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
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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 > 1000.
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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 > 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?
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??