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).

CMBology

ForegroundsCBI, Planck

ForegroundsCBI, Planck

SecondaryAnisotropies (CBI,ACT)

(tSZ, kSZ, reion)

SecondaryAnisotropies (CBI,ACT)

(tSZ, kSZ, reion)

Non-Gaussianity(Boom, CBI, WMAP)

Non-Gaussianity(Boom, CBI, WMAP)

Polarization ofthe CMB, Gravity Waves

(CBI, Boom, Planck, Spider)

Polarization ofthe 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

Probing the linear & nonlinear cosmic web

wide open braking

approach to preheating

Kahler modulus potential T=+i

R ? z = 0

Primary Anisotropies

•Tightly coupled Photon-Baryon fluid oscillations

• viscously damped

•Linear regime of perturbations

•Gravitational redshifting

Dec

oupl

ing

LSS

Secondary Anisotropies

•Non-Linear Evolution

•Weak Lensing

•Thermal and Kinetic SZ effect

•Etc.

z? ø 1100

19 Mpc

reionization

redshift z

time t13.7Gyrs 10Gyrs today

the nonlinear COSMIC WEB

I

N

F

L

A

T

I

O

N

13.7-10-50Gyrs

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

Cosmic Spatial Length Scale (unwrinkled)

Khor(t)=Ha

KNL(t)

phys a t k a= n o w2 1( ) / ,

::::

Momentum Space PROBESMomentum Space PROBES

Khor(t)=Ha

Cosmic Spatial Length Scale (unwrinkled)

Khor(t)=Ha

KNL(t)

phys a t k a= n o w2 1( ) / ,

::::

Cosmic Momentum Space PROBESCosmic Momentum Space PROBESCMB 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”

nonlinear Gas & Dark Matter Structure in the Cosmic Web the cluster/gp web “now”, the galaxy/dwarf system “then”

Khor(t)=Ha

KNL(t):

:

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

Khor(t)=Ha

KNL(t)::

::

nonlinear Cosmic Web SZ/WL

nonlinear Cosmic Web SZ/WL

Cosmic Spatial Length Scale (unwrinkled)

Khor(t)=Ha

KNL(t)

phys a t k a= n o w2 1( ) / ,

::

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 (1st stars) but

gas+NL+feedback

::

calibrated candles: SN1a +

calibrated candles: SN1a +

PROBESPROBES

Cosmic Web & Superclustering: a naturalconsequence of the gravitational instability of ahierarchical Gaussian random density field

massive clusters:

> 100, peak-patches

Filaments ~ 5-10

bridge clusters, groups bead the bridges

Membranes: ~ 2

Voids: < 0

“Molecular” picture

CDM 400 Mpc treeSPH

5123 gas+CDM particles

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

• The most massive, collapsed structures in the universe. They contain galaxies, hot, ionized gas (107-8K) 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)

- =

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

5123 LCDM sim tSZ maps: rotate & translate copies(z) of 400 Mpc box

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

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

Planck08.8

(84 bolometers)

HEMTs @L2

Bpol@L2

ALMA(Interferometer) @Chile

(12000 bolometers)SCUBA2

Quiet1

Quiet2Bicep @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

WMAP3 sees 3rd pk, B03 sees 4th

CBI excess 02

Readhead et al. ApJ, 609, 498 Readhead et al. ApJ, 609, 498 (2004)(2004)

CBI excess 04

state

November 06

state

November 06

CBI excess 06

Current high L state

November 07

Current high L state

November 07

CBI sees 4th 5th pk

CBI excess 07

CBI@5040m

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 4.5o2, 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

What is the redshift range that contributes to the SZ effect?

all from 0 to ~2

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

5123 LCDM sim tSZ,kSZ,X,WL maps: rotate & translate copies(z) of 400 Mpc boxredshift cut

5123 LCDM sim tSZ,kSZ,X,WL maps: rotate & translate copies(z) of 400 Mpc boxHalo mass cut

TSZ

KSZ

5123 LCDM sim SZ power spectra for various realizations

5123 LCDM sim SZ power halo overdensity cut cf. virial density

5123 LCDM sim SZ power halo mass cut

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

σ8 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^7σ8 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

s8 = 0.80 +- .04 if m = 0.3 +- .05

cf. weak lensingcf. weak lensing

Current state

November 07

Current state

November 07

CBI excess 04

cf. CBI excess 07

Current CBI+BIMA PSFit 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.

CBI2@5040m why Atacama? driest desert in the world. thus: cbi, toco, apex,

asti, act, alma, quiet, clover

CBI2 Forecast – 9 Months on CMBForecast 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 Feb07Caltech, NRAO, Oxford, CITA, Imperial by about Feb07

CMB CMB PrimaryPrimary

+SZE +SZE SecondarySecondary 8

7

82

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.

ACT@5170m

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 HaverfordU. KwaZulu-NatalRutgers U. Catolica

Cardiff

UMassCUNY

UBCNISTINAOE NASA/GSFC

UPennU. Pittsburgh U. TorontoPrinceton

Collaboration:

Simulations of mm-wave data.

1.401%

2%

Survey area

High quality area

150 GHz SZ Simulation MBAC 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

Sample forecast for SZ cluster surveys

4000 sq deg with SPT, 22000 clusters

Subha Majumdar & Graham Cox CITA04

The SZ & cluster frontierhigh/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

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

Planck08.8

(84 bolometers)

HEMTs @L2

Bpol@L2

ALMA(Interferometer) @Chile

(12000 bolometers)SCUBA2

Quiet1

Quiet2Bicep @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

PRIMARY END @ 2012? PRIMARY END @ 2012?

CMB ~2009+ Planck1+WMAP8+SPT/ACT/Quiet+Bicep/QuAD/Quiet +Spider+Clover