Optimization of future projects for the measurement of
Cosmic Microwave Background polarization
HOANG Duc-Thuong
The jury:
Francois Couchot
Gérard Rousset
Giampaolo Pisano
Sophie Henrot-Versillé
Damien Prêle
Guillaume Patanchon

Rapporteur
Examinateur
Rapporteur
Examinateur
Co-encadrant
Directeur de thèse

APC, December 17, 2018

Contents★Systematic effect studies:
Bandpass mismatch★QUBIC’s TES array
Response to particles

I.1. LiteBIRD mission

II.1. QUBIC experimentI.2. Bandpass mismatch

II.2. TES & readout system

2.1. Bandpass lter simulation
2.2. Data simulation
2.3. Results
I.3. A correction method

II.3. Radioactive source 241Am
II.4. Glitches analysis
II.5. Cross-talkfi2

The Universe

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Scale a(t)

y
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e

ion

Re

co

m

GW

BB

N

LSS
BAO

Inflation

QSO

Lensingdensityfluctuation

Cosmic Microwave Background
B-mode polarization

gravity waves

neutrinos?
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104<latexit sha1_base64="av51hh/gsnCmHIHb8DlFpgVr0E4=">AAAB7XicbVBNSwMxEJ2tX7V+VT16CRbBU8mKUI9FLx4r2A9o15JNs21sNlmSrFCW/gcvHhTx6v/x5r8xbfegrQ8GHu/NMDMvTAQ3FuNvr7C2vrG5Vdwu7ezu7R+UD49aRqWasiZVQulOSAwTXLKm5VawTqIZiUPB2uH4Zua3n5g2XMl7O0lYEJOh5BGnxDqp5eOH7HLaL1dwFc+BVomfkwrkaPTLX72BomnMpKWCGNP1cWKDjGjLqWDTUi81LCF0TIas66gkMTNBNr92is6cMkCR0q6kRXP190RGYmMmceg6Y2JHZtmbif953dRGV0HGZZJaJuliUZQKZBWavY4GXDNqxcQRQjV3tyI6IppQ6wIquRD85ZdXSeui6uOqf4cr9es8jiKcwCmcgw81qMMtNKAJFB7hGV7hzVPei/fufSxaC14+cwx/4H3+ANPzjp0=</latexit>
sha1_base64="cKazcFVTSi4s0y/0h330jYrJ1bo=">AAAB7XicbZDLSgMxFIbPeK3jrerSTbAIrkpGBN2IRTcuK9gLtGPJpGkbm0mGJCOUoeAjuHGhiFsfxb0738b0stDWHwIf/38OOedEieDGYvztLSwuLa+s5tb89Y3Nre38zm7VqFRTVqFKKF2PiGGCS1ax3ApWTzQjcSRYLepfjfLaA9OGK3lrBwkLY9KVvMMpsc6qBvguOxm28gVcxGOheQimULj49M8fAaDcyn8124qmMZOWCmJMI8CJDTOiLaeCDf1malhCaJ90WcOhJDEzYTaedogOndNGHaXdkxaN3d8dGYmNGcSRq4yJ7ZnZbGT+lzVS2zkLMy6T1DJJJx91UoGsQqPVUZtrRq0YOCBUczcroj2iCbXuQL47QjC78jxUj4sBLgY3uFC6hIlysA8HcAQBnEIJrqEMFaBwD0/wAq+e8p69N+99UrrgTXv24I+8jx9DOpBq</latexit>
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Ly αTime [years]

380 000
1100
1 eV

13.7 billion
25

6

2

0

Redshift
Energy1 meVThe history and the evolution of the Universe in time and scale factor.
3

Standard cosmological model‣ Observational cosmology gives constraint on the ΛCDM cosmological model
parameters ΩΛ, Ωb, Ωc, τ, ns, As, H…

4

Cosmic Microwave Background (CMB)‣ Formation: CMB is radiation from around 380 000 years
after the Universe was born at recombination epoch−

e +p⇌H+γ-> CMB photons were freely travel to the entire theUniverse: decoupling epoch‣Discover: in 1964 by Penzias & Wilson.
‣CMB spectrum is a black-body (COBE) TCMB = 2.725 K .
−5‣Temperature anisotropies 10

K .: Sachs-Wolfe e ect, Doppler e ect.

