self inductance , mutual inductance and coeffecient of coupling
A. Monfardini, IAP 26/06/2012 1 Kinetic Inductance Detectors for CoRE-like applications Potentially...
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Transcript of A. Monfardini, IAP 26/06/2012 1 Kinetic Inductance Detectors for CoRE-like applications Potentially...
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/201211
KKinetic inetic IInductance nductance DDetectors etectors for for
CoRE-like applicationsCoRE-like applicationsPotentially involving (from the technical point-of-view):Potentially involving (from the technical point-of-view):
- Grenoble (Néel, LPSC, IRAM, IPAG, CEA-LETI)Grenoble (Néel, LPSC, IRAM, IPAG, CEA-LETI)- Cardiff (others in UK ?)Cardiff (others in UK ?)- The Netherlands (SRON, Delft)The Netherlands (SRON, Delft)- Paris (APC, CSNSM, IAS, SaP)Paris (APC, CSNSM, IAS, SaP)- RomaRoma- SpainSpain .. others ?.. others ?
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/201222
KIDs working principleKIDs working principle
f
IN-OUT transmission (amplitude)
Dark, T << Tc
Light: increase in Lincrease in Lkk
Change in phase ()
Light: increase in Rincrease in RChange in amplitude (A)
fi
IN-OUT transmission (phase)
From the theory :
f f LLKK P P
f = frequency shift f = frequency shift P = incoming powerP = incoming power
The incoming photons break Cooper pairs (supercurrent carriers)The incoming photons break Cooper pairs (supercurrent carriers)in a superconducting LC resonator in a superconducting LC resonator measurable signals measurable signals
A
f
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/201233
Intrinsic linearity demonstratedIntrinsic linearity demonstrated
( h( h·· << k << k··T )T )
Measured using the NIKA
Sky Simulatorff00 2 GHz 2 GHz
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/201244
KIDs: multiplexing principleKIDs: multiplexing principle
IN from DAC and UPCONVERTERIN from DAC and UPCONVERTER OUT to DOWNCONVERTER and ADCOUT to DOWNCONVERTER and ADC
ff00 ff11 …… ffN-2N-2 ffN-1N-1
Inductance LInductance LKK + L + LGG
Capacitor CCapacitor C
Feedline 50Feedline 50 CLLf
GK
res
1
One of the C lines is modulated by lithography to adjust every resonance (e.g. fres 1.5 0.2 GHz) natural f-domain multiplexingnatural f-domain multiplexing since f/since f/f f 10 1055 high MUX factor is possible high MUX factor is possible
High-Q superconducting (R High-Q superconducting (R 0) LC resonator : 0) LC resonator :Lumped Element KID design :Lumped Element KID design :
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/201255
State-of-the-artState-of-the-art
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/201266
Snapshot taken todaySnapshot taken today
ACHIEVED (mm and sub-mm applications):ACHIEVED (mm and sub-mm applications):
- Background limited (best pixels) for ground-based applications (150-350 GHz)Background limited (best pixels) for ground-based applications (150-350 GHz)- Electrical NEPs in the low 10Electrical NEPs in the low 10-19-19 W/Hz W/Hz0.5 0.5
- Optical NEPs under small loading (0.1pW) in the low 10Optical NEPs under small loading (0.1pW) in the low 10-18-18 W/Hz W/Hz0.50.5 (in Al and TiN) (in Al and TiN)- Full system (hundreds pixels) up and running on a big telescope (NIKA) Full system (hundreds pixels) up and running on a big telescope (NIKA) - Fundamental solutions found for photometric calibration (modulated read-out)Fundamental solutions found for photometric calibration (modulated read-out)- larger interest in the Community larger interest in the Community getting exponential getting exponential
ONGOING:ONGOING:
- kilo-pixels arrays uniformity to be investigated (e.g. NIKA, MUSIC, AMKID ...)kilo-pixels arrays uniformity to be investigated (e.g. NIKA, MUSIC, AMKID ...)- space-adapted configurations (main problem: cosmic-rays interaction)space-adapted configurations (main problem: cosmic-rays interaction)- ............
HUGE evolution from the last « BPol » meeting HUGE evolution from the last « BPol » meeting
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/201277
NIKA run 3 – October 2011NIKA run 3 – October 2011
One week « mostly nights »mostly nights » run at the 30-m IRAM telescope
150 GHz & 240 GHz – 132+132 pixels LEKIDs150 GHz & 240 GHz – 132+132 pixels LEKIDs
NEFD NEFD 20 mJy 20 mJyss0.50.5
Design: GrenobleFabrication: GrenobleElectronics: Grenoble-US
NEFD 100 mJys0.5
Design: GrenobleFabrication: GrenobleElectronics: Grenoble-US NIKA 2011 :NIKA 2011 :
- cryogen-free cryostatcryogen-free cryostat- magnetic screening- improved photometry (< 10%)improved photometry (< 10%)- dual polarisation
Sensitivity at 2 mm is Sensitivity at 2 mm is now comparable tonow comparable tostate-of-the-art TESstate-of-the-art TES(e.g. NASA Goddard).(e.g. NASA Goddard).NEP NEP 10 10-16-16 W/Hz W/Hz0.50.5
DR21(OH) star-forming regionDR21(OH) star-forming region
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/201288
NIKA run 4 NIKA run 4 First permanent KID camera - 06/2012First permanent KID camera - 06/2012
Available for Science until 2015.. waiting for the big (6.5’) CameraSensitivity improved at 1.25mm, more pixels (132+224)
A couple of dedicated observational runs (open to IRAM Community) per year.A couple of dedicated observational runs (open to IRAM Community) per year.
