cryogenic particle detectors - stanford … particle detectors based on superconducting transition...
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CRYOGENIC PARTICLE DETECTORS
Based on Superconducting Transition Edge Sensors
Blas Cabrera
February 19 and 26,1999
LECTURES #19 AND #20
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Cryogenic Particle Detectors Based on
Superconducting Transition Edge Sensors
Blas Cabrera Physics Department, Stanford University
February 19,1999 and February 26, 1999
References:
1.
2.
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4.
5.
6.
7.
8.
“Low Temperature Particle Detectors”, N. Booth, B. Cabrera, and E. Fiorini, Annu. Rev. Nucl Part. Sci. 46, 471-532 (1996).
“A Quasiparticle-Trap-Assisted Transition-Edge Sensor for Phonon-Mediated Particle Detection”, K. D. Irwin, S . W. Nam, B. Cabrera, B. Chugg, and B. Young, Rev. Sci. Znstrum. 66, 5322-6 (1995).
“Bolemetric Sensors for Elementary Particle Detectors”, B. Cabrera, Sixth Interantional Workshop on Low Temperature Detectors, Bern, Switzerland, LTD6, Nucl. Instr. and Meth., A370 150-156 (1996).
“Charge Collection and Trapping in Low Temperature Silicon Detectors”, M, J. Penn, B. L. Dougherty, B. Cabrera, R. M. Clarke, and B. A. Young, J . Appl. Phys. 79, 8179-8186 (1996).
“A Superconducting Bolometer with Strong Electrothermal Feedback”, A. T. Lee, P. L. Richards, S . W. Nam, B. Cabrera, K. D. Irwin, and J. M. Martinis, Appl. Phys. Lett. 69, 1801-3 (1996).
“Operation of an Improved 100 g Si FLIP detector for the CDMS experiment”, R. M. Clarke, P. L. Brink, S. W. Nam, A. K. Davies, B. Chugg, B. A. Young, and B. Cabrera, Proceedings of the Seventh International Workshop on Low Temperature Detectors (LTD-7), held in Munich, Germany from 27 July to 2 August, 1997, pp. 229-23 1, (Max Planck Institute of Physics, 1997).
“Performance of first 100 g Si FLIP detector in the CDMS experiment”, A. K. Davies, P. L. Brink, R. M. Clarke, S . W. Nam, B. A. Young, and B. Cabrera, Proceedings of the Seventh International Workshop on Low Temperature Detectors (LTD-7), held in Munich, Germany from 27 July to 2 August, 1997, pp. 227-228, (Max Planck Institute of Physics, 1997).
“Detection of Single Infrared, Optical, and Ultraviolet Photons Using Superconducting Transition Edge Sensors”, B. Cabrera, R. M. Clarke, P. Colling, A. J. Miller, S. Nam, and R. W. Romani, Applied Physics Letters 73, 735-737 (1 998).
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Particle Detectors. using Transition Edge Sensors Blas Cabrera - Stanford University
Motivation TES Operation - Voltage bias and electrothermal feedback - High resolution demonstrated
- F ibcoup4eb telescope observations - Fast photometry and large arrays
Optical photon detectors
X-Ray detectors - Best resolution for materids characterization
Dark Matter Search - Quasiparticle trap assisted phonon sensor - Status of CDMS (cryogenic dark matter search)
Summary and Conclusions
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TES Technology
Demonstrated Sensitivity with TES
/ Resolution target G- ISCOfISh
M i m e t e r s
for Transition
I
LLNL STJ t Spectrometers
IO'
# >" 2 1 Edgesensors E \ NIST X-Ray TES Specbometers
100
c 0 3 .-.I * m
2 2 lo-'
- #
I .1 I 1 I I 10'' loo 10' lo2 io3 lo4
Photon Energy [eV]
NIST AVAu TES 3.1 eV FWHM @ 1.5 keV
Stanford W TES 0.15 eV FWHM @ 1.5 eV
A factor of 2-3 improvement is likely with an additional factor of 4 to the fundamental limit
Stanford o p b d # # /-- Fundamental limit for Tc = 70 mK
& # with 100% ETF efficiency
# # c # TESsensors e # # #
# # c 0 # #
# # c # # #
# A
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/1
E 3-
V G
a
I
Y
a" m X cd
.- N
(
2c
40
60 Lev photon
recoil \ J'
60
-20 0 20 X axis (pm)
... 60 keV photon
recoil eiectron
J
-20 0 20 Y axis (pm)
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1 o4 E s lo2 > 5 loo 3
I 0-6
..................... ........................... ............ ......... . ............. i
............ ......... ............
