CMB & Fundamental Physics

Dick Bond

PhenomenologyPhenomenology of of CMB+LSS CMB+LSS as as highhigh precision precisionteststests of of Primordial Primordial SpectraSpectra & & Statistics Statistics (scalar (scalar curvat curvature,ure, subdominant subdominant isocurvature, isocurvature, tensor).tensor). Contents Contents of of U U & & its its properties properties (baryons,dark (baryons,dark matter/energy),matter/energy), modified modified gravity,gravity, … … Be Be AwareAware ofof assumedassumed priorprior probabilitiesprobabilities

CMBCMB datadata && expts:expts: L-spaceL-space anomaliesanomalies (low,(low, high)high) – – new new physics physics or or old; old; systematics?systematics? Using Using LSS LSS data data (weak (weak lens, lens, z-surveys, z-surveys, clusters) clusters) “weakly“weakly or or radically radically br brokenoken scale scale invariance”? invariance”? darkdark energy energy “equation “equation of of state” state” – – status status & & prospects prospects

CMBCMB Polarization Polarization DASI DASI 02 02, ,WMAP WMAP 03, 03, CBI, CBI, BOOM2KBOOM2K, ,QUEST, QUEST, BICEP BICEP, , Pique/CAPmap,Pique/CAPmap, Polarbear, Polarbear, AMiBA, AMiBA, B-machine, B-machine, Planck, Planck, CMBpol CMBpol : :break break degeneraciesdegeneracies of of cosmic cosmic parameters parameters

Khor(t)=Ha :: : : KNL(t)

λphys = 21πat()/ k , a= now Cosmic Spatial Length Scale (unwrinkled)

MomentumMomentum SpaceSpace PROBESPROBES

1 Khor(t)=Ha :: : : KNL(t)

λphys = 21πat()/ k , a= now Cosmic Spatial Length Scale (unwrinkled)

MomentumMomentum SpaceSpace PROBESPROBES

Khor(t)=Ha

Khor(t)=Ha :: : : KNL(t)

λphys = 21πat()/ k , a= now Cosmic Spatial Length Scale (unwrinkled) CosmicCosmic MomentumMomentum SpaceSpace PROBESPROBES 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 00-03, Acbar 01-03, WMAP 01/02/03, Planck (ESA/NASA + CdnSA 07), … ACT/SPT…CMBPol nonlinearnonlinear Gas Gas & & Dark Dark Matter Matter Structure Structure in in the theCosmicCosmic Web Web thethe cluster/cluster/gpgp web web “now” “now”,, the the g galaxy/dwarfalaxy/dwarf s systemystem “then” “then”

2 Khor(t)=Ha :: : : KNL(t)

Curved?Curved? No. No. DarkDark Energy! Energy! WhatWhat is is it? it?

DarkDark Matter! Matter! WhatWhat is is it? it?

Inflation/BraneInflation/Brane probesprobes

nonlinearnonlinear Cosmic Cosmic Web Web

Khor(t)=Ha :: : : KNL(t) PROBESPROBES

calibratedcalibrated candles:candles: SN1a + SN1a + λphys = 21πat()/ k , a= now Cosmic Spatial Length Scale (unwrinkled) 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? 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 (1st stars) but gas+NL+feedback

3 VLSSVLSS && z-surveysz-surveys (SDSS, (SDSS, 2dFRS) 2dFRS) LSSLSS probesprobes currentcurrent data data Weak-lens,Weak-lens, CMB, CMB, SZ, SZ, clustersclusters (X-ray, (X-ray, optical): optical): cf.cf. Broad-bandBroad-band power power :: : good-fitgood-fit : ΛΛCDMCDM modelmodel CMBCMB relative relative to to good good fit fit models, models, brokenbroken scale scale invariance? invariance?

4 Cosmic Background Imager (CBI)

BOOMERANG

ACBAR

GrandUnifiedSpectrumGrandUnifiedSpectrum pre-WMAPpre-WMAP cf.cf. post-WMAPpost-WMAP onon Boomerang/CBI Boomerang/CBI bands bands

5 VLSSVLSS && z-surveysz-surveys (2dFRS, (2dFRS, SDSS) SDSS) LSSLSS probesprobes Jan03Jan03 datadata Weak-lens,Weak-lens, CMB, CMB, SZ, SZ, clustersclusters (X-ray, (X-ray, optical): optical): Broad-bandBroad-band power power cf.cf. good-fitgood-fit ΛΛCDMCDM modelmodel CMBCMB

VLSSVLSS && z-surveysz-surveys (SDSS, (SDSS, 2dFRS) 2dFRS) LSSLSS probesprobes currentcurrent data data Weak-lens,Weak-lens, CMB, CMB, SZ, SZ, clustersclusters (X-ray, (X-ray, optical): optical): cf.cf. Broad-bandBroad-band power power :: : good-fitgood-fit : ΛΛCDMCDM modelmodel CMBCMB relative relative to to good good fit fit models, models, brokenbroken scale scale invariance? invariance?

