Kinetic Inductance DetectorsKinetic Inductance DetectorsSRON Stephen Yates, Jochem Baselmans, Andrey Baryshev, Jan Joost Lankwarden, Henk Hoevers.
TNOG. Gerini, A. Neto, D. Bekers.
TU DelftR. Barends, J.R. Gao, T.M. Klapwijk.
Cardiff University S. Doyle, P.D. Mauskopf, P. Ade
Radiation
Al film
1 2Sub-mm
2
SRON: The Netherlands Institute for Space ResearchSRON: The Netherlands Institute for Space Research
• Low Energy Astrophysics;Low Energy Astrophysics;• historically: IRAS, ISO-SWS...historically: IRAS, ISO-SWS...• PI for Herschel HIFI (PI)PI for Herschel HIFI (PI)• ALMA band 9ALMA band 9
• High Energy AstrophysicsHigh Energy Astrophysics• XMM-Newton XMM-Newton
• Sensor Research and TechnologySensor Research and Technology• TES microcalorimeters for IXO (XEUS)TES microcalorimeters for IXO (XEUS)• KIDs researchKIDs research• also HEBsalso HEBs
• Also Also • Earth Orientated ScienceEarth Orientated Science• Engineering Division - ASIC Engineering Division - ASIC
developmentdevelopment
3
SPICA-SAFARISPICA-SAFARI
SPICASPICA Japanese satelliteJapanese satellite
3.5 m 4 K mirror (first ever)3.5 m 4 K mirror (first ever)
-> very low photon background-> very low photon background
European instrument SAFARIEuropean instrument SAFARIFIR-sub-mm FTS imaging spectrometerFIR-sub-mm FTS imaging spectrometer
selected ESA cosmic vision program 2015+selected ESA cosmic vision program 2015+
3 bands3 bands
f/20 implies 31x31 mm arraysf/20 implies 31x31 mm arrays
NEP < 2NEP < 21010-19 -19 W/W/Hz, 3dB roll-off > 20 HzHz, 3dB roll-off > 20 Hz
Instantaneous dynamic range >1000 Instantaneous dynamic range >1000
Band 1
4
KID: Principle of operationKID: Principle of operation
• Superconducting pair breaking detectorSuperconducting pair breaking detector• Measure broken Cooper pairs by Measure broken Cooper pairs by
measuring the Kinetic Inductancemeasuring the Kinetic Inductance• At T<<Tc Superconductor impedance At T<<Tc Superconductor impedance
Zs ~ -iLK
P. Day, et al., Nature 425, 817 (2003).
Photons E > 2
1 2
• Read out ZRead out Zss by resonant circuit @ F=2-8 GHz by resonant circuit @ F=2-8 GHz
• Combine superconductor in series with CCombine superconductor in series with C• Read-out using phase or amplitude!Read-out using phase or amplitude!
EF
E
QuasiparticlesN ~ P /
Cooper Pairs
R
R
Im
Re
F0
f
S2
1 [d
B]
F [Ghz]
Superconductor
Superconductor
1 2
5
Antenna coupled Antenna coupled KIDKID ¼ ¼ resonator @F resonator @Freadoutreadout
Most sensitive @ endMost sensitive @ end
Printed antenna @ FPrinted antenna @ FRFRF
FFRF RF >> F>> Freadoutreadout
Antenna does not Antenna does not influence resonatorinfluence resonator
Needs lens!Needs lens!
21
CPW Through lineReadout signal ~4 GHz
CPW ¼ Resonator
CouplerLength sets Coupling Q
Antenna
Bare substrate
Central conductor
100 m
L= 5 mm @ 6 GHz
Al ground plane
RF Photons E > 2
Most sensitive area
Readoutcurrent
Pos
ition
Coupler
Antenna
1 2
6
Measured Beam PatternMeasured Beam Pattern
X Y
x
y
- +
+
-
x
y
- +
+
-
-20 -15 -10 -5 0 5 10 15 20-25
-20
-15
-10
-5
0
po
we
r re
spo
nse
[dB
]
angle [degr.]