........... ............
10-l 10' lo3 lo5 io7 Electron Energy (eV)
5
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3
0 3
1
0 3
1
0 0 1 4 5
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0 20 40 60 80 100 Electric Field (V/cm)
e le c t ron 4 /
/phonon
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Backscattered iotis = Traitsn i t ted Ions =
Range Strayg le
Latera 1 = 129 Long i tud i na 1 = 25%
Rad ia 1 = 18A Uac./Ion = 164.8 ENERGY LOSS(z1 IONS RECOILS Ionization => 25.84 26.18 Vacancies => 8.42 1.66
8
.-I$. I , - - _ _ ~ . --I--- - _-- . . ..
h -. . ;!* .
C
; E .- VI
I
RECOILS PHONONS I
IONS E 0 k I
c, in bo
8 - Depth ->
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A
9
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I I L
1 2 3 7 Frequency (THz)
2 A N
10
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0.04
-- E bin
E t-
o .02
0
1 I I ' 1 ' 1 , 8 I I I I
0 0.5 I .o Time (ps)
1 1
1.5
, - --3 0.02 0 E bin /E total
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n
0 0 d Y
... .. . . . . .
n
W
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. . . . , . . . . . , .; v ' .. m
- X <I- n - 0 0 Y
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Transition Edge Sen.sors
Steep Resistive Supeconducting Transition
W Tc - 70-90 mK 10-90% < I mK
T .=-I- dR R / dT T
uni tless measure of transition width
Voltage bias is intrinsically stable
The Joule heating produced by bias
VB’ PJ 3. whenR t
is stable whereas for current bias
which is intrinsically unstable
< = i F
P , = I i R - PJ f whenRT
SQUID
R S shunt
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ri. ? Q,
RC -\.pa
1 7
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Thermal Model’
I pJ
Time -b c u photon
Electrothermal Feedback - Voltage bias intrinsically stable
- Past response - =0
- High Sensitivity g = nZTen-l 9 z o = - 9
C
g zecf - 1 + a / n
W W H M - - 2.3554-
For E sat (- C T / a ) e = 10 keV then AEwHM = 1.1 eV
For E,, (- C TJa) = 10 eV then LIE,,, = 42 meV IC! MeV I . ! - m c 7 -
Q \ e h s h t ‘ 1 ~ ~ ; # i ? g a % s 6, ~ m,
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Operation of TES Sensors
I I 1
I # I ' 6
z? Y
0 PI
0 I
-600 -400 -200 0 200 400 600
Current Bias [PA]
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Three Applications
Direct absorption of photon into TES (e. g., optical photon detectors) c/ 1-10eV photon
W Si or Ge
.. \ r
Photon absorber in electicd contact with TES (e. g., x-ray detectors)
Bi AVAg \ r,
1-10 keV x-ray r /
Si,N, 4 Large mass absorbers generate phonons which are converted into quasiparticles and the quasiparticles diffuse to the TES (e. g., dark matter detectors)
W AI \ Si or Ge
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Optical Photon Detectors Demonstration of W TES sensitivitv
J
M acti ve i' sensc AI
voltage rai 1 s
0.6 I I I I I
I I
3 3 0.4- Y a3 C an c
?sub = 43.8341 mK .
Rshusc=O.Wohrns . Rkod = 0.005 ohms
-
6 0.3- 531 nm c photon
0.2-
a' 2 0.1 -
Y
Bias Cumnt [ItA]
6 Q) cn
'3"E 0
-0.1 ' I 1 I I I I 0 100 200 300 - 1 0 0
Time bsec]
Appl. Phys. Lett. A u,u IO. 1998, Cabrera, et al. L
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Monochromator Calibrations
IR ih backeround L
2500
rai 1 B hits .- m
2nd order
Energy [eVI ,
I
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3000-
2500-
m- (d Y
3 1500- u"
1OOO-
500-
23
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c I I I I I I I 1 0.14 -
0.12 -
0.1 -
k' 0.08- 2 Y
E 0.06- p!