6 Jan00Jan00 Jan02Jan02 Jun02Jun02 Jan03Jan03 Mar03Mar03 Boom-NABoom-NA B98_1.8%B98_1.8% CBICBI CBI-2yrCBI-2yr WMAPWMAP TocoToco VSA-extVSA-ext DASIDASI VSAVSA CBI-2yr-calCBI-2yr-cal QMAPQMAP Acbar Acbar VSA-ext-calVSA-ext-cal ViperViper Maxima B98_1.8% Maxima B98_1.8% B98_2.9% PythonPython B98_2.9% AcbarAcbar SuZIESuZIE COBECOBE DASIDASI Archeops Archeops B98_2.9%B98_2.9% Ovro-22,7Ovro-22,7 Other Jan00 Other Jan00 MaximaMaxima DASIDASI DASI CatCat DASI Maxima BAMBAM COBECOBE Maxima MaximaMaxima SK95SK95 COBE Other Jan00 COBE OtherOther Jan00 Jan00 SP94SP94 Other Jan00 OtherOther Jan00 Jan00 ArgoArgo WhiteDishWhiteDish MSAMMSAM cf.cf. WMAPextWMAPext = = MAX MAX WMAP+cbi-1yrWMAP+cbi-1yr TenerifeTenerife +acbar+acbar FIRSFIRS SP91SP91 (&(& calibration calibration X X 2!) 2!) COBECOBE

7 Absolute Calibration WMAP: 94 GHz BOOM/98: 150 GHz

--> Primary calibration for BOOM/03 is with WMAP calibrated BOOM/98 structures

8 Khor(t)=Ha :: : : KNL(t)

200

TE from WMAP TE popular model EE popular model EE from DASI ) 2 100 100 K 100 µ ( π /2 L

0 L(L+1)c

-100 0 200 400 600 multipole L

“The Seven Pillars” of the CMB (of inflationary adiabatic fluctuations)

¾Large Scale Gravitational Potential Minimal Anisotropies (COBE/FIRS) Inflationary parameter ¾Acoustic Peaks/Dips (Boom/CBI/WMAP) set ¾Damping Tail (CBI/Acbar) ¾Gaussianity (COBE/Boom/WMAP) 9Polarization, TE correlation (DASI/WMAP .. CBI/B2K) Quintessence •Cosmic Web Secondary Anisotropies (CBI/Acbar/BIMA) Gravity Waves •Gravity Waves, B-type polarization Broken Scale Invariance neutrino mass, decaying particles, nonGaussian statistics, Isocurvature modes (subdominant, defects), beyond Einstein gravity (JBD), …

9 <~ 2 sigma indication of [dn /dlnk] <0 in <~ 2 sigma indication of [dnss/dlnk] <0 in Mar03Mar03 datadata wQ<-0.7 @2sigma is stable – database or MCMC. Need CMB+SN1 not CMB+HST-h Tensor/Scalar <~ 0.7 @ 2 sigma VeryVery goodgood agreementagreement MCMCMCMC cf.cf. fixedfixed gridgrid ττcc prior prior on on TT TT mimics mimics ττcc constraint constraint from from the the TE TE OK OK

Khor(t)=Ha :: : : KNL(t)

Curved?Curved? No. No. DarkDark Energy! Energy! WhatWhat is is it? it?

DarkDark Matter! Matter! WhatWhat is is it? it?

Inflation/BraneInflation/Brane probesprobes

nonlinearnonlinear Cosmic Cosmic Web Web

10 VLSSVLSS && z-surveysz-surveys (SDSS, (SDSS, 2dFRS) 2dFRS) LSSLSS probesprobes currentcurrent data data Weak-lens,Weak-lens, CMB, CMB, SZ, SZ, clustersclusters (X-ray, (X-ray, optical): optical): cf.cf. Broad-bandBroad-band power power :: : good-fitgood-fit : ΛΛCDMCDM modelmodel CMBCMB relative relative to to good good fit fit models, models, brokenbroken scale scale invariance? invariance?

