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 ?


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


Intrinsic linearity demonstratedIntrinsic linearity demonstrated

( h( h·· << k << k··T )T )

Measured using the NIKA

Sky Simulatorff00 2 GHz 2 GHz


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 :


State-of-the-artState-of-the-art


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


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


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.


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)


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.


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 !)


SRON 1SRON 1

Credit: A. Barishev, J. Baselmans, A. Endo, L. Ferrari, S. YatesCredit: A. Barishev, J. Baselmans, A. Endo, L. Ferrari, S. Yates


SRON 2SRON 2

Credit: A. Barishev, J. Baselmans, A. Endo, L. Ferrari, S. YatesCredit: A. Barishev, J. Baselmans, A. Endo, L. Ferrari, S. Yates


Electronics Electronics (example)(example)


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 quite fundamental A quite fundamental problem:problem:

the electrical cross-talkthe electrical cross-talk


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


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 ..


KIDs KIDs environmentalenvironmental

needsneeds


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).


Cosmics HitsCosmics Hits


Cosmics HFI

Credit: Andrea Catalano – LPSC Grenoble Credit: Andrea Catalano – LPSC Grenoble


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


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


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.


THANKSTHANKS

a. monfardini, iap 26/06/2012 1 kinetic inductance detectors for core-like applications potentially...

Documents

s equilibrium

thermal phonons

highenergy t t c phonons

time s ph qp slide

deposited energy

overgap phonons propagation

measurable signal

ms maximum