Detectors
&
Readout
History: early days
• The infrared range has been discovered by astronomers!
– Friedrich Wilhelm Herschel, using a prism and
balckened bulb thermometers, detects the infrared section of the solar spectrum (calorific rays, 1800)
• The final demonstration that IR is also EM waves happens a bit later
– Macedonio Melloni in 1829 develops the
thermomultiplier, a sensitive IR detector. With this
system he demonstrates that calorific rays have the same nature as light, also demonstrating that they have polarization properties exactly like light rays.
He names the calorific rays “ultrared radiation”.
• The first astronomical observation is carried out soon after:
– IR radiation from the moon is detected by Charles
Piazzi Smyth in Tenerife, using a thermocouple. He
also shows that IR radiation is better detected at
higher altitudes.
History: early days
• The first bolometers were developed for astronomy, and allowed the first IR
spectroscopy of an astronomical source
– Samuel Pierpoint Langley in 1878 develops the bolometer: a thin blackened platinum strip,
sensitive enough to measure the heat of a cow
from a distance of ¼ mile.– The detector works because the resistance of the Pt strip changes when heated by the absorbed radiation.
– The detector is differential: 4 strips are placed in a Wheatstone bridge but only one is blackened and exposed to incoming radiation. Common- mode effects are rejected by the bridge and tiny variations of bolometer resistance can be
measured.
• With his bolometer Langley is able to
measure the IR spectrum of the sun,
discovering atomic and molecular lines.
Old times
• Further developments:
– 1915 : William Coblentz uses thermopiles (an
improved version of Macedonio Melloni’s detector !) to measure the infrared radiation from 110 stars, as well as from planets, such as Jupiter and Saturn, and several nebulae .
– 1920’s : systematic IR observations with vacuum thermopiles (Seth B. Nicholson, Edison Pettit and others): diameters of giant stars
– 1948: IR observations show that the moon is covered by dust.
– 1950s: Lead Sulphide photodetectors – Johnson’s star photometry
– First Semiconductor bolometers, slicing carbon
resistors to make the thermistor (W. S. Boyle and K. F.
Rodgers, J . Opt . Soc . Am . 49 :66 (1959))
One generation ago
• The revolution :
– 1961: Franck J. Low develops the first cryogenic Ge bolometer, boosting the sensitivity by orders of magnitude.
– 1960’s and ff. bolometers and semiconductors detectors with their telescopes are carried to space using stratospheric balloons and
rockets.
• Consequence:
– First sky surveys @ λ 100 μm – 1968 First IR ground based
large area sky survey (2 μm,
from Mt. Wilson)
Few decades ago
• mm-wave bolometers
– cooled at 1.5K or 0.3K – operating from space
• become sensitive enough to measure the finest details of the Cosmic Microwave Background.
• Breakthrough:
– The composite bolometer (absorber and thermistor separated and each optimized independently):
N. Coron, P. Richards …
Circa 1970
Circa 1980
Composite Bolometer
(Coron, Richards …)
monolitic bolometer (Goddard, ..)
Cryogenic Bolometers
• For FIR & mm-waves spectroscopy we need very wide band
detectors. Bolometers provide the optimal choice: they are senitive from mm-waves to the visible range.
filter
(frequency selective) Feed
Horn
(angle selective) Integrating
cavity Radiation
Absorber (ΔT)
Thermometer
(Ge thermistor (ΔR) at low T, or TES)
Incoming Photons
(ΔB)
• Fundamental noise sources are Johnson noise in the thermistor (<ΔV
2> = 4kTRΔf), temperature fluctuations in the thermistor ((<ΔW
2> = 4kGT
2Δf), background radiation noise (T
bkg5) need to reduce the temperature of the detector and the radiative
background.
Load resistor
ΔV
Arno Penzias and Robert Wilson (1965):
We get microwaves isotropically from every direction of the sky. It’s the Cosmic Microwave Background.
Nobel Prize in Physics, 1977
F. Melchiorri (high mountain, 1974), ….
P. Richards et al.
(balloon, 1980) … and then John Mather et al.
(1992) with the FIRAS on the COBE satellite:
these microwaves have exactly a
blackbody spectrum Nobel Prize in Physics, 2006
COBE-FIRAS
• COBE-FIRAS was a Martin-Puplett
Fourier-Transform Spectrometer with
composite bolometers. It was placed in a 400 km orbit.