11 Red-sequence Cluster Survey (RCS): Data taken with CFHT and CTIO. 53 square degrees analysed. Measured > 2x106 galaxy shapes down to R=24.

VIRMOS-DESCART: Data taken with CFHT 11 square degrees analysed 5 Measured > 8x10 galaxy shapes down to IAB=24.5

Deep Lens Survey 28 square degrees (ongoing) CFHT Legacy Survey 140 square degrees (started) RCS2 1000 square degrees (started)

LSST > 104 square degrees (>2008) Pan-STARRS > 104 square degrees (>2012) SNAP (space) few 100 square degrees (>2011)

12 160 000 galaxies

Virmos field F14 dark matter map – preliminary

VirmosV F14 galaxy surface density -- preliminary

13 weak lensing breaks some CMB partial degeneracies

Contaldi, Hoekstra & Lewis (2003)

CMB + LSS (lens/clusters/wea k-shape from z- surveys) flat+weak-h prior

cf. CHL 03 RCS (90 sq deg survey, 53 sq deg applied to weak lensing, Hoekstra, Gladders & Yee) +WMAP+CBI1 yr+Acbar

Broad-bandpower @ ~ k Broad-bandpower @ ~ kNLNL

14 2dFRS (analysis on 147K galaxies Percival etal. 2001)

VLSSVLSS && z-surveysz-surveys (2dFRS, (2dFRS, SDSS) SDSS) LSSLSS probesprobes Jan03Jan03 datadata Weak-lens,Weak-lens, CMB, CMB, SZ, SZ, clustersclusters (X-ray, (X-ray, optical): optical): Broad-bandBroad-band power power cf.cf. good-fitgood-fit ΛΛCDMCDM modelmodel CMBCMB

15 SDSS (analysis on 205K galaxies Tegmark etal 2003)

SDSS (analysis on 205K galaxies Tegmark etal 2003)

16 z-surveysz-surveys (SDSS, (SDSS, 2dFRS) 2dFRS)

Weak-lens,Weak-lens, CMB, CMB, SZ, SZ, clustersclusters (X-ray, (X-ray, optical): optical): Broad-bandBroad-band power power :: ::

CMBCMB relative relative to to good good fit fit models, models, brokenbroken scale scale invariance? invariance?

SDSS

17 Khor(t)=Ha :: : : KNL(t)

λphys = 21πat()/ k , a= now Cosmic Spatial Length Scale (unwrinkled) RelationRelation to to CMB CMB multipoles: multipoles: k = ((L+1/2)22/R 22 + k22)1/2,1/2, k~L/(10000 h-1-1Mpc) ΛCDM k = ((L+1/2) /Rdecdec + k||||) k~L/(10000 h Mpc) ΛCDM RelationRelation to to the the Cosmic Cosmic Web Web & & Large Large Scale Scale Structure Structure k = Γ / (5 h-1-1 Mpc), Γ=Ω h/(Ω h22)1/21/2 , Γ=0.206 +- .006, Γ ~ 0.18 k hor,eqhor,eq= Γ / (5 h Mpc), Γ=Ωmmh/(Ωererh ) , Γ=0.206 +- .006, Γeffeff~ 0.18 SDSSSDSS

σ =0.86 +- .05 but depends on dn/dlnk 0.96 +- .08 σ88 =0.86 +- .05 but depends on dn/dlnk 0.96 +- .08

Anomalies: Systematics, Statistics, AstroPhysics or Fundamental Physics?

“anomalies” @ low L 2,3; ~20-30; check@200, > 600? Issues: L=2,3 how low is the probability? Glitches? non-WMAP data e.g. Acbar/CBI calibration CBI anomalous power @ L > 2000, Sunyaev Zeldovich effect in the cosmic web is plausible is σ8 if ~ 0.9 (nonlinear gasdynamics) Statistical isotropy broken on large scales?

