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Single Photon Counting Detectors for Submillimeter Astrophysics:
Concept and Electrical Characterization
John TeufelDepartment of Physics
Yale University
Yale:Minghao Shen
Andrew SzymkowiakKonrad LehnertDaniel Prober
Rob Schoelkopf
NASA/GSFCThomas Stevenson
Carl Stahle Ed Wollack
Harvey Moseley
Funding from NASA Explorer Tech., JPL, GSFC
Overview
• Types of detectors
•Noise and sensitivity in detectors
•What is the Submillimeter?
•The “SQPC” – a high-sensitivity sub-mm detector
•Dark currents and predicted sensitivities of SQPC
• Time scales and saturation effects
• Future Work
Types of Detectors
Coherent• Measures Amplitude & Phase• For Narrow-band Signals• Sensitivity given in Noise
Temperature [K]• Adds a 1/2 photon of noise
per mode• Minimum Noise Temperature:
TQ=hf/2k
• Example: a mixer
Incoherent• Measures only Amplitude• For Broad-band Signals• Sensitivity given by NEP
[W/rt(Hz)]• No fundamental noise limit on
detector• Ideally limited only by photon statistics of signal or
background• Example: a photomultiplier
8
6
4
2
0
<n
>
0.12 4 6 8
12 4 6 8
10hf/kT
Wien Raleigh-Jeans
Average occupancy per mode
In the Wien limit:
1/2 photon per mode of noise is unacceptable!
When to Use an Incoherent Detector
1
1bbhf kTn
e
1n
bb
Photon Counting in Optical
PMTPhotonsSignal Source
Background Radiation
Ntot=(n + ndark)• t
Ntot = Ntot
nbackground + nsource ndark
Rate of detector false counts
n =Rate of incoming photons
Photons
Direct Detection with Photoconductor
Bandpass Filter, B
P = h (n + n )incident signal background
NEP n Bbg background
Background Radiation, e.g. CMB,
Atmosphere...
Signal Source
Typical NEP ~10 W/ Hz-17bg
V
+
-
-
+• •
100 1
100 1
1
GHz THz
m mm
E h meV
Infrared
What is the Sub-Millimeter?
How Many Photons in the Sub-mm “Dark?”
3 K blackbody
10 % BW
single-mode
Photon-counting (background) limit:
see e.g. SPECS mission concept, Mather et al., astro-ph/9812454
Future NASA projects need NEP’s < 10-19 W/rt(Hz) in sub-mm !
NEP ~ h(n )1/2
The SQPC: Single Quasiparticle Photon Counter
•Antenna-coupled Superconducting Tunnel Junction (STJ)
•Photoconductor direct detector•Each Photon with
excites 2 quasiparticles
Nb antennaAl absorber
(Au)
~ 1 m
STJ detector
junction
sub-mmphoton AuNb Al Al
AlOx
2 2Al Nb
Responsivity = 2e/photon = e/ = 5000A/W
•Incident photons converted to current
Lower Idark=> Higher sensitivity
What is measured
Nb antenna
(Au)
STJ detectorjunction
sub-mmphoton
Ultimate Sensitivity
V
•Current readout should not add noise to measurement
•FET or RF-SET should have noise
•RF-SET is fast and scalable
2 falseI e n n
Photocurrent Dark current
TotalN
false darkn I
Integration of RF Circuits, SETs, and sub-mm Detectors
• 16 lithographic tank circuits on one chip
• one of four e-beam fields, with SETs and SQPC detectors, and bow-tie antenna
Sensitivity and Charge Sharing with Amplifier
Q ~ 1000 e-
CSTJ ~ 250 fF CSET ~ 1/2 fF
FET (2SK152; 1.1 nV, 20 pF) RF-SET (30 nV, ½ fF)
Either FET or SET can readout STJ @ Fano limit,
But only SET is scalable for > 50-100 readouts
0.15 e/rt(Hz) 1 x 10-4 e/rt(Hz)
Collects all charge Collects CSET/CSTJ ~ 0.2%
still ~ 3 times better
Experimental Set-up and Testing
•Small area junctions fabricated using double angle evaporation
1 µm
Bow Tie Antenna
Detector
140 µm
•Device mounted in pumped He3 cryostat (T~250mK)
Fig. 2. (a) SQPC detector strip and tunnel junctions are located between two halves of a niobium bow-tie antenna for coupling to submillimeter radiation. A gold quasiparticle trap is included here in the wiring to just one of two dual detector SQUIDs. (b) Close-up view of detector strip and tunnel junctions made by double-angle deposition of aluminum through a resist mask patterned by electron beam lithography. Pairs of junctions form dc SQUIDs, and critical currents can be suppressed with an appropriately tuned external magnetic field.