• A zero instrument comparing the
specific sky brightness to the brightness of a cryogenic Blackbody
• The output was nulled (within detector noise) for T
ref=2.725 K
• The brightness of empty sky is a
blackbody at the same temperature !
• The early universe was in thermal
equilibrium at high Temperature.
σ (cm
-1) wavenumber
Primeval Fireball Additional
evidence for an early
hot phase
Srinand et al.
Nature 408 931 (2000)
COBE Molecules in
cosmic clouds (rotational levels)
) 1
( z T
T = o +
K
T
o= 2 . 725
Two decades ago
• The spider-web absorber is developed
–It minimizes the heat capacity of the absorber
–It minimizes the cross-section to
cosmic rays, while maintaining high
cross-section for mm-waves
Spider-Web Bolometers
Absorber
Thermistor
Built by JPL Signal wire
2 mm
•The absorber is micro machined as a web of metallized Si
3N
4wires, 2 μm thick, with 0.1 mm pitch.
•This is a good absorber for mm-wave photons and
features a very low cross section for cosmic rays.
Also, the heat capacity is reduced by a large factor with respect to the solid absorber.
•NEP ~ 2 10
-17W/Hz
0.5is achieved @0.3K
•150μK
CMBin 1 s
•Mauskopf et al. Appl.Opt.
36, 765-771, (1997)
1900 1920 1940 1960 1980 2000 2020 2040 2060
10
210
710
1210
17Langley's bolometer
Golay Cell
Golay Cell
Boyle and Rodgers bolometer F.J.Low's cryogenic bolometer
Composite bolometer
Composite bolometer at 0.3K
Spider web bolometer at 0.3K Spider web bolometer at 0.1K 1year
1day 1 hour
1 second
Development of thermal detectors for far IR and mm-waves
ti m e r equi red to m a k e a m eas ur em ent ( s ec onds )
year
Photon noise limit for the CMB
Crill et al., 2003 – BOOMERanG 1998 bolometers, 300 mK
The same kind of bolometer is used now in Planck @100mK
Measured performance of Planck HFI bolometers (0.1K) (Holmes et al., Appl. Optics, 47, 5997, 2008)
= Photon noise limit
Multi-moded
• In steady conditions the
temperature rise of the sensor is due to the background radiative power absorbed Q and to the electrical bias power P:
• The effect of the background power is thus equivalent to an increase of the reference temperature:
Cryogenic Bolometers
P Q
T T
G ( − )
0= +
G T Q
T
T T
G G T Q
T G P
+
=
−
⎥⎦ =
⎢⎣ ⎤
⎡ − +
=
0 0
0 0
'
) ' (
) (
T
0’
Q(pW)
0.27K 0.28K
0.26K
0 1 2
• In presence of an additional signal ΔQ e
jωt(from the sky)
• There is a tradeoff between high sensitivity and fast response. The heat capacity C should be
minimized to optimize both.
• Using a current biased thermistor to readout the temperature change:
Cryogenic Bolometers
Q T
dt G T
C d Δ +
effΔ = Δ
G C dQ G
dT
eff
=
= + τ
ω τ
2 21
1
2
1
2/ ) /
( )
(
ω τ α α
α α
= +
=
= ℜ
=
=
⇒
=
G
effT R i
dQ dT T
i R dQ
dV
T RdT
i idR
dT dV T dR T
R T
Small sensor at low
temperature
Responsivity
• A large α is important for high
responsivity.
• Ge thermistors:
2
1
2/
) ( )
(
ω τ α
α
= + ℜ
=
G
effT R i
dT T dR T
R T
10 − 1
−
≈ K
T
α
Cryogenic Bolometers
• Johnson noise in the thermistor
• Temperature noise
• Photon noise
• Total NEP (fundamental):
Cryogenic Bolometers
df kTR V
d
J4
2
Δ =
( )
22 2 2
2 4
fC G
G kT
df W d
eff T eff
π
= + Δ
( )
( ) e e dx
x h
c T k df
W d
x x Ph BG
∫ − − +
Δ =
2 4
3 2
5 2 5
1 1
4 ε ε
df W d
df W d
df V
NEP d
J T Ph2 2
2 2
2
1 Δ
Δ + Δ +
= ℜ
Again, need of low
temperature and low background
Q
1900 1920 1940 1960 1980 2000 2020 2040 2060
10
210
710
1210
17Langley's bolometer
Golay Cell
Golay Cell
Boyle and Rodgers bolometer F.J.Low's cryogenic bolometer
Composite bolometer
Composite bolometer at 0.3K
Spider web bolometer at 0.3K Spider web bolometer at 0.1K 1year
1day 1 hour
1 second
Development of thermal detectors for far IR and mm-waves
ti m e r equi red to m a k e a m eas ur em ent ( s ec onds )
year
Photon noise limit for the CMB
Spider-Web Bolometers
Absorber
Thermistor
Built by JPL Signal wire
2 mm
•The absorber is micro machined as a web of metallized Si
3N
4wires, 2 μm thick, with 0.1 mm pitch.