18 Is there a case for BSI (yet)? weak indication of [dn /dlnk] <0 in Jan03 and weak indication of [dnss/dlnk] <0 in Jan03 and Mar03Mar03 CMBCMB datadata ComplicatedComplicated by by high high correlations correlations (degeneracies) (degeneracies) among among cosmic cosmic variables, σ -τ -n & dn /dlnk variables, σ88-τCC-nss & dnss/dlnk Optimal spectra in k-space -> BSI?

driven by “anomalies” @ low L (20-30, 2,3) & L > 600 finer ∆L look: changing target space helps to reduce

With WMAPext+LSS (+SSS) – extend the parameter list over the minimal inflation set

• Do we need even more precision on the parameters ? Yes, we want to explore larger parameter spaces. •WMAP: – Running ns – positive slope at low l, negative at higher l COBE-DMR also preferred larger n~1.2 – Low quadrupole & octupole –new physics ? – Gravitational wave (tensor) contribution to dT/T < 0.72 of scalar component

19 weakweak indicationindication ofof [dn /dlnk] <0 in [dnss/dlnk] <0 in Jan03Jan03 andand Mar03Mar03 + dn/dlnk CMBCMB datadata CMB data alone

z-surveysz-surveys (SDSS, (SDSS, 2dFRS) 2dFRS) SDSS

σ8 Weak-lens,Weak-lens, CMB, CMB, SZ, SZ, 2yr CBI SZ clustersclusters (X-ray, (X-ray, optical): optical): Broad-bandBroad-band power power :: CMB :: dn/dlnk

CMBCMB relative relative to to good good fit fit models, models, brokenbroken scale scale invariance? invariance?

20 WMAP z-surveysz-surveys (SDSS, (SDSS, 2dFRS) 2dFRS) dominant to

~khor,eq 0.03 /Mpc

:: WMAPWMAP compressed compressed on on to to 29 29 bands bands

higher res z-surveysz-surveys (SDSS, (SDSS, 2dFRS) 2dFRS) look at the anomaly- not as severe

WMAPWMAP compressed compressed on on to to 49 49 bands bands

CMBCMB radically radically broken broken scalescale invariance? invariance?

21 Changeta rgetmode l helps to reduce “anomali es”

To influence C by “fundamental physics”: To influence CLLby “fundamental physics”: ActAct on on the the k-scales k-scales of of relevance relevance for for the the CMB CMB probe probe – – 3 3 epochs epochs

(1) k (t) on its inward sweep during inflation or inflation-proxy (BSI, (1) khorhor(t) on its inward sweep during inflation or inflation-proxy (BSI, radicalradical or or not, not, waterfall waterfall ends ends to to inflation, inflation, extra extra dimension dimension signatures???signatures??? Small Small topolo topologiesgies and and other other baroqueness) baroqueness) (2) k (t) on its outward sweep through decoupling/damping (2) khorhor(t) on its outward sweep through decoupling/damping (constituents(constituents of of the the universe, universe, modi modifiedfied gravity, gravity, can can there there be be any any true true extraextra dimension dimension signatures signatures from from this this epoch epoch – – JBD JBD only?) only?) (3) k (t) as part of its turn-around to an inward sweep (Q etal) (3) khorhor(t) as part of its turn-around to an inward sweep (Q etal)

Khor(t)=Ha

22 CMB Polarization

200

TE from WMAP TE popular model EE popular model EE from DASI )

2 100 K µ ( π /2 L

0 L(L+1)c

-100 0 200 400 600 multipole L deB03

23 EricEric Hivon Hivon 02 02

Expected Patterns of Polarization in the Sky

Eric Hivon - BICEP

24 25 Summary:Summary: “Standard” “Standard” Inflation-ba Inflation-basedsed model model looks looks very very good, good, ALL ALL parametersparameters come come out out near near to to earlier earlier expectations, expectations, surprises surprises (if (if theythey hold hold up) up) are are not not that that surp surprising.rising. Broad-brush: Broad-brush: Gaussian, Gaussian, adiabaticadiabatic (curvature) (curvature) perturbations, perturbations, amplitude amplitude about about right right to to generategenerate LSS LSS and and even even SSS. SSS. TheThe Λ Λinin Λ ΛCDMCDM was was emerging emerging for for years. years.

IsIs more more needed? needed? Currently Currently no no but but there there are are anomalies anomalies which which may may emergeemerge as as new new physics physics – – which which at at least least for for now now give give theorists theorists aa license license to to generate generate many many theoretical theoretical papers. papers. TheoreticalTheoretical priors priors are are theorist-dependent, theorist-dependent, but but most most anomaly- anomaly- generatorsgenerators are are baroque baroque (to (to me). me). e.g. e.g. radically-broken radically-broken scale scale invarianceinvariance