The Cosmic Web

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The Cosmic Web the CMB high resolution frontier

• Dick Bond

Primary CMB anisotropies are strongly damped by
photon-baryon shear viscosity at high L gt 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 DMgas gravitational energy) ( CMB
weak lensing).
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CMBology
Probing the linear nonlinear cosmic web
Inflation Histories (CMBallLSS)
Kahler modulus potential Ttiq
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-SNWL)
wide open braking approach to preheating
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I N F L A T I O N
the nonlinear COSMIC WEB

• Primary Anisotropies
• Tightly coupled Photon-Baryon fluid oscillations
• viscously damped
• Linear regime of perturbations
• Gravitational redshifting

• Secondary Anisotropies
• Non-Linear Evolution
• Weak Lensing
• Thermal and Kinetic SZ effect
• Etc.

Decoupling LSS
reionization
19 Mpc
13.7-10-50Gyrs
13.7Gyrs
10Gyrs
today
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http//www.mpa-garching.mpg.de/Virgo/
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Momentum Space PROBES
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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/SPTSpiderCMBPol
nonlinear Gas Dark Matter Structure in the
Cosmic Web the cluster/gp web now, the
galaxy/dwarf system then
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resolution P(ln k) dynamics H(ln a) are related
in inflation (HJ) 10 e-folds


dynamics w(ln a) 1 e-folds
nonlinear Cosmic Web
CMB 2010 Planck1WMAP8SPT/ACT/QuietBicep/QuAD/
Quiet SpiderClover
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nonlinear Cosmic Web SZ/WL
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PROBES
calibrated candles SN1a
ULSSVLSSLSS 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.) - SZLensopticalX
hope (gas) streaming pair velocities
rehabilitated? SSS Lyman alpha forest, high-z
(1st stars) but gasNLfeedback
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massive clusters d gt 100, peak-patches Filaments
d 5-10 bridge clusters, groups bead the
bridges Membranes d 2 Voids d lt 0 Molecular
picture
LCDM 400 Mpc treeSPH 5123 gasCDM particles
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1.2 billion light years across gasdark matter
simulation of cosmic structure evolution (LCDM
concordance) biggest gasdynamical simulations
0.3 billion particles Millenium dark matter
simulation 10 billion particles
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Galaxy Clusters

• 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.

X-ray emission
Sunyaev-Zeldovich effect
Light 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)
-

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pass the CMB thru the cosmic web CBI extra
power??
5123 LCDM sim tSZ maps rotate translate
copies(z) of 400 Mpc box
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pass the CMB thru the cosmic web CBI extra
power??
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Quiet2
Bicep _at_SP
CBI pol to Apr05 _at_Chile
(1000 HEMTs) _at_Chile
CBI2 to early08
QUaD _at_SP
Acbar to Jan06, 07f _at_SP
Quiet1
SCUBA2
Spider
(12000 bolometers)
2312 bolometer _at_LDB
APEX
SZA
JCMT _at_Hawaii
(400 bolometers) _at_Chile
(Interferometer) _at_Cal
ACT
Clover _at_Chile
(3000 bolometers) _at_Chile
Boom03_at_LDB
EBEX_at_LDB
2017
2004
2006
2008
LMT_at_Mexico
2005
2007
2009
SPT
Bpol_at_L2
LHC
WMAP _at_L2 to 2009-2013?
(1000 bolometers) _at_South Pole
ALMA
DASI _at_SP
(Interferometer) _at_Chile
Polarbear
(300 bolometers)_at_Cal
CAPMAP
Planck08.8
AMI
(84 bolometers) HEMTs _at_L2
GBT
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WMAP3 sees 3rd pk, B03 sees 4th
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CBI excess 02
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Readhead et al. ApJ, 609, 498 (2004)
CBI excess 04
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CBI excess 06
state November 06
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CBI excess 07
CBI sees 4th 5th pk
Current high L state November 07
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CBI_at_5040m
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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