•This is a good absorber for mm-wave photons and
features a very low cross section for cosmic rays.
Also, the heat capacity is reduced by a large factor with respect to the solid absorber.
•NEP ~ 2 10
-17W/Hz
0.5is achieved @0.3K
•150μK
CMBin 1 s
•Mauskopf et al. Appl.Opt.
36, 765-771, (1997)
Crill et al., 2003 – BOOMERanG 1998 bolometers, 300 mK
Cryogenic Bolometers
• Ge thermistor bolometers have been used in many CMB
experiments:
– COBE-FIRAS, ARGO, MAX,
BOOMERanG, MAXIMA, ARCHEOPS
• Ge thermistor bolometers are extremely sensitive, but slow:
the typical time constant C/G is of the order of 10 ms @ 300mK
• Once bolometers reach BLIP
conditions (CMB BLIP), the
mapping speed can only be
increased by creating large
bolometer arrays.
Bolometer Arrays
• BOLOCAM and MAMBO are examples of large arrays
with hybrid components (Si wafer + Ge sensors)
• Techniques to build fully litographed arrays for the CMB are being developed.
• TES offer the natural
sensors. (A. Lee, D. Benford, A. Golding ..hear Richards..)
Bolocam Wafer (CSO)
MAMBO (MPIfR for IRAM)
SWIPE
• The Short Wavelength
Instrument for the Polarization Explorer• Uses overmoded bolometers, trading angular resolution for sensitivity
• Sensitivity of photon-noise limited bolometers vs # of modes:
3.2 3.3
2.5 NET Focal Plane
(μK/sqrt(Hz))=
30 25
NET (μK/sqrt(Hz) ) = 15
1.6 1.9
2.4 FWHM (deg) =
83 58
37 N det =
1.4 2.1
λ (mm) 3.3
220 145
90 f (GHz)
40 25
15 N modes (geom) =
m 0.8 F =
Instrument
m 0.4 D lens =
Bolometric
0.25 eff =
LSPE - SWIPE
Number of modes actually coupling to the bolometer absorber
SWIPE
• Overmoded detectors are obtained coupling large area bolomete absorbers to Winston horns.
• Example of large-throughput spider-web bolometer (being developed in Italy, F. Gatti)
• SWIPE bolometers will be made also in Cambridge (Withington)
SWIPE
• Overmoded detectors are obtained coupling large area bolometer absorbers to Winston horns.
Simulations confirm that about half of the modes collected by the
Winston horn actually couple to the bolometer absorber
(in single-polarization detectors).
Simulations by L.Lamagna, G.Pisano
EBEX
EBEX Focal Plane
• Total of 1476 detectors
• Maintained at 0.27 K
• 3 frequency bands/focal plane
738 element array 141 element hexagon Single TES
Lee, UCB
3 mm
5 cm
• G=15-30 pWatt/K
• NEP = 1.4e-17 (150 GHz)
• NEQ = 156 μK*rt(sec) (150 GHz)
• τ = 3 msec,
150
150 150
150 250
250 420
Slide: Hanany
William Jones
Princeton University
for the
Spider Collaboration
The Path to CMBpol June 31, 2009
Suborbital Polarimeter for Inflation Dust and the Epoch of Reionization
Suborbital Polarimeter for Inflation Dust and the Epoch of Reionization
Spider: A Balloon Borne CMB Polarimeter
• Long duration (~30 day cryogenic hold time) balloon borne polarimeter
• Surveys 60% of the sky each day of the flight, with ~0.5 degree resolution
• Broad frequency coverage to aid in foreground separation
• Will extract nearly all the information from the CMB E-modes
• Will probe B-modes on scales where lensing does not dominate
• Technical Pathfinder: solutions appropriate for a space mission
Carbon Fiber Gondola
Attitude Control
• flywheel
• magnetometer
• rate gyros
• sun sensor
Flight Computers/ACS
• 1 TB for turnaround
• 5 TB for LDB
Pointing Reconstruction
• 2 pointed cameras
• boresight camera
• rate gyros
Six single freq. telescopes 30 day, 1850 lb, 4K /
1.4 K cryostat
• Constant current bias
• Very high impedance voltage follower as close as possible to the detector (inside dewar)
• Very low noise OP amp amplifier (1 nV/sqrt(Hz)
Ge Bolometer Readout
high impedance (10 MΩ) detector
To A/D converter and data storage
B
+
i
bX 1000
Inside dewar Outside dewar
JFET Preamplifier for differential AC bias
• AC bias current is better
because the
amplifier is used at a frequency far from 1/f noise.