‣~ 10% CMB anisotropies are polarized by free electrons at last scattering surface.
Horn antenna

2001+91989+3

2009+3∼ 400 γ/cm3
ff

ff

5

CMB polarization: Stoke parameters
A monochromatic light in z-direction:

Ex = E0x cos (ω0t − θx); Ey = E0y cos (ω0t − θy)22I ≡ ⟨E0x⟩ + ⟨E0y⟩2
2Q ≡ ⟨E0x⟩ − ⟨E0y⟩

Intensity
Linear polarizationU ≡ ⟨2E0xE0y cos(θy − θx)⟩ Linear polarizationV ≡ ⟨2E0xE0y sin(θy − θx)⟩ Circular polarization

In the second-order spin spherical harmonics of degree ℓ and orderm:(Q ± iU) (θ, φ) = ∑ a±2ℓmY±2ℓm (θ, φ)multipoles coe cientffi‣ Q, U depend on the coordinate system

6

CMB polarization (Thomson scattering)in ation

E ModeB ModeGravity waves from in ation stretch and squeeze space in orthogonal directions.
Gravity waves from in ation would produce tensor perturbations.
Primordial B-mode is due to only tensor perturbation in in ation!

The polarization pattern can be decomposed into 2 components:• Curl-free component, called “E-mode” (electric- eld)or “gradient-mode”• Grad-free component, called “B-mode” (magnetic- eld)or “curl-mode”
fl

fi

fi

fl

fl

fl

7

State of the art
After Planck 2018

• Temperature anisotropies aremeasured with high accuracy• E-mode polarization is well twith concordance model(DASI 2002.)• B-mode is not yet measured!
• Foreground components
challenges

r < 0.12• Systematic e ects challenges

Goal: Tensor-to-scalar ratio r

fi

ff

180∘
ℓ=
θ

8

State of the art

BB

9I.1. LiteBIRD science goal

Measurements with r < 0.002 (95% C.L.) for 2 ≤ l ≤ 200 are important10I.1. LiteBIRD Payload module
Phase A1
4.5 m

• Japan: Rocket, Satellite, LFT

LFT (5K)
HFT (5K)• Europe: HFT, sub-Kelvin Cooler• USA: TES focal plane

PLM

V-groove
30K
100K
200K
SVM/BUS• Canada: Warm readout electronics
JAXA
H3

radiators

HG-antenna

LFT
COJ43

COJ32

st

COJ21

ro
rot
ch
n

• Low frequency telescope (40 cm, 20-70 arcmin)

du

syn

• 3-year at L2 orbit

COJ10

HFT

• High frequency telescope (30 cm, 10-40 arcmin )• Rotating half-wave plate (HWP) modulation• TES focal plane at 100 mK

CMB• The mass and consumption power 2.6 tons, 3.0 kW

11I.1. LiteBIRD Focal planeHigh Frequency Telescope (HFT)

The TES array with corrugated feed horndeveloped for ABS, ACTpol, SPTpol by
UC Boulder, NIST and Stanford

Low Frequency Telescope (LFT)
The TES array with alenslet developed for
POLARBEAR by UC
Berkeley and UCSD

Sinuous antenna

TES• LFT 34 GHz ~ 161 GHz: Synchrotron + CMB• HFT 89 GHz ~ 448 GHz: CMB + Dust

15 frequency bands> 2000 TES detectors

Bandpass ltersfi

12I.1. LiteBIRD scanning strategy
Precession'angle'α"τspin'

Spin'angle'β "Sun

An#$Sun'direc#on'τprec'

α : Precession angle [deg]β : Spin angle [deg]τprec or ωprec : Precession spin [time]τspin or ωspin : Rotating spin [rpm]‣ Many angles to measure polarization

13

I.1. Foreground components

Ssky = I + Q cos 2ψ + U sin 2ψ + n
ψ : Polarizer angle

I = ICMB + Idust + Iother components
Similar for Q and U.
I, Q, U are Stokes parameters.

14

I.2. Potential systematic e ects
Planck HFI lessons:

EE• Beam mismatch• Cosmic rays
• 1/f noise• ADC non-linearity• Bandpass mismatch• Thermal uctuations

Planck: A&A 596, A107 (2016)
ff

fl

15

Bandpass shape of several PlanckHFI detectors

The micro-fabricated technology could
contribute to non-ideality of bandpass
lters (layer to layer misalignment,dielectric constant, dielectric thickness).

