to high L CMB ACT/SPT; Epol Quad, SPTpol, Quiet2, Planck) & tensor At, <nt>, dnt = nt-< nt > (low L <100 Planck, Bicep, EBEX, Spider, SPUD, Clover, Bpol) & isocurvature Ais, <nis>, dnis= nis-< nis> power spectra (subdominant) Blind search for structure (not really blind because of prior probabilities/measures) Fluctuation field power spectra related to dynamical background field trajectories Defines a tensor/scalar functional relation between; both to Hubble & inflaton potential

  23. Standard Parameters of Cosmic Structure Formation Period of inflationary expansion, quantum noise  metricperturbations r < 0.6 or < 0.28 95% CL Scalar Amplitude Density of Baryonic Matter Spectral index of primordial scalar (compressional) perturbations Spectral index of primordial tensor (Gravity Waves) perturbations Density of non-interacting Dark Matter Cosmological Constant Optical Depth to Last Scattering Surface When did stars reionize the universe? Tensor Amplitude What is the Background curvature of the universe? closed flat open

  24. TheParameters of Cosmic Structure Formation Cosmic Numerology: aph/0611198 – our Acbar paper on the basic 7+; bckv07 WMAP3modified+B03+CBIcombined+Acbar06+LSS (SDSS+2dF) + DASI (incl polarization and CMB weak lensing and tSZ) ns = .958 +- .015 .93 +- .03 @0.05/Mpc run&tensor r=At / As < 0.28 95% CL <.36 CMB+LSS run&tensor dns /dln k = -.060 +- .022 -.038 +- .024 CMB+LSS run&tensor As = 22 +- 2 x 10-10 Wbh2 = .0226 +- .0006 Wch2= .114 +- .005 WL = .73 +.02 - .03 h = .707 +- .021 Wm= .27 + .03 -.02 zreh =11.4 +- 2.5

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

  26. CBI pol to Apr’05@Chile Bicep @SP Quiet2 (1000 HEMTs) @Chile CBI2 to early’08 Acbar to Jan’06, 07f @SP QUaD @SP Quiet1 SCUBA2 Spider (12000 bolometers) 2312 bolometer @LDB APEX SZA JCMT @Hawaii (~400 bolometers) @Chile (Interferometer) @Cal ACT Clover @Chile (3000 bolometers) @Chile Boom03@LDB EBEX@LDB 2017 2004 2006 2008 LMT@Mexico 2005 2007 SPT LHC 2009 Bpol@L2 WMAP@L2to 2009-2013? (1000 bolometers) @South Pole ALMA DASI @SP (Interferometer) @Chile Polarbear (300 bolometers)@Cal CAPMAP Planck08.8 AMI (84 bolometers) HEMTs @L2 GBT

  27. ACT@5170m why Atacama? driest desert in the world. thus: cbi, toco, apex, asti, act, alma, quiet, clover CBI2@5040m

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

  29. Current high L state November 07 WMAP3 sees 3rd pk, B03 sees 4th CBI sees 4th 5th pk CBI excess 07

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

  31. SPIDER Tensor Signal • Simulation of large scale polarization signal No Tensor Tensor http://www.astro.caltech.edu/~lgg/spider_front.htm

  32. forecast Planck2.5 100&143 Spider10d 95&150 Synchrotron pol’n Dust pol’n are higher in B Foreground Template removals from multi-frequency data is crucial

  33. Very very difficult to get at with direct gravity wave detectors – even in our dreams (Big Bang Observer ~ 2030) Latham Boyle 07 GW/scalar curvature: current from CMB+LSS: r < 0.6 or < 0.25(.28)95%;good shot at0.0295% CL with BB polarization (+- .02 PL2.5+Spider), .01 target BUT foregrounds/systematics?? But r-spectrum. But low energy inflation

  34. Inflation in the context of ever changing fundamental theory 1980 -inflation Old Inflation New Inflation Chaotic inflation SUGRA inflation Power-law inflation Double Inflation Extended inflation 1990 Hybrid inflation Natural inflation Assisted inflation SUSY F-term inflation SUSY D-term inflation Brane inflation Super-natural Inflation 2000 SUSY P-term inflation K-flation N-flation DBI inflation inflation Warped Brane inflation Tachyon inflation Racetrack inflation Roulette inflation Kahler moduli/axion

  35. Power law (chaotic) potentials V/MP4 ~ l y2n, y=f/MP2-1/2 e=(n/y)2 , e = (n/2) /(NI(k) +n/3), ns-1= - (n+1) / (NI(k) -n/6), nt= - n/ (NI(k) -n/6), n=1, NI~ 60,r = 0.13, ns= .967, nt= -.017 n=2, NI~ 60,r = 0.26, ns= .950, nt= -.034 MP-2= 8pG

  36. PNGB:V/MP4 ~Lred4sin2(y/fred 2-1/2 ) ns~ 1-fred-2 , e = (1-ns)/2 /(exp[(1-ns)NI (k)](1+(1-ns)/6) -1), exponentially suppressed; higherrif lowerNI & 1-ns to match ns=.96, fred~ 5, r~0.032 to match ns= .97, fred~ 5.8, r~0.048 cf.n=1, r = 0.13, ns= .967, nt= -.017 ABFFO93