• Sine wave or triangle wave bias
• Demodulator needed.
• Differential
biasing is better because
differential amplification removes
common
interference.
• Low noise, high CNRR amplifier needed.
AC
B-1 + 1
10MΩ 5 pF
5 pF +Vb
-Vb
180Hz
+
-
VAC
JFETs, x100
Lock-in
VoutREF IN
Planck is a very ambitious
experiment.
It carries a complex CMB experiment (the state of the art, a few years ago) all the way to L2, improving the sensitivity wrt WMAP by at least a factor 10, extending the frequency
coverage towards high frequencies by a factor about 10
PLANCK
ESA’s mission to map the Cosmic Microwave Background Image of the whole sky at wavelengths near the intensity peak of the CMB radiation, with
• high instrument sensitivity (ΔT/T∼10
-6)
• high resolution (≈5 arcmin)
• wide frequency coverage (25 GHz-950 GHz)
• high control of systematics
•Sensitivity to polarization
Launch: 14/May/2009; payload module: 2 instruments + telescope
• Low Frequency Instrument (LFI, uses HEMTs)
• High Frequency Instrument (HFI, uses bolometers)
• Telescope: primary (1.50x1.89 m ellipsoid)
ESA : Jan Tauber
HFI PI : Jean Loup Puget (Paris)
HFI IS : Jean Michel Lamarre (Paris) LFI PI : Reno Mandolesi (Bologna) LFI IS : Marco Bersanelli (Milano)
Almost 20 years of hard
work of a very large team,
coordinated by:
HFI LFI
Scientific Laboratories
Satellite
+ subcontractors National Agencies
PI Puget PI Mandolesi
Ecliptic plane
1 o/day
Boresight
(85o from spin axis)
Field of view rotates at 1 rpm
E M
L2
Observing strategy
The payload will work from L2, to
avoid the emission of the Earth, of the
Moon, of the Sun
Why so far ?
• Good reasons to go in deep space:
– Atmosphere
– Sidelobes
– Stability
• In the case of CMB
observations, the detected brightness is the sum of the brightness from the sky
(dominant for the solid angles directed towards the sky, in the main lobe) and the
Brightness from ground
(dominant for the solid angles directed towards ground, in the sidelobes).
RA( θ )
main lobe
θ
side lobes
FWHM=
λ
/Dboresight
⎥ ⎥
⎥
⎦
⎤
⎢ ⎢
⎢
⎣
⎡
Ω +
Ω
= A ∫ B RA d ∫ B RA d
W
lobes side
Ground lobe
main
sky
( θ , ϕ ) ( θ , ϕ ) ( θ , ϕ ) ( θ , ϕ )
• The angular response (beam pattern) RA( θ , φ )
is usually polarization-dependent
<<3x10-6 7x10-8 srad
1’
<<3x10-4 7x10-6 srad
10’
<<0.01 2x10-4 srad
1o
<<1 2x10-2 srad
10o
<RA
sidelobes>
Ω
mainlobe FWHMGoing to L2 reduces the solid angle occupied by the Earth by a factor 2π/2x10
-4=31000, thus
relaxing by the same factor the required off-axis rejection.