Blue: ground, red: ight
(Planck: A&A 596, A107 (2016))

Leakage from intensity I to polarization Q, U
16
fl

fi

I.2. Bandpass mismatch

I.2. Simulation
latitudeFilterFilter Simulation
Simulationdγ

longitude

CMB
CMB mapmap

Dust
Dust map
map

Data
Data Simulation
Simulation

d=I CMB +γ d I dust

Precession'angle'α"Scanning
Scanning
strategy
strategyτspin'

Spin'angle'β "An#$Sun'direc#on'τprec'

T

−1

−1

T

−1

( A N A) A N d
Mask
Mask 20%
20%
AngularAngular PowerPower Spectrum
Spectrum

C

BB
l

,C

EE
l

17

I.2.1. Bandpass mismatch calibration factor
Filters

CMB: Black body
T0 = TCM B = 2.725
Td = 19K= 1.62⌫0 = 140 GHz

Dust: Grey body

Normalization CMB

32h⌫
Planck’s law B(⌫, T ) = c2

γs, γf, γspin

1h⌫e kB T

118

I.2.1. Bandpass lter
Planck-like errors(1 % vary on edges)

Standard derivation: 0.00626

γd

Typical measurement errors(1GHz top-hat)

Standard derivation: 0.005975

Half of a percent from detector to detector
Calibration detectors by

γd

fi

19

I.2.2. Time order data (TOD) simulation• In order to observe leakage: The e ect of intensity I to polarization Q, U
• Data simulation: Ssky = ICMB + γdIdust + γsIsynchrotron + …
• No polarization• No noise or white noise• Same pixelization between input and output map• Simulation at 140 GHz used di erent scanning strategy con gurations• The focal plane and polarizer orientations for LiteBIRD

I
The map of intensity I and polarization Q, and U is m = Q ,Uthe map-making solution:ff

The pointing matrix for pixel p: A =
ff

−1

−1

(1

T

−1

A N Sskycos (2ψ)sin (2ψ))pfi

m = [A N A]
T

20

Galactic coordinate

I.2.3. Results (1) -> Leakage maps

Ecliptic coordinate

222 detectors and 365 days observation, 140 GHz

α = 65∘, β = 30∘, τprec = 96.1803 minutes, ωspin = 0.1 rpm‣ In ecliptic coordinate: Symmetric patterns around the pole.

21

I.2.3. Results (2) -> Analytic estimationa pair detector

leakage maps

crossing moment‣ Tight correlation between the relative leakage and the crossing moment.
22

I.2.3. Results (3) -> 1 / N detectors
20% masked galactic plane, 74 and 222 detectors and 365 days observation, 10 sims

1
Ndet

74 detectors

222 detectors∘∘

α = 65 , β = 30 , τprec = 96.1803 minutes, ωspin = 0.1 rpm

23I.2.3. Results (4) -> scanning strategies
20% masked galactic plane, 222 detectors and 365 days observation, 10 sims

Precession
angle

CORE

LiteBIRD‣ Scanning strategies with larger precession angle produce less leakage
because of homogeneous scan angle per pixel.

24

I.2.3. Results (5) -> An ideal Half Wave Plate 88 rpm
20% masked galactic plane, 50 detectors and 180 days observation

Numerical simulations

α = 65∘, β = 30∘, τprec = 93 minutes, ωspin = 0.1 rpm‣ An rotating HWP mitigates bandpass leakage by homogenizing theangular coverage each pixel.

25

I.2.3. Results (6) -> precession and spin∘

‣ precession 93 minutes, spin 0.1 rpm∘ ‣ precession 96.1803 minutes, spin 0.1 rpm‣ precession 96.1803 minutes, spin 0.3 rpm

α = 65 , β = 30

‣ The location of the peaks depends on the ratio τprec /τspin26

I.2.3. Results (7) -> A example ratio of

ωprec /ωspin

20% masked galactic plane, 222 detectors and 365 days observationff‣E ects on intermediate angular power spectrum

27

I.2.3. Results (8) -> Vary scanning strategy params
20% masked galactic, 222 detectors and 365 days observation

Amplitudes are rescaled

α = 65∘, β = 30∘, ωspin = 10 minutes

α = 65∘, β = 30∘‣ The location of the peaks changes‣ The location of the peaks depends on the ratio τprec /τspin28

I.3. A correction method: A pair detector

γa1

γb1

γb2 γ
a2

γbn γan

2nd pair

111th pair....

