experimental probe of inflationary cosmology (comparison of three epic versions)
DESCRIPTION
Experimental Probe of Inflationary Cosmology (comparison of three EPIC versions). Asantha Cooray University of California-Irvine. Post-Planck Mission Effort in US. Deliverables. The ell to which measurements are cosmic variance limited. (1) Nolta et al. 2008 - PowerPoint PPT PresentationTRANSCRIPT
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Experimental Probe of InflationaryCosmology
(comparison of three EPIC versions)
Asantha CoorayUniversity of California-Irvine
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Post-Planck Mission Effort in US
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Observable WMAP Planck EPIC
TT 530(1) 1750(2) 3700
TE 900(2) 2700
EE 2600
BB (lensing) 1850(1) Nolta et al. 2008 (2) HFI, based on Planck Blue Book
Deliverables
The ell to which measurements are cosmic variance limited
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Before EPIC-IM (2008): EPIC-LC and EPIC-CS
EPIC (LC) Low-Cost Option
Science Science Requirements Instrument
GW <BB> Detect both l = 5 & l = 100 <BB> bumps at r = 0.01after Galactic foreground removal
1º FWHM @100 GHzAll sky2 μK√s2 years
30 – 300 GHz
EPIC (CS) Comprehensive Science Option
Science Science Requirements Instrument
GW <BB>
Lensing <BB>
<EE>
Detect both l = 5 & l = 100 <BB> bumps at r = 0.001after Galactic foreground removal
Measure lensing <BB> to cosmic variance to l = 1000Potential to subtract lensing <BB>
Measure <EE> to cosmic variance into the damping tail
5' FWHM @100 GHzAll sky2 μK√s2 years
30 – 300 GHz
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Phase I: Two mission options
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EPIC-IM (2008/2009 version)
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EPIC=EPIC IMEPIC CS = Cosmic variance
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This is enabled by the cosmic variance limited E-mode measurement.
Last word on the “Age question”
Our final age determination
will be accurate to 25
Myrs.
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Inflationary Parameters
Quantity Discoverer WMAP Error with
PlanckError with
EPIC
Amplitude of density perturbations
COBE
Scalar spectral index WMAP
Running of the spectral index
Planck?
Inflationary Gravitational Waves
EPIC?
IGW spectral index ?
Running of the IGW index ?
Primordial non-Gaussianity ? 32 +/- 21 5 2
Amplitude of the inflationary gravitational waves depends only on the energy scale of inflation. Interpretation is NOT model-dependent.
The information captured by the inflationary gravitational wave background is unique, it cannot be obtained even with a perfect measurement of the scalar spectral index and its running.
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LensedUnlensed
Difference Foreground Mass
Lensing studieswith EPIC
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Theoretical projectedpotential
Optimal Quadratic (Hu 2001)
Likelihood(Hirata & Seljak 2003)
All Sky Maps of Projected Gravitational Potential
Gravitational potential determined from CMB polarization and temperature mapssensitive to
- neutrino masses- dark energy
All-sky potential map: maps to cosmic limits on the whole sky!- a legacy for every future study of structure formation
8º
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Measuring the lensing power spectrum
NET muK/sqrt(sec) one-year
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Lensing Removal and the Search for Gravitational-wave B-modes
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What is the optimal resolution for lens de-cleaning?
~4 arcmins is the ideal beam size
Scientific Gain =(T/S-limit with lens cleaning)/(without cleaning)
Beam
incr
easi
ng
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Particle physics application of EPIC
Lensing B-modes and CMB Cosmic Shear Reconstruction
neutrino mass (Σmν < 0.05 eV; from the linear regime)
Test SuperK Atmosphere oscillations that suggest Δmν
∼2x10-3 eV2
and distinguish between two mass hierarchies
CMB lensing probes linear fluctuationsSource properties known(Both these lead to systematicerrors in galaxy lensing)
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EPIC can not only measure the total sum of neutrino masses, but when combined with atmospheric oscillation result for the mass-squared difference, establish individual masses of all three neutrino species.
Better than (<) 6 arcmin resolution is a requirement for EPIC to enable CMB lensing studies.
The measurement cannot be achieved with a lensing analysis in a small patch of the sky. All-sky coverage is essential.
What is the neutrino mass hierarchy?
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Did dark energy exist at z> 2?
In some models of dark energy, a small contribution exist to the total energy density budget of the Universe at z >2.
CMB lensing probes cosmology at z of 2 to 4, where the lensing efficiency is highest.
EPIC can constrain the early dark energy density to better than 0.1%.
(Half-sky weak lensing with planned Euclid can only constrain same down to 2.5%. JDEM with 4000 deg2, down to 7.5%)
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When and how did the Universe reionize?
Astrophysics Measurement
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Reionization history
Model-dependent constraints
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Reionization history
Model-independent constraints
EPIC allows cosmic variance extraction of 5 components.
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Mapping Galactic Magnetic Fields over the Whole Sky
Map of full sky with σP < 0.3 %
Planck
EPIC-IM
Mission BandGHz
FWHMarcmin
σ(Q)kJy/sr/beam
Pol. depthAV
Planck 350 5 24 4
EPIC-IM500 2 0.9 0.06
850 1 0.7 0.01How does large-scale Galactic field relatedto field in embedded star-forming regions?
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Summary