1.5Mkm
900km L2
COBE WMAP,
Planck
No day-night changes up there … extreme stability
Planck – HFI polarization sensitive focal plane
Ponthieu et al. 2010
Scan direction
z
NEP b = 15 aW/Hz 1/2 -> 70 μK/Hz 1/2
Total NET (bolo+photon) = 85 μK/Hz 1/2
LFI
LFI
Pseudo-correlation
Differential radiometer Measures I,Q,U
30, 44, 70 GHz
t
Primary
secondary
Focal Plane
Off-axis Dragone
Telescope, wide field, good polarization
properties, 1.89mx1.50m
aperture
Thermal performance :
Planck collaboration: astro-ph/1101:2023
LFI Focal Plane Unit
Thermal performance :
Planck collaboration: astro-ph/1101:2023
Mission :
Planck collaboration: astro-ph/1101:2022
Mission : Planck collaboration: astro-ph/1101:2022
Real data (from just 15 days of operation)
Planck 2013 CMB anisotropy map and power spectrum data (red dots with error bars) Green line is the best fit to a 6-parameters cosmology model (inflationary Λ-CDM)
• A large α is important for high
responsivity.
• Ge thermistors:
• Superconducting transition edge thermistors:
Cryogenic Bolometers
2
1
2) ( )
( 1
ω τ α α
= + ℜ
=
G
effR i
dT T dR T
R
10
−1−
≈ K
T
α
1000
−1≈ K
T α
S.F. Lee et al. Appl.Opt. 37 3391 (1998)
• Have very low R, so work better at constant voltage. Lets’
write in detail the equations:
Voltage-Biased Superconducting Bolometers
[ ]
P Ci
T G P T e
Te Ci
T G P P
Te Ci
Te G
T e T dT
dR R
T R
P V
Te Ci
Te G
dT Te dR R
dR V d
Pe
dt Te C d Te
R G Pe V
dt T dQ
Te T
R G V R
Pe V P
T T
R G P V
i i
i i
b i
t i t
i t
i b
t i
t i t
b i t
i
o t
b i t b
i
o b
ω δ δ α
δ α ω
δ
ωδ δ δ
δ
ωδ δ
δ δ
δ δ
δ δ
δ δ
δ
ϕ ϕ
ϕ ϕ
ϕ
ϕ ω ϕ
ω ϕ
ω ω
ϕ ω ϕ
ω ω
ϕ ω ω
+ +
=
⎥⎦ ⇒
⎢⎣ ⎤
⎡ + +
=
+
⎥⎦ =
⎢⎣ ⎤
− ⎡
+
⎥⎦ =
⎢⎣ ⎤ + ⎡
+
⎥ =
⎦
⎢ ⎤
⎣ + ⎡
⇒
+
− +
⎥ =
⎦
⎢ ⎤
⎣ + ⎡ +
+
−
= +
−
+ +
+
+ +
+
2
) (
) (
) (
2
) (
) 2 (
) (
2 2
2
1
) (
)
(
• The effective thermal conductivity is
• The first part is the Electro-Thermal Feedback (ETF) part.
• When δP increases (a signal arrives) T increases; this increases the resistance which in turns decreases the bias power Pb=Vb2/R. As a result the total power (P + Pb) does not decrease as much, and the temperature does not change much.
• For a given incoming power, the ETF reduced the temperature change.
• It is the reverse of what happens in a semiconductor bolometer, where the negative α produces a negative ETF, increasing the temperature change.
• But here we measure the bias current at constant voltage. The current needed to keep the bias more stable is increased by the ETF. So we define
Voltage-Biased Superconducting Bolometers
P Ci
T G P T e
Te Ci
T G P P
i
i
δ
α ω δ
δ α ω
δ
ϕ ϕ+ +
=
⎥⎦ ⇒
⎢⎣ ⎤
⎡ + +
=
−C i
T G
G
eff= P α + + ω
( )
i
oL G
i C G T
P C
i G
T P
L ω ωτ
α ω
α
ω = +
+ + =
= 1 1
• The Responsivity is
• And using
• We get
• Defining
• We get
Voltage-Biased Superconducting Bolometers
( )
P T T
P V P
R R
R V V P
R
R V
P R V
P
i
bb b
b b
b b
δ δ α δ
δ δ
δ δ
δ δ
δ / 1
21 1
2
= − = −
−
=
=
= ℜ
) 1
(
oi i
i
i L G
e Ci
T G P
e P
P T Ci
T G P T e
ω ωτ δ α
δ δ α ω
δ
ϕ ϕ ϕ+
= + +
+
=
⇒ +
+
=
− − −) 1
( 1 )
1 ( 1
1
o i
b o
i b
b b
b
L i
Le V
i L G
e T
P V P
T T
P
V ωτ ωτ
α δ
δ
α
ϕ ϕ+
− + + =
− +
=
−
=
ℜ
− −+ 1
= L τ
oτ
ωτ
ϕ
i L
L e V
b i
+
− +
=
ℜ 1
1 )
1 ( 1
For large ETF (L>>1):
• the time constant is
reduced wrt the standard one by L+1
• For slow signals (ω<<1/τ) and large ETF the
responsivity is simply
-1/V
bSuch a high value for α (which is >0 for TES) induces a large change in the bias power when
radiation hits the detector (electrothermal feedback) This results in a large
reduction of the time constant and in
stabilization of the
responsivity.
