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