  37. Moduli/brane distance limitation in stringy inflation. Normalized canonical inflaton Dy < 1 over DN ~ 50, e.g. 2/nbrane1/2BM06 e = (dy /d ln a)2so r = 16e < .007, <<? roulette inflation examples r ~ 10-10 & Dy < .002 possible way out with many fields assisting: N-flation ns= .97, fred~ 5.8, r~0.048, Dy ~13 cf.n=1, r = 0.13, ns= .967, Dy ~10 cf.n=2, r = 0.26, ns= .95, Dy ~16

  38. energy scale of inflation & r V/MP4 ~ Ps r (1-e/3)3/2 V~ (1016Gev)4r/0.1 (1-e/3) roulette inflation examples V~ (few x1013Gev)4 H/MP ~ 10-5 (r/.1)1/2 inflation energy scale cf. the gravitino mass (Kallosh & Linde 07) if a KKLT/largeVCY-likegeneration mechanism 1013Gev (r/.01)1/2 ~ H < m3/2cf. ~Tev

  39. String Theory Landscape& Inflation++ Phenomenology for CMB+LSS Hybrid D3/D7 Potential • D3/anti-D3 branes in a warped geometry • D3/D7 branes • axion/moduli fields ... shrinking holes KKLT, KKLMMT BB04, CQ05, S05, BKPV06 f|| fperp large volume 6D cct Calabi Yau

  40. Roulette Inflation: Ensemble of KahlerModuli/Axion Inflations Bond, Kofman, Prokushkin & Vaudrevange 06 end

  41. Roulette: which minimum for the rolling ball depends upon the throw; but which roulette wheel we play is chance too. The ‘house’ does not just play dice with the world. “quantum eternal inflation” regime stochastic kick > classical drift Very smallr’s may arise from string-inspired low-energy inflation models

  42. Ps (ln Ha)Kahlertrajectories observable range But it is much easier to get models which do not agree with observationsi.e. data selectsthe few that ‘work’ from the vast cases that do not

  43. e(ln a) H (ln a) 10-10

  44. New Parameters of Cosmic Structure Formation tensor (GW) spectrum use order M Chebyshev expansion in ln k, M-1 parameters amplitude(1), tilt(2), running(3),... scalar spectrum use order N Chebyshev expansion in ln k, N-1 parameters amplitude(1), tilt(2), running(3), … (or N-1 nodal point k-localized values) Dual Chebyshev expansion in ln k: Standard 6 is Cheb=2 Standard 7 is Cheb=2,Cheb=1 Run is Cheb=3 Run & tensor is Cheb=3, Cheb=1 Low order N,M power law but high order Chebyshev is Fourier-like

  45. lnPsPt(nodal 2 and 1) + 4 params cfPsPt(nodal 5 and 5) + 4 params reconstructed from CMB+LSS data using Chebyshev nodal point expansion & MCMC Power law scalar and constant tensor + 4 params effective r-prior makes the limit stringent r = .082+- .08 (<.22) no self consistency: order 5 in scalar and tensor power r = .21+- .17 (<.53) run+tensor r = .13+- .10 (<.33)

  46. lnPslnPt(nodal 5 and 5) + 4 params. Uniform in exp(nodal bandpowers) cf. uniform in nodal bandpowers reconstructed from April07 CMB+LSS data using Chebyshev nodal point expansion & MCMC: shows prior dependence with current data logarithmic prior r < 0.075 uniform prior r < 0.42

  47. New Parameters of Cosmic Structure Formation Hubble parameter at inflation at a pivot pt =1+q, the deceleration parameter history order N Chebyshev expansion, N-1 parameters (e.g. nodal point values) Fluctuations are from stochastic kicks ~ H/2p superposed on the downward drift at Dlnk=1. Potential trajectory from HJ (SB 90,91):

  48. lnes(nodal 5) + 4 params. Uniform in exp(nodal bandpowers) cf. uniform in nodal bandpowers reconstructed from April07 CMB+LSS data using Chebyshev nodal point expansion & MCMC: shows prior dependence with current data esself consistency: order 5 uniform prior r = (<0.64) log prior r (<0.34; .<03 at 1-sigma!)

  49. lnes(nodal 5) + 4 params. Uniform in exp(nodal bandpowers) cf. uniform in nodal bandpowers reconstructed from April07 CMB+LSS data using Chebyshev nodal point expansion & MCMC: shows prior dependence with current data logarithmic prior r < 0.33, but .03 1-sigma uniform prior r < 0.64

  50. CL BB forlnes(nodal 5) + 4 paramsinflation trajectories reconstructed from CMB+LSS data using Chebyshev nodal point expansion & MCMC Planck satellite 2008.6 Spider balloon 2009.9 uniform prior Spider+Planck broad-band error log prior

More Related