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/201299
Kilo-pixels arrays: NIKA v0Kilo-pixels arrays: NIKA v0- 1,020 pixels (150 GHz)1,020 pixels (150 GHz)- 2,000 pixels (240 GHz)2,000 pixels (240 GHz)
80 mm
80 mm
3/4 feedlines OK (750 pixels). Resonances OK, Optical response OK. For detailed 3/4 feedlines OK (750 pixels). Resonances OK, Optical response OK. For detailed testing (e.g. noise, cross-talk) need 4 final NIKA electronics boards (NIKEL v1)testing (e.g. noise, cross-talk) need 4 final NIKA electronics boards (NIKEL v1)
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20121010
TiN LEKID optical sensitivityTiN LEKID optical sensitivity
Films:Films: TiN JPL (H.G. Leduc)
Way too sensitive.Way too sensitive. Must mount a diaphragm at the cold (0.1K) pupil to reduce the optical loading by a factor 60-70 with respect to the NIKA standards ( 10 pW per pixel).Power per pixel: << 1pW (band 125-170GHz).
Example (7/2/2012 optical measurements): Example (7/2/2012 optical measurements): P = 0.04pW per pixel (80K vs. 0K on focal plane) is detected, on 64 typical pixels, with a S/N per unit band of 2000 8000 Hz0.5 (median 4000) Means, for this loadings, an opticaloptical NEP of 5NEP of 5··1010-18-18 to 2·10 to 2·10-17 -17 W/HzW/Hz0.50.5, constant in the range 0.1 10 Hz !
Caution 1: to be confirmed by further measurements !Caution 1: to be confirmed by further measurements !
Caution 2: changing the T working point we have noticed large variations in theCaution 2: changing the T working point we have noticed large variations in theoptical response. Must measure again at slightly higher T. Measurements optical response. Must measure again at slightly higher T. Measurements reported here performed at 85 mK (working point not optimized, but since we reported here performed at 85 mK (working point not optimized, but since we don’t understand everything .... better being prudent).don’t understand everything .... better being prudent).
Design « NITA 1.2»:classical LEKID meander – not particularly optimised.
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20121111
Noise decorrelatedNoise decorrelated
Credit: Juan Macias-Perez (LPSC Grenoble)Credit: Juan Macias-Perez (LPSC Grenoble)
< 10-17 W/Hz0.5
Raw frequency noiseRaw frequency noise
Decorrelated noiseDecorrelated noise
At 80mK (At 80mK ( T TccDCDC/11) still very sensitive to base T (e.g. 1kHz / mK !)/11) still very sensitive to base T (e.g. 1kHz / mK !)
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20121212
SRON 1SRON 1
Credit: A. Barishev, J. Baselmans, A. Endo, L. Ferrari, S. YatesCredit: A. Barishev, J. Baselmans, A. Endo, L. Ferrari, S. Yates
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20121313
SRON 2SRON 2
Credit: A. Barishev, J. Baselmans, A. Endo, L. Ferrari, S. YatesCredit: A. Barishev, J. Baselmans, A. Endo, L. Ferrari, S. Yates
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20121414
Electronics Electronics (example)(example)
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20121515
Power consumption :Power consumption : negligeable at < 4 K 10 W/ch. at 4 K 100 mW/ch. at 300 K
NIKEL v1: the future NIKA read-outNIKEL v1: the future NIKA read-out
NIKEL board v1 (2012).NIKEL board v1 (2012). 500 MHz, 400 channels (ADC 12 bits, DAC 16 bits)
For details see:For details see: O. Bourrion et al., Journ. of Instrum. 6, Issue 06, 6012 (2011) O. Bourrion et al., in press, arXiv:1204.1415 (2012)
No constrains of power for NIKA. Not optimised at all.
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20121616
A quite fundamental A quite fundamental problem:problem:
the electrical cross-talkthe electrical cross-talk
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20121717
Resonators electrical cross-talkResonators electrical cross-talk
FULL ARRAY (36 PIXELS) SIMULATION FULL ARRAY (36 PIXELS) SIMULATION
Mainly applies to Mainly applies to Lumped Element KIDsLumped Element KIDs
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20121818
Cross-talk hintsCross-talk hints
Best candidate : Best candidate : inductive and/or capacitivecoupling between resonators
Testing :Testing :- Feedline impedance- New meanders- GND plane influence- Trenches ..