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What is the redshift range that contributes to
the SZ effect? all from 0 to 2
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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
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5123 LCDM sim tSZ,kSZ,X,WL maps rotate
translate copies(z) of 400 Mpc box
redshift cut
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5123 LCDM sim tSZ,kSZ,X,WL maps rotate
translate copies(z) of 400 Mpc box
Halo mass cut
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5123 LCDM sim SZ power spectra for various
realizations
TSZ
KSZ
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5123 LCDM sim SZ power halo overdensity cut cf.
virial density
5123 LCDM sim SZ power halo mass cut
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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)
Best parameter determinations (until Nov07 work)
Weak lensing included a small impact on
parameters
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
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s8 Tension of WMAP3
WMAP3cbicomb05 acbar03B03 Std 6 s8SZ7 s8
WMAP3 620 cut 0.790. 053 0.960.10 SZ
(Wm 0.260.038) (t 0.08740.0030)
cf. weak lensing
CFHTLS survey05 0.86 - .05 Virmos-Descart
non-G errors s8 0.80 - .04 if Wm 0.3 - .05
SZ treatment does not include errors from
non-Gaussianity of clusters, uncertainty in SZ CL
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CBI excess 04
cf. CBI excess 07
Current state November 07
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Current CBIBIMA PS
Fit CMBExcess model to CBItot data Red curve SPH
simulation-based template (Bond et al.), 1.03 -
0.07 blue curve analytic (KomatsuSeljak, 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 dont.
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CBI2_at_5040m
why Atacama? driest desert in the world. thus
cbi, toco, apex, asti, act, alma, quiet, clover
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CBI2 Forecast 9 Months on CMB
Caltech, NRAO, Oxford, CITA, Imperial by about
Feb07
Forecast gives 12 error on current excess,
assuming level doesnt 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/Blue9-month spectrum with big dishes,
different scan strategies.
SZE Secondary
s87
CMB Primary
s82
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Sample CBI2 clusters
Clusters from early CBI2 observations. Many
more now (Nov07) CBI2 very good at clusters at
z0.15, close enough so other wavelength
follow-ups are easier.
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ACT_at_5170m
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ACT
Science
Observations
CMB lgt1000
Growth of structure
Eqn. of state
Cluster (SZ, KSZ X-rays, optical)
Atacama Cosmology Telescope
Neutrino mass
Diffuse SZ
Ionization history
OV/KSZ
Inflation
Lensing
Power spectrum
X-ray
Optical
Theory
Collaboration
Columbia
Cardiff
Haverford
CUNY
NIST
INAOE
NASA/GSFC
Princeton
Rutgers
UBC
UPenn
U. Toronto
U. KwaZulu-Natal
U. Catolica
UMass
U. Pittsburgh
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Simulations of mm-wave data.
Survey area
High quality area
150 GHz
SZ Simulation
MBAC on ACT
PLANCK
Burwell/Seljak
2X noise
1.7 beam
MAP
WMAP
ACT
PLANCK
Statistical uncertainties based on 1 season with
best measured noise.
de Oliveira-Costa
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Sample forecast for SZ cluster surveys
4000 sq deg with SPT, 22000 clusters
Subha Majumdar Graham Cox CITA04
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The SZ cluster frontier
high/low s8 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
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Quiet2
Bicep _at_SP
CBI pol to Apr05 _at_Chile
(1000 HEMTs) _at_Chile
CBI2 to early08
QUaD _at_SP
Acbar to Jan06, 07f _at_SP
Quiet1
SCUBA2
Spider
(12000 bolometers)
2312 bolometer _at_LDB
APEX
SZA
JCMT _at_Hawaii
(400 bolometers) _at_Chile
(Interferometer) _at_Cal
ACT
Clover _at_Chile
(3000 bolometers) _at_Chile
Boom03_at_LDB
EBEX_at_LDB
2017
2004
2006
2008
LMT_at_Mexico
2005
2007
2009
SPT
Bpol_at_L2
LHC
WMAP _at_L2 to 2009-2013?
(1000 bolometers) _at_South Pole
ALMA
DASI _at_SP
(Interferometer) _at_Chile
Polarbear
(300 bolometers)_at_Cal
CAPMAP
Planck08.8
AMI
(84 bolometers) HEMTs _at_L2
GBT
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PRIMARY END _at_ 2012?
CMB 2009 Planck1WMAP8SPT/ACT/QuietBicep/QuAD/
Quiet SpiderClover