the cosmic microwave background
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The Cosmic Microwave Background. Lecture 2 Elena Pierpaoli. Lecture 2 – secondary anisotropies. Primary anisotropies: scattering, polarization and tensor modes Effect on parameters Secondary anisotropies : gravitational ISW Early Late Rees- Sciama lensing - PowerPoint PPT PresentationTRANSCRIPT
The Cosmic Microwave Background
Lecture 2Elena Pierpaoli
Lecture 2 – secondary anisotropies
• Primary anisotropies: – scattering, polarization and tensor modes– Effect on parameters
• Secondary anisotropies: gravitational – ISW
• Early • Late• Rees-Sciama
– lensing• Secondary anisotropies: (Re-scattering)
– Reionization (uniform and patchy)– Sunyaev-Zeldovich effect (thermal & kinetic)
The decomposition of the CMB spectrum
Challinor 04
Line of sight approach
Seljak & Zaldarriaga 06
Synchronous gauge
Conformal Newtonian
Visibility function g
Polarization
Due to parity symmetry of the density field, scalar perturbationsHave U=0, and hence only produce E modes.
Scattering and polarization
If there is no U mode to start with, scattering does not generate it. No B mode is generated.
Scattering sources polarization through the quadrupole.
Tensor modes
Parity and rotation symmetry are no longer satisfied with gravity waves. B modes could be generated, along with T and E.
In linear perturbation theory, tensor and scalar perturbations evolve independently.
The tensor modes expansion
Scattering only produces E modes, B Are produced through coupling with E And free streaming.
Power spectra for scalar and tensor perturbations
Tensor to scalar ratio r=1
Effect of parameters
• Effect of various parameters on the T and P spectrum
1)Neutrino mass: Physical effects
Fluctuation on scale enters the horizon
Neutrinos free-stream Neutrinos do not free-stream(I.e. behave like Cold Dark Matter)
Derelativization
on fluctuations
on expansion Expan. factor a
Recombination
Radiation dominated Matter dominatedheavy
light
(T=0.25 eV) – change the expansion rate – Change matter-radiation equivalence (but not recombination)
2) The relativistic energy density Nn
N n = (rrad - rg) / r1n
• Effects: – change the expansion rate– Change matter-radiation equivalence (but not the
radiation temperature, I.e. not recombination)• Model for:
– neutrino asymmetry– other relativistic particles– Gravitational wave contribution
Expan. factor a
Recombination
Radiation dominated Matter dominated3
>3
Neutrino species
Bell, Pierpaoli, Sigurdson 06
Neutrino interactions
Bell Pierpaoli Sigurdson 06
Late ISW
ISW-Galaxy cross correlation
Giannantonio 08
Rees Sciama effect
Seljak 1996
Lensing: temperature
Lewis & Challinor 2006
Lensing: polarization
Lensing: B polrization
Reionization: overall suppression
Reionization: large scale effects
t = 0.0845
Reionization
4) Neutrinos & reionization•Motivation: High redshift reionization required by the TP WMAP CMB power spectrum (t= 0.17), but difficult for stars to reionize “so early”. Decaying particles may provide partial reionization at high redshift.
The neutrino decay model
n p + e
Hansen & Heiman 03
e + ge + gH + g H+ + e-
H + e- H+ + e- + e-
Inverse Compton
Photoionization
Collisional ionization
Reionization history
• mass mn = 140-500 MeV ,• Ee = 0 -180 MeV. • time decay: t15 = / t 1015 s =
2-10 • abundance: = 10Wn -9
Neutrino model parameters
Standard parameters
x
Ionization fraction
X= nH,ion / nH,total
Pierpaoli 2004
Power spectra
• High reionization from decay particles produce a too high optical depth and a too weird TP spectrum
• High-z reionization from stars still needed• Long decay times and low abundances are preferred
Pierpaoli 2004Standard parametersx
Annihilating matter and reionization
Slatyer et al 09
Mapelli Ferrara Pierpaoli 06
Ostriker-Vishniac effect & patchy reionization
Santos et al 03
Zhang et al 04
OV present even if reionization is uniform
The Sunyaev-Zeldovich thermal signature
e-
gg
clusterFrequencies of observation
-Typical dimension: 1-10 arcmin- Typical intensity: 10-4 K - Signal is independent of cluster ‘s redshift- Signal scales as ne
- Need complementary information on redshift from other data. -Both high resolution (SPT, ACT..) And low resolution/all-sky (Planck) planned
Cosmology with future surveys:
Cluster number counts
Cluster power spectrum
DT/T = f(n) y
y Te ne
Clusters number counts
Cluster counts depend mainly on sigma_8, Omega_m, w, and the flux threshold of the survey
Aghanim et al 08
SZ thermal effect-Power spectrum
SZ kinetic effect
-Same frequency dependence as CMB(difficult to separate)
-typically subdominant to Th SZ(5% of the ThSZ signal)
SZ polarization produced by
• Primordial quadrupole (reducing cosmic variance, probing large scale power)
• cluster’s transverse velocity• Clusters’ magnetic fields• Double scattering within the cluster
Magnitude of SZ polarization
Liu et al 2005