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20121919
KIDs KIDs environmentalenvironmental
needsneeds
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20122020
Materials and EnvironmentMaterials and Environment
Substrates:Substrates:- Sapphire.Sapphire. At the very beginning it seemed a must to suppress phae noise. At the very beginning it seemed a must to suppress phae noise. Now demonstrated it’s not necessary.Now demonstrated it’s not necessary.- Silicon.Silicon. OK if not oxidated and clean dielectric/metal interface. OK if not oxidated and clean dielectric/metal interface.
Superconducting films:Superconducting films:- AluminiumAluminium (thin, <40nm). Low-frequency cut-off around 100GHz. (thin, <40nm). Low-frequency cut-off around 100GHz.- TiN.TiN. Still tricky and not fully understood. But potential lower f and NEP. Still tricky and not fully understood. But potential lower f and NEP.- ..... to be studied ... lots of options..... to be studied ... lots of options
Magnetic environment:Magnetic environment: sensitive (resonances shifting). Much less than SQUIDs, sensitive (resonances shifting). Much less than SQUIDs, but more than MIS. Need classical screening (e.g. high-but more than MIS. Need classical screening (e.g. high- + superconductor). + superconductor).
Temperature environment:Temperature environment: much less sensitive than a bolometer. much less sensitive than a bolometer. Optimal base T (e.g. for 150GHz, Al films): 150 mK or lowerOptimal base T (e.g. for 150GHz, Al films): 150 mK or lowerOptimal base T (e.g. for 90GHz, TiN films): 100 mK or lower.Optimal base T (e.g. for 90GHz, TiN films): 100 mK or lower.
Vibrations environment:Vibrations environment: much less sensitive than a bolometer. much less sensitive than a bolometer.
Cosmic hits:Cosmic hits: fundamentally less sensitive than bolometers (see later). How fundamentally less sensitive than bolometers (see later). How better it is in practice still to be demonstrated (e.g. making resonators on the better it is in practice still to be demonstrated (e.g. making resonators on the same suspended structures used for PACS.. CEA-LETI getting involved).same suspended structures used for PACS.. CEA-LETI getting involved).
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20122121
Cosmics HitsCosmics Hits
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20122222
Cosmics HFI
Credit: Andrea Catalano – LPSC Grenoble Credit: Andrea Catalano – LPSC Grenoble
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20122323
LEKIDs under cosmic and x-ray irradiationLEKIDs under cosmic and x-ray irradiation
L. Swenson et al.L. Swenson et al., , Applied Physics Letters, 96, Applied Physics Letters, 96, Issue 26, id. 263511 (2010) Issue 26, id. 263511 (2010)
First ever « cosmic hit movie » (NIKA test array)
Single 6 keV x-ray photon observed on 11 pixelsDedicated 16 pixels LEKIDs array
A. Cruciani et al.A. Cruciani et al., , LTD-14 LTD-14
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20122424
Over-gap phonons propagationOver-gap phonons propagation
D.C.Moore et al., D.C.Moore et al., AAPLPL 100, 100, Issue 23, Issue 23, id. 232601 id. 232601 (2012) (2012)
Propagation speed: 6-9 mm/Propagation speed: 6-9 mm/ss in < 1 < 1 ss the « wave » reaches closest pixels in 10 10 ss a big (e.g. 10cm) array is filled for t > 10 t > 10 ss , phonons decay to thermal andleaks to the housing. At the same time, a part a part (1-10%) of the energy(1-10%) of the energy goes into quasi-particlesand produces a signal.
After t0+10 s equilibrium between
phonons decay/leak (green) phonons decay/leak (green) phph and
quasi-particles lifetime (blue) quasi-particles lifetime (blue) qpqp..
Depending on technology details Depending on technology details one effet might dominate and one effet might dominate and determine the pulse lenght. determine the pulse lenght. Time (Time (s)s)
phph >> >> qpqp
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20122525
Summary: KIDs and CosmicsSummary: KIDs and Cosmics
BASE ASSUMPTIONBASE ASSUMPTION
IN ANY CASE SUSPENDED STRUCTURES ARE NEEDEDIN ANY CASE SUSPENDED STRUCTURES ARE NEEDED
A SMALL LIST OF POINTS (in favour) TO REMEMBER:A SMALL LIST OF POINTS (in favour) TO REMEMBER:
1)1) suspended structure is for cosmics ONLY. Not needed for sensitivity.suspended structure is for cosmics ONLY. Not needed for sensitivity.
2)2) KIDs are relatively fast. Response typically around 0.1ms; maximum notKIDs are relatively fast. Response typically around 0.1ms; maximum notexceeding 1ms for very low background applications and pure metals.exceeding 1ms for very low background applications and pure metals.
3)3) KIDs are not sensitive (very little in fact) to thermal phonons. Only KIDs are not sensitive (very little in fact) to thermal phonons. Only high-energy (T > Thigh-energy (T > Tcc) phonons can produce a signal.) phonons can produce a signal.
4) poor efficiency of energy transfer from phonons to quasi-particles. 4) poor efficiency of energy transfer from phonons to quasi-particles. For a solid wafer only 1-10% of the deposited energy goes into measurable For a solid wafer only 1-10% of the deposited energy goes into measurable signal.signal.
A. Monfardini, IAP 26/06/2012A. Monfardini, IAP 26/06/20122626
THANKSTHANKS