Post on 06-Apr-2018
8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Neutrino Masses with
Lensing of the
Cosmic Microwave Background
(Study of Experimental Probe of Inflationary Cosmology)
Asantha Cooray
University of California-Irvine
8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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O(10-5) perturbations(+galaxy)
Dipole (local motion)
(almost) uniform 2.726K blackbody (Penzias & Wilson)
Universe at 400kyr:the microwave sky
COBE(Mather & Smoot)
WMAP
8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Anisotropies
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8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Around 2013 with Planck
Hu & Dodelson
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Amblard
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8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Hu
8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Lensing distributes anisotropies
from degree scales to damping tailand smooths acoustic peaks
In temperature hard to seebecause of other secondaries
In polarization lensing mixes E & Bmodes. Polarization secondariesare smaller.
8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Non-Gaussianity of lensing
Bad: decreases information content of lensing B-modesfrom the case of a simple Gaussian mode counting.(Beware of Gaussian Fisher predictions of B-modes)
Good: allows a statistical mechanism to reconstruct
foreground mass distribution responsible for lensing
8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Lensing weakly correlates CMB modes with l �= l�:
T (l)T (l�)∗ ∝ φ(l − l�).
Reconstructed field �φ is quadratic in CMB temperature:
�φ( �n) = ∂ aα( �n)∂ aβ ( �n)α( �n) =
d 2l
(2π)2
1
C TT
� + N TT
�
T (l)e i l· b n
β (
�n) =
d 2l
(2π)2
C TT
�
C TT
� + N TT
�
T (l)e i l· b n
Second idea for detecting CMB lensing: look for extra power in �φ.
Compute C φφ� : quadratic in �φ, or four-point in CMB.
(> 50 publications)
Non-Gaussianity of lensing
8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Start(1) ❄
Gaussian fields {g �m, φ�m, aunlensed�m }
❄(2)
❄
(4)Lensed CMB alensed�m
❄(3)
NVSS data
❄(7)
Filtered galaxyfield �g
�m
✁ ✁ ✁ ✁ ☛
WMAP data
❄(5)
Filtered CMB �a�m
❄(6)
Reconstructedpotential �φ�m ❅ ❅ ❅ ❘(8)
Lensing estimator C φg �
�2C φg
� = (33.2± 10.5)× 10−
7
(20 ≤ � ≤ 40, stat .)
3.4σ detection, as a cross-correlation
Smith et al. 07
Hint of lensing in WMAP?
no detection limits on lensing-ISW and lensing-SZ Calabrese et al. 09
8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Next steps
A detection of the lensing potential power spectrum with WMAP-7?
Requires a computation of the 4 point function, work started, results out soon!!! (Joseph Smidt et al. in preparation)
Existing estimators (Hu & Okamoto; Seljak & Hirata) are biased, need
to properly account for the Gaussian part of the trispectrum and
remove noise bias.
Fast, optimized estimators for non-Gaussianity now developed in a
series of papers by Munshi, Smidt et al. (we measured the primordial
trispectrum for the first time ever in 1001.5026)
Still requires a large number of Monte-Carlo simulations.
Limited by computational resources. Out to ell of 900,
~25,000 CPU hours. Naive estimator scales as l4. Fast estimators
scales as l3logl.
8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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CMB lensing
CMB lensing vs. galaxy lensing
Advantages:
1. A precisely known source
2. Linear fluctuations, there isreally no need to model non-
linearities down to sub-percent
precision.
3. Community experience in
analyses of complex CMB
datasets
Disadvantages:
Finite information content!
8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Experimental Probe of Inflationary Cosmology
EPIC
Selected by NASA in 2003 for a 2 to 3-year study, again in 2008-2009In 2008-2009, EPIC was put forward as a general CMB community-supported mission
concept for the CMBpol post-Planck mission. In Europe, B-POL study (but not selected; Euclid selected for dark energy as a Cosmic Visions M class mission).