1st pair• Detector pair subtraction

Sa = γaI + Q cos 2ψa + U sin 2ψa

Sb = γbI − Q cos 2ψa − U sin 2ψa

Sa − Sb (γa − γb) I=+ Q cos 2ψa + U sin 2ψa2
2
29

I.3. A correction method: A pair detector• In case of leakage: The covariant matrix:
−1

T

−1

−1

Cov3;p = (A N A)

σn
=
×
Np

1

⟨cos 2ψ⟩⟨sin 2ψ⟩⟨cos 2ψ⟩

1 + ⟨cos 4ψ⟩2⟨sin 4ψ⟩2⟨sin 2ψ⟩⟨sin 4ψ⟩2

1 − ⟨cos 4ψ⟩2.

• In case of no leakage: The sub-matrix covarianceCov2;p = σn ×

1 + ⟨cos 4ψ⟩2⟨sin 4ψ⟩2⟨sin 4ψ⟩2

1 − ⟨cos 4ψ⟩
2

−1

.

‣ We study the loss of accuracy in two cases numerically.
30

occurrence

I.3. A correction method: A pair detector

α = 65∘, β = 30∘, τprec = 96.1803 minutes, ωspin = 0.1 rpm‣ The loss accuracy of the Q component is of the order of 10% for a given detector pair31

Conclusions
222 detectors and 365 days observation,

τ = 0.055 +/- 0.009

1. Bandpass mismatch is the non-negligible systematic effect.
2. An optimal scanning strategy for future CMB polarization satellite.
−310
3. Tensor-to-scalar r is of the order ofin reionization bump.

4. Tight correlation between leakage maps and cross linking moment.
5. 1/N detectors dependence of the level of the power spectra=> increase number of detectors.
6. An ideal half wave plate mitigates the bandpass mismatch effect.
7. Bandpass mismatch error for satellite CMB experiments II: Correction
effect, Ranajoy et al., [in preparation].

32

II. Interaction of particles with a 256
Transition Edge Sensor (TES) array of the
QUBIC experiment.
HOANG Duc-Thuong
APC, December 17, 201833

The Q & U Bolometric Interferometer for
Cosmology

22 labs
APC Paris, France> 130 persons
C2N Orsay, France
CSNSM Orsay, France
IRAP Toulouse, France
Maynooth University, Ireland
Università di Milano-Bicocca, Italy
Università degli studi, Milano, Italy
Università La Sapienza, Roma, Italy
University of Manchester, UK
Richmond University, USA
France, Italy, Argentina, the U.K. and the U.S.A.
Brown University, USA
University of Wisconsin, USA
NIKHEF, The Netherlands
GEMA, Argentina
Centro Atómico Cóntituyentes, Argentina(Argentina)
Comisión Nacional de Energía Atómico, Argentina
Facultad de CS Astronómicas y Geofísicas, Argentina
Centro Atómico Bariloche and Instituto Balseiro, Argentina
Instituto de Tecnologías en detección y Astropartículas, Argentina
Instituto Argentino de Radio Astronomía, Argentine34II.1. QUBIC science goal & Instrument
Self-calibration: Open/close horn couple

B-Mode30

200
arXiv:1209.4905

σ(r) goal: no foreground: 0.006, with foreground 0.01
35

QUBIC in a Nutshell

36

QUBIC in a Nutshell
STOKES POLARIMETERTO SEPARATE I, Q, U

37

QUBIC in a Nutshell

400 BACK TO BACK HORNSSWITCHES TO OPEN/CLOSEA HORNS COUPLE: BASELINE.

38

QUBIC in a Nutshell
MIRRORS MADE A FIZEAU INTERFEROMETER.
OPENING AND CLOSING THE SWITCHES. WE
CAN CHANGE THE INTERFEROMETRICFRINGES ON THE FOCAL PLANE.