KID 3 in focus H plane E plane E plane model PILRAP
7
SAFARI KID focal plane conceptSAFARI KID focal plane concept
Si microlens arraySi microlens array2nm roughness2nm roughness
7nm spherical precision 7nm spherical precision
250 nm position accuracy250 nm position accuracy
WithWith markers markers
Antenna coupled KID designAntenna coupled KID designPrinted lithographicallyPrinted lithographically
alignment using backside markersalignment using backside markers
present resonator design fits within F/20present resonator design fits within F/20
Alignment antenna-lenses within 1-2 Alignment antenna-lenses within 1-2 mmIdentical misalignment for all pixels (if any)Identical misalignment for all pixels (if any)
+
Radiation
Monolithic Si lens array Many resonators Many resonance features @ different F
0.48 mmBand 3
No show stoppers expected for F/20 for all SPICA arrays
8
Dark NEPDark NEP
• Lifetime ~ 1 msecLifetime ~ 1 msec• BW = 160 HzBW = 160 Hz
• NEP~6NEP~61010-19-19 W/ W/HzHz• 40 nmAl on Sapphire, sputtered40 nmAl on Sapphire, sputtered• 100 nm Al on SI, evaporated100 nm Al on SI, evaporated
101 102 10310-19
10-18
10-17
NE
P
W/
Hz]
F [Hz]
B12 40 nm Al on Si KID 44 Amp KID 44 Phase
B17 100nm Al on Si BAK KID 43 Amp KID 43 Phase
•Dynamic Range: using Dynamic Range: using θθ<90°<90°•P/NEP ~ 10.000P/NEP ~ 10.000Hz (KID 43) Hz (KID 43)
~ 3000 ~ 3000 Hz (KID 44)Hz (KID 44)
•Only optical coupling as uncertaintyOnly optical coupling as uncertainty•Calculations ~agree with optical NEPCalculations ~agree with optical NEP
• Measurements of noise, responsivity and lifetime => NEPMeasurements of noise, responsivity and lifetime => NEP
R
R
Im
Re
9
IRAM cameraIRAM camera
• Take advantage of work for SPICATake advantage of work for SPICA• Planar antenna experiencePlanar antenna experience• Work on electronicsWork on electronics
• Can support KID optionCan support KID option• Demonstrator 1kpixelDemonstrator 1kpixel• array manufacturerarray manufacturer• advise/collaboration readout, electronicsadvise/collaboration readout, electronics
• Need collaboratorsNeed collaborators• Neél/Rome/CardiffNeél/Rome/Cardiff
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Advantages KIDsAdvantages KIDs
• Cryogenically simple:Cryogenically simple:• 1 coax, cryogenic amplifier for ~10000pixels1 coax, cryogenic amplifier for ~10000pixels
• Antenna coupling - can have multi band/polarisation or very widebandAntenna coupling - can have multi band/polarisation or very wideband• Have (electrical) NEPs better than requiredHave (electrical) NEPs better than required• Simple manufacture - high yield (typical~95%) Simple manufacture - high yield (typical~95%) • Sensitivity:Sensitivity:
• vibration insensitivevibration insensitive• magnetic field needs to be constant (i.e. SC shield) but doesn't magnetic field needs to be constant (i.e. SC shield) but doesn't
change performancechange performance
11
Sample holder50 mK
DC blocks50 mK
Magnetic shield(bottom part)
NbTi Coax
DC block
LNA
4 K stage
500 mKlink
Stainless Steel
Coax, can use CuNi
from 4K
• Vericold GMBH• Pulse tube 3.5K• Dual stage ADR• Tmin<50 mK
ADR setupADR setup
Also 3K SC shield
12
SAFARI KID ReadoutSAFARI KID Readout
~ ~
10 MHz reference
DAC
DAC
100Msample/sec DAC’s
DAC
~ ~
2GHz 2.05GHz 2.1GHz
20 mK 4K ADC
ADC
ADC
• Satalite: 20 W , 5 kgSatalite: 20 W , 5 kg• Best first order estimate most optimistic design:Best first order estimate most optimistic design:• Power consumption: ~Power consumption: ~300 W300 W using 180 nm ASIC, using 180 nm ASIC, ~80 W~80 W using 90 nm ASIC using 90 nm ASIC
• 6000 pixels in 1 GHz BW => Highly questionable!!!6000 pixels in 1 GHz BW => Highly questionable!!!• 20 x 50 MHz subbands, 6% dead pixels due to confusion20 x 50 MHz subbands, 6% dead pixels due to confusion• DAC: 53 dB SNR, ENOB=8.6DAC: 53 dB SNR, ENOB=8.6• 40 analog mixers: 40 analog mixers: 4-8 kg4-8 kg
On chip analog microwave cirquits + optimised digital design neededOn chip analog microwave cirquits + optimised digital design needed
ASIC design group within SRONASIC design group within SRON
Digital experience from Eureca - XeusDigital experience from Eureca - Xeus• 4-8 GHz BW would be more realistic -> factor 4 in power4-8 GHz BW would be more realistic -> factor 4 in power
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SAFARI KID cryogenic designSAFARI KID cryogenic design242K – 4K242K – 4K
3 arrays, total 5940 pixels3 arrays, total 5940 pixels
All pixels in 1 pair of cablesAll pixels in 1 pair of cables
SPICA has 11 temperature stagesSPICA has 11 temperature stages
3m from 242K – 4.5K, ~5 dB cable loss 3m from 242K – 4.5K, ~5 dB cable loss
Sub 1.7K CoolerSub 1.7K Cooler
Sorption Cooler + ADR, single shotSorption Cooler + ADR, single shot
LNA’s: HIFI heritageLNA’s: HIFI heritage
100 mK50nW
4.5 K0.3mW0.5m0.9dB
1.7 K1Wtbd0
300 mK0.5Wtbd0
1.6 mm NbTi Coax
LNA12 dB 2 mW
18 K1mW0.5m0.9dB
41 K2mW0.5m0.9dB
60 K3mW0.5m0.9dB
85 K4mW0.5m0.9dB
100 K30mW0.5m0.9dB
242 K
LNA12 dB 2 mW
3.6 mm CuNi Ag cladded coax
2.5 K8Wtbd0
TPloadlengthloss
Sub 1.7 K single shot Cooler
LNA12 dB 2 mW
Warmelectronics
3 arrays in series