• Are the future of this field. See recent reviews from Paul Richards, Adrian Lee, Jamie Bock, Harvey Moseley … et al.
• In Proc. of the Far-IR, sub-mm and mm detector technology workshop, Monterey 2002.
TES arrays
Cryo:
0.3K Space qual.
receiver (1pixel of 1000)
antenna
stripline filter
membrane island
load
TES
Si substrate with Si3N4 film
SQUID Readout
MUX
TES for mm waves
(Cardiff, Phil Mauskopf)
… and many others …
150 μm
PROTOTYPE SINGLE PIXEL - 150 GHz (Mauskopf) Schematic:
Waveguide
Radial probe
Nb Microstrip
Silicon nitride Absorber/
termination
TES Thermal links
Similar to JPL design, Hunt, et al., 2002 but with
waveguide coupled antenna
PROTOTYPE SINGLE PIXEL - 150 GHz (Mauskopf) Details:
Radial probe
Absorber - Ti/Au: 0.5 Ω/square - t = 20 nm Need total R = 5-10 Ω
w = 5 μm → d = 50 μm
Microstrip line: h = 0.3 μm, ε = 4.5 → Z ~ 5 Ω
TES Thermal links
TES Readout
A very low impedance, extremely low current noise amplifier is needed
SQUID (Superconducting quantum interference device) Offers the perfect solution.
Martedi’.
Very resistant: materials are all suitable for satellite and space missions.
Extremely simple cold electronics: one single LNA can be used for 103-104 pixels. The rest of the readout is warm.
Very flexible: different materials and geometries can be chosen to tune detectors to specific needs.
order of 103-104 pixels read with a single coax
Ease of fabrication: one single layer of material is needed.
Kinetic Inductance Detectors
A possible solution:
Main characteristics:
The CPs have zero DC resistance, but the reactance is non-zero and has two distinct contribution kinetic and magnetic L.
KIDs working principle:
In a superconductor below Tc, electrons can bind to form CPs with binding energy E=2Δ =3.5*kbTc .
The total conductivity of the material can be estimated using the two-fluid model
CPs QPs
The values of ss and sn depend on the densities of QPs and CPs. By measuring them, we can get
information on nqp .
J
sJ
n-is2nCP -is2nQP
s1nQP
A better estimate of ss and sn is obtained using the Mattis Bardeen integrals:
A better theory...
Note that:
• Rs decreases exponentially
• Xs becomes constant
• Xs/ Rs grows exponentially
D. C. Mattis and J. Bardeen, in Phys Rev 111 (1958)
How can we measure the small variations of L
k?The superconductor can be inserted in a resonating circuit with extremely high Q, since:
s
s
R
X Q ∝
The resonator is extremely simple to do, and consists of a shorted length of superconducting line capacitevely coupled to the feedline l/4 resonator
Cc
RQP Lkin
Lmag
Cl
KIDs are intrinsically multiplexable:
• Unitary transmission off resonance
• Q values very large (~106)
Multiplexing
Each resonator acts at the same time as detector and filter
Cnc
RnQP Lnkin
Lnmag
Cnl C1c
R1QP L1kin
L1mag
C1l
C2c
R2QP L2kin
L2mag
C2l RF carrier (f1+ f2+ ... + fn )
Pixel 1, f1 Pixel 2, f2 Pixel n, fn
One single amplifier needed!