39

QUBIC in a Nutshell

T H E D I C H R O I C S E PA R AT E S T H E
RADIATION ON TWO DIFFERENT FOCALPLANES AT 150 GHz and 220 GHz.
~2000 Transition-Edge Sensors (TES)40

II.1. QUBIC’s Cryostat

1K box

October 25 2018

‣QUBIC cryostat at APC 1.6 m x 1.8 m‣10 days need to cool down to mK‣Transition Edge Sensor (TES) focal plane
Lab cryostat: Triton 200/400

41II.2. Transition Edge Sensor (TES)

ΔT

ΔR

Superconducting
transition
regime‣A strong negative ElectroThermal Feedback (ETF) speeds the detector by the loop gainCparameter τthermal =, ℒ = 10 − 100
G(ℒ + 1)V2bias‣In a voltage-bias mode: TES is self-calibrating in its transition temperature. Pj =.
RTES=>TES array

1‣Linear response, the current responsivity is −
.
Vbias
42

II.2. TES & READOUT CHAIN‣An array of 256-TES‣4x32 SQUIDs read out signal‣128:1 Time Domain Multiplexing‣2-ASIC‣FPGA (PID controller)‣QUBIC studio interface‣Electronic readout chain time constant:Rfb
τelec =
HSQGgainMfbKI

bias

G

ext

Rf b
fb

[ 0]

[ 0]
+

Vout

⌘

-

ext
fb

Hsq

[V]

G

tot
[ 0]

Mf b

[A]

KP ID

[V]

Vout

1
Rf b

43

II.2. IV curves measurement‣ Superconducting regime Transition regime

Normal regime‣IV curves help us to determine TES behavior and calibrate.
‣Determine position of radioactive source.
44

II.3. Radioactive source 241Am
Study TES behavior‣241 Am:- 5.4 MeV alpha particles

Radioactive Americium- 80 keV gamma rays
- 8 particles per second‣5 mm from detector‣In front of the pixel 88
241Am
241Am

45

II.4. Glitches data analysis~ 10 minutes
Maximums
TOD
TOD
Glitches
Glitches Detection
Detection
Maximum
Maximum
Correction
Correction

μ ,σGlitches
Glitches
Baseline
Baseline

Median lter method

Glitches
Processing
Stacking
Stacking
MethodMethodMedianMedian
MethodMethodFit
Fit Glitches
Glitches2
χ , σnInterpretation
Interpretation
Time
Time constants
constants

Crosstalk
Crosstalk

Noise
Glitchesfi46II.4. Glitches detection & processing

Glitches detection:• A Glitch: 750 bins sample (200+550)

Glitches Processing:• Median baseline

Glitches Maximum• Maximum correction47

II.4. Template tting

S(t) = a (exp)−(t − t0)/τ0
1 − exp

Amplitude

Rising time−(t − t0)/τ1+c

Decay time

τ0 : Rising time

τ1 : Decay timeffc : O setfi

48

II.4. Fitted glitches, chi2 estimation49

II.4. Time constants distributions‣ Two populations of the rising time constantrising time constant τ0

decay time constant τ1

50

II.4. Time constants distributions
2 populations of the rising time constant:τ0 ∼ 10 ms ≡ τelec(1)
τ1 ∼ 40 ms ≡ τthermalτ0 ∼ 40 ms ≡ τthermal(2)τ1 ∼ 40 ms ≡ τthermal51II.4. Interpretation
μm

Substrate Pixel‣ NbSi 293μm holes‣ Si substrate 500 μm‣ Absorber: 50x50‣ ~3 mm a pixel

1. The st population: Particles hit directly to the sensor (thermometer TES or the absorber), thermal
e ect propagates very quickly to the thermometer and the rising time constant τ0 is the electronic
readout time constant. The thermal equilibrium process is rapidly established due to the depositedenergy on the absorber which has a thickness of 1 μm .
2. The second population: Particles could hit the Si substrate, the deposited energy is huge due to thethickness of 500 μm . Because the thermal coupling is not perfect between the Si wafer and the backcopper (thermal bath). The edge of the array is well pressed over the back copper. However the centerof the array is not uniformly pressed over this copper then the heat ows could transfer slower than theedge. Consequently, these heat ows arise the increment of the background reference temperature inwhich is nally detected by the sensor through a rising time. Problem: We do not see coincident eventsin neighbor pixel => cross-talk.
3. A proposed solution: We can add a gold layer on the back side of the Si substrate in order to x anduniform the Si bulk temperature which thus could played better the role of thermal bath.

fi

fl

fl

fi

fi

ff

4. Space application: In the aspect of Cosmic Rays and a satellite's focal plane using TES arrays, theSilicon substrate surface plays an important role to reduce the impact of CRs.
52

II.5. Thermal Cross-talkdead pixels‣Fix a reference pixel 88 d0‣When glitches occur i(g)i(g)‣Estimate the thermal elevation
among pixels Nj , C1, C2, C‣Estimate baseline noise b

Neighbor pixels

Cross-talk estimator:

Ng

Nj

1 1
C(b, pixel area) =∑Ng Nj ∑
g=1 j=1

Baseline estimation positionjjjdi(g) − 0.5di(g)−b − 0.5di(g)+bd0i(g)
reference pixel.
53

II.5. Thermal Cross-talk‣The thermal cross-talk is constrained to less than 0.1 %. The low statistic, complex
noise do not allow to put a better constraint.