1 µm
junction
detector strip
SQUIDloop
quasiparticle trap
antennaantenna
Al/AlOx/Al Junctions: ~ 60 x 100 nm
XB
Detector Junctions form a SQUID 40
20
0
-20
-40
Cu
rren
t [n
A]
4002000-200-400Voltage [mV]
Supercurrent Suppression
3
2
1
0
Cu
rren
t [n
A]
2.01.51.00.50.0Magnetic Field [mT]
4
3
2
1
0
Cu
rren
t [p
A]
280270260250Magnetic Field [mT]
Supercurrent Contributions to Dark Current
Supercurrent
•Cooper pair tunneling affects the subgap current both at zero and finite voltages
•DC Josephson effect:
•AC Josephson effect:2 ( ) Re ( )
( )2
c Jdark
bias
BB
I ZI
V
Zen Ic sin(J t)
21Re[ ( )]
2RF C JP I Z DC biasP IV
V
Zen
SQPC
RF PowerDC Power
cos( )C oI I
( )
2C J
J
I I sin t
eV
*
*Holst et al, PRL 1994
80
60
40
20
0
Cur
rent
[pA
]
4003002001000Voltage [mV]
Magnetic Field Dependence of Sub-gap Current
2 ( ) Re ( )( )
2c J
darkbias
BB
I ZI
V
60
40
20
0C
urr
ent
[pA
]1.51.00.50.0
Magnetic Field [mT]
BCS Predictions for Dark Current
2 2( )
2 2 2BTk
dark on B B
eV eVI e eV Sinh K
eR e TkT
V k T
T=1.6 K
T=250 mK
{} eV
-8
-6
-4
-2
0
2
4
6
8
Cu
rre
nt
[nA
]
-400 -200 0 200 400Voltage [mV]
10-13
10-12
10-11
10-10
10-9
Cu
rre
nt
[A]
2 3 4 5 6 7 8 91
Temperature [K]
Rn= 13.1 kW
Rn= 9 kW
Rn= 47 kW
Thermal Dark Current Measurements
BCS Predicts:
Tc =1.4 K
I @ 50 V
( ) Bkdark
TTI e
20
10
04002000
BCS (357mK) 357 mK 256 mK
I/500
Cu
rren
t [p
A]
Voltage [µV]
1912min ~ 10I pA NEP W Hz
Recombination and Tunneling Times
absorber
lead
(large
volume)
sub-mmx-ray
Vabs
RN
tunnel
1000 m3 0.01 m3
½
2 s
50 k
2 s
Vabs
thermal recomb ~ 100 s
@ 0.26 K
tunnel ~ VabsRN
tunnel << recomb
so quantum efficiency
is high
at low power:
False count rate = Idark/e = 3 MHz for ½ pA
Saturation: Recombination vs. Tunneling
Current
Power (P)Idark
(or photon rate, N)
Noise
N~ Id/e
rec ~ tunn
Nsat ~ (th/tun) Id/e
Psat~ 0.02 pW; scales as 1/RN
Absorber gap reduced by excess q.p.’s
I ~ P
NEP ~ P1/2
NEP ~ P1/4
I ~ P1/2
Demonstration of an RF-SET Transimpedance Amplifier
Trim gate
Input gate
0.5 fF
Electrical Circuit Model and Noise
2
2
42 n
bdark
kT ee
ZII
R
Shot Noise
Johnson Noise
Amplifier Noise
:
2 dark
Sensitivity
I eI
VRb
en
SQPC
4
610
-16
2
4
610
-15
2
4
Cu
rre
nt N
oise
[A/r
t (H
z)]
100
101
102
103
104
Frequency [Hz]
610
-20
2
4
610
-19
2
4
610
-18
NE
P [W
/rt.(Hz)]
Total Noise Amplifier Noise Johnson Noise Shot Noise
•Problem: Need to couple known amount of sub-mm radiation to detector
•Solution: Use blackbody radiation from a heat source in the cryostat
Future Work: Detecting Photons
10-15
10-14
10-13
10-12
10-11
Po
we
r [W
]
12 4 6 8
10Blackbody Temperature [K]
10-13
10-12
10-11
10-10
10-9
Cu
rren
t [A]
Cryogenic Blackbody as Sub-mm Photon Source
1 cm
104
105
106
107
108
Re
sist
an
ce [W
]
1 10
Temperature [K]
~oTTe
V•Hopping conduction thermistor
•Micro-machined Si for low thermal conduction
Coming Soon: Photoresponse Measurement
T= 1-10K
T= 250 mK
Quartz Window
Si Chip with SQPC
Advantages of SQPC
• Fundamental limit on noise = shot noise of dark current
•Low dark currents imply NEP’s < 10-19 W / rt.Hz
•High quantum efficiency – absorber matched to antenna
• High speed – limited by tunneling time ~ sec
• Can read out with FET, but SET might resolve single ’s
• Small size and power (few m2 and pW/channel)
• Scalable for arrays w/ integrated readout
Summary
• When hf>kTbb, a photon counter is preferred
•In the sub-mm, no such detector exists
•The SQPC would be a sub-mm detector with unprecedented sensitivity
•Contributions to detector noise have been measured and are well-understood
•Photocurrent measurements in near future