0.04-
0.02 -
L 3
-0.02 1
-I
(J
I I I
0 100 I I I I I I
200 300 400 500 600 700 800 Time (c(s]
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Fiber-coupled Telescope Data
Fiber-coupled Celestron 8 - 98 06 16 2oOo.
1500r c ~1OOo: , 0
."+I 500-
0 --c_i--
0 100 200 300 400 500 600 700 800
"0 100 200 300 400 500 600 700 800
i NGC6572
1
100 200 300 400 500 600 700 800
I streetlamp
I 2200- i
100 - I
OO 100 200 300 400 500 600 700 800
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First TES Observation of Crab Pulsar
1 -
Crab Pulsar, livetime = 1988 sec, period = 33.4938 msec 11 I I I I 1 I I
.. - . .
, I I 1 I 1 I I
n X 8 E
Y
s
i 20 :: 0 0 0.5 1 1.5 2 2 5 3 3.5 4
Energy Spectrum of Crab Pulsar 8 I I I r 1 I I
n *. 5 -
4 -
L 3 '
s 5 2 - E 2
i t -
O - I J ' , I I I
0 -0.5 1 1.5 2 2.5 3 3.5 4 i
Photon Energy [eV]
26
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Histograms of Energy vs Phase
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Histograms of Energy vs Phase
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"
31
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TES X-Ray Detectors
ilecaj probabl! because energj h deposited in AI quasiparticle
68.5 1 2 1 I 3 681 ~ <> .;tern and released o w - a
First W TES on Ge test device
electron temperatw
J :,
I,
'L
quasi particles 25 prn A1 8 ,/ wirebonds 40 nm W TES I
P . A / " v 6 keV iy - ra v s
-\ 150pm by .5 mm square Ge
1 3 - I I
I
,- 1 coup1 ed electrons I
and phonons j
i decay time constanls j
sirnuhion with
4 I
,
produces t i l o
0 5 I 10
---
2.5 /,
/
I
P I
rr*b=l - os
0
4 s 0 :5 I l:5 2 2:5 3 3 5 i- 0 0.5 I 1.5 2 2.5 3 35 rim lml Time [ms]
69
dam has more complicated I 1
d "6!5 0 0.5 1 1.5 2 2.5 1 35
Time lmsl
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sum of two is good
3
2.5
2 -
n
U VI
5 1.5-
m .-
I 1 1 I I
-
Tail satisfies rate equation for self - recombination of quasiparticles
I I I I I 1
0.5 I 1.5 2 2.5 3 3.5 Time [ms]
Start satisfies equation for electrothermal relaxation
with time constant rerf
I ( t ) = I,, exp( -t I rev)
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m 3
00 cc 2 n 0 c W
Counts per 2 eV bin
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W cn
A P a 01
-. P CD 0
-.A
P CD UI
A VI 0 0
, A ul 0 VI
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W pads
5.9 and CU Collimator
x-rays kev Fe- 55 source
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7 - ?
0 7
X
aq - ?
0 ’ ..
2-g Y
E ‘ti= 0
T-7 - 0
X .-
c9 0
u?z $
‘ti=
0 Y
E 0
0
I
WE] JUeJJfl=) [due] iuaun=>
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c9 0
a ' 9% O P
2 W
=P w- 3 9r)
I).
d W
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250
200
k 150 d)
00
50
I 1 f
61
16 -4 -2 0 2 4 6 Delay X [psec]
1 2 ' 3 ' 4 5 6 7 0 0 -
X-Ray Energy [keV]
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1
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Energy [kev]
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I
W/Al QET Sensors forCDMS
Photograph c of Phonon Sensor
Trapping Schematic Energetic
Quasi particles
Trapping Phonon Absorption Diffusion i h c i - I J O O L , '
;? ,.- ' ) i l 1 ' ) ! t i \ < , . ,
!
