Cosmic Microwave Background Polarization measurements...
Transcript of Cosmic Microwave Background Polarization measurements...
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Experimental Cosmology and Astrophysics
Cosmic Microwave Background Polarization measurements with one of the Highest Telescopes on Earth
Michael Niemack, Cornell University October 2015
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Cosmic Microwave Background (CMB)
WMAP satellite measurements
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Atacama Cosmology Telescope (ACT)
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1920’s Edwin Hubble discovers: Other galaxies
exist Universe is
expanding!
Michael Niemack, Cornell
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Courtesy of NASA WMAP team
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Big Bang! Today
3 min. 4x105 yrs. 5x109 yrs.
Nuclei form
CMB released
Galaxies form
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50 year anniversary of CMB discovery
Still much to learn from CMB measurements
CMB T = 2.725 K
Michael Niemack, Cornell
1978 Nobel Prize
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CMB Measurement Timeline
• 1965 – First detected by Penzias and Wilson
• 1970s – Dipole measured
CMB T = 2.725 K
Dipole ΔT = 0.0034 K
Our velocity is 370 kilometers/second with respect to the CMB!
Michael Niemack, Cornell
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CMB Measurement Timeline
• 1965 – First detected by Penzias and Wilson
• 1970s – Dipole measured
CMB T = 2.725 K
Dipole ΔT = 0.0034 K
Homogeneous and isotropic?
Michael Niemack, Cornell
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CMB Measurement Timeline
• 1965 – First detected by Penzias and Wilson
• 1970s – Dipole measured
CMB T = 2.725 K
Dipole ΔT = 0.0034 K
Homogeneous and isotropic? ⇒ Inflationary paradigm
exponential expansion < 10-30 sec after big bang Michael Niemack, Cornell
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3 min. 4x105 yrs. 5x109 yrs. Inflationary expansion
~ 102 GeV
GUT ~ 1015 GeV
Inflation energy scale ~ grand unification
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CMB Measurement Timeline
• 1965 – First detected by Penzias and Wilson
• 1970s – Dipole
• 1992 – Anisotropies detected by COBE
CMB T = 2.725 K
Dipole ΔT = 0.0034 K
Anisotropies ΔT = 0.000018 K
Cosmic Background Explorer 2006 Nobel Prize
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Will the Universe expand forever? 1990s Gravity vs. Expansion
Infinite Expansion or
Big Crunch?
Flat
Closed
Open
Michael Niemack, Cornell
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Ωtotal = ρ/ρc = 1 Ωtotal > 1 Ωtotal < 1 Courtesy of NASA WMAP team
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Expansion of the Universe is Accelerating!
1998 - Science magazine “Breakthrough of the Year” 2011 Nobel Prize
A type Ia supernova lights up
Teams measuring Type 1a Supernova
show expansion is accelerating!
Michael Niemack, Cornell
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2003 - “Breakthrough of the Year” - Science
WMAP measurements
confirm bizarre cosmology
Wilkinson Microwave Anisotropy Probe (WMAP)
Precision measurement of CMB anisotropies
Michael Niemack, Cornell
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Courtesy of NASA WMAP team
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Information from CMB Temperature
2003 WMAP results δT(θ,ϕ) = almYlm(θ ,ϕ)
l ,m∑
Cl =1
2l +1alm
2
m∑
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Information from CMB Temperature Geometry of Universe Change in angular scale
Dark Energy Not much change
Atomic matter Peak height ratios
Dark matter Amplitude
Plots from Wayne Hu
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Information from CMB Temperature
At release of CMB Universe Today
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CMB Polarization • Linear polarization (like black iPad syndrome)
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CMB ‘E-mode’ Polarization • Mirror symmetric patterns
=> ‘E-mode’ polarization
• Generated by classical scattering of light with electrons
• First detected in 2002
cold spot
hot s
pot
Animation from Wayne Hu
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Temperature
Temperature & Polarization Signals 10° 1° 0.1° angular scale
[K2 ]
Temperature
E-mode B-mode
primordiallensing
10 100 1000
104
102
100
10-2
BICEPDASICAPMAP
QUADMAXIPOL
BOOMERANG
WMAP
ACBAR
SPT
ACT
QUIET
dashed horizontal lines- limits on B-modessolid vertical lines - measurements of T and E
measurements
CBI
CMB Polarization
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Signatures of Inflation
Scalar temperature
Scalar ‘E-modes’ • Inflationary models predict
primordial gravity waves
• Gravity waves generate B-mode polarization
• The amplitude of this signal tells us the energy scale of inflation
Detection of primordial gravity waves probes GUT energies,
~1012 times higher than the largest particle collider
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BICEP2 E-mode Map 2014
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BICEP2 B-mode Map 2014
They thought they’d detected B-mode polarization from inflationary gravity waves
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Galactic Dust from Planck Satellite
=> BICEP2 has not detected inflationary gravity waves yet
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With ACT we are exploring a new regime in CMB physics.
PLANCK SATELLITE
Figure from Toby Marriage
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ACT
ACT measures the CMB on arcminute angular scales with microKelvin sensitivity
Our Universe and Secondary Anisotropies
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How are we doing it?
• Location: 17,030 ft Atacama Desert, Chile
Michael Niemack, Cornell
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San Pedro / base camp
ACT (on Cerro Toco)
Atacama Large Millimeter Array
(ALMA)
San Pedro Transportation
Michael Niemack, Cornell
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Driving to ACT
Vicuña inteligente
Vicuñas no inteligente
Michael Niemack, Cornell
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Photo from Mark Devlin
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How are we doing it? • Careful optical design
~1 meter cryogenic camera Michael Niemack, Cornell
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How are we doing it? Superconducting polarization sensitive arrays of
detectors cooled to near absolute zero.
5mm 1.5m
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Superconducting detectors
Polarized light collectors
0.02
0.04
0.06
0 0.150 0.151 0.152
Temperature (K)
Res
ista
nce
(Ω)
Superconducting Transition
Michael Niemack, Cornell
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Deploying an array in Chile
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ACT Scanning
Movie of ACT before it was shipped to Chile
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First 3 months of Observing in 2013
• 4 patches on the sky • 1/3 of full ACTPol instrument
Michael Niemack, Cornell
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Temperature and Polarization Maps from ACT
We also see signals from ancient galaxy clusters and galaxies in our maps
Michael Niemack, Cornell
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Best measurements of CMB Power Spectra
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What next? • By end of this year we will have ~10x
better data than I showed today – Francesco is analyzing data to measure
galaxy cluster velocities and dark energy
• Better search for gravity waves from
inflation with Advanced ACTPol – Shawn is developing new detector arrays to
measure CMB & foregrounds
• Need order of magnitude more detectors for future CMB surveys – I am designing telescope optics for future
CMB surveys with 10x more detectors
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Thank you
and thank you to our collaborators.
Cornell Group Members: Francesco De Bernardis, Shawn Henderson, Brian Koopman, Patricio Gallardo, Jason Stevens, Eve Vavagiakis
Michael Niemack, Cornell