Jamie Bock (JPL), PI
Bock et al. 0906.1188
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8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Richness of the CMB Polarization Landscape
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8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Precision Cosmology
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Mapping NASA Objectives to EPIC Instrument Requirements
NASA
Research
Objective*
NASA
Targeted Outcome*
Measurement
Criteria
Instrument
Criteria
Test the Inflationhypothesis of the Big
Bang
Measure inflationary
B-mode power
spectrum toastrophysical limits for2 < _ < 200 at r = 0.01
after foreground
removal
_ All-sky coverage
_ wp-1/2 < 6 µK-
arcmin_ 30 – 300 GHz_ 1˚ resolution
_ Control systematicerrors below r =
0.01
Precisely determinethe cosmological
parameters governing
the evolution of the
universe
Measure EE to cosmic
variance into the Silkdamping tail to probe
primordial densityperturbations
_ 10' resolution
What are theorigin,
evolution, andfate of the
universe?
Improve our knowledgeof dark energy, themysterious cosmic energy
that will determine thefate of the universe
Investigate the seeds of cosmic structure in the
cosmic microwave
background
Measure thedistribution of dark
matter in the universe
Measure lensing-BB to
cosmic limits to probeneutrino physics and
early (z~2) darkenergy density and
equation of state
_ wp-1/2 < 2 µK-
arcmin
_ 6' resolution
Determine themechanism(s) by which
most of the matter of theuniverse became
reionized
Measure EE to cosmic
variance to distinguishreionization histories
_ Primary missionparameters above
How do planets,stars, galaxies and
cosmic structurescome into being?
Study the birth of stellar
and planetary systems
Map Galactic magneticfields via dust
polarization
_ 500 and 850 GHz
bands
*Taken from NASA 2007 Science Plan Primary Objective
Secondary Objective
EPIC-low cost just for this
EPIC-IM optimizedfor the goal of
measuring CMB
lensing with
deliverables of
neutrino masses.
8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Optimizing an experiment for a science goal
8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Particle physics application of EPIC
Lensing B-modes and CMB Cosmic Shear Reconstruction
A deliverable: neutrino mass (Σmν < 0.05 eV or better at
95% confidence level)
Test SuperK Atmosphere oscillations that suggest Δmν
2∼ 2x10 -3 eV 2
and distinguish between two mass hierarchies
CMB lensing probes linear fluctuationsSource properties known(Both these lead to systematic
errors in galaxy lensing)
EPIC study reports
8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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Neutrino mass hierarchy from cosmology
For the LCDM cosmological model, EPIC, as currently configured, reaches a sum of the neutrino masses of 0.042 eV and
if the equation of state of dark energy is allowed to vary this constraint is at 0.047eV at the same 95% confidence level.
This is not a simple Gaussian Fisher matrix estimate. It accounts for the full covariance, part of which was based on simulations.
8/3/2019 Asantha Cooray- Neutrino Masses with Lensing of the Cosmic Microwave Background
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EPIC-IM Specification Sheet
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Mass similar to the Planck satellite mission
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Experimental Probe of Inflationary Cosmology – Intermediate Mission (Bock, JPL)
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High Throughput, Multi-Band Focal Plane
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‘Moore’s Law’ for Sensitivity and Mapping Speed
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Neutrino mass hierarchy from cosmology
Can we do better?
Further optimize EPIC(at a very high cost), factor of 1.2 to 1.3 at mostimprovement with CMB polarization alone
Better, Combine EPIC with Euclid/JDEM-WL for a factor of ~2 to 3 improvement through z-binned lensing
+ a good model for non-linearities for galaxylensing.
lensing of 21-cm: highly
futuristic
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Summary
• Planck should do BB lensing, and get down to ~0.2 eV level
• Post-Planck EPIC satellite for CMB polarization is well developed.
• US-based CMB community has requested NASA to start a project
office after the 2010 Astronomy Decadal Survey, based onrecommendations on CMB sciences.
• If started, EPIC phase-A to begin around 2015, launch around
2020-2021.
• Will Planck provide a hint of tensors and/or primordial non-
Gaussianity? motivation for EPIC will be clearer then.