II.5. Cross-talk of the electronic readout system

1

33

65

97

2

34

69

101

11

43

75

107

24

56

88

120

32

64

96

128

MUX
4:1

‣Time Domain Multiplexing

ASIC 128:1

32 SQUIDs

4 SQUIDs

55

II.5. Cross-talk of the electronic readout system‣We used a fast sampling rate of 0.64 ms (1562.6 Hz)‣The frequency acquisition (sample rate) of time domain multiplexing can introduce
the cross-talk between two successive pixel.
‣This study needs a deeper work, => a new topic
56

Summary

1. I measured two time constants: The electronic readout chain time
constant (7-30 ms) and the thermal time constant (20-60 ms).
2. The possible interpretation of 2 populations of the the rising time
constant: Absorber events and Si substrate events.
3. The thermal cross-talk is estimated.
4. I found the cross-talk of the electronic readout system due tofrequency acquisition. This study needs a deeper work, => a new
topic

57

Thank you!

58

BACK UP SLIDES

59

I. Backup(1) Scanning strategy params ωprec /ωspin

93 minutes, 10 minutes [9,3,3]

96.61803398 minutes, 10 minutes [9,1,1,1,……..]

Mathematically number theory:ωprec /ωspin = θ = [a0, a1, a2, . . . ] = a0 +1
a1+
a2 + …

rational number
irrational numberfi

The most irrational number:Golden ratio : Φ =

(1 +

2

5)

1

(M.B)

(Limited)(in nite)= 1.61803398875[1,1,1,1,……..]60

I. Backup (2) -> Planck leakage
20% masked galactic, 222 detectors and 365 days observation‣Planck scanning strategy is not optimize for polarization measurement61II.4. Time constants and the PID controller, V_bias

1. (left) When we increase K_I parameter, the time constant corresponding to thereadout bandwidth must decrease.
2. (right) If we increase the voltage bias, the electrical time constant will decrease dueto the inverse proportion of the current responsively and the voltage bias.
3. (right) If we increase the voltage bias, the thermal time constant increase because
TES enters to the normal state, the logarithmic sensitivity to temperatureparameter is small.
62

Time constant & scattering operating point of TESs

63

LiteBIRD basic parameter64

7.4. Stacking glitches & Median glitches methods
MeanMedianDi erent values: Scattering operating point TESs => e ect of ETF. SQUID non-uniform
ff

ff

65

Cross talk evidence in the second population of time constant

66

QUBIC general information

Scanning strategy: We perform azimuth scan of 40 degrees xing the HWP angle. After we change HWP
angle and the elevation (ranging from 45 to 65 degrees) then scan again in azimuth.
fi

67

The practical TES bias circuit
Ibias

Ibias

RL

Rpara

I
Min

Min

Rshunt

VT H
RT ES

RT ES
I

68

The logarithmic sensitivity to temperature

ℒ∝α

69

IV curves
measurements

Blue: ASIC1
Green: ASIC2

70

The scan strategy and possible sky patches

Scanning strategy in local coordinate:
We perform azimuth scan of 40 degrees xing the HWP angle. Afterwe change HWP angle and the elevation (ranging from 45 to 65
degrees) then scan again in azimuth.

fi

71

TES technologies

NIST (OMT tech, feed-horn) ACT, SPT,
LiteBIRD (High frequency) …

BERKELEY (planar sinuous antenna coupled
TES tech) ACT, POLARBEAR, LiteBIRD (lowmid frequency)…
72

APC (no antenna tech) QUBIC

Caltech (planar antenna
coupled TES tech), BICEPTBCS theory
1 Vibrations of lattice are minimal (virtual phonons) below Tc

-

-

+

-

+

+

+

+

+

2

Electron traveling in front distorts the lattice3

Virtual phonons moved closer

-

+
+

+

-+ + -

+
+

-

+

+

+

+

--

+
+

4

A positive region created behind the 1st electron

5

The 2nd electron is attracted to the positive region andthe lattice rebounds back into its original shape