Many potential applications
M. Calvo et al. in Conf. Proc. of 1st International LDB Workshop (2008) E.Andreotti et al. in NIMR A 572 (2008)
How do we actually measure the incoming radiation?
n′CP< nCP QPs
CPs
• Suppose a photon hits the detector
• If its energy is high enough (hν > 2ΔE) it can break CPs
• The density of CPs therefore changes
• This leads to a variation of Lkin
The same effect can be accomplished by increasing the temperature of the superconductor
The readout is accomplished by
monitoring the phase of the transmitted signal
L
f
0∝ 1
dq
Readout technique
Usually the phase is redefined and referred to the center of the resonant circle:
This kind of plots can give all the information regarding resonator parameters
It is also the basis for actual measurements of radiation Remember that:
δ T δϑ
n
QPδ
) δϑ
T
(
n
QPCryogenic system overview
SCN-CN coax
VNA / IQ mixers
2xDC block 2xDC block
2x10dB atten
1xDC block 1xDC block
1x10dB atten
KID
300K 30K 2K 300mK
SCN-CN coax SS-SS coax
warm amplifier cold amplifier
KIDs readout system
0.3K 2K
Re(S21)
Im(S21)
DAQ
fsynt fsynt
PC DAC
ADC
fsynt
fsynt± f0 , fsynt± f1...
f0, f1...
f0, f1...
fsynt± f0 , fsynt± f1...
Single pixel readout system Multipixel readout system
Both systems share the core components!
0.3K 2K
Re(S21)
Im(S21)
PC DAC
ADC
fsynt
fsynt f0, f1...
f0, f1...
fsynt± f0 , fsynt± f1...
10 mm
8 mm
capacitive coupling
2.5 mm
0.7 mm
Al CPW (200nm) SiO2 (1μm)
Silicon Substrate (0.5mm)
KID chip description
Material: Aluminium
6 resonators of varying length Substrate:
The dielectric constant is not exactly determined!
Base temperature characterization
All 6 resonances observed!
Typical resonance amplitude curve
10
51
≈ . 1 ⋅
QEffect of temperature variation - 1
Higher T Higher nqp Higher losses
Higher T Lower nqp Lower f0
Amplitude
Phase
Effect of temperature variation - 2
) T ( f L
TOT
1
0 ∝
TOT kin
L
= L
α L ( )
) T ( L )
( f
) T ( f
kin kin
0 2
1
0 0
0 = − αδ
δ
Quality factor increase
Estimate of kinetic inductance fraction
α
≈ 0.0182D data analysis
A fitting procedure has been developed to estimate the parameters of the resonators and the effect of the IQ mixers
The results are in very good agreement with the data:
Temperature variation - 3
The blue points correspond to the base temperature resonant frequency
We obtain sensitivities of 10-3-10-2 deg/nqp equivalent to 10-9-10-8 deg/Nqp
Optical measurements
System modified by adding a filter chain
Polyethilenewindow Fluorogold(400GHz lowpass) Fluorogold+145GHz bandpassfilter
Horn KID Gunn diode
Quasiparticle lifetime
To estimate the absorbed power that induces the signal we still need one piece of information:
QP qp abs
P n
ητ
= Δ
τ
QP ≈ 30μsWhen T decreases, the quasiparticle lifetime increases (nQP smaller!)
A possible solution: LEKID
Distributed element KIDs
Lumped element KIDs
Needs some sort of antenna
Response depends on where the photon hits the sensor
C L
It is possible to tune the meanders to match free space impedance!
ADS simulation
Electrical NEP measurement
Dominant contribution given by the warm readout components!
Still too high for real applications, but:
High sample rate data acquired
(
2 2)
2
2 1 QP
QP QP
S N
NEP +ω τ
⎥⎥
⎦
⎤
⎢⎢
⎣
⎡
δ δϑ Δ
= ητ
− ϑ
Theoretical limit given by GR noise is as low as 10-20W/Hz0.5 at 100mK
P. K. Day et al. Lett. Nature 425 (2003)
Conclusions
The KIDs concept has been studied and theoretical models have been developed to analyze their reponse
The experimental testbench has been completed and characterized
The first chip has been made and thouroughly tested
The first results are very promising
Yet still some open issues
• High Q factors even at 300mK multiplexing!
• Good agreement with theoretical predictions
• First light already seen
• Develop a system to reach lower T (dilution fridge?)
• Optimize optical coupling LEKID