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Quasiparticle Loss Measurement Test Structures (UCB & Stanford)
BondPad WTES AI Absorber
b i . 1 WIAI Trap \ / 1
\
2 0 pin I Si Substrate
0*45 t 0.4
0.35
>1 0.3
T0.25 2
P) 24
: 0.2 Lil L L & 0.15
0.1
0.05
0 50 Number
0.45
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0.35 - c
0.3 24 L.
k W 0.15 a
0.1
0.05
I
I
1 4 0
0 0.1 0.2 0.3 0.4 A ETF Energy [keV]
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1 I I Y
I O ' loo t
IO"1 1 o 3 1 0" 10 '
Temperature [ K]
I*+
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Ionization + Phonon Readout I
-- .>
> .- P I & - 3~'iisw-s plus ionizatk::?
~ - ~ - ~- - - ~ _ _
100 g Si Crystal 1 cmThick 3" Diameter - --
0 Imaging Capability -I At=25ps across 3" -
Muon Veto =: 100 p s
lOnlzalbn and Phonon Evm( m 100 g Si Detector 700,
Ionization 6 o o L signal defines
\tart time 5 o o c
200 - 1
100 - A -4 * 0 -
-100 I
-30 -20 -10 0 10 20 30 40 50 Bo 70 1
Time m1
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i
X-Y Imaging with Phonons
-15 -10 -5 0 5 10 15 X Delay bs]
-15
blockcci iw
- .. . . . . . _ .
- . . .
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-5
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X Delay bsl
lcm lcm PhononSide
w* Charge Side
lead 241Am Sources
Above 70 keV
-10 -5 0 5 IO IS X Delay [PI
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CDMS I - Stanford shallow site
Panama Street
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100 g Si detector in CDMS Run 18
3
8 60- > 25 0
. . 5 4 0 . .
"0 20 40 60 80 100 Recoil [keV]
I 20 40 60 80 100
Recoil [keV]
. ' . 100- . . . . ,,. . ,' . . .. muon
~
"0 20 40 60 80 100
Two months of continuous
Recoil [keV]
! \ I P candidates ~ ( - ..I- :toed rieutrons iexpz:: -.
- hat, operation! ! ! -. 1 . ' l J L L c ~ distribution (t~x':: ~ - - -c,.
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Phonon Risetime Information
Risetime Distribution from 6oCo
0' I 0 50 100 0 15 30
Phonon Sum [keV] Calibration data with % p s RT Cut
1 Electrons (low Q,lP)
80-
- 8 60- %
5 4 0 -
- C C
20
0" . 0 20 40 60 80 I 00 0 20 40 60 80 100
Recoil [ keV] Recoil [keVJ
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FLIP fast phonon physics
Particle interactions creat e-h pairs Phonons generated - Plasma cloud (diffuse) - Drifting charge (ballistic) - Recombination (ballistic)
Phonon Sensors /
'.. Ionization Electrode
+ IVeV, Erecoil = P - N e V + 'recomb tot P = P p Lasma tot
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Risetime Discrimination Shown Icebox Gamma set
'̂ i----
I . .t . . . . . .. . :... . . . , .: ~
,: 4
. ;. . ,;.' .: i
. :. . . . . . . . . . . ; . . ... ' > . . . / . . . . . . .
5 2
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CDMS New Limit & Goals
.
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C057 long 1 20K rqmat 150
0 50 100 Ftcimn Energy Eke4
Co57 long-1 20K rqmaf
I " " " ~ " "
Charge Energy [kevee]
GOkeV neut 1 20K rama!
1 - . - . . . .. .
50 100 Phonon Energy [kev
0 10 20 30 40 M 60 70 80 90 100 110 120 130 1 4 0 '50 Charge Energy[Kebee]
60 keV wut 1 first 20K everts
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Summary
TES’s are progressing rapidly and have demonstrated excellent performance For optical photon detection - From IR (5 pm or 0.25 eV) to UV (350 nm or
4 eV) energy resolution is 4 . 1 5 eV FWHM - Immediate use for fast spectrophotometry - Rapid progress on arrays for space and ground
For x-ray spectroscopy - State-of-the-art is NIST AI/Ag bilayer with
- Immediately useful to characterize materials - Astrophysics x-ray spectroscopy from space
3.1 eV FWHM at I .5 keV and 7.1 eV at 6 keV
For Dark Matter searches - W/A1 QET fast athermal phonon sensors - Demonstrated imaging & discrimination - Scheduled for use in CDMS-II(42 detectors)
Much interesting phonon and quasiparticle physics still to understand!
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